Star Forming Regions in Cepheus

Handbook of Star Forming Regions Vol. I 

Astronomical Society of the Pacific, 2008 

Bo Reipurth, ed. 

Star Forming Regions in Cepheus 

Mária Kun 

Konkoly Observatory, H-1525 Budapest, P.O. Box 67, Hungary 

Zoltán T. Kiss 

Baja Astronomical Observatory, P.O. Box 766, H-6500 Baja, Hungary 

Zoltán Balog 1 

Steward Observatory, University of Arizona, 933 N. Cherry Av., Tucson AZ 

85721, USA 

Abstract. The northern Milky Way in the constellation of Cepheus (100 ◦ ≤ l ≤ 

120 ◦ ;0 ◦ ≤ b ≤ 20 ◦ ) contains several star forming regions. The molecular clouds of 

the Cepheus Flare region at b > 10 ◦ , are sites of low and intermediate mass star formation 

located between 200 and 450 pc from the Sun. Three nearby OB associations, 

Cep OB2, Cep OB3, Cep OB4, located at 600–800 pc, are each involved in forming 

stars, like the well known high mass star forming region S 140 at 900 pc. The reflection 

nebula NGC 7129 around 1 kpc harbors young, compact clusters of low and intermediate 

mass stars. The giant star forming complex NGC 7538 and the young open cluster 

NGC 7380, associated with the Perseus arm, are located at d > 2 kpc. 

1. Overview 

In this chapter we describe the star forming regions of the constellation of Cepheus. 

A large scale map of the constellation, with the boundaries defined by IAU overlaid, 

and the most prominent star forming regions indicated, is shown in Fig. 1. This huge 

area of the sky, stretching between the Galactic latitudes of about 0 ◦ and +30 ◦ , contains 

several giant star forming molecular cloud complexes located at various distances from 

the Sun. According to their distance they can be ranged into three large groups: 

(1) Clouds nearer than 500 pc located mainly at b ≥ 10 ◦ , in the Cepheus Flare. 

(2) Three OB associations, Cep OB 2, Cep OB 3 and Cep OB 4 between 600–900 pc. 

(3) Star forming regions associated with the Perseus spiral arm at 2–3 kpc. 

In the following we discuss the first two of these groups. 

Fig. 2 shows the distribution of dark clouds perpendicular to the Galactic plane 

(Dobashi et al. 2005), with the outlines of the major star forming complexes overplotted. 

The large-scale 13 CO observations performed by Yonekura et al. (1997) led to 

a refinement of division of the clouds into complexes. The groups listed in Table 2, 

1 on leave from Dept. of Optics and Quantum Electronics, University of Szeged, Dóm tér 9, Szeged, 

H-6720, Hungary 

1

2 

Figure 1. Positions of the major star forming regions of Cepheus, overplotted on 

a schematic drawing of the constellation. 

adopted from Yonekura et al. (1997), were defined on the basis of their positions, radial 

velocities, and distances, where distance data were available. 

Table 1 lists the dark clouds identified in the Cepheus region from Barnard (1927) 

to the Tokyo Gakugei University (TGU) Survey (Dobashi et al. 2005), and the molecular 

clouds, mostly revealed by the millimeter emission by various isotopes of the carbon 

monoxide (Dobashi et al. 1994; Yonekura et al. 1997). The cloud name in the first column 

is the LDN (Lynds 1962) name where it exists, otherwise the first appearance of 

the cloud in the literature. Equatorial (J2000) and Galactic coordinates are listed in 

columns (2)–(5), and the area of the cloud in square degrees in column (6). Column (7) 

shows the radial velocity of the cloud with respect to the Local Standard of Rest. The 

number of associated young stellar objects is given in column (8), and the alternative 

names, following the system of designations by SIMBAD, are listed in column (9). We

note that the LDN coordinates, derived from visual examination of the POSS plates, 

may be uncertain in several cases. 

Figure 3 shows the distribution of the pre-main sequence stars and candidates over 

the whole Cepheus region. 

3 

Cepheus Flare Shell 

20 

Cep OB4 Shell 

Cepheus Flare clouds 

15 

NGC 7023 

Galactic latitude ( o ) 

10 

5 

Cep OB4 

Be 59 

S171 

Cep OB3 

S155 

Cep OB2 

NGC 7129 

Cepheus Bubble 

NGC 7160 

S140 

IC 1396 

0 

Cep OB6 

120 115 110 105 100 95 

Galactic longitude ( o ) 

Figure 2. Distribution of the visual extinction in the Cepheus region in the [l,b] 

plane (Dobashi et al. 2005) with outlines of the major star forming regions, discussed 

in this chapter, overplotted. Solid rectangles indicate the nominal boundaries 

of the OB associations (Humphreys 1978; de Zeeuw et al. 1999), and the dashed 

rectangle shows the Cepheus Flare cloud complex; giant HII regions are marked by 

solid grey circles, and star symbols indicate young open clusters. Three large circles, 

drawn by radial dashes, show giant shell-like structures in the interstellar medium. 

The Cepheus Flare Shell (Olano et al. 2006) belongs to the nearby Cepheus Flare 

complex, and the Cepheus Bubble (Kun et al. 1987) is associated with the association 

Cep OB2, and the Cepheus OB4 Shell (Olano et al. 2006) is associated with 

Cep OB4.

4 

Figure 3. Pre-main sequence stars and candidates in the Cepheus region overlaid 

on the map of visual extinction obtained from 2MASS data based on interstellar 

reddening using the NICER method (Lombardi & Alves 2001). Large circles denote 

those clouds from Table 1 which have been associated with young stars. The 

meaning of different symbols are as follows: Filled triangles - T Tauri stars; Filled 

squares - Herbig Ae/Be stars; Filled circles - Weak-line T Tauri stars; Diamonds - 

Tr 37 ROSAT X-ray sources; Open triangles - PMS members of Tr 37; Open squares 

- Candidate and possible PMS members of Cep OB3b; X - Hα emission stars; + - 

T Tauri candidates selected from a 2MASS color-color diagram.

Table 1.: List of clouds catalogued in Cepheus. 

Cloud name RA(2000) Dec(2000) l b Area v LSR n star Alternative names 

(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1122 20 32.7 +65 20.3 99.97 +14.81 0.041 4.8 0 YMD CO 1, TGU 597 

LDN 1089 20 32.8 +63 30.3 98.40 +13.78 0.244 −2.4 0 TDS 366, TGU 586 

LDN 1094 20 32.8 +64 00.3 98.83 +14.06 0.002 0.1 1 CB 222 

TGU 667 20 33.9 +73 51.6 107.53 +19.33 2.460 1 [KTK2006] G107.1+19.3, [KTK2006] 

G107.5+19.8, [KTK2006] G107.9+18.9 

LDN 1152 20 34.4 +68 00.4 102.37 +16.14 0.025 2.9 0 YMD CO 8 

CB 223 20 34.7 +64 10.7 99.10 +13.98 0.003 −2.7 0 

LDN 1100 20 34.8 +64 00.4 98.96 +13.88 0.007 −2.7 1 CB 224 

LDN 1033 20 37.2 +57 10.5 93.44 +9.69 0.714 −2.4 0 TDS 343, TDS 345, TDS 346, 

TGU 549, DBY 093.1+09.6, 

DBY 093.5+09.4 

LDN 1036 20 38.2 +57 10.6 93.52 +9.58 0.088 −2.1 1 DBY 093.5+09.4 

LDN 1041 20 38.2 +57 30.6 93.79 +9.78 0.022 −2.1 0 DBY 093.5+09.4 

LDN 1157 20 39.5 +68 00.7 102.65 +15.75 0.005 2.9 1 [DE95] LDN 1157 A1, YMD CO 8, TGU 619 

LDN 1147 20 40.5 +67 20.8 102.14 +15.29 0.127 2.9 0 YMD CO 8, TDS 379, TGU 619, 

JWT Core 36, [LM99] 340, 

[BM89] 1-99, [LM99] 344 

LDN 1148 20 40.5 +67 20.8 102.14 +15.29 0.015 2.9 1 YMD CO 8, TGU 619 

LDN 1044 20 41.2 +57 20.8 93.90 +9.35 0.006 −2.1 0 DBY 093.5+09.4 

LDN 1049 20 42.2 +57 30.8 94.12 +9.35 0.005 0.6 0 DBY 094.1+09.4 

LDN 1039 20 42.3 +56 50.8 93.58 +8.94 0.079 −2.1 0 DBY 093.5+09.4 

LDN 1051 20 42.7 +57 30.9 94.16 +9.29 0.010 0.6 0 DBY 094.1+09.4 

LDN 1155 20 43.5 +67 40.9 102.60 +15.25 0.006 2.9 0 YMD CO 8, TGU 619 

LDN 1158 20 44.5 +67 41.0 102.66 +15.17 0.111 0.9 0 TDS 388, [BM89] 1-100, [LM99] 346, TGU 619 

[BM89] 1-102, [BM89] 1-103, [LM99] 348 

LDN 1038 20 46.3 +56 21.0 93.53 +8.20 0.660 −2.1 0 [BM89] 1-104, DBY 093.5+09.4 

LDN 1076 20 49.3 +59 51.2 96.57 +10.04 0.008 −2.2 0 DBY 096.8+10.2 

LDN 1082 20 51.1 +60 11.3 96.98 +10.07 0.111 −2.6 8 Barnard 150, GF 9, TDS 362, [LM99] 350, 

DBY 097.1+10.1, [BM89] 1-105, [LM99] 351 

LDN 1171 20 53.5 +68 19.5 103.71 +14.88 0.002 3.4 0 CB 229 

LDN 1037 20 54.4 +55 26.5 93.53 +6.75 0.591 0 TGU 551 

LDN 1168 20 56.6 +67 36.6 103.31 +14.21 0.003 0 

5

Table 1.: Continued. 

6 


(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1061 20 58.3 +57 21.7 95.36 +7.56 0.618 −2.1 0 DBY 095.2+07.4, DBY 095.2+07.4 

LDN 1071 20 58.3 +58 11.7 96.00 +8.10 0.092 −0.4 0 Barnard 354, DBY 096.0+08.1, TGU 569 

LDN 1056 20 58.4 +56 01.7 94.35 +6.69 0.036 0 

TGU 730 20 58.8 +78 11.8 112.23 +20.50 0.803 −8.0 3 [BM89] 1-108, [BM89] 1-109, 

[B77] 48, [BM89] 1-112, GN 21.00.4, RNO 129 

LDN 1228 20 59.0 +77 31.8 111.67 +20.10 0.086 −7.6 4 YMD CO 66, MBM 162, TGU 718 

LDN 1170 21 01.7 +67 36.9 103.63 +13.84 0.215 2.8 0 TDS 392, TGU 629, GSH 093+07+9 

[LM99] 359, [LM99] 361 

LDN 1058 21 02.4 +56 01.9 94.72 +6.27 0.869 −1.1 1 TDS 354, TGU 558 

LDN 1174 21 02.6 +68 11.9 104.15 +14.14 0.294 2.8 

∼ 

> 15 TDS 393, [LM99] 358, [BM89]1-110, 

[B77] 39, [BM89] 1-113, [LM99] 360, 

[BM89] 1-114, [BM89] 3B- 9, 

[BM89] 1-111, PP 100, [BM89] 1-115 

Ced 187, GN 21.01.0, YMD CO 14 

LDN 1172 21 02.7 +67 41.9 103.76 +13.82 0.010 2.7 

∼ 

> 4 YMD CO 14, TGU 629 

LDN 1167 21 03.7 +67 02.0 103.30 +13.32 0.062 2.8 0 YMD CO 11 

LDN 1173 21 04.7 +67 42.0 103.88 +13.67 0.006 2.7 0 YMD CO 14 

LDN 1068 21 06.3 +57 07.1 95.89 +6.59 0.027 0.2 0 Barnard 359, DBY 095.9+06.6, TGU 570 

LDN 1063 21 07.4 +56 22.2 95.44 +5.97 0.025 0.3 0 Barnard 151, Barnard 360, 

DBY 095.5+06.5, TGU 561 

LDN 1065 21 07.4 +56 32.2 95.56 +6.09 0.023 0.3 0 DBY 095.5+06.5, TGU 568 

LDN 1069 21 08.4 +56 52.2 95.90 +6.21 0.018 0.3 0 DBY 095.5+06.5 

LDN 1067 21 09.4 +56 42.3 95.87 +6.00 0.012 0.3 0 DBY 095.5+06.5, TGU 568 

Sh 2-129 21 11.3 +59 42.3 98.26 +7.84 1.190 3.7 2 DBY 097.3+08.5, BFS 9 

LDN 1060 21 11.5 +55 17.4 95.02 +4.82 0.031 −0.9 0 DBY 090.5+02.4 

LDN 1119 21 13.2 +61 42.4 99.91 +9.03 0.010 2.5 0 DBY 100.1+09.3, TGU 598 

LDN 1062 21 13.5 +55 32.4 95.40 +4.79 0.003 −0.9 0 DBY 090.5+02.4 

LDN 1064 21 13.5 +55 37.4 95.46 +4.85 0.001 −0.9 0 DBY 090.5+02.4 

LDN 1125 21 14.7 +61 42.5 100.04 +8.90 0.010 2.5 1 Barnard 152, TDS 376, [LM99] 365, 

DBY 100.1+09.3, TGU 598 

LDN 1072 21 16.5 +56 12.6 96.18 +4.95 1.510 −0.6 0 Barnard 153, TDS 358, TGU 574, 

DBY 096.3+05.2 

LDN 1177 21 18.8 +68 15.7 105.22 +13.06 0.005 2.9 2 CB 230, TGU 641



(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

TGU 589 21 19.7 +59 27.7 98.83 +6.90 0.560 2 

LDN 1162 21 20.0 +65 02.8 102.92 +10.76 0.004 0 

LDN 1080 21 21.5 +56 32.8 96.91 +4.69 0.001 0 Barnard 154 

YMD CO 23 21 22.2 +69 22.6 106.27 +13.60 0.056 −9.4 2 TGU 656 

LDN 1108 21 26.4 +59 33.1 99.49 +6.37 0.046 0 

DBY 098.4+05.2 21 26.8 +57 55.9 98.40 +5.17 0.107 1.0 0 

LDN 1086 21 28.5 +57 33.2 98.30 +4.74 0.095 −4.6 18 DBY 098.8+04.2, TGU 584, [PGS95] 2, 

IC 1396 W, FSE 1 

LDN 1176 21 31.0 +66 43.3 104.93 +11.15 0.446 −10.4 0 YMD CO 17, TGU 634, 

JWT Core 44, GAL 104.9+11.2 

LDN 1145 21 31.3 +62 43.3 102.14 +8.24 0.183 0 TGU 622, [PGH98b] Cloud 11 

LDN 1146 21 31.3 +62 43.3 102.14 +8.24 0.183 0 

LDN 1096 21 31.5 +58 03.3 98.93 +4.83 0.001 0 TGU 590 

LDN 1102 21 32.5 +58 03.3 99.03 +4.74 0.008 0 

LDN 1085 21 33.3 +56 44.6 98.23 +3.69 0.010 3.4 0 WWC 156 

LDN 1093 21 33.5 +57 38.4 98.85 +4.34 0.034 −4.6 20 DBY 098.8+04.2, TGU 587, FSE 3 

[PGS95] 8 

LDN 1083 21 33.6 +55 58.0 97.72 +3.11 0.761 8.7 WCC 178–179 

LDN 1098 21 34.5 +57 38.0 98.95 +4.25 0.025 −4.6 20 DBY 098.8+04.2, FSE 3 

Barnard 365 21 34.9 +56 43.0 98.36 +3.53 0.010 7.6 WWC 140 

TGU 639 21 35.5 +66 32.0 105.13 +10.70 0.280 1 [KTK2006] G105.0+10.7 

LDN 1087 21 35.6 +56 33.5 98.32 +3.35 0.013 7.4 2 TDS 364 

LDN 1090 21 35.6 +56 43.5 98.43 +3.48 0.028 0 Barnard 365 

LDN 1199 21 35.9 +68 33.5 106.57 +12.15 0.235 −11.5 1 TDS 398, TGU 653 

[KTK2006] G106.4+12.0, 

[KTK2006] G106.7+12.3 

LDN 1099 21 36.5 +57 23.5 98.98 +3.88 0.008 −8.0 22 DBY 099.1+04.0, FSE 5 

LDN 1116 21 36.5 +58 33.5 99.76 +4.75 0.034 3 [IS94] 7, [PGS95] 16, [IS94] 14, SFO 35, 

[G85] 5, [PGS95] 17, [PGS95] 19, FSE 6 

LDN 1105 21 37.1 +57 33.5 99.15 +3.95 0.008 −8.0 22 TDS 369, [B77] 37, DBY 099.1+04.0, FSE 5 

YMD CO 19 21 37.3 +67 01.2 105.60 +10.93 0.279 −10.2 1 TGU 642, [KTK2006] G105.5+10.8, 

[KTK2006] G105.7+10.8 

LDN 1092 21 37.6 +56 58.5 98.81 +3.48 0.014 1 

7


8 


(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1112 21 38.5 +58 03.6 99.63 +4.20 0.013 −0.3 0 DBY 099.7+04.1 

LDN 1117 21 38.5 +58 18.6 99.79 +4.39 0.004 −0.7 0 WWC 114–116 

LDN 1088 21 38.6 +56 13.6 98.41 +2.83 0.019 7.2 2 Barnard 160, TGU 585, 

DBY 098.4+02.9 

LDN 1135 21 39.4 +60 38.6 101.44 +6.06 0.054 0 

LDN 1110 21 39.5 +57 53.6 99.62 +3.99 0.007 −0.3 2 DBY 099.7+04.1 

LDN 1111 21 39.5 +57 53.6 99.62 +3.99 0.002 −0.3 2 Barnard 161, DBY 099.7+04.1, CB 233 

LDN 1123 21 39.5 +58 28.6 100.00 +4.43 0.003 0 

LDN 1126 21 39.5 +58 33.6 100.06 +4.49 0.006 0 

LDN 1101 21 39.6 +56 58.6 99.01 +3.30 0.095 0 

LDN 1131 21 40.0 +59 33.7 100.77 +5.20 0.046 −0.4 0 Barnard 366, TDS 378, 

DBY 100.9+05.3, TGU 609 

LDN 1140 21 40.4 +60 53.7 101.70 +6.16 0.240 0 

LDN 1121 21 40.5 +58 16.7 99.97 +4.19 0.008 −0.2 

∼ 

> 25 DBY 100.0+04.2, [IS94] 5, [G85] 14, 

[LM99] 379, [IS94] 17, IC 1396 N, 

SFO 38, [PGS95] 24, FSE 19, TGU 599 

CB 234 21 40.5 +70 18.6 108.09 +13.15 0.044 −5.0 0 

LDN 1127 21 40.9 +58 33.7 100.20 +4.37 0.004 0 TGU 599 

TDS 395 21 40.9 +66 35.7 105.57 +10.38 0.161 −10.8 1 [KTK2006] G105.5+10.3, YMD CO 18 

LDN 1124 21 41.5 +58 13.7 100.04 +4.07 0.015 −0.2 20 DBY 100.0+4.2, IC 1396 N 

LDN 1128 21 41.5 +58 33.7 100.26 +4.32 0.015 1.2 0 TGU 599, WWC 117 

LDN 1134 21 41.5 +60 13.7 101.35 +5.58 2.630 −0.4 0 [PGH98b] Cloud 19, DBY 100.9+05.3, 

[PGH98b] Cloud 21, 

DBY 101.7+05.0 

LDN 1103 21 41.7 +56 43.7 99.07 +2.92 0.003 0 

LDN 1104 21 42.1 +56 43.7 99.11 +2.89 0.006 4.1 2 Barnard 163, TDS 371, WWC 184, 

[G85] 17, [LM99] 381 

LDN 1181 21 42.1 +66 08.7 105.36 +9.97 0.008 −9.9 0 YMD CO 18, TGU 645 

LDN 1183 21 42.1 +66 13.7 105.42 +10.03 0.090 −9.9 >84 Ced 196, GM 1-57, [B77] 40, TDS 395, 

[FMS2001] NGC 7129, 

[MPR2003] HI Ring, [MPR2003] HI Knot, 

BFS 11, JWT Core 46 

LDN 1095 21 42.6 +56 18.8 98.89 +2.52 0.012 0



(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1106 21 42.6 +56 53.8 99.27 +2.97 0.009 −0.4 0 [PGS95] 28 

LDN 1113 21 44.6 +57 11.8 99.67 +3.02 0.002 4.5 1 Barnard 367, WWC 186 

LDN 1130 21 44.6 +58 18.8 100.40 +3.87 0.012 −3.0 8 TGU 604, [PGS95] 32, FSE 8 

LDN 1136 21 45.5 +59 58.9 101.57 +5.06 0.012 −2.9 0 DBY 101.7+05.0 

DBY 100.0+03.0 21 46.3 +57 25.1 100.00 +3.03 0.015 −1.9 16 IC 1396 E,SFO 39, FSE 9 

LDN 1115 21 46.6 +56 58.9 99.74 +2.68 0.002 0 

LDN 1118 21 46.6 +57 12.9 99.89 +2.86 0.001 −2.1 0 SFO 42, [PGS95] 38 

LDN 1129 21 46.6 +57 53.9 100.33 +3.38 0.041 −2.1 0 [PGS95] 36, DBY 100.4+03.4, WWC 40–42 

LDN 1132 21 46.6 +58 43.9 100.87 +4.02 0.003 0 

LDN 1120 21 47.6 +57 09.0 99.96 +2.72 0.001 0 

LDN 1114 21 49.7 +56 24.0 99.69 +1.96 0.016 −1.8 0 TDS 375, DBY 099.9+01.8 

LDN 1241 21 50.0 +76 44.1 113.08 +17.48 1.380 −3.7 0 YMD CO 72, YMD CO 75, 

TGU 728, TGU 739 

LDN 1144 21 50.5 +60 07.1 102.14 +4.77 0.027 −2.2 1 Barnard 166, DBY 102.1+04.8 

LDN 1137 21 51.6 +59 04.1 101.58 +3.87 0.018 −10.5 0 [G85] 31, DBY 101.5+03.8 

LDN 1138 21 51.6 +59 04.1 101.58 +3.87 0.018 −10.5 0 DBY 101.5+03.8 

LDN 1109 21 51.7 +55 49.1 99.55 +1.33 0.150 −1.5 0 DBY 099.5+01.2 

Barnard 167 21 52.0 +60 04.0 102.25 +4.61 0.005 1 

LDN 1139 21 55.6 +58 34.3 101.68 +3.15 0.015 0.1 15 Barnard 169, DBY 101.3+03.00, TGU 620, 

[LM99] 386, [PGH98b] Cloud 27, FSE 10 

LDN 1141 21 55.6 +58 44.3 101.78 +3.28 0.010 0.1 0 Barnard 171, DBY 101.3+03.00, 

LDN 1142 21 56.6 +59 04.3 102.09 +3.47 0.002 0.1 0 CB 235, DBY 101.3+03.00 

LDN 1143 21 57.6 +58 59.3 102.14 +3.32 0.020 0.1 1 Barnard 170, TDS 380, DBY 101.3+03.00 

LDN 1149 21 57.6 +59 07.3 102.22 +3.43 0.015 0.1 0 DBY 101.3+03.00 

LDN 1151 21 59.6 +59 04.4 102.40 +3.23 0.027 0.1 0 DBY 101.3+03.00 

LDN 1153 22 00.6 +58 59.5 102.45 +3.09 0.079 0.1 0 TDS 383, DBY 101.3+03.00 

LDN 1133 22 02.7 +56 14.5 101.02 +0.72 0.248 0 

LDN 1160 22 04.7 +58 59.6 102.87 +2.78 0.019 0.1 0 DBY 101.3+03.00 

LDN 1166 22 05.7 +59 34.6 103.32 +3.18 0.001 −3.0 0 CB 236 

LDN 1159 22 06.7 +58 34.7 102.84 +2.29 2.790 −1.0 17 Barnard 174, TDS 384, TDS 391, [LM99] 389, 

[GA90] 3-36, DSH J2206.2+5819, 

DBY 102.9+02.4, [G85] 32, 

DBY 102.8+02.1, DBY 103.3+02.8, 

9


10 


(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

DBY 103.2+01.8, [PGH98b] Cloud 30, 

DBY 103.5+02.0, GSH 103+02-66 

LDN 1164 22 06.7 +59 09.7 103.18 +2.76 0.019 −2.2 36 DBY 103.3+02.8, FSE 11 

LDN 1165 22 07.2 +59 04.7 103.18 +2.66 0.019 −2.2 1 DBY 103.3+02.8 

LDN 1169 22 07.2 +59 44.7 103.57 +3.20 0.004 −3.2 0 CB 237 

TGU 659 22 09.0 +64 29.7 106.53 +6.93 1.070 1 [KTK2006] G106.9+07.1 

LDN 1178 22 09.1 +62 19.8 105.27 +5.16 0.005 0 

LDN 1243 22 10.6 +75 20.0 113.16 +15.61 0.081 −2.9 0 YMD C0 74 

LDN 1219 22 11.6 +70 59.9 110.58 +12.06 0.003 −4.6 1 Barnard 175, TDS 414, YMD CO 57 

LDN 1182 22 13.1 +61 54.9 105.42 +4.55 0.004 0 

LDN 1217 22 13.1 +70 44.9 110.54 +11.79 0.186 −4.6 1 Ced 201, YMD CO 57, TDS 414, TGU 696 

LDN 1186 22 13.6 +62 07.9 105.59 +4.70 0.005 0 TGU 649 

LDN 1175 22 13.7 +60 44.9 104.81 +3.55 0.015 0 TGU 635 

LDN 1191 22 14.1 +62 24.9 105.80 +4.90 0.004 0 

LDN 1193 22 14.6 +62 24.9 105.85 +4.87 0.002 0 

LDN 1235 22 14.9 +73 25.0 112.24 +13.88 0.037 −4.0 4 YMD CO 69, TDS 426, HCL 1F, 

TGU725, [BM89] 1-117, [LM99] 390 

TGU 627 22 15.2 +58 47.6 103.87 +1.83 0.210 3 

LDN 1150 22 15.8 +56 00.0 102.37 −0.53 0.007 −6.9 0 Barnard 369, TDS 385, TGU 621 

LDN 1188 22 16.7 +61 45.0 105.67 +4.18 0.398 −10.6 

∼ 

> 20 YMD CO 21, TGU 652, 

[PGH98b] Cloud 33, [ADM95] 3, 

[ADM95] 4, [ADM95] 5, [ADM95] 7, 

[ADM95] 13, [ADM95] 8, GN 22.15.0 

LDN 1154 22 16.8 +56 13.0 102.61 −0.43 0.007 0 

TGU 636 22 16.9 +60 11.6 104.83 +2.87 0.240 2 

TGU 640 22 17.6 +60 36.5 105.13 +3.17 0.330 2 DG 181, DG 182, GN 22.14.9 

LDN 1156 22 19.9 +55 45.1 102.71 −1.05 0.043 0 

LDN 1161 22 19.9 +56 08.1 102.92 −0.73 0.006 0 [KC97c] G102.9-00.7 

YMD CO 29 22 20.2 +63 53.1 107.20 +5.73 0.018 −11.0 13 Sh2-145, SFO 44 

LDN 1184 22 20.7 +60 45.1 105.53 +3.08 0.124 0 TGU 643, TGU 644 

LDN 1247 22 20.8 +75 15.2 113.66 +15.17 0.167 −5.1 0 TDS 430, TGU 742 

LDN 1163 22 20.9 +56 10.1 103.05 −0.78 0.007 0 

LDN 1201 22 23.6 +63 30.2 107.31 +5.21 0.009 0 TGU 661



(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1202 22 26.7 +63 05.3 107.38 +4.67 0.004 0 TGU 661 

LDN 1204 22 26.7 +63 15.3 107.47 +4.82 2.500 −7.6 

∼ 

> 100 YMD CO 27, TDS 399, TDS 401, 

TDS 403, TDS 404, TDS 405, [KC97c], 

[PGH98b] Cloud 32, [PGH98b] Cloud 37, 

[PGH98b] Cloud 38, [G84b] 12, 

DG 185, [PGH98b] Cloud 36, Sh2-140, 

GSH 108+05-46, GN 22.21.5, TGU 661 

LDN 1180 22 26.8 +59 15.3 105.37 +1.41 7.000 −3.6 19 YMD CO 20, YMD CO 24, TDS 396, TDS 397, 

CB 240, TGU 631, TGU 638, TGU 655, 

TGU 658, Min 2-72, [PGH98b] Cloud 34, 

[KC97c] G104.6+01.4, KR 47, 

[LM99] 394, [KC97c] G105.6+00.4, 

Sh 2-138, [GSL2002] 109, [GSL2002] 110, 

[P85b] 18, [LM99] 396, 

DSH J2222.5+5918B, TGU 657, 

LDN 1195 22 26.8 +61 15.3 106.42 +3.11 0.017 1 [B77] 42, [LM99] 391, GN 22.24.9 

LDN 1196 22 26.8 +61 15.3 106.42 +3.11 0.029 1 

LDN 1179 22 27.3 +59 02.3 105.31 +1.19 0.002 0 

LDN 1203 22 27.7 +63 00.3 107.43 +4.54 0.016 0 TGU 661 

TGU 719 22 27.8 +71 21.4 111.90 +11.63 0.510 3 

LDN 1221 22 28.4 +69 00.4 110.67 +9.61 0.020 −4.9 3 TDS 416, [KTK2006] G110.6+09.6, 

[LM99] 392, TGU 702 

LDN 1206 22 28.7 +64 25.4 108.27 +5.70 0.083 0 TGU 673, [PGH98b] Cloud 35 

LDN 1185 22 29.3 +59 05.4 105.56 +1.10 0.006 0 

LDN 1207 22 29.7 +64 25.4 108.36 +5.64 0.047 0 

LDN 1209 22 29.7 +64 45.4 108.53 +5.93 0.111 −8.8 3 Sh2-150, TGU 680 

LDN 1208 22 30.7 +64 25.4 108.46 +5.58 0.018 0 

LDN 1190 22 30.9 +59 08.4 105.75 +1.04 0.004 0 

LDN 1242 22 31.2 +73 15.4 113.15 +13.11 0.793 0 

LDN 1213 22 31.6 +65 25.5 109.06 +6.39 0.006 −9.2 0 YMD CO 48, TGU 686, Sh2-150 

LDN 1194 22 32.9 +59 05.5 105.95 +0.87 0.009 0 

LDN 1214 22 33.6 +65 45.5 109.41 +6.57 0.256 −8.5 1 TDS 407, YMD CO 48, Sh2-150 

LDN 1192 22 33.9 +58 35.5 105.81 +0.37 0.007 −3.6 0 CB 240 

11


12 


(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

TDS 417 22 35.5 +69 13.1 111.33 +9.47 0.014 −7.2 1 YMD CO 65, [B77] 46, GN 22.33.6 

[KTK2006] G101.9+15.8 

TGU 679 22 35.9 +63 35.2 108.53 +4.57 0.170 1 

LDN 1251 22 36.1 +75 15.6 114.51 +14.65 0.195 −3.8 

∼ 

> 20 YMD CO 79, TGU 750, [SMN94] B, 

HCL 1A, [SMN94] C, [SMN94] D, 

[LM99] 397, [NJH2003] 5, [TW96] H2, 

[SMN94] E, [TW96] H1, 

[KTK2006] G114.4+14.6 

LDN 1198 22 36.9 +59 25.6 106.57 +0.90 0.054 −11.91 2 

TGU 672 22 37.5 +62 20.6 108.07 +3.40 0.360 1 

LDN 1197 22 37.9 +58 55.6 106.43 +0.40 0.009 0 

LDN 1187 22 38.0 +57 15.6 105.62 −1.06 0.145 0 

LDN 1189 22 39.0 +57 15.6 105.74 −1.12 0.473 0 

TGU 671 22 44.1 +60 16.1 107.77 +1.20 0.200 2 

LDN 1210 22 44.9 +62 05.8 108.70 +2.77 0.011 −10.0 0 YMD CO 40, TGU 699 

Sh 2-142 22 45.0 +57 55.8 106.76 −0.92 1.063 −41.0 14 Ced 206, GM 2-42, TGU 663, SFO 43, 

[KC97c] G107.2-01.0, [KC97c] G107.3-00.9 

LDN 1205 22 45.9 +60 25.8 108.04 +1.24 0.095 0 

LDN 1200 22 46.0 +58 45.8 107.27 −0.24 0.020 −3.7 3 YMD CO 28, TDS 402, TGU 665 

TGU 678 22 46.5 +61 12.8 108.47 +1.90 0.170 1 

LDN 1211 22 46.9 +62 10.8 108.95 +2.74 0.011 −11.1 4 YMD CO 40, TGU 699 

LDN 1212 22 47.9 +62 12.9 109.07 +2.71 0.014 −10.0 0 YMD CO 40, TGU 699 

TGU 689 22 50.2 +62 51.5 109.60 +3.17 0.160 2 

TGU 692 22 50.7 +63 15.4 109.83 +3.50 0.240 2 

YMD CO 38 22 51.1 +60 51.6 108.80 +1.33 0.028 −8.5 1 TGU 606, [KTK2006] G100.6+16.2 

YMD CO 49 22 51.1 +62 38.9 109.60 +2.93 0.014 −9.6 1 TGU 690 

LDN 1215 22 51.9 +62 06.0 109.44 +2.40 0.021 0 TGU 699 

LDN 1216 22 51.9 +62 16.0 109.52 +2.55 0.142 −9.5 11 Cep F, TDS 408, 

GN 22.51.3, TGU 699 

LDN 1236 22 52.7 +68 56.0 112.56 +8.49 0.044 −5.0 0 YMD CO 73, TGU 729 

YMD CO 51 22 56.2 +62 02.7 109.87 +2.13 0.489 −10.2 

∼ 

> 15 Cep A 

LDN 1223 22 56.9 +64 16.1 110.89 +4.11 1.010 1 TGU 703, [BKP2003] 455 

GN 22.58.2, GSH 111+04-105



(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

TGU 715 22 57.0 +65 53.5 111.60 +5.57 1.280 0 

TGU 684 22 57.4 +59 27.5 108.90 −0.27 0.230 −47.0 6 [KC97c] G109.1-00.3, [G82a] 13 

TGU 705 22 59.5 +63 26.0 110.80 +3.23 0.410 2 

LDN 1218 23 02.0 +62 16.2 110.58 +2.05 1.590 −5.1 >400 YMD CO 53, YMD CO 51 

YMD CO 56, YMD CO 58, YMD CO 59, YMD CO 62, 

YMD CO 63, TDS 418, Cep A, Cep A west, 

[THR85] Cep A-3, GAL 109.88+02.11, 

[HW84] 7d, [B77] 44, [TOH95] Ridge, 

[TOH95] C, [TOH95] B, [TOH95] A, 

Cep B, GN 22.55.2, [KC97c] G110.2+02.5, Cep E, 

Cep E South, Cep E North, [YNF96] a, 

[YNF96] b, TGU 699 

YMD CO 55 23 02.1 +61 29.2 110.27 +1.33 0.056 −7.3 2 

LDN 1224 23 04.0 +63 46.2 111.39 +3.33 0.016 0 

LDN 1220 23 04.1 +61 51.2 110.63 +1.57 0.006 −10.1 1 YMD CO 58, Cep E 

LDN 1222 23 05.1 +61 46.2 110.70 +1.45 0.002 −10.1 0 YMD CO 58, Cep E, TGU 699 

TGU 707 23 09.0 +61 04.8 110.87 +0.63 0.160 1 

TGU 700 23 09.7 +60 06.4 110.57 −0.30 0.650 −52.8 10 BFS 18 

LDN 1226 23 10.1 +62 16.3 111.44 +1.68 0.009 −10.7 0 YMD CO 63, TGU 699 

LDN 1227 23 10.1 +62 19.3 111.46 +1.73 0.008 −10.7 0 YMD CO 63, TGU 699 

LDN 1240 23 11.0 +66 26.3 113.12 +5.50 0.126 0 

LDN 1225 23 12.1 +61 36.3 111.41 +0.97 0.036 −10.9 4 TDS 419, CB 242, TGU 699 

LDN 1239 23 12.3 +66 04.3 113.11 +5.11 0.005 −7.6 0 CB 241 

NGC 7538 23 14.1 +61 29.4 111.58 +0.77 0.011 −57.0 ∼2000 [KSH92] CS 5, [KSH92] CS 4, [M73] C, 

[KSH92] CS 3, Ced 209, [WAM82] 111.543+0.7, 

[M73] B, [M73] A, [KSH92] CS 2, Sh2-158 

GAL 111.53+00.82, [WC89] 111.54+0.78, [KSH92] CS 1 

LDN 1229 23 14.1 +61 59.4 111.78 +1.24 0.004 −10.0 0 Cep D, TGU 699 

LDN 1230 23 14.1 +62 01.4 111.79 +1.27 0.002 −10.0 0 Cep D, TGU 699 

LDN 1233 23 16.5 +62 20.4 112.15 +1.47 0.001 −10.0 0 Cep D 

LDN 1232 23 17.2 +61 46.4 112.03 +0.91 0.004 −10.6 0 YMD CO 68, TGU 699 

LDN 1234 23 17.2 +62 24.4 112.25 +1.51 0.004 0 

TGU 717 23 17.3 +60 48.1 111.70 0.00 0.200 −30.1 

∼ 

> 9 

13


14 


(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

TGU 757 23 17.3 +69 56.0 114.97 +8.53 0.270 1 

LDN 1231 23 18.2 +61 16.4 111.97 +0.40 0.013 −11.2 0 TDS 424 

LDN 1250 23 22.1 +67 16.5 114.45 +5.89 2.630 −8.6 1 YMD CO 78, YMD CO 80, 

TDS 432, TGU 747 

GSH 114+06-47 

LDN 1259 23 22.9 +74 16.5 116.93 +12.44 0.035 3.9 0 YMD CO 101, TGU 772 

LDN 1244 23 25.2 +62 46.5 113.25 +1.53 0.007 0 

LDN 1246 23 25.2 +63 36.5 113.52 +2.32 0.002 −11.1 0 CB 243, [GA90] 3-40, [LM99] 400 

LDN 1261 23 27.0 +74 16.5 117.20 +12.35 0.030 3.9 2 YMD CO 101, TDS 447, TGU 772, 

TDS 448, CB 244, [LM99] 401 

LDN 1262 23 27.0 +74 16.5 117.20 +12.35 0.066 3.9 2 [BM89] 3B-10, [BM89] 1-119, TGU 772 

YMD CO 85 23 32.6 +67 02.0 115.33 +5.33 0.084 −5.4 0 

YMD CO 86 23 35.8 +66 26.2 115.47 +4.67 0.056 −7.0 0 

YMD CO 87 23 39.3 +65 42.4 115.60 +3.87 0.168 −25.3 2 

TGU 767 23 42.9 +68 52.9 116.80 +6.83 0.400 2 

LDN 1264 23 52.5 +68 16.7 117.50 +6.03 0.102 0 

LDN 1266 23 57.5 +67 16.7 117.75 +4.95 2.540 −6.8 14 YMD CO 103, YMD CO 104, YMD CO 105, 

YMD CO 108, YMD CO 111, TDS 449, TDS 451, 

TGU 774, [LM99] 404, [YF92] C1, 

[LM99] 405, [YF92] C2, GN 23.56.1, 

[KC97c] G118.1+05.0, [LM99] 406, [GA90] 1-1, 

[GA90] 1-1a, [LM99] 1, [KC97c] G118.4+04.7, 

DG 1, [GA90] 3-41, [GA90] 3-42, 

SFO 1, SFO 3, DSH J2359.6+6741 

LDN 1274 23 57.5 +70 56.7 118.52 +8.54 0.032 −2.5 0 YMD CO 109 

LDN 1268 23 59.5 +67 26.7 117.97 +5.07 0.158 −6.2 3 Sh2-171, YMD CO 104, TGU 774 

LDN 1269 00 00.6 +67 09.7 118.01 +4.78 0.025 0 TGU 774 

LDN 1270 00 01.6 +67 09.7 118.11 +4.76 0.009 2 TGU 774 

LDN 1271 00 01.6 +67 16.7 118.13 +4.87 0.010 −15.1 0 YMD CO 108, TGU 774 

LDN 1272 00 02.6 +67 16.7 118.23 +4.85 8.690 −6.3 23 YMD CO 97, YMD CO 98, YMD CO 110, 

YMD CO 112, YMD CO 113, YMD CO 114, 

YMD CO 116, TGU 779, SFO 2, [GA90] 3-1, 

[GA90] 1-1b, GSH 119+05-74



(h m) ( ◦ ′ ) ( ◦ ) ( ◦ ) (sq.deg.) (km s −1 ) 

LDN 1273 00 02.6 +68 31.7 118.46 +6.08 0.199 −8.8 4 YMD CO 114 

LDN 1275 00 06.6 +67 26.7 118.64 +4.95 0.020 0 TGU 781 

References: [ADM95] – Ábrahám et al. (1995); Barnard – Barnard (1927); [B77] – Bernes (1977); [BKP2003] – Brunt et al. (2003); [BM89] – 

Benson & Myers (1989); BFS – Blitz et al. (1982); CB – Clemens & Barvainis (1988); Ced – Cederblad (1946) DBY – Dobashi et al. 

(1994); [DE95] – Davis & Eislöffel (1995); DG – Dorschner & Gürtler (1964); DSH – Kronberger et al. (2006); [ETM94] – Eiroa et al. 

(1994); [FMS2001] – Font et al. (2001); FSE – Froebrich et al. (2005); [G82a] – Gyulbudaghian (1982) [G85] – Gyulbudaghian (1985); 

[GA90] – Gyulbudaghian & Akopyan (1990); GAL – Kerber et al. (1996); GF – Schneider & Elmegreen (1979); GM – Magakian (2003); 

GN – Magakian (2003); GSH – Ehlerova & Palous (2005); [GSL2002] – Giveon et al. (2002) HCL – Heiles (1967); [HW84] – Hughes & 

Wouterloot (1984); [IS94] – Indrani & Sridharan (1994); JWT Core – Jessop & Ward-Thompson (2000); [KC97c] – Kuchar & Clark (1997); 

KR – Kallas & Reich (1980); [KSH92] – Kawabe et al. (1992); [KTK2006] – Kiss et al. (2006); LDN – Lynds (1962); [LM99] – Lee & Myers 

(1999); [M73] – Martin (1973); MBM – Magnani et al. (1985); Min – Minkowski (1947); [MPR2003] – Matthews et al. (2003); [NJH2003] – 

Nikolić et al. (2003); [P85b] – Petrossian (1985) [PGH98b] Cloud – Patel et al. (1998); [PGS95] – Patel et al. (1995); PP – Parsamian & 

Petrosian (1979); RNO – Cohen (1980) SFO – Sugitani et al. (1991); Sh 2- – Sharpless (1959); [SMN94] – Sato et al. (1994); TDS – Taylor et 

al. (1987); TGU – Dobashi et al. (2005); [THR85] – Torrelles et al. (1985); [TOH95] – Testi et al. (1995); [TW96] – Tóth & Walmsley (1996); 

[WAM82] – Wink, Altenhoff & Mezger (1982); [WC89] – Wood & Churchwell (1989); WWC – Weikard et al. (1996); YMD CO – Yonekura 

et al. (1997); [YF92] – Yang & Fukui (1992); [YNF96] – Yu et al. (1996). 

15

16 

2. The Cepheus Flare 

2.1. Large-scale Studies of the Cepheus Flare 

The term ‘Cepheus flare’ was first used by Hubble (1934) who recognized that the zone 

of avoidance of external galaxies, confined to the Galactic plane, extended to higher 

latitudes at certain segments of the plane, suggesting significant obscuration outside 

the main Galactic belt. He called these wide segments for Galactic disk flares. The 

Cepheus Flare can be found at 100 ◦ ≤ l ≤ 120 ◦ : there is a large amount of dense ISM 

above b ≥ 10 ◦ (Lynds 1962; Taylor, Dickman & Scoville 1987; Clemens & Barvainis 

1988; Dobashi et al. 2005). 

Heiles’ (1967) study of the HI distribution in the region revealed two kinematically 

separate sheets of interstellar gas in the Galactic latitude interval +13 ◦ ≤ b ≤ +17 ◦ , 

moving at a velocity of ∼ 15 km s −1 relative to each other. Heiles speculated that the 

two sheets probably represent an expanding or colliding system at a distance interval 

of 300–500 pc. Berkhuijsen (1973) found a giant radio continuum region Loop III 

centered on l=124±2 ◦ , b=+15.5±3 ◦ and stretching across 65 ◦ , and suggested that it 

was a result of multiple supernova explosions. The HI shell reported by Hu (1981) at 

l=105 ◦ , b=+17 ◦ and v centr =+3 km s −1 also indicates that the interstellar medium in this 

region is in a state of energetic motion. The wide range in the velocity thus may reflect 

disturbances from various shocks. 

Lebrun’s (1986) low-resolution CO survey revealed that, in this region, the clouds 

constitute a coherent giant molecular cloud complex. Based on Racine’s (1968) study 

of reflection nebulae, Lebrun placed the Cepheus Flare molecular clouds between 300 

and 500 pc. Grenier et al. (1989) extended the CO survey to a region of 490 deg 2 in 

Cepheus–Cassiopeia above b=+10 ◦ . They found that the clouds could be divided into 

two kinematically well separated subsystems around the radial velocities of v LSR ∼ 

0 km s −1 and −10 km s −1 , respectively. They also detected CO emission around 

v LSR ∼ 0 km s −1 at higher longitudes (124 ◦ < l < 140 ◦ ) in Cassiopeia, and found an 

area free of CO emission at 118 ◦ < l < 124 ◦ . They suggested that the void between 

the Cepheus and Cassiopeia clouds is a supernova bubble. They estimated the age of 

the bubble as 4 × 10 4 years, and proposed that it may result from a Type I supernova. 

Yonekura et al. (1997) conducted a large-scale 13 CO survey of the Cepheus– 

Cassiopeia region at an 8-arcmin grid spacing and with 2. ′ 7 beam size. Out of the 

188 molecular clouds found in the whole surveyed region 51 fall in the Cepheus Flare 

region. Their surface distribution, adopted from Yonekura et al. (1997), is shown in 

Fig. 4. 

These clouds, distributed over the velocity interval of (−15,+6) km s −1 , were classified 

into three kinematically different components by Yonekura et al. (see Table 2). 

The high latitude part of the molecular complex is included in Magnani et al.’s (1985) 

catalog of high latitude molecular clouds. Ammonia observations of dense cores have 

been reported by Benson & Myers (1989) and Tóth & Walmsley (1996). In addition to 

the two major catalogs of dark clouds (Lynds 1962; Dobashi et al. 2005), dark cloud 

cores were catalogued by Lee & Myers (1999). 

Kun (1998) determined cloud distances using Wolf diagrams, and presented a list 

of candidate YSOs found during an objective prism Hα survey, and selected from the 

IRAS Catalogs. 

Kiss et al. (2006) performed a complex study of the visual and infrared properties 

of the ISM in the Cepheus Flare region using USNO, 2MASS, DIRBE, IRAS, and

17 

Table 2. Cloud groups in Cepheus, classified by Yonekura et al. (1997). 

N Longitude Latitude V LSR D M Associated Ref. 

l l l u b l b u V l V u (pc) (M⊙) objects 

( ◦ ) ( ◦ ) ( ◦ ) ( ◦ ) (km s −1 ) 

Close Group 

1 99 105 13 18 1 5 440 3900 NGC 7023, L1157 1, 2 

2 102 104 16 18 −4 −1 300 90 3 

3 105 110 −1 1 −4 −1 300 110 L1200 3 

4 106 116 13 19 −8 −1 300 3600 Cepheus Flare 4 

5 110 116 4 12 −9 −3 300 730 L1221, L1250 3 

6 110 117 19 21 −9 −4 300 680 L1228 3 

7 115 117 −4 −1 −4 −1 140 20 L1253, L1257 5 

8 116 118 12 13 3 5 200 26 L1262 6 

9 117 124 6 10 −3 −1 300 200 L1304 3 

Distant Group 

10 ∗ 95 99 3 7 −8 2 624 4000 IC 1396 17 

13 103 111 9 15 −21 −8 1000 12000 NGC 7129 7, 8 

14 105 110 0 7 −14 −6 910 11000 S 140 9 

15 108 117 0 4 −17 −4 730 15000 Cep OB3 10 

16 115 116 3 5 −26 −23 1000 1400 M115.5+4.0 11 

17 116 124 −2 7 −22 −2 850 27000 Cep OB4 12 

Clouds in Perseus Arm 

22 111 112 −1 1 −31 −30 2200 2500 MWC1080 13, 14 

23 112 113 −3 −2 −37 −34 3000 5400 Cas A 15 

24 123 124 −7 −6 −32 −30 2100 2000 NGC 281 16 

References. (1) Viotti (1969); (2) Shevchenko et al. (1989); (3) Grenier et al. (1989); (4) Kun & Prusti 

(1993); (5) Snell (1981); (6) Myers & Benson (1983); (7) Racine (1968); (8) Shevchenko & Yakubov 

(1989); (9) Crampton & Fisher (1974); (10) Crawford & Barnes (1970); (11) Yang (1990); (12) Mac- 

Connell (1968); (13) Levreault (1985); (14) Levreault (1988); (15) Ungerechts & Thaddeus (1989); (16) 

Hogg (1959); (17) de Zeeuw et al. (1999). 

∗ The 13 CO clouds in the region of IC 1396 are included in Dobashi et al. (1994), not in Yonekura et al. 

(1997). 

Figure 4. Distribution of 13 CO clouds in the Cepheus Flare (adopted from 

Yonekura et al. 1997)

18 

ISO data. Based on the distribution of visual extinction they identified 208 clouds, 

and divided them into 8 complexes. They examined the morphology of clouds, and 

established several empirical relationships between various properties of the clouds. 

Olano et al. (2006) studied the space distribution and kinematics of the interstellar 

matter in Cepheus and Cassiopeia, using the Leiden–Dwingeloo HI data and the 

Columbia Survey CO data. They found that the broad and often double-peaked spectral 

line profiles suggest that the Cepheus Flare forms part of a big expanding shell that 

encloses an old supernova remnant. Assuming a distance of 300 pc for the center of 

the shell, located at (l,b) ≈ (120 ◦ ,+17 ◦ ), they derived a radius of approximately 50 pc, 

expansion velocity of 4 km s −1 , and HI mass of 1.3 × 10 4 M⊙ for the Cepheus Flare 

Shell. The supernova bubble proposed by Grenier et al. (1989), the radio continuum 

structure Loop III (Berkhuijsen 1973), and the Cepheus Flare Shell are various observable 

aspects of the supernova explosion(s) that shaped the structure of the interstellar 

medium and triggered star formation in the Cepheus Flare during the past few million 

years. 

2.2. Distance to the Cepheus Flare Clouds 

Spectroscopic and photometric studies of stars illuminating reflection nebulae in the 

Cepheus Flare (Racine 1968) indicated, long before the discovery of the molecular 

cloud complex, that interstellar dust can be found at several distances along the line of 

sight in this region. The presence of clouds at different velocities also suggests that 

there are clouds at various distances (Grenier et al. 1989). 

At the low Galactic latitude boundary of the Cepheus Flare we find the associations 

Cep OB2 and Cep OB3 at a distance of ∼ 800 pc. Therefore Grenier et al. (1989) 

propose that the negative velocity component of the Cepheus flare clouds (v LSR ∼ 

−10 km s −1 ) is an extension of these local arm features, while the more positive (v LSR ∼ 

0 km s −1 ) velocity component corresponds to a nearby cloud complex at a distance of 

300 pc. 

Table 2 suggests a more complicated pattern of cloud distances. Both the close 

and the distant components are composed of several complexes, probably located at 

different distances. Other distance determinations found in the literature support this 

suggestion. Below we list some results and problems related to the distance of Cepheus 

Flare clouds. 

Distances of individual clouds can reliably be derived by studying the effects of 

the clouds on the light of associated stars. Racine (1968), in a spectroscopic and photometric 

study of stars in reflection nebulae, obtained a distance of 400±80 pc for the 

Cepheus R2 association above the latitude +10 ◦ . Both velocity components are represented 

among the clouds being illuminated by the stars of Cep R2. 

A prominent object of the distant component, in addition to the possible outer 

parts of Cep OB2 and Cep OB3, is NGC 7129. Though Kun, Balázs & Tóth (1987) and 

Ábrahám, Balázs & Kun (2000) proposed that NGC 7129 may be associated with the 

Cepheus Bubble, and thus with Cep OB2, other observations suggest that NGC 7129 

may be farther than Cep OB2. Racine (1968) investigated three member stars, and derived 

m −M ≈ 12.2 for BD+65 ◦ 1637, and 10.0 for both BD+65 ◦ 1638 and LkHα 234, 

and labeled each value as uncertain. Shevchenko & Yakubov (1989), based on an A V 

vs. distance diagram, derived 1250 pc for NGC 7129. Yonekura et al. (1997) found 

a group of clouds at l ∼ 107 ◦ − 111 ◦ , b ∼ +13 ◦ at similar velocity, and regarded 

them as an extension of the NGC 7129 clouds to the northeast (group 13 in Table 2).

19 

Table 3. Distance measured for the clouds within the Cepheus Flare region together 

with their probable lower and upper limits and the method of determination. 

Cloud l b d (∆d) Method Ref. 

( ◦ ) ( ◦ ) (pc) 

L1147/L1158 102.0 15.0 325±13 A V vs. distance 4 

L1167/L1174 104.0 15.0 440±100 spectroscopy & photometry of HD 200775 1 

L1167/L1174 104.0 15.0 288±25 A V vs. distance 4 

L1167/L1174 104.0 15.0 430 +160 

−90 Hipparcos parallax of HD 200775 10 

L1177 105.14 13.12 300±30 Wolf diagram 6 

L1199 106.50 12.21 500±100 Wolf diagram 6 

L1199 106.50 12.21 800 spectroscopy & photometry of HD 206135 2 

TDS400 107.01 16.78 300 +50 

−10 Wolf diagram 6 

CB 234 108.10 13.15 300 +50 


TDS406 108.50 18.15 300 +50 


L1217 110.34 11.41 400 +50 


L1219 110.60 11.96 400 +50 


L1219 110.60 11.96 400 spectroscopy & photometry of BD+69 1231 2, 8 

TDS420 111.57 14.25 300 +50 


L1228 111.63 20.14 200 +100 


L1228 111.63 20.14 180 +30 

−10 spectroscopy & photometry of BD+76 825 

TDS421 111.71 13.80 250 +30 


L1235 112.22 13.86 200 A V vs. distance 3 

L1235 112.22 13.86 300 +50 


L1235 112.22 13.86 400±80 spectroscopy & photometry of HD 210806 2, 8 

L1235 112.22 13.86 300 +80 

−40 Hipparcos parallax of HD 210806 7 

L1241 113.03 17.51 300 +50 


L1242 113.08 13.14 300 +30 


L1243 113.10 15.64 300 +50 


L1247 113.60 15.20 300 +50 


L1251 114.45 14.68 300±50 A V vs. distance 5 

L1251 114.45 14.68 300 +50 


L1251 114.45 14.68 337±50 star count analysis 9 

MBM163–165 116.00 20.25 200 +100 


L1259–1262 117.00 12.40 180 +40 


References: (1) Viotti (1969); (2) Racine (1968); (3) Snell (1981); (4) Straizys et al. (1992); (5) Kun & 

Prusti (1993); (6) Kun (1998); (7) ESA (1997); (8) Kun et al. (2000); (9) Balázs et al. (2004); (10) van 

den Ancker et al. (1997) 

This result suggests that a considerable part of the Cepheus Flare clouds is located at 

about 1 kpc. The situation is, however, far from clear. Simonson & van Someren Greve 

(1976) found a large HI cloud coinciding both in position and velocity with the molecular 

clouds of Yonekura et al.’s group 13. They associated this cloud not with NGC 7129, 

but with the reflection nebulae of Cep R2 (Racine 1968) at a distance of some 400 pc. 

The Wolf diagrams constructed by Kun (1998) show two layers of extinction towards 

b ∼ +11 ◦ − +13 ◦ , at 300 pc and ∼ 450 pc, respectively, thus it is tempting to identify 

the two velocity components with these two layers. 

Another direct distance determination within the area of the Cepheus Flare is that 

of Viotti (1969), who derived 440±100 pc for the reflection nebula NGC 7023, based on 

high resolution spectroscopy and UBV photometry of its illuminating star, HD 200775.

20 

In spite of the large uncertainty of this value, this is the most frequently cited distance of 

NGC 7023. Alecian et al. (2008) pointed out that HD 200775 is a spectroscopic binary 

with two nearly identical components, thus its observed luminosity has to be partitioned 

on both components, which suggests a distance of about 350 pc. The distance from the 

Hipparcos parallax of HD 200775, 430 +160 

−90 pc (van den Ancker et al. 1997) has to be 

treated with some caution, since part of the measured displacement of the star resulted 

from its orbital motion. The projected separation of the components, estimated by 

Alecian et al. (2008), 16 ± 9 mas, commensurates with the measured parallax, and the 

orbital period of 1412 days suggests that Hipparcos might have measured the position 

of the star at any point of the orbit. 

Straizys et al. (1992) determined the visual extinction A V vs. distance using photometric 

measurements of 79 stars in the Vilnius photometric system for the L1147/1158 

and NGC 7023 (L 1167/1174) regions. They obtained a distance 288±25 pc for NGC 

7023, and the same method resulted in 325±13 pc for the L1147/L1158 group. 

Snell (1981) studied the interstellar reddening towards L 1235 and pointed out the 

presence of an absorbing layer at a distance of 200 pc. This value is frequently assumed 

to be the distance of several other clouds in the region as well (e.g. Benson & Myers 

1989). 

Kun & Prusti (1993) found a distance of 300±50 pc for L 1251 by examining 

the interstellar reddening as a function of distance moduli of field stars. Kun (1998) 

determined distances of dark clouds over the whole area of the Cepheus Flare using 

Wolf diagrams. The Wolf diagrams indicated that the interstellar matter in the Cepheus 

Flare is concentrated at three characteristic distances: 200, 300 and 450 pc. The three 

components, though partly overlapping, can be separated along the Galactic latitude. 

The three absorbing layers can be identified with Yonekura et al.’s (1997) groups 6, 

4, and 1, respectively. The overlap of the layers makes the distance determination 

of some dark clouds ambiguous. For instance, both the 300 pc and 200 pc layers can 

be recognized towards L 1228. However, L 1228 differs in radial velocity from the 

other clouds of the 300 pc component. Moreover, the star BD+76 ◦ 825 (spectral type: 

F2 V, B=11.21, V=10.62) is projected within a compact group of pre-main sequence 

stars of L 1228 and illuminates a faint reflection nebula (Padgett et al. 2004). Thus the 

photometric distance of this star, 180 pc, is a good estimate of the distance of L 1228. 

The Cepheus Flare shell, proposed by Olano et al. (2006), may explain the existence 

of dark clouds at both 200 and 300 pc (see Fig. 5). Table 3 summarizes the results 

of distance determinations in the Cepheus Flare region. The group of clouds whose 

distance remains controversial is associated with the negative velocity component at 

l ∼ 107 ◦ − 111 ◦ , b ∼ +13 ◦ . 

2.3. Star Formation in the Cepheus Flare 

Star formation takes place in dense cores of molecular clouds. Dense cores within 

dark clouds are usually designated with letters appended to the name of the cloud, e.g. 

L 1082 A, L 1251 E. Several dense cores and IRAS sources of the Cepheus Flare clouds 

have been included in large molecular surveys aimed at studying their various properties 

and the associated young stellar objects. Below we list some major survey papers 

including key data for Cepheus Flare clouds, cores, and IRAS sources. 

Myers et al. (1983) – CO observations (L1152, L1155 H, L1155 D, L1082 C, L1082 A, 

L1082 B, L1174, L1172 D, L1172 B, L1262 A); 

Clemens & Barvainis (1988) – positions, radial velocities, and IRAS associations of

21 

300 

l=180 o 

Loop III - old supernova shell 

200 

Cepheus Flare 

Shell 

Y (pc) 

100 

0 

Sun 

UMa 

Polaris 

Flare 

L1333 

L1261 

L1228 

L1082? 

Local Bubble 

L1251 

L1235 

NGC 7023 

L1157 

L1219 

l=90 o 

0 100 200 300 400 500 

X (pc) 

300 

b=90 o 

110 o < l < 120 o 

Z (pc) 

200 

100 

Local Bubble Cepheus 

L1228 

Flare 

Shell 

Loop III 

L1241 

L1251 

L1235 

L1219 

b=+15 o 

0 

Sun 

L1261 

b=0 o 

0 100 200 300 400 500 

X (pc) 

Figure 5. Upper panel: Distribution of the most prominent molecular clouds of 

the Cepheus Flare and nearby interstellar shells, projected on the Galactic plane, and 

viewed from the direction of the North Galactic pole. Lower panel: the same objects 

projected onto a plane perpendicular to the Galactic equator. 

small, optically selected molecular clouds (CB 222, CB 224, CB 229 (L1171), CB 230, 

CB 232, CB 244); 

Benson & Myers (1989) – NH 3 observations (L1152, L1155 B, L1155 C, L1155 D, 

L1155 G, L1158, L1082 C, L1082 A, L1174, L1174 B, L1172 D, L1172 A, L1172 B, 

L1228 C, L1228 B, L1235, L1251 A, L1262 A); 

Goodman et al. (1993) – velocity gradients (L1152, L1082 A, L1082 B, L1082 C, L1174, 

L1172 A, L1251 A, L1251 E, L1262 A); 

Benson et al. (1998) – N 2 H + , C 3 H 2 , and CCS observations (L1155, L1152, L1152 (IR), 

L1082 A, L1082 C, L1174, L1172 A, L1228, L1228 D, L1221, L1251 A, L1251 E, L1262);

22 

Myers et al. (1988) – search for outflows (L1152, L1082 A, L1174, L1172 D, L1262); 

Fukui (1989) – search for outflows (PV Cep, L1228, L1172, NGC 7129, LkHα 234, 

L1221, L1251 A, L1251 B, L1262); 

Furuya et al. (2003) – search for H 2 O masers (L1082, L1082 A, L1082 B, L1228, 

L1174, L1172 D, L1221, L1251 A, L1251 B, L1262); 

Mardones et al. (1997) – search for protostellar infall (IRAS 20353+6742, 

IRAS 20386+6751, IRAS 21017+6742, IRAS 22343+7501, IRAS 22376+7455, IRAS 

23238+7401). 

Table 4. 

Molecular outflows and sources in the Cepheus Flare. 

Cloud RA(2000) Dec(2000) Source References 

L 1157 20 39 06 +68 02 13 IRAS 20386+6751 5,17 

L 1157 20 45 54 +67 57 39 PV Cep 5,10,12 

L 1082 20 47 56.6 +60 04 14 IRAS 20468+5953 22 

L 1082 20 51 30.1 +60 18 39 GF9–2 22,23 

L 1082 20 53 13.6 +60 14 40 IRAS 20520+6003 22 

L 1228 A 20 57 13 +77 35 47 IRAS 20582+7724 5,7,9 

L 1228 B 20 57 06 +77 36 56 HH 200 IRS 9 

L 1174 A 21 00 22 +68 12 52 L 1174 A 21 

L 1172 21 02 24 +67 54 27 IRAS 21017+6742 2, 5,13, 

L 1174 21 03 02 +68 06 57 RNO 131A 1,3,20 

L 1177 21 17 40 +68 17 32 IRAS 21169+6804 19, 21 

L 1183 21 42 57 +66 04 47 RNO 138 1,3,24 

L 1183 21 43 01 +66 03 37 NGC 7129 FIRS 2 4,5,8,10 

L 1183 21 43 02 +66 06 29 LkHα 234 4,5,8,10 

L 1183 21 43 00 +66 11 28 V350 Cep 24 

L 1219 22 14 08 +70 15 05 IRAS 22129+7000 14,25 

L 1221 22 28 03 +69 01 13 IRAS 22266+6845 6,11,18 

TDS 417 22 35 06 +69 10 53 IRAS 22336+6855 6 

L 1251 A 22 35 24 +75 17 06 IRAS 22343+7501 5,15 

L 1251 B 22 38 47 +75 11 29 IRAS 22376+7455 5,15,16 

L 1262 23 25 46 +74 17 33 IRAS 23238+7401 5,17,20 

References. 1: Armstrong (1989); 2: Beichman, Myers & Emerson (1986); 3: Cohen (1980); 4: Edwards 

& Snell (1983); 5: Fukui (1989); 6: Haikala & Dietrich (1989); 7: Haikala & Laureijs (1989); 8: Harvey, 

Wilking & Joy (1984); 9: Bally et al. (1995); 10: Lada (1985); 11: Lee et al. (2002); 12: Levreault (1984); 

13: Myers et al. (1988); 14: Nikolić & Kun (2004); 15: Sato & Fukui (1989); 16: Sato et al. (1994); 17: 

Terebey et al. (1989); 18: Umemoto et al. (1991); 19: Wang et al. (1995); 20: Wu et al. (1992); 21: Yun 

& Clemens (1992); 22: Wiesemeyer et al. (1999); 23: Furuya et al. (2006); 24: Liseau & Sandell (1983); 

25: Goicoechea et al. (2008). 

The Cepheus Flare cloud cores can be found among the targets of infrared, submillimeter 

and millimeter continuum surveys of embedded low mass young stellar objects 

as well: 

Connelley et al. (2007) – a K-band atlas of reflection nebulae (IRAS 20353+6742, IRAS 

20453+6746, IRAS 21017+6742, IRAS 22266+6845, IRAS 22376+7455); 

Young et al. (2006) – submillimeter (450 and 850 µm) survey of cores included in 

the Spitzer c2d project (L 1152, CB 224, L 1157, L 1082 C, L 1082 A, L 1228, L 1177 

(CB 230), L 1221, L 1251 C, L 1251 E, L 1155 C); 

Rodríguez & Reipurth (1998) – VLA observations of HH exciting sources (L 1152, 

L 1157, L 1221).

We find these objects in statistical studies of dense cores and young stellar objects: 

Fuller & Myers (1992) – line width–size relations (L 1152, L 1262); 

Myers et al. (1991) – shapes of cores (L 1152, L 1251, L 1262); 

Wu et al. (2004) – properties of outflows (L 1152, L 1155, L 1082, L 1174, L 1172, 

L 1228, L 1177, L 1221, L 1251, L 1262); 

Wu et al. (2007) – submm (350 µm) survey of cores included in the Spitzer c2d project 

(L 1152, L 1157, L 1148, L 1177, L 1228, RNO 129, L 1221, L 1251). 

The molecular outflows discovered in the Cepheus Flare and their driving sources 

are listed in Table 4, and the Herbig–Haro objects and driving sources can be found in 

Table 5. 

Figure 3 shows the surface distribution of pre-main sequence stars and candidates 

in the Cepheus Flare. Apparently star formation occurs in small aggregates, especially 

along the boundaries of the complex. The central part of the cloud complex contains 

clouds of low density and is avoided by known signposts of star formation. 

The samples of T Tauri stars, displayed in Fig. 3, result from several surveys for 

Hα emission stars conducted in the region of Cepheus Flare. Only 10 pre-main sequence 

objects are catalogued in the Herbig–Bell Catalog (Herbig & Bell 1988, hereinafter 

HBC). Ogura & Sato (1990) reported on 69 detected and 49 suspected Hα emission 

stars in a wide environment of L 1228. Kun (1998) reported 142 Hα emission 

stars, distributed over the whole area of the Cepheus Flare, identified on objective prism 

photographic Schmidt plates and 128 IRAS sources as possible YSOs. Spectroscopic 

follow up observations of both samples are underway (Kun et al., in preparation). We 

show in Fig. 3 and list in Table 7 those stars from these two surveys whose pre-main 

sequence nature has already been confirmed. The known Herbig Ae/Be stars are also 

listed in Table 7. 

Tachihara et al.’s (2005) spectroscopic observations toward the ROSAT X-ray 

sources resulted in detecting 16 Li-rich stars, representing weak line T Tauri stars. The 

main properties of these WTTSs are listed in Table 6. 

The distribution of the WTTSs in the Cepheus Flare differs from that of other 

YSOs. In the CO void found by Grenier et al. (1989), a group of WTTSs is separated 

from the 13 CO cloud by ∼ > 10 pc. The cloud-to-WTTS separations are significantly 

larger in Cepheus than in other nearby SFRs such as Chamaeleon. Because of their 

grouping, Tachihara et al. propose the in-situ formation model for them. From the 

total mass of the group of TTSs, a ∼ 800 M⊙ molecular cloud might have formed 

them, while only ∼ 200 M⊙ molecular gas remained in their vicinity. An external 

disturbance might have dissipated the molecular cloud within several 10 5 yr. As the 

distances to the WTTSs are unknown, Tachihara et al. suggest two possible scenarios 

for the history of the formation of the WTTS sample isolated from the cloud complex: 

(1) The WTTSs in the CO void were formed at 300 pc and affected by the supernova 

shock discussed by Grenier et al. (1989); or (2) They are at 200 pc and an unknown 

supernova explosion has the responsibility for the parent cloud dissipation. Radial velocity 

measurements might help to find the relationship between the stars and the cloud 

complex. Taking into account the picture of the Cepheus Flare Shell, the same supernova 

might have triggered star formation at both 200 and 300 pc. 

2.4. Notes on Individual Objects 

L 1147/L 1158 The cloud group often referred to as the L 1147/L 1158 complex consists 

of the clouds Lynds 1147, 1148, 1152, 1155, 1157, and 1158. L 1157 harbors a 

23

24 

Table 5. 

Herbig–Haro objects and their sources in the Cepheus Flare. 

Name RA(2000) Dec(2000) Source Cloud D(pc) Reference 

HH 376B 20 35 06.1 +67 48 47 IRAS 20359+6745 L1152 440 11,13 

HH 376A 20 36 02.4 +67 54 28 IRAS 20359+6745 L1152 440 11,13 

HH 376 20 36 55.3 +67 59 28 IRAS 20359+6745 L1152 440 15,19 

HH 375 20 39 06.2 +68 02 15 IRAS 20386+6751 L1157 440 2,18,19 

HH 315C 20 45 06.9 +68 04 50 PV Cep L1158 500 2,8,13 

HH 315 20 45 34.0 +68 03 25 PV Cep L1158 500 2,8,13 

HH 315B 20 45 34.0 +68 03 25 PV Cep L1158 500 2,8,13 

HH 315A 20 45 38.4 +68 00 55 PV Cep L1158 500 2,8,13 

HH 215 20 45 53.8 +67 57 39 PV Cep L1158 500 10,12,13 

HH 415 20 46 04.6 +68 00 28 L1158 500 8,11,16 

HH 315D 20 46 06.4 +67 54 13 PV Cep L1158 500 2,8,13 

HH 315E 20 46 28.1 +67 52 20 PV Cep L1158 500 2,8,13 

HH 315F 20 47 09.9 +67 50 05 PV Cep L1158 500 2,8,13 

HHL 65 20 53 06.0 +67 10 00 300 7 

HH 199R3 20 54 49.1 +77 32 16 IRAS 20582+7724 L1228 200 4 

HH 199R2 20 54 56.2 +77 32 21 IRAS 20582+7724 L1228 200 4 

HH 200B6 20 55 09.4 +77 31 20 HH 200 IRS L1228 200 4 

HH 199R1 20 55 12.2 +77 33 11 IRAS 20582+7724 L1228 200 4 

HH 200B5 20 55 22.5 +77 32 17 HH 200 IRS L1228 200 4 

HH 200B4 20 55 33.9 +77 33 07 HH 200 IRS L1228 200 4 

HH 200B4a 20 56 11.0 +77 34 18 HH 200 IRS L1228 200 4 

HH 200B3 20 56 22.2 +77 35 01 HH 200 IRS L1228 200 4 

HH 200B2 20 56 35.9 +77 35 34 HH 200 IRS L1228 200 4 

HH 200B1 20 56 51.2 +77 36 21 HH 200 IRS L1228 200 4 

HH 199B1 20 57 27.2 +77 35 38 IRAS 20582+7724 L1228 200 4 

HH 199B2 20 57 31.0 +77 35 44 IRAS 20582+7724 L1228 200 4 

HH 199B3 20 57 34.1 +77 35 53 IRAS 20582+7724 L1228 200 4 

HH 199B4 20 58 21.7 +77 37 42 IRAS 20582+7724 L1228 200 4 

HH 199B5 20 59 08.0 +77 39 25 IRAS 20582+7724 L1228 200 4 

HH 198 20 59 09.7 +78 22 48 IRAS 21004+7811 L1228 200 4,14,16,17 

HH 200R1 20 59 48.2 +77 43 50 HH 200 IRS L1228 200 4 

HH 199B6 21 00 27.4 +77 40 54 IRAS 20582+7724 L1228 200 4 

HHL 67 21 05 00.0 +66 47 00 300 7 

HH 450 22 14 24.1 +70 14 26 IRAS 22129+7000 L1219 400 5 

HH 450X 22 14 50.1 +70 13 47 L1219 400 5 

HH 363 22 27 46.7 +69 00 38 IRAS 22266+6845 L1221 200 1,9 

HH 149 22 35 24.2 +75 17 06 IRAS 22343+7501 L1251 300 3,13 

HH 373 22 37 00.0 +75 15 16 L1251 300 16 

HH 374 22 37 39.1 +75 07 31 L1251 300 16 

HH 374A 22 37 39.2 +75 07 31 L1251 300 1 

HH 374B 22 37 50.0 +75 08 13 L1251 300 1 

HH 364 22 38 19.2 +75 13 07 L1251 300 16 

HH 189C 22 38 39.4 +75 09 49 L1251 300 6 

HH 189 22 38 39.9 +75 10 41 IRAS 22376+7455? L1251 300 6 

HH 189B 22 38 40.0 +75 10 40 KP 44? L1251 300 6 

HH 189E 22 38 40.3 +75 13 52 L1251 300 1 

HH 189A 22 38 40.4 +75 10 53 L1251 300 6 

HH 189D 22 38 44.2 +75 13 28 L1251 300 1 

HH 358 23 24 39.0 +74 12 35 L1262 180 1,16 

HH 359 23 26 29.0 +74 22 28 L1262 180 1,16 

References. 1: Alten et al. (1997); 2: Arce & Goodman (2002); 3: Balázs et al. (1992); 4: Bally et al. 

(1995); 5: Bally & Reipurth (2001); 6: Eiroa et al. (1994); 7: Gyulbudaghian et al. (1987); 8: Gómez et al. 

(1997); 9: Lee et al. (2002); 10: Moreno-Corral et al. (1995); 11: Movsessian et al. (2004); 12: Neckel et 

al. (1987); 13: Reipurth, Bally, & Devine (1997); 14: Movsessian & Magakian (2004); 15: Rodríguez & 

Reipurth (1998); 16: Wu et al. (1992); 17: Brugel & Fesen (1990); 18: Devine, Reipurth & Bally (1997); 

19: Davis & Eislöffel (1995).

Class 0 object, L 1157-mm, with L bol ∼ 11 L⊙. It coincides with IRAS 20386+6751 

and drives a spectacular outflow. The L 1157 outflow has been studied in detail through 

many molecular lines, such as CO (Umemoto et al. 1992; Gueth, Guilloteau & Bachiller 

1996; Bachiller & Pérez Gutiérrez 1997; Hirano & Taniguchi 2001), SiO (Mikami et 

al. 1992; Zhang et al. 1995; Gueth, Guilloteau & Bachiller 1998; Zhang, Ho & Wright 

2000; Bachiller et al. 2001), H 2 (Hodapp 1994; Davis & Eislöffel 1995), NH 3 (Bachiller 

et al. 2001; Tafalla & Bachiller 1995; Umemoto et al. 1999), and CH 3 OH (Bachiller et 

al. 1995, 2001; Avery & Chiao 1996). Many other lines have been detected (Bachiller 

& Pérez Gutiérrez 1997; Bachiller et al. 2001; Beltrán et al. 2004; Benedettini et al. 

2007; Arce et al. 2008), making L 1157 the prototype of chemically active outflows. 

Gas phase shock chemistry models have been used by Amin (2001) to study the production 

of the observed species in the L 1157 outflow . Arce & Sargent (2006) studied 

the outflow–envelope interaction on a 10 4 AU scale using high angular resolution multiline 

observations. Velusamy et al. (2002) detected spatially resolved methanol emission 

at 1 mm from L 1157. Their results indicate the presence of a warm gas layer in the 

infall–disk interface, consistent with an accretion shock. Regarding the protostar itself, 

dust continuum observations have been carried out at 2.7 mm (Gueth et al. 1996, 1997; 

Beltrán et al. 2004), 1.3 mm (Shirley et al. 2000; Chini et al. 2001; Gueth, Bachiller & 

Tafalla 2003; Beltrán et al. 2004), 850 µm (Shirley et al. 2000; Chini et al. 2001; Young 

et al. 2006), 450 µm (Chini et al. 2001), as well as 60, 100, 160, and 200 µm (Froebrich 

et al. 2003). Using the VLA, Rodríguez & Reipurth (1998) detected the protostar 

as a radio continuum source at 3.6 cm. Froebrich et al. (2003) obtained a far-infrared 

spectrum of the L 1157 protostar using the LWS on board ISO. Deep Spitzer IRAC images 

of L 1157 reveal many details of the outflow and the circumstellar environment of 

the protostar. Looney et al. (2007) report on the detection of a flattened structure seen 

in absorption at 8 µm against the background emission. The structure is perpendicular 

to the outflow and is extended to a diameter of 2 arcmin. This structure is the first 

clear detection of a flattened circumstellar envelope or pseudo-disk around a Class 0 

protostar. 

25 

Table 6. Weak-line T Tauri stars in the Cepheus Flare (Tachihara et al. 2005) 

ID GSC RA(2000) Dec(2000) Sp. Type V V − I C M 1 (M ⊙) Age(Myr) 1 

4c1 0450001478 00 38 05.4 +79 03 21 K1 10.43 0.92 1.6 2 

4c2 00 38 05.4 +79 03 21 K7 13.86 1.77 0.8 15 

5c1 0450001549 00 39 06.1 +79 19 10 K6 12.18 1.52 0.6 1 

5c2 00 39 06.1 +79 19 10 M2 2 14.12 2.10 0.4 1 

19 0458901101 20 20 29.3 +78 07 22 G8 10.39 0.82 1.6 6 

20 0445900083 20 25 15.4 +73 36 33 K0 10.62 0.84 1.6 4 

28 0458601090 21 11 29.4 +76 14 29 G8 11.66 0.81 1.0 25 

34 0460801986 22 11 11.0 +79 18 00 K7 13.09 1.55 0.7 3 

36c1 0427200174 22 27 05.3 +65 21 31 K4 12.92 1.13 0.9 20 

36c2 22 27 05.3 +65 21 31 M4 2 15.55 2.50 0.2 0.2 

37c1 0448000917 22 33 44.9 +70 33 18 K3 11.63 1.65 1.0 0.4 

38 0460400743 22 39 58.1 +77 49 40 K2 11.88 1.03 1.2 8 

40 0460502733 23 00 44.4 +77 28 38 K0 10.98 0.88 1.4 6 

41 0460500268 23 05 36.1 +78 22 39 K6 13.19 1.59 0.8 7 

43c1 0448900036 23 09 43.4 +73 57 15 K7 13.21 1.86 0.3 4 

43c2 23 09 43.4 +73 57 15 M3 2 15.55 2.50 0.7 3 

44 0460500170 23 16 18.1 +78 41 56 K4 11.77 1.24 1.0 2 

45 0447900348 23 43 41.9 +68 46 27 K2 12.64 1.00 0.9 25 

46 0461001318 23 51 10.0 +78 58 05 K1 11.34 0.93 1.3 6 

1 Derived from the evolutionary tracks by D’Antona & Mazzitelli (1994). 

2 Derived only from the V − I C color.

26 

The K ′ image of the outflow source, presented by Hodapp (1994), is dominated by 

nebulosity of bipolar morphology, indicative of an in-plane bipolar outflow. Knots of 

nebulosity extend to the north and south of the outflow position. Both the northern and 

the southern lobes contain bow shock fronts. 

X-ray observations of L 1157, performed by the ASCA satellite, have been published 

by Furusho et al. (2000). 

The molecular cloud L 1155 was mapped by Harjunpää & Mattila (1991) in the 

lines of C 18 O, HCO + , and NH 3 . The observations revealed that L 1155 consists of two 

separate clumps, L1155 C1 and L1155 C2. The optically visible pre-main sequence star 

associated with L 1152 is HBC 695 (RNO 124), studied in detail by Movsessian et al. 

(2004). 

Recently Kauffmann et al. (2005), using the data base of the Spitzer Space Telescope 

Legacy Program From Molecular Cores to Planet Forming Disks (c2d, Evans 

et al. 2003) found a candidate sub-stellar (M ≪ 0.1M⊙) mass protostellar object in 

L 1148. The object L 1148–IRS coincides with IRAS F20404+6712. 

PV Cep The highly variable pre-main sequence star PV Cep lies near the northeastern 

edge of the dark cloud complex L 1147/L 1158. It is a bright IRAS source, and has been 

detected in radio continuum (Anglada et al. 1992). It illuminates a reflection nebula, 

known as GM–29 (Gyulbudaghian & Magakian 1977) and RNO 125 (Cohen 1980). 

A dramatic brightening of the star (an EXor-like outburst) was observed in the period 

1976–1978, and at the same time the shape of the associated nebula changed drastically 

(Cohen, Kuhi & Harlan 1977). 

The stellar parameters of PV Cep are somewhat uncertain. Most of its optical 

spectrograms available show no photospheric absorption features. Cohen et al. (1977), 

based on measurements of narrow-band continuum indices, estimated a spectral type 

about A5. Cohen et al. (1981) found the same spectral type based on the strength of the 

Hδ absorption line, apparent in two blue spectra. They note, however, that the hydrogen 

features probably represent merely a shell spectrum. Magakian & Movsessian (2001) 

estimated a spectral type of G8–K0, based on a spectrum taken in July 1978, when 

the star was some 2 magnitudes fainter than during the outburst. No other estimate of 

spectral type can be found in the literature (see Hernández et al. 2004, for a review). 

The spectral type of F, quoted by Staude (1986) and Neckel et al. (1987) is also based 

on the spectral information presented by Cohen et al. (1981). 

Cohen et al. (1981) found a distance of about 500 pc for PV Cep. Their estimate 

was based on three independent arguments. (1) PV Cep is probably related to 

NGC 7023. The spectroscopic and photometric data of its illuminating star, HD 200775, 

suggest a distance of 520 pc. (2) The spectroscopic and photometric data of the nebulous 

star RNO 124, located in the same cloud complex as PV Cep, suggest the same 

distance. (3) A similar distance can be obtained from the light travel time from the star 

to a nebular spike which brightened about a year after the outburst of the star. On the 

contrary, Straizys et al. (1992) obtained a distance of 325 pc for the L 1147/L 1158 dark 

cloud complex (see Table 3). 

The environment of the star shows a bipolar and rapidly changing optical morphology 

(Cohen et al. 1981; Neckel & Staude 1984; Staude 1986; Neckel et al. 1987; 

Levreault & Opal 1987; Scarrott et al. 1991a,b), as well as a bipolar CO outflow parallel 

to the symmetry axis of the reflection nebula (Levreault 1984). Neckel et al. (1987) detected 

several HH-knots, known as HH 215, emanating from PV Cep. Reipurth, Bally, 

& Devine (1997) and Gómez, Kenyon & Whitney (1997) discovered a giant (∼ 2.3 pc

long) Herbig-Haro flow, HH 315, consisting of 23 knots. HH 215 is also part of this 

giant flow. Reipurth, Bally, & Devine (1997) detected a further small knot, HH 415, located 

north-east of PV Cep, but this may be a dwarf galaxy with Hα redshifted into the 

[SII] passband (Bally, priv. comm.). Near-infrared spectroscopy of PV Cep is presented 

by Hamann & Persson (1994) and Greene & Lada (1996), and optical spectroscopy by 

Corcoran & Ray (1997). 

Far-infrared data obtained by ISOPHOT (Ábrahám et al. 2000) indicate the presence 

of an extended dust component on arcminute scale around PV Cep. The existence 

of a dust core close to PV Cep is also supported by the 13 CO (J=1–0) mapping of the 

region by Fuente et al. (1998b), who found a molecular core with a size of some 60 ′′ . 

27 

Figure 6. Optical image of a field of 36 ′ × 24 ′ of L 1082, obtained by Giovanni 

Benintende (http://www.astrogb.com/). 

L 1082 is a remarkable filamentary cloud (see Fig. 6), first catalogued by E. E. Barnard 

(1927) as Barnard 150. It appears as GF 9 in the catalog of globular filaments by 

Schneider & Elmegreen (1979). Several dense cores, namely L 1082 A,B,C (Myers et 

al. 1983), and LM99 349, 350, 351 (≡ L 1082 C), 352 (Lee & Myers 1999), as well as 

four IRAS sources, IRAS 20468+5953, 20503+6006, 20520+6003, and 20526+5958 

are found along the filament. A finding chart for the objects in L 1082 is given in Figure 

7. 

No distance determination is available in the literature for L 1082. Several authors 

assume that L 1082 is close to NGC 7023 not only on the sky, but also in space, and 

thus accept 440 pc as its distance (e.g. Ciardi et al. 1998). We note that the angular 

separation of 10 ◦ between NGC 7023 and L 1082 corresponds to 70 pc at the distance 

of NGC 7023. If both objects belong to the same complex, a similar difference can 

be expected between their distances. Wiesemeyer et al. (1997), based on statistical

28 

arguments, assume a distance of 100±50 pc. Furuya et al. (2003) refer to 150 pc, and 

Furuya et al. (2006) derive the physical parameters of GF 9–2 using 200 pc. Kun (2007) 

speculates that L 1082 may lie at the interaction region of the Local Bubble and Loop III 

(Cepheus Flare Shell). In this case its likely distance is about 150 pc. 

Ciardi et al. (1998) performed near-infrared observations of a core and a filament 

region within GF 9 (GF 9-Core and GF 9–Fila, see Fig. 7). They found that neither the 

core nor the filament contains a Class I or Class II YSO. The extinction maps of the two 

7 ′ × 7 ′ fields observed reveal masses 26 and 22 M⊙ in the core and the filament, respectively 

(at a distance of 440 pc). The core contains a centrally condensed extinction 

maximum that appears to be associated with IRAS 20503+6006, whereas GF 9–Fila 

does not show centrally peaked dust distribution. 

60 30 

IRAS 20520+6003 

L 1082 C 

[LM99] 351 

GF9−2 = IRAS 20503+6006 

[LM99] 350 

60 20 

IRAS 20526+5958 

[LM99] 349 

Dec(J2000) 

60 10 

L 1082 B 

L 1082 A 

[LM99] 352 

Core 

Fila 

IRAS 20468+5953 

60 00 

59 50 

20 55 20 54 20 53 20 52 20 51 20 50 20 49 20 48 20 47 

RA(J2000) 

Figure 7. Finding chart for the structure of L 1082, based on Poidevin & Bastien’s 

(2006) Fig. 1 and Wiesemeyer et al.’s (1998) Fig. 1. Crosses indicate the positions of 

the IRAS and ISOCAM point sources, open cirles mark the dense cores L 1082 A, B, 

and C (Benson & Myers 1989), diamonds show the dense cores catalogued by Lee 

& Myers (1999). Two rectangles show the regions GF 9 Core and GF 9 Fila, studied 

in detail by Ciardi et al. (1998; 2000). The size of the underlying DSS red image is 

70 ′ × 50 ′ . 

Wiesemeyer et al. (1998) presented mid-infrared ISOCAM observations of L 1082. 

They identified 9 sources along the filament, and designated them as GF 9–1, 2, 3a, 

3b, 4, 5, 6, I6, and 7. The designations probably follow Mezger (1994) who labeled 

dense cores along the filament by the same numbers. GF 9–2 coincides in position 

with IRAS 20503+6006, GF 9–3b with IRAS 20520+6003, GF 9–I6 with IRAS 

20468+5953, and GF 9–4 lies at 12 ′′ west of IRAS 20526+5958. They find that these 

latter two sources are Class 0 protostars, both associated with CO outflows, whereas

GF 9–6 and GF 9–7 are most likely reddened background stars. They speculate that the 

other ISOCAM sources, not associated with outflows, may be transitional objects between 

prestellar (Class −1) and Class 0 evolutionary stages. Wiesemeyer et al. (1999) 

presented far-infrared ISOPHOT and millimeter continuum measurements for GF 9–2, 

GF 9–3a/3b, and GF 9–4. 

Ciardi et al. (2000) performed CO, 13 CO, and CS observations of the GF 9–Core 

and GF 9–Fila regions, determined excitation temperatures, densities and masses. The 

CS observations reveal that both regions contain centrally condensed, high-density gas 

cores. The temperatures and masses of the two regions and of the cores contained within 

the regions are similar, but the densities in GF 9–Core are twice those of GF 9–Fila. 

De Gregorio Monsalvo et al. (2006) detected CCS emission from GF 9–2. The 

structure of the magnetic field associated with GF 9 was studied by Jones (2003) and 

Poidevin & Bastien (2006). 

Furuya et al. (2003) detected H 2 O maser emission from GF 9–2. Furuya et al. 

(2006) studied in detail the spatial and velocity structure of GF 9–2, using several 

molecular transitions obtained by single-dish and interferometric radio observations 

and 350 µm continuum data. The observations revealed a dense core with a diameter 

of ∼ 0.08 pc and mass of ∼ 3 M⊙. Within the core a protostellar envelope with a 

size of ∼ 4500 AU and mass of ∼ 0.6 M⊙ could be identified. The radial column 

density profile of the core can be well fitted by a power-law form of ρ(r) ∝ r −2 for the 

0.003 < r/pc < 0.08 region. The power-law index of −2 agrees with the expectation 

for an outer part of the gravitationally collapsing core. They found no jet-like outflow, 

but a compact, low-velocity outflow may have formed at the center. They discovered a 

potential protobinary system with a projected separation of ∼ 1200 AU, embedded in a 

circumbinary disk-like structure with ∼ 2000 AU radius at the core center. The binary 

consists of a very young protostar and a pre-protostellar condensation. The studies led 

to the conclusion that GF 9–2 is very likely at an extremely early stage of low-mass star 

formation before arriving at its most active outflow phase. 

Stecklum, Meusinger & Froebrich (2007) discovered 14 Herbig–Haro objects in 

the GF 9 region which apparently belong to at least three large HH-flows. Five HHobjects 

and GF 9–2 are linearly aligned, suggesting that they constitute an HH-flow 

driven by IRAS 20503+6006. Its overall length amounts to 43.5 arcmin, which corresponds 

to 2.3 pc for an assumed distance of 200 pc. The presence of a well-developed, 

parsec-scale outflow from GF 9–2 indicates a more advanced evolutionary stage of this 

source than previously believed. 

Furuya et al. (2008) mapped GF 9 in the NH 3 (1,1) and (2,2) inversion lines, using 

the Nobeyama 45-m telescope, with an angular resolution of 73 ′′ . The large-scale map 

reveal that the filament contains at least 7 dense cores, as well as 3 candidates, located 

at regular intervals of ∼ 0.9 pc (at an assumed distance of 200 pc). The cores have 

kinetic temperatures of ∼ < 10 K and LTE-masses of 1.8 – 8.2 M⊙, making them typical 

sites of low-mass star formation, probably formed via the gravitational fragmentation 

of the natal filamentary cloud. 

29 

NGC 7023 is a reflection nebula, illuminated by the young massive star 

HD 200775 and a group of fainter stars. It was discovered by William Herschel in 

1794. HD 200775 (also known as V380 Cep and HBC 726) is a Herbig Be star that has 

been extensively studied (e.g. Herbig 1960; Altamore et al. 1980; Pogodin et al. 2004; 

Alecian et al. 2008). The surrounding reflection nebula has been observed in detail (e.g.

30 

Slipher 1918; Witt & Cottrell 1980; Witt et al. 1982; Rogers et al. 1995; Laureijs et al. 

1996; Fuente et al. 2000; Werner et al. 2004; Berné et al. 2008). Figure 8 shows an 

optical image of the reflection nebula. 

Figure 8. Optical image of NGC 7023, illuminated by the Herbig Be star 

HD 200775. The size of the field is about 30 ′ × 20 ′ . Courtesy of Richard Gilbert of 

the Star Shadows Remote Observatory. 

Weston (1953) found that, centered on the reflection nebula, there is a small cluster 

consisting of stars which are variable and show Hα line in emission. Some two dozens 

of variable stars of the region were studied by Rosino & Romano (1962). Nevertheless, 

the HBC lists only four of these stars (HBC 726, 304, 306, 307, see Table 7) as 

confirmed T Tauri type stars. Recently Goodman & Arce (2004) speculated that the 

young Herbig Ae star PV Cep, located more than 10 pc to the west of the cluster, might 

have been ejected from NGC 7023 at least 100,000 years ago. HD 200775 is located 

at the northern edge of an elongated molecular cloud, corresponding to the dark clouds 

L 1167, 1168, 1170, 1171, 1172, 1173 and 1174, referred to as the L 1167/L 1174 complex. 

The cloud complex has been mapped in CO by Elmegreen & Elmegreen (1978). 

They found that the size of the cloud is 0.5 ◦ ×1.0 ◦ , or 3.9 pc×7.7 pc, and the mass of 

the molecular hydrogen is some 600 M⊙.

Table 7.: Pre-main sequence stars in the Cepheus Flare – (A) Classical T Tauri stars 

Names IRAS 2MASS J/ 2MASS magnitudes IRAS fluxes 

RA,Dec(J2000) J H K F(12) F(25) F(60) F(100) 

HBC 695n, RNO 124, K98 6 20359+6745 20361986+6756316 11.364 9.739 8.781 0.44 1.05 1.81 

GSC 04472-00143 20535+7439 20530638+7450348 10.149 9.405 8.861 0.42 0.63 0.68 

HH 200 IRS, L 1228 VLA 4 20570670+7736561∗ 

FT Cep, K98 26 20587+6802 20592284+6814437 10.588 9.342 8.532 0.55 0.92 0.89 

K98 30, OSHA 42 F20598+7728 20584668+7740256 11.513 10.365 9.699 0.09 0.16 

RNO 129 S1, OSHA 44, K98 32 21004+7811 20591409+7823040 9.437 7.530 6.319 6.23 11.12 36.30 76.60: 

RNO 129 S2, OSHA 44, K98 32 21004+7811 20591256+7823078 10.993: 12.060 9.174 

RNO 129 A 20590373+7823088 12.565 11.280 10.726 

HBC 304, FU Cep, LkHα 427 21009+6758 21014672+6808454 11.792 10.798 10.159 

K98 35, PRN S5 F21016+7651 21005285+7703149 11.290 10.288 9.773 0.12 0.15 0.34 

F21022+7729 21011339+7741091 12.676 11.202 10.327 0.08 0.13 0.17 

NGC 7023 RS 2 21012706+6810381 12.323 11.150 10.417 

NGC 7023 RS 2 21012637+6810385 11.107 10.084 9.571 

PW Cep, LkHα 425, NGC 7023 RS 3 21013590+6808219 12.336 11.564 11.052 

NGC 7023 RS 5 21014250+6812572 11.911 10.892 10.421 

LkHα 428, NGC 7023 RS 8 21022829+6803285 11.141 10.457 9.723 

HZ Cep, NGC 7023 RS S3 21014358+6809361 11.218 10.415 10.156 

HBC 306, FV Cep, LkHα 275, K98 38 F21017+6813 21022039+6825240 11.513 10.529 9.880 0.12 0.14 

PRN S1(b) 21012508+7706540 17.212: 14.640 13.156 

PRN S1(a) 21012638+7707029 16.460: 14.622 13.244 

OSHA 48, PRN S6 21012919+7702373 9.919 9.093 8.563 

OSHA 49, K98 40, PRN S7 F21023+7650 21013097+7701536 11.669 10.910 10.614 0.17 0.23 0.72 

OSHA 50, K98 41, PRN S8 21013267+7701176 11.993 11.060 10.419 0.08 0.08 0.09 

PRN S4 21013505+7703567 13.217 12.018 11.084 

PRN S2 21013945+7706166 15.399 14.007 12.973 

PRN S3 21014960+7705479 12.449 11.272 10.802 

OSHA 53, K98 43, PRN S9 F21028+7645 21020488+7657184 11.108 10.352 10.027 0.09 0.20 0.24 

FW Cep, NGC 7023 RS 9 21023299+6807290 11.559 10.713 10.411 

NGC 7023 RS 10 21023+6754 21025943+6806322 13.871 13.083 12.357 0.27 0.39 

K98 46 F21037+7614 21030242+7626538 11.585 10.843 10.471 0.13 0.18 

HBC 307, EH Cep, LkHα 276, K98 42 21027+6747 21032435+6759066 9.538 8.767 8.196 0.59 0.71 

∗ No 2MASS counterpart. 

31

Table 7.: Pre-main sequence stars in the Cepheus Flare – (A) Classical T Tauri stars (cont.) 

32 


RA/Dec(J2000) J H K F(12) F(25) F(60) F(100) 

OSHA 59, K98 49 F21066+7710 21055189+7722189 10.689 9.755 9.086 0.17 0.24 0.18 

K98 53 21153595+6940477 11.585 10.843 10.471 0.13 0.18 

K98 58 F21202+6835 21205785+6848183 14.318 13.035 11.866 0.20 5.49: 

RNO 135, K98 61 21326+7608 21323108+7621567 11.101 10.072 9.688 1.46 5.01 

K98 66 21355434+7201330 11.323 10.724 10.463 

K98 71 F21394+6621 21402754+6635214 11.344 10.540 10.046 0.34 0.64 2.56 

HBC 731, SVS 6 21425961+660433.8 12.886 11.624 10.948 

HBC 732, V350 Cep, MMN 13 21430000+6611279 12.714 11.691 11.008 

NGC 7129 S V1 21401174+6630198 13.161 12.173 11.591 

NGC 7129 S V2 21402277+6636312 13.882 12.671 11.890 

NGC 7129 S V3 21403852+6635017 13.108 11.888 11.267 

V391 Cep, K98 72 F21404+6608 21413315+6622204 11.680 10.555 9.750 0.36 0.40 

NGC 7129 MMN 1 21422308+6606044 15.059 14.050 13.394 

NGC 7129 HL85 14, MMN2 2 21423880+6606358 14.796 13.479 12.514 

NGC 7129 MMN 3 21424194+6609244 15.179 14.340 13.987 

NGC 7129 MMN 5 21425142+6605562 15.199 14.128 13.573 

NGC 7129 MEG 1 21425177+6607000 16.679 15.546 14.675 

NGC 7129 MMN 6 21425262+6606573 13.821 12.650 11.803 

NGC 7129 MMN 7 21425314+6607148 14.338 13.193 12.679 

NGC 7129 MMN 8 21425346+6609197 16.990 15.497 14.578 

NGC 7129 MMN 9 21425350+6608054 13.214 12.365 12.124 

NGC 7129 MMN 10 21425481+6606128 14.192 13.254 12.907 

NGC 7129 MEG 2 21425476+6606354 14.183 13.179 12.564 

NGC 7129 MMN 11 21425626+6606022 12.423 11.657 11.406 

RNO 138, V392 Cep 21425771+6604235 14.567: 14.478 13.658 

NGC 7129 MMN 12 21425810+6607394 14.299 13.532 13.030 

NGC 7129 MEG 3 21425878+6606369 13.487 12.561 12.337 

NGC 7129 MMN 14 21430024+6606475 14.161 12.778 12.085 

NGC 7129 MMN 15 21430246+6607040 14.004 13.109 12.256 

GGD 33A 21430320+6611150 16.619 15.461 14.337 

NGC 7129 MMN 17 21431162+6609115 12.605 11.800 11.487 

∗ No 2MASS counterpart.

Table 7.: Pre-main sequence stars in the Cepheus Flare – (A) Classical T Tauri stars (cont.) 



NGC 7129 MMN 18 

2143124+661238 ∗ 

NGC 7129 MMN 19 21431683+6605487 14.184 13.300 13.123 

NGC 7129 MMN 20 21433183+6608507 13.935 12.894 12.295 

NGC 7129 MMN 21 21433271+6610113 14.986 13.792 13.547 

NGC 7129 MMN 22 21434345+6607308 13.655 12.609 12.146 

K98 73 21443229+7008130 11.777 10.939 10.535 0.14 0.25 

K98 95 22131219+7332585 10.987 10.048 9.498 0.3 0.26 0.32 0.28 

GSC 04467-00835 22129+6949 2214068+7005043 9.620 9.072 8.753 0.254 0.567 0.484 0.50: 

K98 108 22190203+7319252 10.666 9.947 9.561 0.15 0.26 0.3 

K98 109 22190169+7346072 11.677 10.738 10.234 0.06 0.12 0.16 0.4 

K98 110 22190343+7349596 12.848 12.264 12.162 0.15 0.19 0.12 0.16 

K98 119 22256+7102 22265660+7118011 10.967 9.646 8.525 1.74 2.28 2.48 4.17 

KP 1, XMMU J223412.2+751809 22331+7502 22341189+7518101 10.095 8.808 7.827 

KP 39, XMMU J223516.6+751848 22351668+7518471 11.808 10.589 9.858 

KP 2, XMMU J223605.8+751831 22350+7502 2236059+7518325 11.957 10.894 10.253 

KP #10 22355+7505 2236345+7521352 11.984 10.628 10.026 0.11 0.24 0.23 

KP 43, XMMU J223727.7+751525 22372780+7515256 11.289 10.202 9.854 

KP 3, XMMU J223750.1+750408 22374953+7504065 11.785 10.974 10.680 

ETM Star 3, XMMU J223818.8+751154 22381872+7511538 11.248 9.815 8.912 

KP 44, ETM Star 1, XMMU J223842.5+751146 22384249+7511455 12.166 11.313 11.028 

KP 45, XMMU J22397.3+751029 22392717+7510284 11.748 10.851 10.377 

KP 46, XMMU J223942.9+750644 22385+7457 22394030+7513216 10.920 9.481 8.698 

GSC 04601-03483 F22424+7450 22433926+7506302 10.958 10.379 10.216 0.080 0.240 0.522 

K98 128 22490470+7513145 12.011 11.208 10.814 

TYC 4601-1543-1 22480+7533 22491626+7549438 9.938 9.256 8.727 0.61 0.90 0.81 

HBC 741, AS 507, K98 140 23189+7357 23205208+7414071 8.308 7.754 7.480 

∗ No 2MASS counterpart. 

33

34 

Table 7. 

Pre-main sequence stars the Cepheus Flare – (B) Herbig Ae/Be stars 

Names IRAS 2MASS J 2MASS magnitudes IRAS fluxes 


HBC 696n, PV Cep, K98 9 20453+6746 20455394+6757386 12.453 9.497 7.291 12.82 32.93 48.85 57.92 

HBC 726, HD 200775, MWC 361 21009+6758 21013691+6809477 6.111 5.465 4.651 26.700 76.800 638.000 1100.000 

HD 203024 21153+6842 21160299+6854521 8.377 8.209 8.120 3.680 10.800 4.260 

GSC 04461-01336, BD+68 ◦ 1118 21169+6842 21173917+6855098 9.269 8.741 8.105 1.570 3.480 4.130 2.59 

HBC 730, V361 Cep, AS 475, BD +65 ◦ 1637 21425018+6606352 8.973 8.729 8.474 

HBC 309, LkHα 234, V373 Cep 21418+6552 21430682+6606542 9.528 8.201 7.081 14.78 78.96 687.70 1215.00 

HBC 734, BH Cep, K98 83 22006+6930 22014287+6944364 9.686 8.993 8.310 0.524 1.200 1.390 

HBC 735, BO Cep, K98 100 F22156+6948 22165406+7003450 10.319 9.849 9.581 0.285 1.428 

HBC 736, SV Cep, K98 113 22205+7325 22213319+7340270 9.350 8.560 7.744 4.22 5.22 2.66 1.76 

GSC 04608-02063 22219+7908 22220233+7923279 11.509 10.920 10.266 

References to star names: NGC 7023 RS – variable stars from Rosino & Romano (1962); OSHA – Hα emission stars from Ogura & Sato (1990); KP – Hα emission 

star from Kun & Prusti (1993), Table 2; KP# – IRAS point source from Kun & Prusti (1993), Table 3; ETM – Eiroa et al. (1994); K98 – Hα emission stars from Kun 

(1998); NGC 7129 MEG – Miranda et al. (1993); NGC 7129 MMN – Magakian et al. (2004); PRN – Padgett et al. (2004); NGC 7129 S – Semkov (2003); XMMU – 

Simon (2006)

35 

Figure 9. 13 CO contours of the molecular cloud associated with NGC 7023, 

overplotted on the DSS red image (Elmegreen & Elmegreen 1978). Positions of 

HD 200775 and lower mass pre-main sequence stars, as well as the protostar IRAS 

21017+6742 are indicated. 

Watt et al. (1986) found a bipolar outflow associated with HD 200775. The region 

of the outflow has been mapped in 13 CO(1-0) by Fuente et al. (1998). These observations 

show that the star is located within a biconical cavity, which has probably been 

excavated by a bipolar outflow. However, Fuente et al. found no evidence for current 

high-velocity gas within the lobes of the cavity. 

Myers et al. (1988) detected another molecular outflow centered on the IRAS 

source IRAS 21017+6742. Hodapp’s (1994) K ′ image of the L 1172 outflow shows 

four stars associated with localized nebulosity. None of them are close to the nominal 

outflow position. Visser, Richer & Chandler (2002) detected three submillimeter

36 

sources at the position of IRAS 21017+6742: L 1172 SMM 1–SMM 3. They found that 

L 1172 SMM 1, located at RA(2000)=21 h 02 m 21.5 s , Dec(2000)=+67 ◦ 54 ′ 14 ′′ is a protostar 

and the driving source of the outflow, whereas SMM 2 and SMM 3 are starless 

dust clumps. Figure 9 shows the 13 CO contour map of the L 1167/L 1174 complex, 

adopted from Elmegreen & Elmegreen (1978). Known pre-main sequence stars of the 

region are also indicated. 

L 1177 (CB 230) contains a molecular outflow driven by the IRAS source 21169+6804 

(Yun & Clemens 1994). Near infrared observations by Yun (1996) revealed this source 

to be a binary protostar with a projected separation of 12 ′′ , and embedded in a common 

infrared nebula. The stars can be found near the center of a dense core whose size is 

about 360 ′′ (0.5 pc at 300 pc). Further CO and infrared studies can be found in Clemens, 

Yun & Heyer (1991). Submillimeter polarization measurements by Wolf, Launhardt & 

Henning (2003) reveal a magnetic field strength of 218 µG for the envelope of CB 230. 

Wolf et al. found that the outflow is oriented almost perpendicular to the symmetry 

axis of the globule core, whereas the magnetic field is parallel to the same axis. They 

discuss the possibility that the orientation of the magnetic field relative to the outflow 

directions reflects the evolutionary stage of the globule. Two A-type emission line stars, 

HD 203024 and BD +68 ◦ 1118 can be found to the north of the globule, at the edge of 

the diffuse outer part of the cloud. Their formation history may be connected to each 

other (Kun 1998). Miroshnichenko et al. (1997) and Kun, Vinkó & Szabados (2000) 

classify these objects as candidate Herbig Ae/Be stars, whereas Mora et al. (2001) state 

that they are main sequence stars. 

L 1228 is a small cloud stretching some 3 ◦ along a north-south direction. Its most 

probable distance is 180 pc (see Sect. 2.2.). L 1228 differs kinematically from the rest of 

the Cepheus Flare molecular clouds, suggesting that the cloud is located on the near side 

of the Cepheus Flare shell. Numerous Hα emission stars have been found around this 

cloud (Ogura & Sato 1990; Kun 1998), as well as several molecular outflows (Haikala 

& Laureijs 1989) and Herbig–Haro objects (Bally et al. 1995). 

The elongated cloud consists of three centers of star formation. 

(1) The northernmost part is a small, nebulous group of stars, RNO 129, associated 

with IRAS 21004+7811. Bally et al. (1995) found Herbig–Haro emission from 

RNO 129. A detailed study of RNO 129 can be found in Movsessian & Magakian 

(2004). Arce & Sargent (2006) included RNO 129 in their study of the evolution of 

outflow-envelope interactions in low-mass protostars. 

(2) The L 1228 core or L 1228 A contains the Class I source IRAS 20582+7724. A 

13 CO map of the cloud is presented in Miesch & Bally (1994). A dense core, mapped 

in ammonia by Anglada, Sepúlveda & Gómez (1997), contains at least two sources 

driving molecular outflows as well as two Herbig-Haro flows, HH 199 and HH 200, 

revealed by the Hα image of L 1228 A, obtained by Bally et al. (1995) and shown 

in Fig. 10. HH 199 emerges from IRAS 20582+7724, associated with an east–west 

oriented infrared reflection nebula (Hodapp 1994; Reipurth et al. 2000). Whereas the 

molecular outflow and the HH 199 flow have a position angle of about 60 ◦ , Hodapp 

(1994) and Bally et al. (1995) found a well-collimated H 2 emission flow at a position 

angle of about 100 ◦ . Either IRAS 20582+7724 is a possibly wide binary where each 

component is launching a separate flow, or one of the components of a very close binary 

is precessing rapidly, giving rise to the two very different flow angles. HH 200 is driven 

by an embedded T Tauri star about 1.5 arcmin further to the northwest (Bally et al.

37 

Figure 10. Hα + [SII] image of L 1228 A, based on KPNO 4 m images obtained 

with the Mosaic 1 prime focus CCD camera through narrow-band Hα and [SII] filters 

(80A passband). HH objects discussed in Bally et al. (1995) are marked. (Courtesy 

of John Bally). 

1995). A low-resolution 3.6 cm survey of the L 1228 cloud by Rodríguez & Reipurth 

(1996) revealed two sources. L 1228 VLA 1 is associated with the IRAS source, and 

the other, VLA 2, has no known counterpart but is located in the direction of the high 

extinction part of the L 1228 core. Reipurth et al. (2004) detected two further 3.6 cm 

sources, VLA 3 and VLA 4. VLA 4 is supposed to be the driving source of the HH 200 

flow. The environment of IRAS 20582+7724 was studied in detail by Tafalla & Myers 

(1997), Arce & Sargent (2004), and Arce & Sargent (2006). 

The K ′ image of L 1228 A, presented by Hodapp (1994), shows a star associated 

with a parabola-shaped nebula, located near the molecular outflow position. Two other 

stars further north at offsets (−21 ′′ ,72 ′′ ) and (12 ′′ ,75 ′′ ) are also associated with some 

less extended nebulae. The relatively bright stars in this region clearly stand out against 

the faint background stars, so that Hodapp classified this region as a cluster. 

(3) L 1228 South contains a small aggregate of low-mass pre-main sequence stars. 

Padgett et al. (2004) identified 9 infrared sources in the images taken with IRAC on 

board the Spitzer Space Telescope (see Table 7). 

L 1219 (B 175) is a small cometary shaped cloud at the southernmost edge of the 

Cepheus Flare cloud complex. The cloud is illuminated by the B9.5V type star BD +69 ◦ 

1231, associated with the reflection nebula Ced 201 (see Cesarsky et al. 2000, and references 

therein). Two cold IRAS sources, 22129+7000 and 22127+7014, are projected

38 

within the dark cloud. By an imaging and spectroscopic study Bally & Reipurth (2001) 

discovered a Herbig-Haro object, HH 450, emerging from IRAS 22129+7000. Furthermore, 

they found several parsec-scale filaments of emission that trace the rim of 

a new supernova remnant, G 110.3+11.3, which appears to be approaching the globule 

(see Figure 11). At 400 pc, G 110.3+11.3 is one of the closest known supernova 

remnants. The supernova remnant and the HH flow appear to be heading toward a 

frontal collision in about 1000 yr. Nikolić & Kun (2004) discovered a CO outflow from 

IRAS 22129+7000. Goicoechea et al. (2008) present Spitzer IRAC and MIPS data, 1.2- 

mm dust continuum map, as well as observations of several molecular lines for IRAS 

22129+7000. They detected a collimated molecular outflow in the CO J = 3 − 2 line, 

whereas the profile of the HCO + J = 1 − 0 line suggested inward motion. Based on 

the SED they classified the object as either a transition Class 0/I source or a multiple 

protostellar system. They discuss the role of the photodissociation region associated 

with Ced 201 in triggering the star formation in L 1219. 

Figure 11. Left: An image of B 175 (L 1219) from Bally & Reipurth (2001). 

Right: the map of visual extinction, obtained from the 2MASS data using the NICER 

algorithm of Lombardi & Alves (2001), shows the northern core of the cloud centered 

on IRAS 22127+7014. 

Three known pre-main sequence stars can be found to the south of L 1219: the 

Herbig Ae stars BH Cep and BO Cep (HBC 734 and 735, respectively) and a T Tauri 

star, associated with IRAS 22129+6949. The head of the cometary globule with IRAS 

22129+7000 is pointing toward south. The embedded source IRAS 21127+7014, located 

to the north of IRAS 22129+7000, may be the youngest object associated with 

this cloud. The left panel of Fig. 11 shows the head of the globule B 175 and the supernova 

filaments, adopted from Bally & Reipurth (2001), and the right panel shows the 

extinction map of the whole cloud, revealing another core to the north. 

L 1221 is a small, isolated cometary dark cloud to the south of the main body of 

the Cepheus Flare cloud complex. No distance determination has been published for 

this cloud. A frequently assumed distance is 200 pc (e.g. Fukui 1989; Umemoto et al. 

1991). Inside the cloud, Umemoto et al. (1991) found an unusual U-shaped CO outflow

associated with a low-luminosity (2.7L⊙) Class I source, IRAS 22266+6845. More recent 

CO observations at high resolution showed that the U-shaped outflow may actually 

consist of two bipolar outflows, an east-west outflow associated with the IRAS source 

and a north-south outflow about 25 ′′ to the east of the IRAS source, interacting with 

each other (Lee et al. 2002). To the south of the IRAS source, a fairly bright compact 

object, HH 363, is detected in Hα and [S II] (Alten et al. 1997). There are three infrared 

sources within the error ellipse of the IRAS source: a close binary consisting of an east 

source and a west source around the IRAS source position and another source 45 ′′ to 

the southeast. The east source is identified as the IRAS source. Furuya et al. (2003) 

detected H 2 O maser emission associated with IRAS 22266+6845. Lee & Ho (2005) 

mapped IRAS 22266+6845 in 3.3 mm continuum, CO, HCO + , and N 2 H + . Continuum 

emission is seen around the east source and the southeast source at 3.3 mm, probably 

tracing the dust around them. Assuming a temperature of 40 K, the masses of the dust 

plus gas are estimated to be 0.02 and 0.01 M⊙ around the east source and southeast 

source, respectively. No continuum emission is seen toward the west source. The east– 

west outflow is likely powered by the east source, which shows a southeast extension 

along the outflow axis in the K ′ image (Connelley et al. 2007). Wu et al. (2007) detected 

two submillimeter sources in the cloud, L 1221 SMM 1 and L 1221 SMM 2, 

apparently coinciding with the binary and the southeast source, respectively. 

L 1251 is a cloud elongated east–west at the eastern boundary of the Cepheus Flare 

molecular complex. Its cometary shape suggests interaction with the supernova bubble 

described by Grenier et al. (1989). Recent star formation is indicated by two molecular 

outflows, driven by IRAS 22343+7501 and IRAS 22376+7455, respectively (Sato & 

Fukui 1989). 

The distance of L 1251 was determined by three different methods (see Table 3). 

The cloud has been mapped in several molecular lines, such as 13 CO, C 18 O, H 13 CO + , 

SiO (Sato et al. 1994), NH 3 (Benson & Myers 1989; Tóth & Walmsley 1996), HNC, 

HCN, HCO + , CS (Nikolić, Johansson, & Harju 2003). Kun & Prusti (1993) studied the 

YSO population and reported on 12 Hα emission stars and IRAS point sources as YSO 

candidates. Balázs et al. (1992) discovered an optical jet, HH 149, originating from 

IRAS 22343+7501. Rosvick & Davidge (1995) found that this IRAS source is associated 

with a cluster of five near-infrared sources spread over a 10 ′ × 10 ′ area (sources 

A–E). Meehan et al. (1998) found two thermal radio continuum sources, VLA A and 

VLA B, coinciding with the near infrared sources D and A, respectively. Beltrán et 

al. (2001) found 9 radio continuum sources around IRAS 22343+7501, two of them, 

VLA 6 and VLA 7 separated by 7 ′′ , are located within the error ellipse of the IRAS 

source and identical with Meehan et al.’s VLA A and VLA B, respectively. Beltrán et 

al. found a third source, VLA 5 to be a probable YSO, based on the positive spectral index. 

Nikolić et al. (2003) concluded that both VLA 6 and VLA 7 are protostars driving 

their own outflow. 

The high resolution VLA observations by Reipurth et al. (2004) revealed four radio 

continuum sources in the region around IRAS 22343+7501, three of which were known 

from previous studies. The high resolution VLA A map has revealed a new source, 

VLA 10, close to VLA 6, with which it was blended in the earlier low-resolution data 

of Meehan et al. (1998). The designations VLA 10 and 11 is a continuation of the 

numbering scheme of Beltrán et al. (2001). Meehan et al. (1998) suggest that VLA 6 

corresponds to the very red and embedded source IRS D, while VLA 7 is the brighter 

source IRS A. 

39

40 

Eiroa et al. (1994) discovered a chain of Herbig–Haro objects, HH 189A,B,C near 

IRAS 22376+7455 (L 1251 B). The Spitzer Space Telescope observed L 1251 B as part 

of the Legacy Program From Molecular Cores to Planet Forming Disks (Evans et al. 

2003) at wavelengths from 3.6 to 70 µm. The observations revealed a small cluster 

of protostars, consisting of 5 Class 0/I and 14 Class II objects (Lee et al. 2006). 

Three Class 0/I objects are projected on IRAS 22376+7455, the most luminous is 

located 5 ′′ north of the IRAS position. Thus the molecular outflow observed from 

IRAS 22376+7455 (Sato & Fukui 1989) is probably a combined effect of more outflows. 

Lee et al. (2007) studied the complex motions in the region, based on both 

single-dish and interferometric molecular line observations. The data have shown very 

complex kinematics including infall, rotation, and outflow motions. The well-known 

outflow, associated with L 1251 B, was resolved into a few narrow and compact components. 

They detected infall signatures in the shape of HCO + , CS, and HCN lines 

to the east of L 1251 B, where no infrared object has been detected, and an extended 

emission has been found at 850 µm. This result shows that, in addition to the Class 0– 

Class II objects, the young cluster contains a pre-protostellar core as well. Results of 

spectroscopic follow-up observations of the optically visible candidate YSOs reported 

by Kun & Prusti (1993) are given in Eredics & Kun (2003). Simon (2006) detected 

41 X-ray sources in the image obtained with the XMM-Newton telescope. The list of 

X-ray sources contains both outflow sources and 8 optically visible T Tauri stars. 

The structure of the cloud and the properties of its dust grains were studied, based 

on optical extinction maps, by Kandori et al. (2003) and Balázs et al. (2004). 

Young et al. (2006) and Wu et al. (2007) observed submm sources associated with 

the dense cores L 1251 A, B, and C. 

L 1261/L 1262 (CB 244) are small clouds to the east of the main body of the Cepheus 

Flare cloud complex, at a probable distance of 180 pc from the Sun (Kun 1998). Two 

young, low luminosity objects, the G2 type classical T Tauri star HBC 741 (AS 507) 

and the cold IRAS source IRAS 23238+7401 are projected on the cloud. A CO outflow 

centered on IRAS 23238+7401 was found by Parker et al. (1988). Wolf et al.’s 

(2003) submillimeter polarization measurements resulted in a magnetic field strength 

of 257 µG for the envelope of CB 244. 

2.5. NGC 7129 

Though NGC 7129 lies in the Cepheus Flare, it is more distant than the clouds discussed 

above. NGC 7129 (Ced 196) is a reflection nebula in the region of a young cluster, 

containing three B-type stars, namely BD +65 ◦ 1637, BD +65 ◦ 1638, and LkHα 234, as 

well as several low-mass pre-main sequence stars (e.g. Herbig 1960; Strom, Vrba & 

Strom 1976; Cohen & Schwartz 1983; Magakian, Movsessian & Nikogossian 2004, 

see Table 7). Whereas BD +65 ◦ 1638 is regarded a young main sequence star (but see 

Matthews et al. 2003), BD +65 ◦ 1637 and LkHα 234 are pre-main sequence stars (Herbig 

1960; Hernández et al. 2004). An optical image of NGC 7129, displaying several 

spectacular signposts of the interactions between the young stars and their environments, 

is shown in Fig. 12. A finding chart for the most prominent objects, related to 

star formation, is displayed in Fig. 13. 

LkHα 234 and its environments It has been suggested that LkHα 234 is the youngest 

among the three B-type stars (Hillenbrand et al. 1992). This star and its environment

41 

Figure 12. An optical image of NGC 7129, displaying the young cluster, embedded 

in a reflection nebula, as well as several HH objects. The size of the area is about 

15 ′ × 18 ′ . Photograph by Robert Gendler. 

have been studied extensively at optical, infrared, radio, centimeter to submillimeter 

wavelengths. Photometric and spectroscopic variability of LkHα 234 have been studied 

by Shevchenko et al. (1991) and Chakraborty & Mahadevan (2004), respectively. 

Wilking et al. (1986) presented high-resolution continuum and molecular-line observations 

of the circumstellar environment of LkHα 234. Sandell & Olofsson (1981) 

and Tofani et al. (1995) detected three H 2 O maser sources from the environment of

42 

LkHα 234. Ray et al. (1990) identified an optical jet originating from this region. 

Mitchell & Matthews (1994) detected a molecular jet associated with LkHα 234, and 

Schultz et al. (1995) observed shocked molecular hydrogen in the LkHα 234 region. 

VLA observations by Trinidad et al. (2004) of water masers and radio continuum emission 

at 1.3 and 3.6 cm show that the LkHα 234 region contains a cluster of YSOs. In 

a field of ∼ 5 ′′ they detected five radio continuum sources (VLA 1, VLA 2, VLA 3A, 

VLA 3B, and LkHα 234) and 21 water maser spots. These water masers are mainly 

distributed in three clusters associated with VLA 1, VLA 2, and VLA 3B. The VLA 

observations suggest that there are at least four independent, nearly parallel outflows in 

the LkHα 234 region. Probably all sources observed in this region (∼ 5 ′′ in diameter) 

form a cluster of YSOs, which were born inside the same core in the NGC 7129 molecular 

cloud. This fact could explain that the major axes of the outflows have nearly 

the same orientation. Marvel (2005) performed VLBI observations of maser sources 

around LkHα 234, and detected maser emission associated with LkHα 234–VLA 2 

and LkHα 234–VLA 3b. No maser source associated with LkHα 234 itself has been 

detected. 

Tommasi et al. (1999) obtained far-infrared spectra of the LkHα 234 region, using 

the Long Wavelength Spectrograph of ISO. The observed spectra are consistent with a 

photodissociation region, associated with not LkHα 234, but with BD +65 ◦ 1637. Morris 

et al. (2004) have obtained mid-IR spectroscopy of regions around LkHα 234, with 

the Spitzer Space Telescope Infrared Spectrograph (IRS). They detected warm material 

at 16 µm around BD +65 ◦ 1638 which clearly shows that this region is not free of gas 

and dust. Wang & Looney (2007) identified a group of low-mass young stars around 

LkHα 234 using the Spitzer data base. 

Interstellar matter associated with NGC 7129 Molecular line observations of the region 

(Bechis et al. 1978; Font, Mitchell & Sandell 2001; Miskolczi et al. 2001; Ridge 

et al. 2003) revealed a kidney-shaped molecular cloud of about 11 pc in extent to the 

east and south of the cluster. BD +65 ◦ 1637 and most of the fainter cluster members 

are found in a cavity of the cloud, bordered by a prominent molecular ridge, while 

LkHα 234, located to the east of the main cluster, is associated with a peak of 13 CO 

emission. The optical jet detected by Ray et al. (1990) is pointing southwest into the 

cavity. Torrelles et al. (1983) and Güsten & Marcaide (1986) presented ammonia observations 

of NGC 7129. 

Matthews et al. (2003) observed the region in the 21 cm line of H I with an angular 

resolution of 1 ′ . The observations revealed a ring of H I emission about 30 ′ in extent. 

The H I ring appears to be part of the surface of a molecular cloud and is centered on a 

relatively dense concentration of H I with unusually wide line profiles and positionally 

coincident with BD +65 ◦ 1638. An infrared point source, IRAS 21418+6552, coincides 

within the positional errors with the H I knot. 

A continuum source coincident with BD +65 ◦ 1638 has also been detected at 1420 

MHz, which shows a significant extension to the northeast overlapping the position 

of LkHα 234. Comparing the radio continuum data with other radio observations of 

BD +65 ◦ 1638, Matthews et al. (2003) found that BD +65 ◦ 1638 has a flat centimeterwave 

spectrum, consistent with an optically thin H II region around the star. The authors 

conclude that the physical association of the star with the H I knot indicates that 

BD +65 ◦ 1638 belongs to a rare class of “dissociating stars”, having an extremely young 

age of not more than a few thousand years. BD +65 ◦ 1638 itself is found to be a 6 M⊙ 

star that has just emerged from its cocoon and lies on the birthline.

43 

66 14 

GGD 33a,b 

V350 Cep 

66 12 

66 10 

Dec(J2000) 

66 08 

66 06 

66 04 

66 02 

GGD 35 

BD +65 o 1638 

GGD 34 

MM 4 

HH 105 

LkHα 234 

= FIRS 1 

MM 5 

SVS 6 

MM 3 

MM 2 

RNO 138 

FIRS 2 

BD +65 o 1637 

MM 1 

Molecular Ridge 

GGD 32 

HH 103 

21 44 00 21 43 30 21 43 00 21 42 30 21 42 00 

RA(J2000) 

Figure 13. A DSS 2 red image of NGC 7129 in which the crude position of the 

molecular ridge, bordering the cluster, is overplotted by white cross-dashed lines. 

The B-type cluster members, HH objects, and some interesting low-mass young stars 

are labeled. Crosses indicate the far-infrared sources FIRS 1 and FIRS 2, and diamonds 

stand for the compact millimeter sources detected by Fuente et al. (2001) 

outside the FIRS 1 and FIRS 2 regions. 

Embedded young stellar objects in NGC 7129 Bechis et al. (1978) identified two 

far-infrared sources in NGC 7129: FIRS 1 coincides with LkHα 234, while FIRS 2, 

a deeply embedded protostellar object is located three arcminutes to the south of the 

cluster, at the primary peak of the 13 CO emission. It was found to coincide with an 

H 2 O maser (Cesarsky et al. 1978; Rodríguez et al. 1980b; Sandell & Olofsson 1981). 

NGC 7129 FIRS 2 has not been detected in the optical and near infrared. From the 

far-infrared and submillimeter observations, Eiroa, Palacios & Casali (1998) derived a 

luminosity of 430 L⊙, a dust temperature of 35 K, and a mass of 6 M⊙. The low dust 

temperature and the low L bol /L 1.3 mm ratio of this source suggest that it is an intermediate 

mass counterpart of Class 0 sources. Fuente, Neri & Caselli (2005a) detected a hot

44 

molecular core associated with FIRS 2, and Fuente et al. (2005b) carried out a molecular 

survey of FIRS 2 and LkHα 234 with the aim of studying the chemical evolution of 

the envelopes of intermediate-mass young stellar objects. Fuente (2008) present high 

angular resolution imaging of the hot core of NGC 7129 FIRS 2, using the Plateau de 

Bure Interferometer. This is the first chemical study of an intermediate-mass hot core 

and provides important hints to understand the dependence of the hot core chemistry 

on the stellar luminosity. 

Two molecular outflows were found in NGC 7129 by Edwards & Snell (1983). 

They seem to be associated with LkHα 234 and FIRS 2. Weintraub et al. (1994), via 

near infrared polarimetry, identified a deeply embedded source, NGC 7129 PS 1, located 

about 3 ′′ northwest of LkHα 234. This source was not identified in the direct 

near-infrared images of LkHα 234, which revealed 5 sources (IRS 1–IRS 5, IRS 1 ≡ 

LkHα 234) in a 20 ′′ × 20 ′′ field centered on LkHα 234. Weintraub et al. (1996) detected 

NGC 7129 PS 1 at 3.8 µm, and proposed that it was the actual outflow source 

instead of LkHα 234. 

Cabrit et al. (1997) present high-resolution imaging of the region around LkHα 234 

in the 10 µm and 17 µm atmospheric windows and in the H 2 v=1-0 S(1) line and adjacent 

continuum. The cold mid-infrared companion, detected at 2.7 ′′ to the north-west 

of the optical star, corresponds to NGC 7129 PS 1. The companion illuminates an arcshaped 

reflection nebula with very red colors, and is associated with a radio continuum 

source, H 2 O masers, and a bright extended H 2 emission knot, indicating that it is deeply 

embedded and has strong outflow activity. Cabrit et al. (1997) refer to this star as IRS 6, 

extending Weintraub et al.’s notation. 

Fuente et al. (2001) obtained single-dish and interferometric continuum images at 

2.6 mm and 1.3 mm of both FIRS 2 and LkHα 234. They identified two millimeter 

sources associated with FIRS 2: FIRS 2–MM1, apparently associated with the CO outflow, 

and a weaker source, FIRS 2–MM2, which does not present any sign of stellar activity. 

The interferometric 1.3 mm continuum image of FIRS 1 reveals that LkHα234 is 

a member of a cluster of embedded objects. Two millimeter clumps are associated with 

this far-infrared source. The stronger is spatially coincident with IRS 6. A new millimeter 

clump, FIRS 1–MM1, is detected at an offset (−3.23 ′′ , 3.0 ′′ ) from LkHα 234. The 

extremely young object FIRS 1–MM1 (it has not been detected in the near- and midinfrared) 

is the likely driving source of the H 2 jet. There is no evidence for the existence 

of a bipolar outflow associated with LkHα 234. In addition to FIRS 1 and FIRS 2, six 

other compact millimeter clumps are detected in the region, NGC 7129 MM1 to MM5 

(see Fig. 13), and the sixth coincides with the bipolar nebula RNO 138. 

Submillimeter continuum observations by Font et al. (2001) revealed three compact 

sources: LkHα 234 SMM 1, LkHα 234 SMM 2 and FIRS 2. SMM 1 coincides 

with IRS 6, which, according to the submillimeter observations, may be a deeply embedded 

Herbig Be star, whereas SMM 2 is a newly discovered source (see Figure 14). 

Table 8 shows the coordinates, wavelengths of detection, measured fluxes and sizes of 

the deeply embedded young stellar objects in NGC 7129, observed in submillimeter, 

millimeter, and centimeter continuum. 

Low-mass pre-main sequence members of NGC 7129 were identified as Hα emission 

objects by Hartigan & Lada (1985), Miranda et al. (1993), and Magakian et al. (2004), 

as variable stars (Semkov 2003) and near-infrared sources (Strom et al. 1976; Cohen 

& Schwartz 1983). Muzerolle et al. (2004) presented observations of NGC 7129 taken 

with the Multiband Imaging Photometer for Spitzer (MIPS). A significant population

45 

Table 8. Embedded YSOs in NGC 7129. 

Name RA(2000) Dec(2000) λ(mm) Flux(mJy) Ref. 

NGC 7129 FIRS1 IRS6 21 43 06.4 66 06 55.6 2.6 91 1 

NGC 7129 FIRS1 IRS6 21 43 06.5 66 06 55.2 1.3 313 1 

NGC 7129 FIRS1 MM 1 21 43 06.3 66 06 57.4 1.3 180 1 

LkHα 234 21 43 06.8 66 06 54.4 1.3 < 20 1 

NGC 7129 FIRS2 MM 1 21 43 01.7 66 03 23.6 2.6 72 1 

21 43 01.7 66 03 23.6 1.3 381 1 

NGC 7129 FIRS2 MM 2 21 43 01.6 66 03 26.1 2.6 22 1 

21 43 01.7 66 03 24.7 1.3 137 1 

NGC 7129 FIRS2 IR 21 43 01.8 66 03 27.4 2.6

46 

Figure 14. Dust continuum emission of NGC 7129, observed at 850 µm by Font 

et al. (2001). Near-infrared sources are marked by star symbols, and H 2 O maser 

sources by triangles. 

source of RNO 138. Another interesting star is V350 Cep (denoted as IRS 1 by Cohen 

& Schwartz 1983), which brightened about 4 mag in the 1970’s (Semkov 2004), and 

has been staying at the high level since then. Liseau & Sandell (1983) detected CO 

outflows associated with both RNO 138 and V350 Cep. Herbig (2008) has shown that 

V350 Cep does not belong to the class of the EXor-type eruptive young stars. The 

list of low-mass pre-main sequence stars in NGC 7129, based on a literature search, is 

given in Table 7. 

Herbig–Haro objects In the optical, a large number of HH-objects in and near NGC 

7129 have been reported (Gyulbudaghian, Glushkov & Denisyuk 1978; Hartigan & 

Lada 1985; Eiroa, Gómez de Castro & Miranda 1992; Gómez de Castro, Miranda & 

Eiroa 1993; Miranda, Eiroa, & Birkle 1994; Gómez de Castro & Robles 1999, see 

Table 9). Molecular hydrogen emission in the near-infrared has been detected from

47 

Figure 15. Mosaic of the NGC 7129 region in the 1-0 S(1) line of H 2 + cont. at 

2.12 µm, adopted from Eislöffel (2000). Emission from several molecular outflows, 

as well as from a probable photodissociation region to the east and south of the stellar 

cluster can be seen. Some H 2 outflows and H 2 counterparts of optical Herbig–Haro 

objects are labeled. 

several of the optical Herbig–Haro objects (Wilking et al. 1990). An infrared search 

for the exciting sources of the optical HH objects was presented by Cohen & Schwartz 

(1983). Spectroscopic observations of HH objects are presented by Cohen & Fuller 

(1985). Fuente et al. (2001) suggest that NGC 7129 MM4 is the illuminating star of the 

nebular object GGD 34. Eislöffel (2000) used deep imaging in the near-infrared 1-0 

S(1) line of H 2 at 2.12 µm to search for parsec-scale outflows in NGC 7129 (Fig. 15). 

They identified numerous outflows (see Table 9), but likely driving sources could be 

identified for only three of them. For most of the other emission-line knots and molecular 

flows no evident sources could be identified. The Spitzer observations revealed 

several distinct outflow arcs, traced by 4.5 µm bright knots, associated with FIRS 2 

(Muzerolle et al. 2004). The multipolar nature of this outflow system, in general agreement 

with the outflow analysis of Fuente et al. (2001), supports the claim by Miskolczi 

et al. (2001) that FIRS 2 is a multiple protostellar system.

48 

Table 9. Herbig–Haro objects in NGC 7129. 

name RA(2000) Dec(2000) Source Reference 

HH 822 21 41 42.1 +66 01 45 LkHα 234 5 

HH 103A 21 42 23.8 +66 03 47 LkHα 234 5,13 

HH 103B 21 42 24.7 +66 03 40 LkHα 234 1,13 

HH 232, GGD 32 21 42 26.9 +66 04 27 6,8 

HH 242 21 42 38.7 +66 06 36 6,10,12 

HH 825 21 42 39.2 +66 10 56 IRAS 21416+6556 5 

HH 238 21 42 40.3 +66 05 41 LkHα 234 6,10 

HH 237 21 42 42.3 +66 05 23 LkHα 234 6,10 

HH 239 21 42 44.1 +66 06 37 LkHα 234 6,10 

HH 824 21 42 56.9 +66 09 10 IRAS 21416+6556 4,10 

HH 236 21 42 59.2 +66 07 39 LkHα 234 6,10 

HH 233, GGD 33 21 43 00.0 +66 12 00 GGD 33a 1,3,13 

HH 167 21 43 06.7 +66 06 54 LkHα 234 4 

HH 105B 21 43 19.8 +66 07 53 LkHα 234 1,6,9 

HH 105A 21 43 22.1 +66 07 47 LkHα 234 1,6,9 

HH 823 21 43 27.9 +66 11 46 4 

HH 234 21 43 29.7 +66 08 38 6 

GGD 34 21 43 30.4 +66 03 43 NGC 7129 MM 4 1,2,7,11 

HH 235, GGD 35 21 43 42.0 +66 09 00 6,8,13 

HH 821 21 43 43.4 +66 08 47 LkHα 234 5 

HH 820 21 43 47.9 +66 09 50 LkHα 234 5 

HH 818 21 43 57.7 +66 10 26 LkHα 234 5 

HH 819 21 44 01.0 +66 09 52 LkHα 234 5 

HH 817 21 44 13.3 +66 10 55 LkHα 234 5 

HH 816 21 44 26.4 +66 10 58 LkHα 234 5 

HH 815 21 44 29.9 +66 13 42 LkHα 234 5 

References: 1 – Eiroa, Gómez de Castro & Miranda (1992); 2 – Gómez de Castro & Robles (1999); 3 – 

Miranda, Eiroa, & Birkle (1994); 4 – Moreno-Corral, Chavarría-K., & de Lara (1995); 5 – McGroarty et 

al. (2004); 6 – Wu et al. (2002); 7 – Gómez de Castro et al. (1993); 8 – Cohen & Schwartz (1983); 9 – 

Hartigan & Lada (1985); 10 – Miranda et al. (1993); 11 – Fuente et al. (2001); 12 – Avila et al. (2001); 13 

– Cohen & Fuller (1985). 

3. Star Formation in the Association Cep OB2 

The association Cep OB2 was discovered by Ambartsumian (1949). Simonson (1968) 

identified 75 bright members, including the runaway O6 Iab star λ Cep (HIP 109556). 

The clusters NGC 7160 and Trumpler 37 (Tr 37), with its associated H II region IC 1396 

(Fig. 16), have similar distances as Cep OB2, about 800 pc. Simonson & van Someren 

Greve (1976) suggested the division of Cep OB2 into two subgroups. The younger subgroup, 

Cep OB2b is Tr 37, one of the youngest known open clusters, with an age of 

3.7 Myr (e.g., Marschall, Karshner & Comins 1990). Garrison & Kormendy (1976) 

suggested that the bright star µ Cep (HIP 107259, M2 Ia) is a member of Tr 37. The 

main source of excitation of IC 1396 is the O6 star HD 206267 (HIP 106886), a Trapeziumlike 

system (Harvin 2004). IC 1396 and neighboring areas contain a large number of 

Hα emission objects (e.g. Kun 1986; Kun & Pásztor 1990; Balázs et al. 1996), classical 

T Tauri stars (Sicilia-Aguilar et al. 2004, 2005) and several globules containing embedded 

young stellar objects (e.g., Duvert et al. 1990; Schwartz, Wilking & Gyulbudaghian 

1991). The other subgroup, Cep OB2a, contains a large number of evolved massive

stars that are spread over a large area, between 100 ◦ ≤ l ≤ 106 ◦ and +2 ◦ ≤ b ≤ +8 ◦ . 

The age of this subgroup is about 7-8 Myr, and contains NGC 7160. This subgroup is 

surrounded by a 9 ◦ diameter infrared emission ring, the Cepheus Bubble (see Fig. 2), 

which possibly resulted from a supernova explosion (Kun et al. 1987). This supernova 

might have triggered star formation in the ring, as suggested by the presence of several 

H II regions, and a number of infrared sources that have the characteristics of embedded 

young stellar objects (Balázs & Kun 1989). 

49 

Figure 16. 

De Martin. 

Optical image of the HII region IC 1396. Color composite by Davide

50 

De Zeeuw et al. (1999) determined the distance of Cep OB2, based on Hipparcos 

results on 76 members (one O, 56 B, 10 A, five F, one G, two K, and one M type stars). 

They obtained a mean distance of 615±35 pc. 

Daflon et al. (1999) studied the chemical abundances of OB stars in Cep OB2. 

Their results indicate that this association is slightly metal-poor. The highest mass 

association members have been involved in several studies of the interstellar matter in 

the region of the association. Clayton & Fitzpatrick (1987) detected anomalous dust in 

the region of Tr 37, by studying the far-ultraviolet extinction curves of 17 early-type 

stars. In order to measure the value of R V = A V /E B−V , Roth (1988) combined nearinfrared 

photometry of OB stars with existing optical and ultraviolet data of the same 

sample. The results suggest anomalous grain size distribution with respect to an average 

Galactic extinction curve. Morbidelli et al. (1997) performed VRIJHK photometry of 

14 bright cluster members. They obtained the normal Galactic value of R V = 3.1. 

In order to establish the velocity structure and column density of the interstellar 

matter in the region of Cep OB2, Pan et al. (2004; 2005) studied several interstellar 

absorption lines in high resolution spectra of early-type association members. Their 

results are consistent with the large-scale structure suggested by radio molecular maps, 

and suggest significant variations in the column density on small (∼ 10000 AU) scales. 

Cep OB2 was mapped in the 21 cm line of HI by Simonson & van Someren Greve 

(1976). They detected an HI concentration of 2 × 10 4 M⊙ surrounding the HII region 

and bright-rimmed dark clouds associated with Cep OB2b, and found no significant 

amount of neutral hydrogen associated with Cep OB2a. Wendker & Baars (1980) constructed 

a three-dimensional model of the ionized region based on a 2695 MHz radio 

continuum map. The first molecular study of IC 1396 was performed by Loren, Peters 

& Vanden Bout (1975). Heske & Wendker (1985) surveyed the dark clouds of IC 1396 

in the 6 cm absorption line of the H 2 CO. Large-scale 12 CO and 13 CO mapping of the 

dark clouds in IC 1396 are presented by Patel et al. (1995) and Weikard et al. (1996). 

Both IC 1396 and NGC 7160 have been included in the CO survey of regions around 

34 open clusters performed by Leisawitz, Bash, & Thaddeus (1989). 

The low and intermediate mass members of Cep OB2 belong to different populations, 

born in various subgroups during the lifetime of the association. Significant low 

mass populations, born together with and thus nearly coeval with the high luminosity 

members, are expected in both Cep OB2b and Cep OB2a. Younger subgroups are being 

born in the clouds bordering the HII region IC 1396, due to triggering effects by the 

luminous stars of Cep OB2b. 

3.1. Pre-main Sequence Stars in the Open Cluster Tr 37 

Marschall & van Altena (1987) derived kinematic membership probabilities for stars 

of Tr 37, and identified 427 probable members. Marschall et al. (1990) performed 

UBV (RI) C photometry of 120 members, most of them brighter than V ≈ 13.5. Their 

HR diagram indicated a number of probable pre-main sequence members. 

During a search for intermediate mass pre-main sequence members of Tr 37, Contreras 

et al. (2002) found three emission-line stars (MVA 426, MVA 437, and Kun 314S). 

They suggest that the low frequency of emission-line activity in the sample of B–A type 

stars indicates that inner disks around intermediate-mass stars evolve faster than those 

of low-mass stars. 

Sicilia-Aguilar et al. (2004), based on spectroscopic and photometric observations 

of candidate objects, presented the first identifications of low-mass (spectral types K–

M) pre-main sequence members of Tr 37 and NGC 7160. They expanded the studies 

in a second paper (Sicilia-Aguilar et al. 2005). In all, they identified and studied 130 

members of Tr 37, and ∼30 for NGC 7160. They confirmed previous age estimates of 

4 Myr for Tr 37 and 10 Myr for NGC 7160, and found active accretion in ∼40% of the 

stars in Tr 37, with average accretion rates of 10 −8 M⊙yr −1 , derived from their U-band 

excesses. These results expand the existing samples of accreting stars. Only 1 accreting 

star was detected in the older cluster NGC 7160, suggesting that disk accretion ends 

before the age of 10 Myr. 

In order to follow the evolution of protoplanetary accretion disks through the ages 

∼3–10 Myr, Sicilia-Aguilar et al. (2006a) utilized the wavelength range 3.6–24 µm, 

offered by the IRAC and MIPS instruments of the Spitzer Space Telescope. They found 

detectable disk emission in the IRAC bands from 48% of the low mass stars of Tr 37. 

Some 10% of these disks have been detected only at wavelengths > 4.5 µm, indicating 

optically thin inner disks. Comparison of the SEDs of Tr 37 members with those of the 

younger Taurus region indicates that the decrease of infrared excess is larger at 6–8 µm 

than at 24 µm, suggesting that disk evolution is faster at smaller radii. 

Sicilia-Aguilar et al. (2004, 2005) also investigated the spatial asymmetries in 

Tr 37 and the possible presence of younger populations triggered by Tr 37 itself. They 

found a spatial east-west asymmetry in the cluster that cannot yet be fully explained. 

The low-mass Tr 37 members are concentrated on the western side of the O6 star 

HD 206267. In contrast, the B-A stars (Contreras et al. 2002) are more uniformly distributed, 

with a small excess to the east. Both the high and intermediate-mass stars 

and the low-mass stars show a clear “edge” to the east of HD 206267. The youngest 

stars are found preferentially on the western side of HD 206267. The presence of dense 

globules in this region suggests that the expansion of the HII region into an inhomogeneous 

environment triggered this later epoch of star formation. Larger amounts of 

interstellar material on the western side may also have helped to shield disk systems 

from the photoevaporating effects of the central O6 star. 

Sicilia-Aguilar et al. (2006b) obtained high-resolution spectra of a large number 

of stars in the region of Tr 37. They derived accretion rates from the Hα emission line, 

and found lower average accretion rate in Tr 37 than in the younger Taurus. They used 

radial velocities as membership criterion, and thus confirmed the membership of 144 

stars and found 26 new members. They also calculated rotational velocities, and found 

no significant difference between the rotation of accreting and non-accreting stars. In 

order to study the dust evolution in protoplanetary disks, Sicilia-Aguilar et al. (2007) 

studied the 10 µm silicate feature in the Spitzer IRS spectra of several members of 

Tr 37. GM Cep, a solar-type member of Tr 37 exhibiting EXor-like outbursts, was 

studied in detail by Sicilia-Aguilar et al. (2008). 

Tr 37 was searched for X-ray sources as possible WTTSs by Schulz, Berghöfer 

& Zinnecker (1997). Soft X-ray observations with the ROSAT PSPC revealed X-ray 

emission from an area of 30 ′ radius around the center of globule IC 1396A, which was 

resolved into 85 discrete sources of which 13 sources were identified as foreground 

objects. Most of the detected X-ray sources, except HD 206267, are very weak, which 

causes the measured luminosity function to be cut off at logL x < 30.3 erg s −1 . X-ray 

sources are located not only in Tr 37 but are also scattered around the molecular globules 

IC 1396A and B (see Sect. 3.2.). Their X-ray spectra appear hard with luminosities 

between log L∼ 30 and 31. LkHα 349, a 10 5 yr old pre-main sequence star at the very 

51

52 

center of globule A, appears very luminous with L x = 5.1 × 10 30 erg s −1 . The source 

density within 5 ′ of the center of emission is 270 sources per square degree. 

Getman et al. (2007) detected 117 X-ray sources in a field centered on the globule 

IC 1396N (see Sect. 3.2.), of which 50-60 are likely members of Trumpler 37. 

Table 10. A. Bright rimmed globules and dark clouds associated with IC 1396. 

Names 

RA(J2000) D(J2000) IRAS Source Ref. 

[h m] [ ◦ ′ ] 

FSE 12 21 25 57 53 

FSE 13 21 25 58 37 

FSE 1, IC 1396 W 21 26 57 58 21246+5743 4,14,16,17 

FSE 14, LDN 1086 21 28 57 31 

BRC 32 21 32 24 57 24 08 21308+5710 

BRC 33, Pottasch IC 1396C 21 33 12 57 29 33 21316+5716 

BRC 34, GRS 3, Pottasch IC 1396D 21 33 32 58 03 29 21320+5750 

GRS 1 21 32 25 57 48 44 

FSE 2, GRS 2 21 33 54 57 49 44 21312+5736 

FSE 15 21 33 59 30 

FSE 16, LDN 1102 21 33 58 09 

FSE 3, LDN 1093, LDN 1098, 21 34 11 57 31 06 21324+5716 29 

GRS 4, Pottasch IC 1396B 

Weikard Rim I 21 34 35 58 19.5 

FSE 4, Pottasch IC 1396A, 21 36 12 57 27 34 21346+5714 5,6,7,14,19, 

GRS 6, BRC 36 29,32,33 

GRS 5, BRC 35 21 36 05 58 32 17 21345+5818 

FSE 5, LDN 1099, LDN 1105, GRS 6 21 36 54 57 30 21352+5715 

FSE 6, LDN 1116 21 37 58 37 21354+5823 

FSE 17, LDN 1088, GRS 9 21 38 56 56 07 36 

GRS 7 21 37 56 57 47 57 

Weikard Rim J 21 38 56 56 21.3 

FSE 7, GRS 12, BRC 37, 21 40 25 56 35 52 21388+5622 8,9,10,11,14,20, 

Pottasch IC 1396H 25,28,31,33,34 

WB89 108 21 40 38 56 48 21390+5634 

GRS 13 21 40 30 57 46 28 

GRS 14 21 40 41 58 15 52 

FSE 19, IC 1396 N(orth), LDN 1121, 21 40 43 58 20 09 21391+5802 1,2,3,13,14,15, 

GRS 14, WB89 110, 18,25,30,32 

BRC 38, Pottasch IC 1396E 

FSE 8, GRS 20, LDN 1130, 21 44 00 58 17 00 21428+5802 29 

Pottasch IC 1396F 

GRS 26 21 44 51 57 08 00 

GRS 23 21 45 05 56 59 22 21443+5646 

GRS 24 21 45 09 56 47 52 

LDN 1132 21 45 45 58 29.3 

GRS 25, WB89 122 21 45 58 57 13 54 21436+5657 

GRS 27 21 46 03 57 08 41 

GRS 28 21 46 27 57 18 07 

FSE 9, IC 1396 E(ast), 21 46 38 57 25 55 21445+5712 14,21,25,33 

WB89 123, LDN 1118, GRS 29, 

BRC 39, Pottasch IC 1396 G 

BRC 40 21 46 14 57 08 59 21446+5655 

BRC 41 21 46 29 57 18 41 21448+5704 

BRC 42 21 46 37 57 12 25 21450+5658 

FSE 21, LDN 1129 21 46 27 57 46 37 

FSE 22 21 49 56 43 

References to globule names and column 5 can be found under Table 10 B.

53 

Table 10. 

uncertain. 

B. Other clouds in the IC 1396 region whose relation to Cep OB2 is 

Names 

RA(J2000) D(J2000) IRAS source Ref. 

[h m] [ ◦ ′ ] 

FSE 18, LDN 1131 21 40 59 34 

FSE 20, LDN 1131 21 41 59 36 

FSE 10, LDN 1139 21 55 36 58 35 21539+5821 14 

FSE 23, LDN 1153 22 01 58 54 

FSE 11, LDN 1165, LDN 1164 22 07 00 59 02 22051+5848 

GRS 32, LDN 1165 22 07 00 59 00 22051+5848 12,14,15,22,23, 

24,25,26,27,28 

FSE 24, LBN 102.84+02.07 22 08 58 23 

FSE 25, LBN 102.84+02.07 22 08 58 31 

References to globule names: Pottasch–Pottasch (1956); GRS–Gyulbudaghian (1985); WB89–Wouterloot 

& Brand (1989); BRC–Sugitani et al. (1991); Weikard–Weikard et al. (1996); FSE–Froebrich et al. (2005). 

References to column 5. 1. Beltrán et al. (2002); 2. Nisini et al. (2001); 3. Codella et al. (2001); 4. 

Froebrich & Scholz (2003); 5. Nakano et al. (1989); 6. Hessman et al. (1995); 7. Reach et al. (2004); 

8. Duvert et al. (1990); 9. Sugitani et al. (1991); 10. de Vries et al. (2002); 11. Ogura et al. (2002); 12. 

Reipurth & Bally (2001); 13. Reipurth et al. (2003); 14: Schwartz et al. (1991); 15: Reipurth, Bally, & 

Devine (1997); 16: Froebrich et al. (2003); 17: Zhou et al. (2006); 18: Getman et al. (2007); 19: Sicilia- 

Aguilar et al. (2006a); 20: Sugitani et al. (1997); 21: Serabyn et al. (1993); 22: Reipurth & Aspin (1997); 

23: Tapia et al. (1997); 24: Parker et al. (1991); 25: Connelley et al. (2007), 26: Visser et al. (2002); 27: 

Slysh et al. (1997); 28: Bronfman et al. (1996); 29: Moriarty-Schieven et al. (1996); 30: Neri et al. (2007); 

31: Ogura et al. (2007); 32: Valdettaro et al. (2005); 33: Valdettaro et al. (2008); 34: Ikeda et al. (2008). 

Dec(J2000) 

59 30 

59 00 

58 30 

58 00 

57 30 

L1165 

FSE 25 

FSE 24 

L1153 

L1139 

L1131 

E (IC 1396 N) 

µ Cep 

L1132 

I 

F 

L1112 

G 

B161 A 

D 

C 

B 

FSE 2 

IC 1396W 

L1086 

57 00 

56 30 

FSE 22 

H 

B367 

B163 

HD 206267 

L1088 

22 10 22 05 22 00 21 55 21 50 21 45 21 40 21 35 21 30 21 25 

RA(J2000) 

Figure 17. Distribution of the globules listed in Table 10 and other dark clouds 

projected near IC 1396, overplotted on a DSS red image of the region (open circles). 

Star symbols show the embedded protostars, and plusses mark the IRAS sources of 

uncertain nature (Schwartz et al. 1991). 

J 

B365

54 

3.2. Star Formation in Globules of IC 1396 

The HII region IC 1396 is powered by the O6.5 V star HD 206267. It appears that the 

expansion of this HII region has resulted in sweeping up a molecular ring of radius 

12 pc (Patel et al. 1998). Patel et al. derive an expansion age of the molecular ring of 

about 3 Myr. 

The ring-like HII region, shown in Fig. 16, is some 3 ◦ in diameter and is surrounded 

by a number of bright-rimmed globules which are probable sites of triggered 

star formation due to compression by ionization/shock fronts and radiation pressure. 

Many bright rimmed clouds harbor IRAS point sources of low dust temperature. They 

also frequently contain small clusters of near-IR stars. The most prominent globules 

are located in the western and northern portions of the H II region. 

The globules of IC 1396 received different designations during various studies. 

Pottasch (1956) labeled the most prominent bright rimmed globules with letters from 

A to H, in the order of their increasing distance from the exciting star. Weikard et 

al. (1996) supplemented this list by rims I and J. IC 1396A corresponds to the famous 

Elephant Trunk Nebula. Gyulbudaghian (1985) identified 32 globules in the region of 

Cep OB2, and designated them as GRS (globules of radial systems) 1–32. Four radial 

systems of globules have been identified near IC 1396. One system, consisting of 

16 globules, is centered on IC 1396. Another system of 12 globules, slightly south of 

IC 1396, appears to be associated with BD +54 ◦ 2612, whereas two further radial systems 

have been identified to the east and south-east of the main system of globules surrounding 

HD 206267. The system associated with HD 206267 is dominated by brightrimmed 

globules with diffuse tails generated by the radiation field of HD 206267. The 

other systems appear as opaque globules without rims. The systems partially overlap 

spatially. Gyulbudaghian, Rodríguez & Cantó (1986) have surveyed the GRS globules 

for CO emission. They found that the radial systems separate in radial velocity. The 

mean LSR velocity of the HD 206267 system is −2.8 ± 2.4 km s −1 , whereas the same 

for the BD+54 ◦ 2612 system is +6.5 ± 1.0 km s −1 . Two of the globules, GRS 12 and 

GRS 14, are associated with H 2 O masers (Gyulbudaghian, Rodríguez & Curiel 1990). 

Schwartz et al. (1991) used the IRAS data base to locate young stellar object candidates 

associated with the globules of IC 1396. They found that only six globule-related 

sources have point-like structure and luminosities considerably in excess of that which 

can be caused by external heating. Most of the IRAS point sources associated with the 

globules are probably externally heated small-scale dust structures not related to star 

formation. Eleven globules of IC 1396 can be found in the catalog of bright rimmed 

clouds by Sugitani, Fukui & Ogura (1991) (BRC 32–42). Froebrich et al. (2005) presented 

a large-scale study of the IC 1396 region using new deep NIR and optical images, 

complemented by 2MASS data. They identified 25 globules (FSE 1–25) using extinction 

maps and the list of Schwartz et al. (1991). Four of them were previously uncatalogued 

in the SIMBAD database. In all but four cases the masses (or at least lower 

limits) of the globules could be determined, and the size could be measured properly for 

all but seven objects. For ten globules in IC 1396 they determined (J−H, H−K) colorcolor 

diagrams and identified the young stellar population. Five globules contain a rich 

population of reddened objects, most of them probably young stellar objects. The five 

globules with many red objects include the targets with the highest extinction values, 

suggesting a correlation of the strength of the star formation activity with the mass of 

the globule.

Moriarty-Schieven et al. (1996) have made the first arcminute resolution images 

of atomic hydrogen toward IC 1396, and have found remarkable “tail”-like structures 

associated with the globules IC 1396A, B and F, extending up to 6.5 pc radially away 

from the central ionizing star. These H I “tails” may be material which has been ablated 

from the globule through ionization and/or photodissociation and then accelerated away 

from the globule by the stellar wind, but which has since drifted into the “shadow” of 

the globules. 

Star formation in small globules is often thought to be strongly influenced by the 

radiation pressure of a nearby bright star. Froebrich et al. therefore investigated how 

the globule properties in IC 1396 depend on the distance from the O star HD 206267. 

The masses of the globules have clearly shown positive correlation with the distance 

from this star, suggesting that evaporation due to photo-ionization affects the mass distribution 

of the globules around HD 206267. Their data are consistent with a scenario 

in which the radiation pressure from the O-type star regulates the star forming activity 

in the globules, in the sense that the radiation pressure compresses the gas and thus 

leads to enhanced star formation. 

The names and coordinates of the known globules of IC 1396, as well as their 

associated IRAS sources are listed in Table 10, and the distribution of the same objects 

with respect to the HII zone is shown in Fig. 17. Some of the globules in IC 1396 were 

already investigated in detail and/or are known to harbor outflow sources. We give 

references for the works on individual globules in the last column of the table. 

Ogura et al. (2002) performed Hα grism spectroscopy and narrow band imaging 

observations of the BRCs listed by Sugitani et al. (1991) in order to search for candidate 

pre-main sequence stars and Herbig-Haro objects. They have detected a large number 

of Hα emission stars down to a limiting magnitude of about R = 20. Their results for 

IC 1396 are reproduced in Table 11, and the finding charts for the Hα emission stars are 

shown in Fig. 18. Submillimeter observations of bright rimmed globules are presented 

by Morgan et al. (2008). 

The primary indicators of star formation in the globules are the embedded IRAS 

point sources, molecular outflows and Herbig–Haro objects. Table 12 lists the Herbig– 

Haro objects found for the IC 1396 region. 

3.3. Notes on Individual Globules 

IC 1396 W lies about 1. ◦ 75 W–NW of HD 206267. In the center of the small (about 

6 ′ ) dark cloud, the IRAS source 21246+5743 can be found. This source is not detected 

at 12 µm. The very red IRAS colors and the extended appearance in the 100 µm IRAS 

image suggest a young, deeply embedded source. Observations of this object with the 

photometer ISOPHOT confirmed that IRAS 21246+5743 is a Class 0 source that will 

reach about one solar mass on the main sequence (Froebrich & Scholz 2003). The 

ISOPHOT maps at 160 and 200 µm show two further cold objects (2.5 arcmin SW and 

NE, respectively) in the vicinity of the central source. This might be an indication of 

other newly forming stars or cold dust in the IC 1396 W globule. 

Froebrich & Scholz (2003) have observed the IC 1396 W globule in J, H, K ′ , and 

a narrow band filter centered on the 2.122 µm 1-0 S(1) line of molecular hydrogen. 

They detected three molecular outflows in the field. The flow axes are parallel within 

3 ◦ in projection. Magnetic fields cannot consistently explain this phenomenon. A 

parallel initial angular momentum of these objects, caused by the fragmentation of 

small clouds/globules, might be the reason for the alignment. NIR photometry, IRAS 

55

56 

Table 11. Hα emission stars associated with bright rimmed clouds in IC 1396, 

identified by Ogura et al. (2002), and revised by Ikeda et al. (2008) 

N RA(J2000.0) Dec(J2000.0) EW N RA(J2000.0) Dec(J2000.0) EW 

BRC 33 BRC 38 

1 21 34 19.8 57 30 01 53.4 4 21 40 31.7 58 17 55 · · · 

2 21 34 20.8 57 30 47 3.3 5 21 40 36.7 58 13 46 4.0 

3 21 34 49.2: 57 31 25: 66.2 6 21 40 37.0 58 14 38 63.3 

BRC 34 7 21 40 37.2 58 15 03 29.8 

1 21 33 29.4 58 02 50 43.0 8 21 40 40.5 58 13 43 · · · 

2 21 33 55.8 58 01 18 · · · 9 21 40 41.3 58 15 11 26.1 

BRC 37 10 21 40 41.7 58 14 25 14.8 

1 21 40 25.3 56 36 43 · · · 11 21 40 45.0 58 15 03 75.7 

2 21 40 26.1 56 36 31 18.4 12 21 40 48.1 58 15 38 19.0 

3 21 40 26.8 56 36 23 40.9 13 21 40 48.9 58 15 00 · · · 

4 21 40 27.2 56 36 30 · · · 14 21 40 49.0 58 15 12 · · · 

5 21 40 27.4 56 36 21 · · · 15 21 40 49.2 58 17 09 22.2 

6 21 40 28.2 56 36 05 · · · 16 21 41 02.0 58 15 25 · · · 

7 21 40 28.8 56 36 09 78.8 BRC 39 

8 21 40 32.4 56 38 39 14.4 1 21 45 50.3 57 26 49 · · · 

BRC 38 2 21 46 01.6 57 29 38 3.1 

1 21 40 26.2 58 14 24 22.2 3 21 46 07.1 57 26 31 13.0 

2 21 40 27.4 58 14 21 59.3 4 21 46 26.0 57 28 28 · · · 

3 21 40 28.1 58 15 14 20.7 5N 21:45:54.08 57:28:18.5 9.3 

and ISOPHOT observations (Froebrich et al. 2003) led to the discovery of the driving 

sources of the outflows. The brightest outflow is driven by the Class 0 source IRAS 

21246+5743. Two flows are driven by more evolved Class I/II objects. The JHK photometry 

of the globule also revealed a population of young stars, situated mainly in a 

dense embedded subcluster, about 2.5 arcmin south-west of IRAS 21246+5743. This 

cluster coincides with a clump of dense gas. The other young stars are almost uniformly 

distributed in the observed field. 

Zhou et al. (2006) mapped IC 1396 W in the CO(1-0) line, and found that its 

CO molecular cloud may consist of three physically distinct components with different 

velocities. They detected neither molecular outflows nor the dense cores associated 

with candidate driving sources. One possible reason is that CO(1-0) and its isotopes 

cannot trace high density gas, and another is that the beam of the observation was too 

large to observe them. The CO cloud may be part of the natal molecular cloud of 

IC 1396 W, in the process of disrupting and blowing away. The CO cloud seems to be 

in the foreground of the H 2 outflows. 

IC 1396A, Elephant Trunk nebula contains an intermediate mass (M ∼ 3 M⊙, Sp. 

type: F9 – Hernández et al. 2004) pre-main sequence star, LkHα 349 (Herbig & Rao 

1972; Hessman et al. 1995) and a K7 type T Tauri star LkHα 349c (Cohen & Kuhi 

1979; Herbig & Bell 1988). No other YSOs were known before the Spitzer Space 

Telescope. Radio continuum maps of IC 1396A at 6 cm and 11 cm were obtained by 

Baars & Wendker (1976). The maps suggested the presence of an HII region within the 

globule.

57 

Figure 18. Hα emission stars in bright rimmed globules of IC 1396, found by 

Ogura et al. (2002). Top: BRC 33, BRC 34; middle: BRC 37, BRC 38(≡ IC 1396 N); 

bottom: BRC 39. The position of the IRAS source associated with the globule is 

drawn by a pair of thick tick marks.

58 

Table 12. Herbig–Haro objects in IC 1396 

name RA(J2000) Dec(J2000) source Ref. 

HH 864 A 21 26 01.4 57 56 09 IRAS 21246+5743 1 

21 26 02.0 57 56 09 IRAS 21246+5743 1 

HH 864 B 21 26 07.9 57 56 03 IRAS 21246+5743 1 

HH 864 C 21 26 21.3 57 57 40 IRAS 21246+5743 1 

21 26 18.6 57 57 12 IRAS 21246+5743 1 

HH 588SW2D 21 40 10.5 56 33 46 IRAS 21388+5622 2 

HH 588SW2C 21 40 12.2 56 34 08 IRAS 21388+5622 2 

HH 588SW2A 21 40 16.7 56 33 55 IRAS 21388+5622 2 

HH 588SW2B 21 40 18.4 56 34 16 IRAS 21388+5622 2 

HH 777 21 40 21.6 58 15 49 IRAS 21391+5802 3 

HH 778 21 40 22.8 58 19 19 3 

HH 588SW1A 21 40 24.6 56 35 07 IRAS 21388+5622 2 

HH 588SW1B 21 40 26.6 56 34 40 IRAS 21388+5622 2 

HH 588SW1C 21 40 27.5 56 34 55 IRAS 21388+5622 2 

HH 588 21 40 29.1 56 35 55 IRAS 21388+5622 2 

HH 588NE1B 21 40 32.1 56 36 25 IRAS 21388+5622 2 

HH 588NE1C 21 40 32.1 56 36 30 IRAS 21388+5622 2 

HH 588NE1A 21 40 33.5 56 36 16 IRAS 21388+5622 2 

HH 588NE1D 21 40 33.5 56 36 32 IRAS 21388+5622 2 

HH 588NE1E 21 40 34.6 56 36 33 IRAS 21388+5622 2 

HH 589C 21 40 35.0 58 14 37 IRAS 21391+5802 2 

HH 590 21 40 35.1 58 17 52 2 

HH 591 21 40 35.8 58 18 21 2 

HH 592 21 40 36.8 58 17 02 2 

HH 589A 21 40 37.5 58 14 45 IRAS 21391+5802 2 

HH 589B 21 40 37.7 58 14 25 IRAS 21391+5802 2 

HH 593 21 40 45.2 58 16 09 2 

HH 588NE2E 21 40 45.6 56 37 15 IRAS 21388+5622 2 

HH 588NE2D 21 40 47.8 56 37 02 IRAS 21388+5622 2 

HH 779 21 40 47.9 58 13 35 3 

HH 588NE2C 21 40 49.0 56 37 07 IRAS 21388+5622 2 

HH 588NE2B 21 40 49.3 56 37 09 IRAS 21388+5622 2 

HH 588NE2A 21 40 49.7 56 37 27 IRAS 21388+5622 2 

HH 780 21 40 53.1 58 14 16 3 

HH 594 21 40 53.8 58 17 02 2 

HH 595 21 41 00.2 58 16 52 2 

HH 588NE3 21 41 00.0 56 37 19 IRAS 21388+5622 1 

21 41 01.0 56 37 25 IRAS 21388+5622 1 

HH 865A 21 44 28.5 57 32 01 IRAS 21445+5712 1 

21 44 29.3 57 32 24 IRAS 21445+5712 1 

HH 865B 21 45 10.5 57 29 51 IRAS 21445+5712 1 

GGD 36 21 58 30.0 58 56 00 4 

HH 354 22 07 42.5 59 11 53 IRAS 22051+5848 1,5 

References. 1 – Froebrich et al. (2005); 2 – Ogura et al. (2002); 3 – Reipurth et al. (2003); 4 – Gyulbudaghian 

et al. (1987); 5 – Reipurth, Bally, & Devine (1997). 

Spitzer Space Telescope images at 3.6, 4.5, 5.8, 8, and 24 µm (Reach et al. 2004) 

revealed this optically dark globule to be infrared-bright and to contain a set of previously 

unknown protostars. The mid-infrared colors of the sources detected at 24 µm 

indicate several very young (Class I or 0) protostars and a dozen Class II stars. Three of 

the new sources (IC 1396A γ, 1396Aδ, and 1396Aǫ) emit over 90% of their bolometric 

luminosities at wavelengths longer than 3 µm, and they are located within 0.02 pc of 

the ionization front at the edge of the globule. Many of the sources have spectra that are 

still rising at 24 µm. The two previously known young stars LkHα 349 and 349c are 

both detected, with component c harboring a massive disk and LkHα 349 itself being

are. About 5% of the mass of the globule is presently in the form of protostars in the 

10 5 –10 6 yr age range. 

The globule mass was estimated to be 220 M⊙ from a high-resolution CO map 

(Patel et al. 1995), much smaller than the virial mass, estimated as 300–800 M⊙ (Patel 

et al. 1995; Weikard et al. 1996). 

59 

Figure 19. YSOs in IC 1396A, discovered by Spitzer Space Telescope (Sicilia- 

Aguilar et al. 2006a), overplotted on the DSS red image of the globule. Circles mark 

Class I, and star symbols Class II sources. Diamonds mark uncertain members. 

Sicilia-Aguilar et al. (2006a), based on IRAC and MIPS photometry, identified 57 

YSOs born in the Elephant Trunk. Most of them have no optical counterparts. Based on 

the color indices and the shape of the SEDs, Sicilia-Aguilar et al. identified 11 Class I 

and 32 Class II objects. Their average age is about 1 Myr. The surface distribution of 

these objects is displayed in Fig. 19, adopted from Sicilia-Aguilar et al. (2006a). 

Valdettaro et al. (2005, 2008) detected H 2 O maser emission from the direction 

of IRAS 21345+5714, associated with IC 1396A. Probably each protostar observed by 

Spitzer contribute to the fluxes of the IRAS source. 

BRC 37, IC 1396H High resolution 12 CO, 13 CO and CS observations of this globule 

have been performed by Duvert et al. (1990). They detected a bipolar outflow and 

identified the possible optical counterpart of the driving source IRAS 21388+5622. 

Sugitani et al. (1997) reported on interferometric 13 CO observations of BRC 37. They 

found evidence of interaction with the UV radiation from the exciting star of IC 1396. 

Bronfman et al. (1996) included IRAS 21388+5622 in their CS(2–1) survey of IRAS 

point sources with color characteristic of ultracompact H II regions. In order to study 

the age distribution of stars Ogura et al. (2007) undertook BV I c JHK s photometry 

of stars in and around some bright rimmed globules including BRC 37. Their results 

indicate that star formation proceeds from the exciting star outward of the HII region. 

Ikeda et al. (2008) carried out near-IR/optical observations of BRC 37 in order to study

60 

the sequential star formation in the globule. Several results published by Ogura et al. 

(2002) are revised in the paper. Valdettaro et al. (2008) detected H 2 O maser emission 

from IRAS 21388+5622. 

IC 1396N Serabyn et al. (1993) estimated the density and temperature structure of 

this globule (they use the designation IC 1396E), and found evidence of the possibility 

that recent internal star formation was triggered by the ionization front in its southern 

surface. On the basis of NH 3 data, gas temperatures in the globule are found to 

increase outward from the center, from a minimum of 17 K in its tail to a maximum 

of 26 K on the surface most directly facing the stars ionizing IC 1396. Sugitani et al. 

(2000) performed 2 mm continuum observations of IC 1396N (BRC 38). Codella et al. 

(2001) reported mm-wave multiline and continuum observations of IC 1396N. Singledish 

high resolution observations in CO and CS lines reveal the cometary structure of 

the globule with unprecedented detail. The globule head contains a dense core of 0.2 

pc, whereas the tail, pointing away from the exciting star, has a total length of 0.8 pc. 

Two high velocity bipolar outflows have been identified in the CO maps: the first one 

is located around the position of the strong infrared source IRAS 21391+5802 in the 

head of the globule, and the second one is located in the northern region. The outflows 

emerge from high density clumps which exhibit strong line emission of CS, HCO + , 

and DCO + . The sources driving the outflows have been identified by mm-wave continuum 

observations (e.g. Beltrán et al. 2002). The globule head harbors two YSOs 

separated by about 10 4 AU. SiO line observations of the central outflow unveil a highly 

collimated structure with four clumps of sizes pc, which are located along the outflow 

axis and suggest episodic events in the mass loss process from the central star. 

Nisini et al. (2001) presented near infrared images of IC 1396N in the H 2 2.12 µm 

narrow band filter as well as in broad band J, H, and K filters. They detected several 

chains of collimated H 2 knots inside the globule, having different luminosities 

but similar orientations in the sky. Most of the knots are associated with peaks of 

high velocity CO emission, indicating that they trace shocked regions along collimated 

stellar jets. From the morphology and orientation of the H 2 knots, they identify at 

least three different jets: one of them is driven by the young protostar associated with 

IRAS 21391+5802, while only one of the two other driving sources could be identified 

by means of near infrared photometry. The NIR photometry revealed the existence of a 

cluster of young embedded sources located in a south-north line which follows the distribution 

of the high density gas and testifies to a highly efficient star formation activity 

through all the globule. Valdettaro et al. (2005) and Furuya et al. (2003) detected H 2 O 

maser emission from IC 1396N. 

Saraceno et al. (1996) present a far-infrared spectrum of IRAS 21391+5802, together 

with submillimeter and millimeter photometry. A rich spectrum of CO, OH, and 

H 2 O lines are detected in the ISO-LWS spectrum, indicative of a warm, dense region 

around the source. They also obtained an accurate measure of the bolometric luminosity 

and an estimate of the total envelope mass. 

Reipurth et al. (2003) identified a major Herbig-Haro flow, HH 777, that is bursting 

out of the IC 1396N cometary cloud core. Near- and mid-infrared images reveal a very 

red object embedded in the center of the core, located on the symmetry axis of the large 

HH 777 flow, suggesting that this is likely the driving source. The projected separation 

of the working surface from the source is 0.6 pc. Additionally, 0.4 pc to the east of the 

source and on the flow axis, there is a faint, previously known HH object (HH 594) that

61 

HH 778 

HH 777 IRS 

HH 777 

HH 780 

HH 779 

Figure 20. Members of the young cluster born in IC 1396N, overplotted on the 

DSS red image of the globule. Star symbols show the X-ray sources associated with 

Class II objects, plusses mark those corresponding to Class I objects (Getman et 

al. 2007), diamonds show the Hα emission stars detected by Ogura et al. (2002), 

and open circles indicate the near-infrared sources found by Nisini et al. (2001). 

Positions of the HH objects, discovered by Reipurth et al. (2003), are indicated and 

a large thick cross shows the position of HH 777 IRS. 

may be part of the counterflow (Ogura et al. 2002). It thus appears that we are seeing a 

blowout of a parsec-scale flow into the surrounding H II region. 

IC 1396N has been observed with the ACIS detector on board the Chandra X-Ray 

Observatory (Getman et al. 2007). 25 of the 117 detected X-ray sources are associated 

with young stars formed within the globule. Infrared photometry (2MASS and 

Spitzer) shows that the X-ray population is very young: 3 older Class III stars, 16 classical 

T Tauri stars, and 6 protostars including a Class 0/I system. The total T Tauri 

population in the globule, including the undetected population, amount to ∼30 stars, 

which implies a star formation efficiency of 1%-4%. Four of the X-ray-selected members 

coincide with near-infrared sources reported by Nisini et al. (2001), and 9 of them 

correspond to Hα emission stars detected by Ogura et al. (2002). An elongated spatial 

distribution of sources with an age gradient oriented toward the exciting star is discovered 

in the X-ray population. The geometric and age distribution is consistent with 

the radiation-driven implosion model for triggered star formation in cometary globules 

by H II region shocks. The large number of X-ray-luminous protostars in the globule 

suggests either an unusually high ratio of Class I/0 to Class II/III stars or a nonstandard 

initial mass function favoring higher mass stars by the triggering process. The Chandra 

source associated with the luminous Class 0/I protostar IRAS 21391+5802 is one of the 

youngest stars ever detected in the X-ray band. Table 13 shows the list of young stars 

identified by their X-ray emission, together with their NIR (2MASS) and MIR (Spitzer

62 

Table 13. Young stellar objects in IC 1396N detected by Chandra, and their infrared 

counterparts (Getman et al. 2007) 

Source NIR(2MASS) MIR 

No. CXOU J J H K s [3.6] [4.5] [5.8] Class Other Id. ∗ 

(mag) (mag) (mag) (mag) (mag) (mag) 

41 214027.31+581421.1 14.30 13.30 12.88 11.62 11.09 10.74 II OSP 2 

49 214031.58+581755.2 14.03 12.89 12.39 11.51 11.16 10.23 II OSP 4 

53 214036.57+581345.8 13.51 12.58 12.24 12.13 11.94 12.01 III OSP 5 

55 214036.90+581437.9 11.90 10.89 10.23 9.38 9.10 8.76 II OSP 6 

60 214039.62+581609.3 11.29 9.42 8.31 I a NMV 2 

61 214039.87+581834.8 >18.29 15.30 13.36 11.63 10.95 10.21 II NMV 3 

62 214041.12+581359.0 12.96 12.08 11.77 11.61 11.72 11.49 III 

63 214041.16+581511.2 12.97 11.61 10.68 9.15 8.61 8.05 II OSP 9 

65 214041.56+581425.5 13.65 12.62 12.17 11.40 11.20 10.68 II OSP 10 

66 214041.81+581612.3 11.30 8.90 7.50 0/I b 

67 214041.91+581523.1 15.68 14.30 13.65 12.69 12.49 >9.82 II 

68 214042.89+581601.0 10.60 8.78 7.60 I c 

70 214043.47+581559.7 12.89 11.95 >9.85 I/II 

71 214043.64+581618.9 >17.89 >16.09 13.51 9.97 8.72 8.00 I NMV 10 

72 214044.34+581513.3 16.05 14.59 13.60 12.42 11.64 10.60 II 

73 214044.84+581605.1 >15.85 14.28 12.89 11.73 11.15 10.68 II NMV 11 

74 214044.85+581503.4 14.62 13.35 12.66 12.29 11.40 10.96 II OSP 11 

76 214045.18+581559.8 11.95 10.82 10.03 I 

77 214045.51+581511.4 14.65 13.71 13.11 12.54 12.21 11.82 II 

78 214045.53+581602.9 15.68 13.73 12.85 12.23 11.84 >10.37 II 

80 214045.79+581549.0 12.59 11.19 10.04 I 

81 214046.49+581523.2 12.81 11.95 11.65 11.37 11.33 11.39 III 

82 214046.89+581533.3 15.30 13.55 12.63 11.97 11.80 11.15 II 

85 214048.03+581537.9 13.89 12.95 12.67 12.08 11.91 10.77 II OSP 12 

87 214049.09+581709.3 14.14 12.86 12.13 10.77 10.19 9.69 II OSP 15 

∗ OSP: Ogura et al. (2002); NMV: Nisini et al. (2001) 

a X-ray source 60 is offset by 3.2 ′′ to the north of the radio continuum source VLA 1 and by 5.0 ′′ to the 

northwest of the millimeter source BIMA 1 of Beltrán et al. (2002). 

b X-ray source 66 is within 0.5 ′′ of the radio continuum source VLA 2 and millimeter source BIMA 2 of 

Beltrán et al. (2002). This is also millimeter source A of Codella et al. (2001). 

c X-ray source 68 is within 1.0 ′′ of the radio continuum source VLA 3 and millimeter source BIMA 3 of 

Beltrán et al. (2002). 

IRAC) magnitudes. Positions of the young stars born in this globule and some of the 

associated HH objects are displayed in Fig. 20. 

Neri et al. (2007) investigated the mm-morphology of IC 1396N at a scale of 

∼250 AU. They have mapped the thermal dust emission at 3.3 and 1.3 mm, and the 

emission from the J=13 k → 12 k hyperfine transitions of methyl cyanide (CH 3 CN) in 

the most extended configurations of the IRAM Plateau de Bure interferometer. The 

observation revealed the existence of a sub-cluster of hot cores in IC 1396 N, consisting 

of at least three cores, and distributed in a direction perpendicular to the emanating 

outflow. The cores are embedded in a common envelope of extended and diffuse 

dust emission. The CH 3 CN emission peaks towards the most massive hot core and is 

marginally extended in the outflow direction. The protocluster IC 1396N has been in-

cluded in a high angular resolution imaging survey of the circumstellar material around 

intermediate mass stars conducted by Fuente (2008), as well as in a study of clustering 

properties of Class 0 protostars by Fuente et al. (2007). 

IC 1396 East (IC 1396G) IRAS 21445+5712, associated with this globule, coincides 

with a faint, red, nebulous star (Schwartz et al. 1991). Ogura et al. (2002) detected 

Hα emission in the spectrum of this star (BRC 39 No. 3). Fukui (1989) detected a 

molecular outflow associated with IRAS 21445+5712. Connelley et al. (2007) found 

a small, elongated near-infrared nebula around the star. IRAS 21445+5712 has been 

included in several surveys for H 2 O maser sources (Felli et al. 1992; Wouterloot et al. 

1993; Furuya et al. 2003; Valdettaro et al. 2008). High-resolution VLA observations by 

Valdettaro et al. (2008) resulted in the first detection of water maser emission associated 

with IRAS 21445+5712. 

L 1165 This cloud, harboring IRAS 22051+5848, is included in several studies of 

the globules associated with IC 1396 (e.g. Schwartz et al. 1991; Gyulbudaghian 1985; 

Froebrich et al. 2005), though it lies at 2.6 ◦ east of the H II zone (corresponding to 

some 30 pc at the distance of IC 1396). IRAS 22051+5848 is associated with a small 

reflection nebula, catalogued as Gy 2–21 by Gyulbudaghian (1982). Schwartz et al. 

(1991) note that, according to its CO radial velocity (Gyulbudaghian et al. 1986), this 

globule may be foreground to IC 1396. Parker, Padman & Scott (1991) observed a 

bipolar CO outflow originating from IRAS 22051+5848. Tapia et al. (1997) presented 

near-infrared, IJHK, images of the globule. They identified the NIR counterpart of 

the IRAS source and an extended infrared nebula around it. Reipurth, Bally, & Devine 

(1997) detected a giant Herbig–Haro flow, HH 354, associated with IRAS 22051+5848. 

Reipurth & Aspin (1997) obtained a near-infrared spectrum of the source, also known as 

HH 354 IRS. They concluded that the detected CO absorption and the high luminosity 

of the star suggest that HH 354 IRS is probably a FUor. Visser et al. (2002) detected a 

submillimeter source, L 1165 SMM 1, associated with the globule. Slysh et al. (1997) 

observed an OH maser emission at the position of the IRAS source. L 1165 is included 

in the CS(2–1) survey of IRAS point sources with colors characteristic of ultracompact 

H II regions published by Bronfman et al. (1996). The distance of L 1165 is uncertain. 

Several authors (e.g. Reipurth, Bally, & Devine 1997; Froebrich et al. 2005) associate 

this cloud with IC 1396, whereas others, e. g. Tapia et al. (1997) assume a kinematic 

distance of 200 pc, and Visser et al. (2002) use 300 pc, with a reference to Dobashi et 

al. (1994). This value is based on the assumption that the cloud is part of the Lindblad 

ring. Gyulbudaghian et al. (1986) associate L 1165 with a radial system of globules 

centered on the A0 type giant HD 209811. The Hipparcos parallax of this star suggests 

a distance of about 400 pc. 

63 

4. Star Formation along the Cepheus Bubble 

The Cepheus Bubble is a giant far infrared ring-like structure around Cep OB2a, described 

by Kun et al. (1987), and identified as an HI shell by Patel et al. (1998) and 

Ábrahám et al. (2000). Several HII regions, such as IC 1396, S 140, S 134, S 129, and 

G 99.1+07.4 (Kuchar & Clark 1997) are located on the periphery of the ring. The 

similarity of the distances of these HII regions (700–900 pc) and the presence of the 

infrared ring-like structure apparently connecting them suggest that the infrared ring is

64 

22 20 22 00 21 40 21 20 21 00 

66 00 

NGC 7129 

66 00 

64 00 

S145 

S140 

64 00 

Dec (J2000) 

62 00 

L1188 

HD 207198 

62 00 

60 00 

G99.1+07.4 

S129 

60 00 

58 00 

S134 

VDB 140 

58 00 

56 00 

IC 1396 

56 00 

22 20 22 00 21 40 21 20 21 00 

RA (J2000) 

Figure 21. IRAS 100 µm (IRIS) image of the Cepheus Bubble. The HII regions 

and reflection nebulae, probably associated with the Bubble (Kun et al. 1987), 

are indicated. Star symbols show the O-type and supergiant members of Cep OB2 

(Humphreys 1978). 

a real feature and is physically connected with the HII regions. It was probably created 

by the stellar winds and supernova explosions of the evolved high-mass members 

of Cep OB2a. In particular, the O9 IIe type star HD 207198, located near the center 

of the Bubble, may be a major source of powerful stellar wind (Ábrahám et al. 2000). 

Figure 21 shows the distribution of the IRAS 100 µm emission over the area of the Bubble. 

The known HII regions and reflection nebulae, as well as the O-type and supergiant 

members of Cep OB2 are indicated in the figure. CO observations performed by Patel 

et al. (1998) over the 10 ◦ × 10 ◦ area of the Cepheus Bubble revealed the molecular 

clouds associated with it. They found a total molecular mass of 1 × 10 5 M⊙. Most of 

the molecular mass is associated with L 1204/S 140 and IC 1396, but there are further 

molecular clouds whose star forming activity has not yet been studied. Patel et al. have 

shown that the shapes and kinematic properties of the IC 1396 globules indicate their 

interaction with the Bubble. The most comprehensive list of clouds and star forming re-

gions associated with the Cepheus Bubble can be found in Kiss, Moór & Tóth’s (2004) 

Table C. 

4.1. Star Formation in S 140 

The HII region S 140 is located at the southwestern edge of the L 1204 dark cloud, along 

the Cepheus Bubble (Ábrahám et al. 2000), at a distance of about 900 pc from the Sun 

(Crampton & Fisher 1974). The ionization of the clouds is maintained by HD 211880, a 

B0V star (Blair et al. 1978). It is separated from L 1204 by a nearly edge-on ionization 

front. The core of the cloud is totally invisible in optical images while even the earliest 

infrared and radio observations have suggested that there is a dense cluster in the center 

of the core. Rouan et al. (1977) detected far-infrared emission from a region in L 1204, 

a few arcmin NE of S 140. They deduced a dust temperature of about 35 K, computed 

the total IR intensity, and estimated a mass of 600 M⊙ for the observed area. Further 

infrared and submillimeter studies of the infrared source, S 140 IRS (Tokunaga et al. 

1978; Dinerstein et al. 1979; Beichman et al. 1979; Little et al. 1980; Hackwell et al. 

1982; Thronson et al. 1983) confirmed that the heating source of the cloud is a small 

cluster of embedded stars. 

Several observational studies have been carried out to study the region in different 

wavelength regimes. These are mostly focused on the photon-dominated region (PDR) 

at the edge of L 1204, and on the embedded infrared sources located right behind it 

(e.g. Hayashi et al. 1985; Keene et al. 1985; Lester et al. 1986; Schwartz et al. 1989; 

Hasegawa et al. 1991; Golynkin & Konovalenko 1991; Smirnov et al. 1992; Plume et 

al. 1994; Wilner & Welch 1994; Zhou et al. 1994; Schneider et al. 1995; Minchin et 

al. 1995a,c; Stoerzer et al. 1995; Park & Minh 1995; Preibisch & Smith 2002; Bally et 

al. 2002; Poelman & Spaans 2006, 2005). VLA observations of the 6 cm H 2 CO line 

by Evans et al. (1987) revealed absorption of the cosmic background radiation towards 

a 4 ′ × 3 ′ region of the S 140 molecular cloud with structures on scales from 20 ′′ to 4 ′ . 

They attributed these structures to clumps with masses around 40 M⊙ and suggested 

that the clumps represent the first stages of the fragmentation of this portion of the 

cloud (although they did not rule out the possibility that the absorption maxima are low 

density holes surrounded by high-density regions). VLA observation of NH 3 by Zhou 

et al. (1993), however, showed absence of significant NH 3 (1,1) emission at the H 2 CO 

absorption peaks, indicating that the peaks correspond to low density “holes” rather 

than high-density clumps. The high density molecular gas was studied by Ungerechts et 

al. (1986), who mapped the region using NH 3 (1,1) and (2,2), and found that the column 

density and rotational temperature peak at the position of the embedded infrared source. 

The kinetic temperature is peaked at 40 K and decreasing smoothly to 20 K within the 

neighborhood of the infrared source. Zeng et al. (1991) studied the hyperfine structures 

of HCN (1-0) emission from the high density molecular core. 

Several optical, near-, mid- and far-infrared, and radio surveys were carried out 

looking for young stars in the region (e.g. Rouan et al. 1977; Beichman et al. 1979; 

Hayashi et al. 1987; Evans et al. 1989; Persi et al. 1995; Ogura et al. 2002; Bally et al. 

2002; Preibisch & Smith 2002). Beichman, Becklin & Wynn-Williams (1979) provided 

the first catalog of young stellar objects, consisting of three infrared sources, IRS 1, 2, 3. 

Later Evans et al. (1989) added two additional sources (VLA 4 and NW) to the catalog 

from observations using the VLA at 6 and 2 cm. The positions of the sources can 

be found in Table 14. From the spectral indices of IRS 1–3 they concluded that the 

radio emission from these sources originates from optically thin HII regions ionized 

65

66 

by Lyman-continuum photons from single, main sequence stars with spectral type of 

B1.5-B2. Evans et al. (1989) also carried out near-IR photometry using the NOAO 

infrared camera at 1.2, 1.65, and 2.2 µm. They detected all known far-IR sources 

except IRS 2 and found additional 11 sources in the near-IR. At least five of these near- 

IR sources appear to be discrete sources, suggesting that a deeply embedded young 

cluster is forming in the region. Another cluster, containing about 100 near-IR sources 

associated with S 140, was discovered north of the region by a K ′ -band imaging survey 

by Hodapp (1994). 

Joyce & Simon (1986) carried out a near-infrared polarization study and found an 

extremely high level of 2.2 µm polarization towards S 140 IRS 1, indicating an outflow 

directed nearly along our line of sight. This finding was later confirmed by Hayashi 

et al. (1987) who observed the HII region in 12 CO and 13 CO. Minchin et al. (1993) 

found that the blue and redshifted lobes of the CO bipolar outflow have position angles 

of 160 ◦ and 340 ◦ , respectively. The high-resolution CS map obtained by Hayashi & 

Murata (1992) reveals a prominent V-shaped ridge or a ring around the S 140 IR cluster 

encircling the blue and red lobes of the molecular outflow, with no emission detected 

in the vicinity of the IR sources. The observations suggest that the CS ring is a remnant 

of a nearly pole-on massive gaseous disk interacting with the high-velocity outflow. 

Figure 22. Schematic representation of the S 140/L 1204 region showing the plane 

that contains the observer, the external illuminating star HD 211880, the HII region/molecular 

cloud interface and the embedded molecular outflow. Fig 2. of 

Minchin et al. (1995b). 

A self-consistent model of the region, consistent with all the molecular, atomic 

and submm continuum data was provided by Minchin et al. (1995b) (see Fig. 22). 

According to their model the eastern ridge is the dense, clumpy edge of the blueshifted 

outflow lobe that is closest to the observer. This outflow has expanded towards the edge 

of the molecular cloud so its blueshifted lobe is bounded by the HII region. Outside this

67 

Figure 23. Optical and NIR images of S 140 (Preibisch & Smith 2002). 

edge is an externally illuminated PDR. The CI emission emanates from the outer edge 

of the cloud, with the CS emission tracing the compressed high density gas between the 

expanding outflow and PDR regions. The NH 3 and continuum emission emanate from 

the inner edge of the outflow lobe, shielded from the external UV field.

68 

Optical and near-infrared images of S 140, adopted from Preibisch & Smith (2002) 

are displayed in Fig. 23. According to the catalog of Porras et al. (2003) the S 140 region 

contains two young stellar groups. One is S 140 itself, another one is S 140 N identified 

by Hodapp (1994). 

Schwartz (1989) found that the IRS 1 radio source consists of a core source with 

a jetlike appendage pointing toward an extended radio source suggesting ejection of an 

interstellar bullet of material from IRS 1. 

Harker et al. (1997) observed the protostellar system in S 140 at 2.2, 3.1 and 

3.45 µm. They developed a simple model of the region which has been used to derive 

the physical conditions of the dust and gas. IRS 1 is surrounded by a dense dusty 

disk viewed almost edge-on. Photons leaking out through the poles of the disk illuminate 

the inner edge of a surrounding shell of molecular gas as seen at locations NW 

and VLA4. Their thick disk model can explain both the observed K−[3.45] color and 

scattered light intensity distributions. The observed K−[3.45] color of the bluest regions 

implies a cool radiation field with a color temperature of 850-900K. Most likely, 

these cool temperatures are the result of reprocessing of the protostellar radiation field 

by dust close to the protostar. 

K band (2.0-2.3 µm) and H 2 observations have revealed two bipolar outflows in the 

region (Preibisch & Smith 2002; Weigelt et al. 2002), one of them with an orientation 

similar to the CO outflow (160/340 ◦ ) and the other one in the 20/200 ◦ direction. Both 

bipolar outflows seem to be centered on IRS 1. 

Ogura et al. (2002) catalogued 8 stars with visible Hα emission (Table 15, Fig. 24). 

The emission line stars are mostly concentrated around the tip of the bright rim, similarly 

to the distribution found for near-IR clusters in the vicinity of an IRAS source. 

Figure 24. Finding chart for Hα emission objects in S 140. G designate ghost 

images. (Ogura et al. 2002) 

Tafalla et al. (1993) observed the dense gas in the L 1204/S 140 molecular complex 

using CS(J = 1-0) and NH 3 . The large-scale CS(J = 1-0) maps show that L 1204 

is formed by three filamentary clouds, each being fragmented into cores of a few hundred 

solar masses and surrounded by low-level emission. The most prominent core is 

associated with S 140, the star-forming activity, however, is not restricted to the vicinity 

of the HII region, but extends throughout the complex; very red IRAS sources lie

69 

Table 14. Position of far-infrared sources in S 140 

number RA (J2000) Dec (J2000) 

IRS 1 22 19 18.4 +63 18 55 

IRS 2 22 19 18.2 +63 19 05 

IRS 3 22 19 19.6 +63 18 50 

VLA 4 22 19 17.5 +63 18 41 

NW 22 19 18.8 +63 18 57 

Table 15. List of Hα emission objects in S 140 (Ogura et al. 2002; Ikeda et al. 2008) 

number RA (J2000) Dec(J2000) EW(Hα) 

1 22 18 47.8 +63 18 18 · · · 

2 22 18 48.5 +63 16 40 13.6 

3 22 18 49.6 +63 18 56 · · · 

4 22 18 59.0 +63 18 12 94.8 

5 22 18 59.4 +63 19 07 · · · 

6 22 19 03.5 +63 18 01 · · · 

7 22 19 09.9 +63 17 21 26.4 

8 22 19 16.9 +63 17 22 163.5 

Table 16. List of HH objects in S 140 

Name RA (J2000) Dec (J2000) Remark from Bally et al. (2002) Ref. 

HH 615 22 19 15.6 +63 17 29 [S II] jet aimed at HH 616A 1 

HH 616A 22 19 05.9 +63 16 43 Northern tip 1 

HH 616B 22 19 05.9 +63 16 26 Middle tip 1 

HH 616C 22 19 05.7 +63 16 19 Southern tip 1 

HH 616D 22 19 07.1 +63 16 40 Inner shock 1 

HH 616E 22 19 12.8 +63 16 43 [S II] edge, southern rim of HH 616 1 

HH 616F 22 19 14.3 +63 16 28 [S II] edge, southeastern rim of HH 616 1 

HH 617 22 19 03.0 +63 17 53 Northern bow; tip of northern breakout 1 

HH 623 22 19 55.0 +63 19 30 Faint knot east of S 140IR 1 

HH 618A 22 19 53.0 +63 19 29 Western part of pair, east of S 140IR 1 

HH 618B 22 19 54.9 +63 19 30 Eastern part of pair, east of S 140IR 1 

Filament 22 18 52.1 +63 16:08 Hα filament at P.A. = 300 ◦ 1 

HH 251 22 19 34.4 +63 32 57 − 2 

HH 252 22 19 37.8 +63 32 38 − 2 

HH 253 22 19 45.0 +63 31 45 − 2 

HH 254 22 19 49.6 +63 31 14 − 2 

HH 619 22 19 16.4 +63 32 49 Two knots in east-west flow 1 

HH 620 22 19 27.6 +63 32 50 Cluster of three knots south of nebular star 1 

HH 621 22 19 21.5 +63 34 44 Cluster of knots: HH 251-254 counterflow 1 

HH 622 22 19 50.6 +63 35 18 Pair of knots at P.A. = 220 ◦ from nebular star 1 

HH 609 22 21 28.8 +63 30 02 Southwestern [S II] knot in chain of two 1 

HH 610 22 21 33.3 +63 37 34 Tiny knot west of reflection nebula 1 

HH 611 22 21 39.5 +63 36 53 Compact groups of [S II] knots 1 

HH 612 22 21 54.5 +63 34 39 Compact diffuse [S II] knot 1 

HH 613 22 21 58.5 +63 33 23 Faint [S II] group 1 

HH 614 22 22 01.2 +63 27 56 Diffuse [S II] complex 1 

References: (1) Bally et al. (2002); (2) Eiroa et al. (1993).

70 

Table 17. List of Class II/I/0 objects in S 140 (Megeath et al. 2004) 

RA (J2000) Dec (J2000) [3.6] [4.5] [5.8] [8.0] Class 

22 18 21.6 +63 15 32 12.38 12.07 11.65 11.09 Class II 

22 18 37.2 +63 13 01 12.91 12.49 12.20 11.65 Class II 

22 18 48.5 +63 16 40 9.94 9.65 9.22 8.77 Class II 

22 18 47.6 +63 18 17 13.03 12.82 12.26 11.38 Class II 

22 18 58.8 +63 18 11 11.84 11.32 10.50 9.87 Class II 

22 19 03.4 +63 18 00 12.10 11.78 10.99 10.13 Class II 

22 19 24.5 +63 14 26 11.81 11.50 11.50 10.92 Class II 

22 19 09.7 +63 17 20 11.97 11.62 11.32 10.62 Class II 

22 19 28.3 +63 15 07 12.35 11.56 11.43 10.58 Class II 

22 19 25.9 +63 18 24 11.70 10.90 10.23 9.50 Class II 

22 19 20.4 +63 19 38 10.74 9.98 9.59 8.95 Class II 

22 19 28.5 +63 18 49 11.92 11.32 10.51 9.54 Class II 

22 19 27.1 +63 19 22 9.80 9.16 7.93 7.06 Class II 

22 19 48.7 +63 16 41 11.37 11.22 11.23 10.46 Class II 

22 19 29.1 +63 21 01 13.64 12.89 12.29 11.30 Class II 

22 19 38.1 +63 19 32 12.85 12.56 11.78 10.83 Class II 

22 20 19.2 +63 16 23 13.01 12.65 12.27 11.31 Class II 

22 20 21.0 +63 16 14 13.09 12.62 11.81 10.90 Class II 

22 20 07.5 +63 18 45 13.32 12.76 12.24 11.18 Class II 

22 19 37.0 +63 25 31 12.54 12.36 11.63 10.65 Class II 

22 20 27.3 +63 17 07 11.51 11.20 11.02 10.47 Class II 

22 20 27.2 +63 17 58 12.31 11.58 11.10 10.34 Class II 

22 19 37.9 +63 17 10 11.43 11.18 10.83 9.54 Class II 

22 19 15.6 +63 19 33 11.29 9.75 8.90 7.87 Class 0/I 

22 19 25.7 +63 18 49 10.61 9.56 8.74 8.12 Class 0/I 

22 19 30.9 +63 18 32 11.16 10.13 9.19 8.54 Class 0/I 

22 19 32.5 +63 19 24 9.96 8.38 6.24 4.83 Class 0/I 

22 19 39.4 +63 19 03 11.94 10.92 10.43 9.70 Class 0/I 

22 19 43.5 +63 20 08 11.91 11.18 10.57 9.30 Class 0/I 

22 19 52.3 +63 19 01 14.73 12.78 11.86 11.00 Class 0/I 

22 19 48.3 +63 20 27 14.24 12.42 11.62 10.86 Class 0/I 

22 19 45.5 +63 21 21 14.59 13.01 12.39 11.47 Class 0/I 

22 20 18.5 +63 18 57 12.12 10.73 10.07 8.91 Class 0/I 

22 20 19.4 +63 19 05 13.90 12.75 11.90 11.05 Class 0/I 

22 19 35.1 +63 20 26 14.80 13.40 12.43 12.14 Class 0/I 

close to most of the cores, and molecular outflows have been detected in half of them. 

The ammonia observations reveal velocity shifts of about 0.5-0.8 km/s in the dense gas 

inside the cores with embedded stars. These velocity shifts, although small, are systematic 

and tend to divide the cores into two velocity regimes with little overlap. Fast 

rotation of the cores or the interaction between the bipolar outflows and the dense gas 

(or a combination of both) are the most likely causes for these velocity shifts. Minchin 

et al. (1996) studied the structure of the magnetic field by measuring the 800 µm polarization 

at three positions towards S 140. Several studies reported detection of water 

maser emission toward the S 140 IRS region (e.g. Lekht et al. 1993; Tofani et al. 1995; 

Lekht & Sorochenko 2001; Trinidad et al. 2003). 

Bally et al. (2002) carried out a wide field CCD survey of Herbig–Haro objects 

in the S 140 HII region and reported several new Herbig–Haro objects in the vicinity 

of S 140 (Table 16). They found two large bow shocks, HH 616 and HH 617. The 

northern shock, HH 617, is probably associated with the molecular hydrogen outflow

from IRS 3, while the source of the larger velocity southern bow shock, HH 616, is still 

unclear. It appears to trace an outflow from an unknown source south of S 140. 

Recently a survey using InfraRed Array Camera (IRAC) on board the Spitzer 

Space Telescope was carried out by Megeath et al. (2004). They used the IRAC color 

plane to identify 12 Class 0/I and 23 Class II objects (Table 17). The list of Megeath et 

al. (2004) contains 5 stars (1, 2, 4, 6, 7 in Table 15) with Hα emission from Ogura et 

al. (2002). 

Using H- and K s -band imaging polarimetry for S 140 and spectropolarimetry from 

1.26 to 4.18 µm for IRS 1, Yao et al. (1998) discovered two reflection nebulae, illuminated 

by IRS 1 and IRS 3, which seem to be physically connected. Based on the location 

and orientation of the reflection lobes around IRS 1, Yao et al. (1998) suggest that S 140 

IRS 1 may drive a quadrupolar outflow. Schertl et al. (2000) studied the structure of the 

envelope around the central protostar in IRS 1 using high resolution bispectrum speckle 

interferometry and speckle polarimetry. Their high resolution images showed bright 

emission which can be attributed to light reflected from the inner walls of a cavity in 

the circumstellar material around IRS 1. Given that the orientation of the evacuated 

cavity agrees with the direction of the molecular outflow they suggest that the cavity 

has been carved out by the strong outflow from IRS 1. Recently Hoare (2006) obtained 

multiepoch high-resolution radio continuum maps of IRS 1 using the full MERLIN array. 

The observations revealed a highly elongated source that changes over time and 

is perpendicular to the larger scale bipolar molecular outflow. He explained the phenomenon 

with an equatorial wind driven by radiation pressure from the central star 

and inner disk acting on the gas in the surface layer of the disk. Jiang et al. (2008) 

obtained K-band polarimetric images with the Coronagraphic Imager with Adaptive 

Optics (CIAO) mounted on the Subaru telescope. They found that S140 IRS 1 shows 

well-defined outflow cavity walls and a polarization disk which matches the direction 

of previously observed equatorial disk wind (Hoare 2006), thus confirming that the 

polarization disk is actually the circumstellar disk. Preibisch et al. (2001) obtained a 

bispectrum speckle interferometric K-band image with a resolution of 150 mas and a 

seeing-limited molecular hydrogen line emission image of IRS 3. Their speckle image 

resolves IRS 3 into three point sources, a close binary with separation 0. ′′ 63 and a 

third component 1. ′′ 3 away. A rough assessment of the system stability suggests that 

the IRS 3 triple system is unstable. The speckle image also reveals extended diffuse 

emission of very complex morphology around IRS 3. 

Trinidad et al. (2007) present results of 1.3 cm continuum and H 2 O maser emission 

observations made with the VLA in its A configuration toward IRS 1 and also present 

results of continuum observations at 7 mm and re-analyse observations at 2, 3.5 and 

6 cm (previously published). IRS 1A is detected at all wavelengths, showing an elongated 

structure. Three water maser spots are detected along the major axis of the radio 

source IRS 1A. They have also detected a new continuum source at 3.5 cm (IRS 1C) 

located some 0. ′′ 6 northeast of IRS 1A. The presence of these two YSOs (IRS 1A and 

1C) could explain the existence of the two bipolar molecular outflows observed in the 

region. In addition, they have also detected three continuum clumps (IRS 1B, 1D and 

1E) located along the major axis of IRS 1A, and they discuss two possible models to 

explain the nature of IRS 1A: a thermal jet and an equatorial wind. 

Several papers have studied the physical processes in photon dominated regions 

of S 140 using sub-mm and radio observations (see e.g. Li et al. 2002; Poelman & 

Spaans 2005, 2006; Rodríguez et al. 2007, and references therein). Ashby et al. (2000) 

71

72 

detected H 2 O in S 140 using the Submillimeter Wave Astronomy Satellite. They used 

Monte Carlo simulation to model the radiative transport and to interpret the detected 

557 GHz line profiles. Their model required significant bulk flow in order to explain 

the relatively single-peaked H 2 O line. However, they were not able to discriminate 

between infall and outflow. 

4.2. L 1188 

L 1188 is one of the molecular clouds along the Cepheus Bubble. Ábrahám et al. (1995) 

mapped the cloud in 13 CO, and found a molecular mass of ∼ 1800 M⊙ within a field 

of 74 ′ ×44 ′ . They selected 6 IRAS point sources as candidate YSOs in the field, and 

found 15 Hα emission stars during a photographic objective prism survey. Figure 25 

shows the 100 µm optical depth image of the L 1188/L 1204 region, suggesting that 

these clouds are connected to each other, and the distribution of the candidate YSOs 

in and around L 1188. Könyves et al. (2004) studied the SEDs of the IRAS sources 

associated with L 1188 using 2MASS, MSX, IRAS, and ISOPHOT data. 

4.3. S 145 

S 145 is an extended HII region, located at (l,b)=(107. ◦ 67, +5. ◦ 69), in the north-eastern 

part of the Cepheus Bubble. Both its distance and velocity suggest its relation to the 

bubble (Patel et al. 1998; Kiss et al. 2004). S 145 is associated with a bright rimmed 

cloud BRC 44 (Sugitani et al. 1991), in which Ogura et al. (2002) found 13 Hα emission 

stars (Table 18, and Fig. 26). 

Table 18. Hα emission stars associated with BRC 44 from Ogura et al. (2002) 

(EW-s and remarks revised by Ikeda et al. (2008) are shown.) 

N RA(J2000) Dec(J2000) EW (Å) Remarks 

1 22 28 19.01 64 13 54.0 55.8 

2 22 28 21.00 64 14 13.2 4.2 reflection nebula ? 

3 22 28 41.77 64 13 11.6 · · · contam. from nearby star 

4 22 28 43.54 64 13 19.1 · · · double star 

5 22 28 43.98 64 13 26.0 50.6 

6 22 28 44.12 64 13 31.2 20.1 very weak cont. 

7 22 28 44.74 64 13 12.0 · · · contam. from nearby stars 

8 22 28 45.31 64 13 05.6 22.5 bad pix. 

9 22 28 45.48 64 13 23.0 · · · contam. from No. 11 star 

10 22 28 45.77 64 13 24.9 · · · contam. from Nos. 5 and 12 stars 

11 22 28 45.96 64 13 22.1 53.5 contam. from No. 9 star 


13 22 28 47.12 64 13 14.3 9.5 

4.4. S 134 

Two star-forming molecular clouds, associated with this HII region, can be found in the 

literature. Yonekura et al. (1998) observed a head-tail structured molecular cloud and 

CO outflow associated with IRAS 22103+5828, whereas Dobashi & Uehara (2001) 

reported on a CO outflow and molecular cloud associated with IRAS 22134+5834.

73 

Figure 25. Left: 100 µm optical depth image of the L 1188/L 1204 region. Right: 

Distribution of the molecular gas, IRAS point sources and Hα emission stars in the 

region of L 1188 (From Ábrahám et al. 1995). 

Figure 26. Finding chart for Hα emission objects in BRC 44, a bright-rimmed 

dark cloud associated with S145 (Ogura et al. 2002).

74 

The latter source proved to be a high-mass protostar at a very early evolutionary stage 

(Sridharan et al. 2002). It is associated with H 2 O maser emission (Cesaroni et al. 1988). 

5. Star Formation in the Association Cep OB3 

Blaauw, Hiltner & Johnson (1959) made the first detailed photometric investigation 

of the association Cep OB3. They found 40 early-type members at 725 pc. Blaauw 

(1964) found evidence for two subgroups, Cep OB3a and Cep OB3b, with ages of 8 

and 4 Myr, respectively. The luminous stars of the younger subgroup, Cep OB3b, excite 

the HII region S 155. Garmany (1973) suggested an expansion age of 0.72 Myr, based 

on the relative motion of the two subgroups. Seventeen of the 40 Cep OB3 members 

compiled by Blaauw et al. are contained in the Hipparcos Catalog. However, de Zeeuw 

et al. (1999) could not identify Cep OB3 as a moving group using the Hipparcos data. 

Hoogerwerf et al. (2001) have shown that the parent association of the runaway star 

λ Cep is probably not Cep OB2, but Cep OB3. 

Several photometric studies (Crawford & Barnes 1970; Garrison 1970; Jordi, Trullors 

& Galadí-Enríquez 1996) refined the Blaauw et al. membership list, and extended 

it to fainter stars. Moreno-Corral et al. (1993) performed JHK ′ LM photometry for the 

40 luminous stars in Blaauw et al.’s list. A comprehensive summary of all previous 

membership studies was given by Jordi et al. (1996), who obtained ages of 7.5 and 

5.5 Myr for the two subgroups. 

Simonson & van Someren Greve (1976) found an expanding HI shell centered on 

the young subgroup in Cep OB3 but did not detect significant H I associated with the 

older subgroup. 

Sargent (1977, 1979) mapped the vicinity of Cep OB3 in the J=1-0 transition of 

12 CO, and found a 20 pc×60 pc molecular cloud complex at the average radial velocity 

of −10 km s −1 , close to the velocity range of the association members and S 155. Sargent’s 

CO observations revealed several clumps in the Cep OB3 molecular cloud. She 

labeled them as Cep A,B,C,D,E,F, and concluded that some of them, especially Cep A, 

are sites of triggered star formation due to the interaction of the expanding HII region 

S 155 and the molecular cloud. Elmegreen & Lada (1977) considered Cep OB3 as one 

of the examples of sequential star formation. Felli et al. (1978) measured the thermal 

radio emission from Cep OB3 and S 155. Ammonia maps around the IRAS sources associated 

with the Cep A–Cep F clouds are presented in Harju, Walmsley & Wouterloot 

(1993). The distribution of the luminous stars of Cep OB3 and the associated molecular 

cloud as shown up in the extinction map of the region (Dobashi et al. 2005) is displayed 

in Fig. 27. 

5.1. Pre-main Sequence Stars and Candidates in Cep OB3b 

Naylor & Fabian (1999) discovered over 50 X-ray point sources in the region of Cep 

OB3 with ROSAT PSPC and HRI, the majority of which are probably T Tauri stars. 

Using the ratio of high-mass to low-mass stars to constrain the initial mass function, 

Naylor & Fabian (1999) found that it is consistent with that for field stars. Most of the 

T Tauri stars are close to, but outside the molecular cloud. 

Pozzo et al. (2003) identified 10 T Tauri stars and 6 candidates using UBVI photometry 

and follow-up multi-fiber spectroscopy. Their optical survey covered an area 

of some 1300 arcmin 2 . The newly discovered pre-main sequence stars have masses in

75 

4 

Cep F 

V733 Cep 

Galactic latitude [deg] 

3 

2 

Cep D 

Cep C 

Cep B 

HW2 

L1211 

MM1-MM4 

Cep A 

Cep E mm 

1 

Cep E 

112 

111 110 

Galactic longitude [deg] 

109 

Figure 27. Distribution of the visual extinction (Dobashi et al. 2005) and the 

young, luminous stars in the region of Cep OB3b. The dense clumps Cep A–Cep 

F, identified in the distribution of CO by Sargent (1977), the dark cloud Lynds 1211, 

as well as the most prominent associated young stars are labeled. The lowest contour 

of the extinction is at A V = 1 mag, and the increment is 0.7 mag. Star symbols mark 

the luminous members of Cep OB3, listed by Garmany & Stencel (1992). 

the range ∼ 0.9 − 3.0 M⊙ and ages from < 1 Myr to nearly 10 Myr. Out of the 10 

definite TTS, four have a ROSAT X-ray counterpart in Naylor & Fabian (1999). 

Mikami & Ogura (2001) presented a list and finding charts of Hα emission stars in 

the region of Cep OB3. Their objective prism survey covered an area of 36 square degrees. 

They found 108 Hα emission stars, 68 of which are new. The surface distribution 

of the Hα emission stars outlines a ring-like area, which almost coincides with that of 

the heated dust shown by the IRAS images. The surveyed area is much larger than that 

occupied by the stars of Cep OB3, and extends to the south of the associated molecular 

cloud. It includes NGC 7419, a cluster at 2 kpc, and King 10, below the Galactic plane. 

Further objects, not associated with Cep OB3 but included in the surveyed area and 

lying along the shell-like surface, are S 157, NGC 7654, and S 158. 

A portion of the Cep OB3b and the molecular cloud Cepheus B have been observed 

with the ACIS detector on board the Chandra X-ray Observatory (Getman et 

al. 2006). The observations resulted in the discovery of two rich clusters of pre-main 

sequence stars. The cluster projected outside the molecular cloud is part of the association 

Cep OB3b. The X-ray observations detected 321 pre-main sequence members.

76 

Figure 28. Pre-main sequence stars and candidates in the Cep OB3 region overlaid 

on the map of visual extinction, obtained from 2MASS data based on interstellar 

reddening using the NICER method (Lombardi & Alves 2001). Large circles denote 

the clouds from Table 1 associated with young stars. The meaning of the different 

symbols are as follows: Filled triangles - T Tauri stars; Filled squares - Herbig Ae/Be 

stars; Filled circles - Weak-line T Tauri stars; Open squares - Photometric candidate 

and possible PMS members; X - Hα emission stars; + - T Tauri candidates selected 

from 2MASS. 

This is the best census of the stellar population of the region. The results suggest that 

the X-ray luminosity function, and thus probably the IMF, of Cepheus OB3b differs 

from that of the Orion Nebula Cluster: more stars of M < 0.3M⊙ can be found in 

Cepheus OB3b than in Orion. 

Figure 28 shows the distribution of pre-main sequence stars and catalogued clouds 

overlaid on the visual extinction in the Cep OB3 region (Dobashi et al. 2005). Figure 29 

shows the field of view and the main results of the X-ray observations. 

5.2. Star Formation in the Molecular Cloud associated with Cep OB3 

Cepheus A is a very active high-mass star-forming region within the molecular cloud 

associated with Cep OB3. It shows strings of sources whose spectra suggest that some 

are thermal and some nonthermal (Hughes & Wouterloot 1984; Hughes 1985, 1988), 

several compact HII regions (Beichman et al. 1979; Rodríguez et al. 1980a), OH, H 2 O, 

and CH 3 OH masers (Blitz & Lada 1979; Wouterloot, Habing & Herman 1980; Lada 

et al. 1981; Cohen, Rowland & Blair 1984; Mehringer, Zhou & Dickel 1997; Patel et 

al. 2007), and strong infrared emission (Koppenaal et al. 1979; Beichman et al. 1979; 

Evans et al. 1981) within an area smaller than 1 arcmin. Cep A has been therefore an

77 

62 50 

HD 217486 

62 45 

Dec(J2000) 

62 40 

62 35 

Hα knot 

62 30 

AFGL 3000 

HD 217061 

62 25 

Radio source No.9 

22 59 00 

22 58 00 

22 57 00 

RA(J2000) 

22 56 00 

22 55 00 

Figure 29. R-band image covering 0. ◦ 5 × 0. ◦ 5 of the Cep B and Cep OB3b neighborhood 

from the Digitized Sky Survey (DSS). North is up, and east is to the left. 

The Chandra 17 ′ × 17 ′ ACIS-I field (Getman et al. 2006) is outlined by the square, 

and the dashed rectangle shows the region in which Ogura et al. (2002) searched for 

Hα emission stars. Cep B, the hottest component of the Cepheus molecular cloud, is 

at the bottom left corner of the Chandra field. To the north and west lies Cep OB3b, 

the younger of two subgroups of the Cep OB3 association. The interface between 

Cep B and Cep OB3 is delineated by the H II region S 155. The most massive and 

optically bright stars in the field, HD 217086 (O7n) and HD 217061 (B1V), are labeled. 

Black plusses indicate the T Tauri stars identified by Pozzo et al. (2003). 

Blue crosses show the X-ray sources which are probably members of a cluster belonging 

to Cep OB3b. Red triangles indicate the X-ray emitting members of an 

embedded cluster in the molecular cloud Cep B, whereas green diamonds show the 

X-ray sources whose 2MASS counterparts are indicative of K-band excess, originating 

from accretion disks. Small, thick red plusses within the dashed rectangle show 

the Hα emission stars found by Ogura et al. (2002). Black circle outlines the bright 

Hα knot on the ionization front, associated with a compact cluster and studied in 

detail by Moreno-Corral et al. (1993) and Testi et al. (1995). A star symbol shows 

the infrared source AFGL 3000, and a thick black cross is the bright radio continuum 

source No. 9 discovered by Felli et al. (1978).

78 

exciting target for high-resolution interferometric observations and has a huge literature. 

Figure 30. Structure of Cepheus A (Hartigan & Lada 1985). Solid lines show 

the 20 cm continuum contours (Rodríguez & Cantó 1983), dot-dash and longdashed 

lines show the distribution of the redshifted and blueshifted CO, respectively 

(Rodríguez et al. 1980a), and a short-dashed line shows the extent of the NH 3 emission 

(Ho, Moran & Rodríguez 1982). Triangles are reflection nebulae, plus signs 

indicate HH objects, and filled circles are visible stars. The hatched circular area 

is an extended 20 µm emission area (Beichman et al. 1979). Small numbered open 

circles show the 6 cm continuum sources, detected by Hughes & Wouterloot (1984) 

and shown in more detail in Fig. 31. 

A powerful molecular outflow was discovered by Rodríguez et al. (1980a) and 

studied in further detail by among others Richardson et al. (1987), Torrelles et al. 

(1987), Hayashi, Hasegawa & Kaifu (1988), Bally & Lane (1990), Torrelles et al. 

(1993), Narayanan & Walker (1996), and Froebrich et al. (2002). Water maser emission 

has been detected from several centers of activity (Torrelles et al. 1996), and numerous 

thermal and nonthermal radio sources (Garay et al. 1996; Hughes 2001). The HH object 

HH 168 (original name GGD 37), consisting of several knots (Hartigan & Lada 1985), 

lies about 2 ′ west of Cep A. It was studied in detail by Hartigan & Lada (1985), Lenzen 

et al. (1984), Hartigan et al. (1986), Lenzen (1988), Garay et al. (1996), Wright et al. 

(1996), and Hartigan, Morse & Bally (2000). An apparent counter-flow of HH 168, 

HH 169 was discovered by Lenzen (1988) 2 ′ northeast of Cep A. The objects are part 

of a larger, elliptical region containing several fainter HH objects (Corcoran, Ray & 

Mundt 1993). A comprehensive summary of the literature of HH 168 and 169 can be 

found in Reipurth (1999).

79 

Figure 31. VLA map at 6 cm of Cep A East, observed by Hughes & Wouterloot 

(1984), displaying two chains of 14 compact sources. 

Hughes & Wouterloot (1982) mapped Cep A at 21 cm. The map has shown the 

presence of two sources, Cep A West and Cep A East, separated by ∼ 1. ′′ 5. Cep A West 

is associated with optical nebulosities and an optically visible star at its peak contour 

level. It is named HW object (Hartigan & Lada 1985), and appears to be an H II region 

on the near side of the cloud. Hughes (1989) obtained radio maps of Cep A West, 

and found it to consist of two compact sources, W 1 and W 2. The first component is 

constant in time, while the second is variable, and there is a third, diffuse component, 

W 3. The HW object was found to be nonstellar, radiating mainly in Hα, and suggested 

to be an HH object. Garay et al. (1996) studied in detail the three sources within Cep A 

West, and found that the energy source, powering the activity observed in Cep A West, 

is probably W 2, associated with a low-luminosity embedded pre-main sequence star, 

whereas emission of the shocked gas flowing from W 2 can be observed from the diffuse 

component W 3. Wright et al. (1996), based on observations by ISO SWS, studied the 

molecular hydrogen emission from the GGD 37 complex in Cep A West. 

OH and H 2 O maser sources are situated near the center of Cep A East, which 

appears younger and more heavily extincted than Cep A West. Hughes & Wouterloot 

(1984) performed radio observations of Cep A East, with resolutions down to 1 ′′ at 

21 cm and 6 cm, using both the Westerbork Synthesis Radio Telescope and VLA. The 

maps have shown two strings of 14 compact radio sources, numbered as HW 1a, 1b, 2, 

3a–d, 4, 5, 6, 7a–d, (see Fig. 31) which were interpreted as HII regions, being produced 

by about 14 stars, each of which mimics main-sequence B3 stars; the length of each 

string is about 0.1 pc. Hughes (1988; 1993) reported on the variability and high proper 

motion of some compact radio sources of Cep A East and discovered two new, highly 

variable compact radio sources (sources 8 and 9). He suggested that, contrary to the 

original interpretation, some of the compact sources are probably not H II regions, but 

Herbig–Haro objects. Garay et al. (1996), based on multifrequency, high resolution radio 

continuum observations, classified the 16 compact sources into two groups: sources 

2, 3a,3c, 3d, 8, and 9 harbor an energy source, whereas sources 1a, 1b, 4, 5, 6, 7a, 7b,

80 

7c, and 7d are excited by an external source of energy. Of the stellar sources, HW 2, 3c, 

and 3d are probably associated with high luminosity stars, while the variable sources 

3a, 8, and 9 are probably low-mass pre-main sequence stars. The nature of source 

3b remained uncertain. Torrelles et al. (1998) detected a new continuum source (Cep 

A:VLA 1) in an 1.3 cm VLA map. Goetz et al. (1998) present new infrared images, 

including near-infrared broadband (K, L ′ , and M ′ ) and spectral line ([Fe II] emission 

line at 1.644 µm and H 2 1-0 S[1] line at 2.122 µm) observations of Cep A East. The 

images show two regions of shock-excited line emission from separate bipolar flows. 

Figure 30, adopted from Hartigan & Lada (1985), shows the schematic structure of the 

region of Cep A, and Fig. 31 shows the distribution of the radio continuum sources in 

Cep A East, discovered by Hughes & Wouterloot (1984). 

Both the compact radio continuum and H 2 O maser sources in Cep A exhibit remarkable 

variations on various time scales. Hughes (1985; 1988; 1993; 2001) reported 

on the variability of sources HW 2, 3c, and 3d, and pointed out that the strong variability 

results in appreciable changes in the spectra. Variations of H 2 O maser emission have 

been detected by Mattila et al. (1985; 1988), Cohen & Brebner (1985), and Rowland & 

Cohen (1986). 

Patel et al. (2007), using the Submillimeter Array (SMA), detected the 321.226 

GHz, 10 29 − 9 36 ortho-H 2 O maser emission from Cep A. The 22.235 GHz, 6 16 − 5 23 

water masers were also observed with the Very Large Array 43 days following the 

SMA observations. Three of the nine detected submillimeter maser spots are associated 

with the centimeter masers spatially as well as kinematically, while there are 36 

22 GHz maser spots without corresponding submillimeter masers. The authors interpret 

the submillimeter masers in Cepheus A to be tracing significantly hotter regions 

(600-2000 K) than the centimeter masers. 

Rodríguez et al. (1994) obtained multifrequency VLA radio continuum observations 

of HW 2, the most luminous radio continuum source of the region. They have 

shown HW 2 to be a powerful thermal radio jet, and suggest that it is responsible for 

at least part of the complex outflow and excitation phenomena observed in the region. 

HW 2 proved to be a complex object, consisting of several components (e.g. Gómez 

et al. 1999; Curiel et al. 2002, 2006; Jiménez-Serra et al. 2007; Brogan et al. 2007), 

including a hot core (Martín-Pintado et al. 2005). Torrelles et al. (2001) report three 

epochs of VLBA water maser observations toward HW 2. VLBA data show that some 

of the masers detected previously with the VLA (Torrelles et al. 1998) unfold into unexpected 

and remarkable linear/arcuate “microstructures,” revealing, in particular three 

filaments (R1, R2, R3) with length sizes ∼ 3–25 mas (2–18 AU) and unresolved in 

the perpendicular direction ( ∼ < 0.1 AU), an arcuate structure (R4-A) of ≈ 20 mas size 

(15 AU), and a curved chain of masers (R5) of ≈ 100 mas size (≈ 72 AU). Some of 

these structures unfold into even smaller linear “building blocks” (down to scales of 

0.4 AU) shaping the larger structures. 

Jiménez-Serra et al. (2007) present VLA and PdBI subarcsecond images (0.15 ′′ − 

0.6 ′′ ) of the radio continuum emission at 7 mm and of the SO 2 J = 19 2,18 − 18 3,15 

and J = 27 8,20 − 28 7,21 lines toward the Cep A HW 2 region. The SO 2 images reveal 

the presence of a hot core internally heated by an intermediate-mass protostar, and a 

circumstellar rotating disk around the HW 2 radio jet of size 600 × 100 AU and mass 

1 M⊙. The high-sensitivity radio continuum image at 7 mm shows, in addition to the 

ionized jet, an extended emission to the west (and marginally to the south) of the HW2 

jet, filling the southwest cavity of the HW 2 disk.

Torrelles et al. (2007) report SMA 335 GHz continuum observations with angular 

resolution of ∼ 0. ′′ 3, together with VLA ammonia observations with ∼ 1 ′′ resolution 

toward Cep A HW 2. The observations have shown a flattened disk structure of the dust 

emission of ∼ 0. ′′ 6 size (450 AU), peaking on HW 2. In addition, two ammonia cores 

were observed, one associated with a hot core previously reported and an elongated 

core with a double peak separated by ∼ 1. ′′ 3, with signs of heating at the inner edges 

of the gas facing HW 2. The double-peaked ammonia structure, as well as the doublepeaked 

CH 3 CN structure reported previously (and proposed to be two independent hot 

cores), surround both the dust emission as well as the double-peaked SO 2 disk structure 

found by Jiménez-Serra et al. (2007). 

81 

Figure 32. Hα emission stars in Cep B found by Ogura et al. (2002). 

Pravdo & Tsuboi (2005) report the discovery of X-rays from both components of 

Cepheus A, East and West, with the XMM-Newton observatory. They detected prominent 

X-ray emission from the complex of compact radio sources and call this source 

HWX. Its hard X-ray spectrum and complex spatial distribution may arise from one or 

more protostars associated with the radio complex, the outflows, or a combination of the 

two. They also detected 102 X-ray sources, many presumed to be pre-main sequence 

stars on the basis of the reddening of their optical and IR counterparts. 

Sonnentrucker et al. (2008) report the first fully sampled maps of the distribution 

of interstellar CO 2 ices, H 2 O ices and total hydrogen nuclei, as inferred from the 9.7 µm 

silicate feature, toward Cepheus A East with the IRS instrument on board the Spitzer 

Space Telescope. They find that the column density distributions for these solid state 

features all peak at, and are distributed around, the location of HW2. A correlation 

between the column density distributions of CO 2 and water ice with that of total hydrogen 

indicates that the solid state features mostly arise from the same molecular clumps 

along the probed sight lines. 

Comito et al. (2007) employed the Plateau de Bure Interferometer to acquire 

(sub-)arcsecond-resolution imaging of high-density and shock tracers, such as methyl 

cyanide (CH 3 CN) and silicon monoxide (SiO), towards the HW2 position. They find 

that on the 1 arcsec (∼ 725 AU) scale, the flattened distribution of molecular gas around 

HW2 appears to be due to the projected superposition, on the plane of the sky, of at

82 

least three protostellar objects, of which at least one is powering a molecular outflow 

at a small angle with respect to the line of sight. The presence of a protostellar disk 

around HW2 is not ruled out, but such structure is likely to be detected on a smaller 

spatial scale, or using different molecular tracers. 

Cepheus B is located at the edge of the HII region S 155. Felli et al. (1978) and 

Panagia & Thum (1981) suggested that a younger subgroup of Cep OB3 originated 

from the Cep B/S 155 complex. Several features of the Cep B/S 155 interface indicate 

triggered star formation in Cep B, for instance a bright Hα nebula located near the 

ionization front, referred to as the Hα knot by Moreno-Corral et al. (1993) and Testi et 

al. (1995), a compact radio continuum source (source #9) detected by Felli et al. (1978), 

and the bright infrared source AFGL 3000. 

Moreno-Corral et al. (1993) studied the S 155/Cep B interface with Hα and 

BV (RI) C imaging, and identified a cluster of pre-main sequence stars in the Hα knot. 

Testi et al. (1995) performed radio and near infrared observations of the Hα knot. The 

unresolved radio source #9 lies on top of the diffuse emission. Far infrared and high 

resolution CO observations indicate that an embedded B1–B0.5 star is the source of 

heat for the molecular hot spot and the source of ionization of #9. More than 100 low 

luminosity stars have been found in an area of about 3 ′ ×2 ′ , and most of them lie above 

and to the right of the main sequence. Many of them are associated with reflection 

nebulosities. Testi et al. (1995) concluded that they are pre-main sequence stars. They 

identified new Herbig Ae/Be stars among the cluster members. Ogura et al. (2002) 

found 33 Hα emission stars in Cep B. The list of these candidate pre-main sequence 

stars is given in Table 19, and the finding chart, adopted from Ogura et al. (2002) is 

displayed in Fig. 32. Getman et al. (2006) identified 64 members of the cluster embedded 

in Cep B, based on deep X-ray observations with the Chandra Observatory (see 

Fig. 29). Mookerjea et al. (2006) studied the emission from the photon dominated regions 

in Cepheus B, based on 15 ′ × 15 ′ fully sampled maps of [C I] at 492 GHz and 

12 CO (4-3) observed at 1 ′ resolution. They estimated the column densities of neutral 

carbon in Cepheus B and studied the factors which determine the abundance of neutral 

carbon relative to CO. 

Cepheus C The mass of this clump, estimated from the formaldehyde observations 

obtained by Few & Cohen (1983) is ∼ 3600 N⊙, which ranks Cep C as the most massive 

clump of the Cep OB3 molecular cloud. The region contains a cluster of infrared 

sources (Hodapp 1994) and is associated with water maser emission (Wouterloot & 

Walmsley 1986) and an outflow (Fukui 1989). The Cep C cluster, first identified in a 

near-IR survey by Hodapp (1994), was included in the Young Stellar Cluster survey 

performed by the Spitzer Space Telescope (Megeath et al. 2004). In addition to the 

near-IR cluster, the IRAC data show Class I and II sources distributed over a 3 pc diameter 

region. The molecular gas traced by the C 18 O is visible in the IRAC images as 

filamentary dark clouds obscuring a diffuse nebulosity extending across the entire mosaic. 

Two Class I objects appear outside the C 18 O emission; 13 CO emission is found 

toward both of these sources. 

Cepheus E is the second most massive and dense clump (M ∼2100 M⊙) of the 

Cep OB3 molecular cloud according to the H 2 CO map (Few & Cohen 1983). An 

outflow was identified in Cepheus E based on millimeter CO observations (Sargent

83 

Table 19. 

et al. 2002) 

Hα emission stars associated with bright rimmed cloud Cep B (Ogura 

N RA(J2000) Dec(J2000) EW ∗ Remarks ∗ 

1 22 56 37.97 62 39 51.1 69.7 

2 22 56 38.12 62 40 58.7 104.7 very weak cont. 

3 22 56 39.33 62 38 15.5 80.1 

4 22 56 39.58 62 38 43.1 17.2 very weak cont. 

5 22 56 39.93 62 41 37.1 14.6 M-star ? 

6 22 56 43.54 62 38 07.5 · · · invisible cont. 

7 22 56 45.33 62 41 15.8 8.0 M-star ? 

8 22 56 47.79 62 38 14.0 22.4 

9 22 56 48.02 62 38 40.2 125.6 very weak cont. 

10 22 56 48.23 62 39 11.1 62.3 very weak cont. 

11 22 56 49.54 62 41 10.0 21.4 

12 22 56 49.77 62 40 30.1 81.3 very weak cont. 


14 22 56 52.40 62 40 59.6 63.6 contam. from nearby star 

15 22 56 53.87 62 41 17.7 19.0 

16 22 56 54.65 62 38 57.8 16.8 weak cont., contam. from bright rim 


18 22 56 57.83 62 40 14.0 59.8 

19 22 56 58.65 62 40 56.0 · · · Hα ? 

20 22 56 59.68 62 39 20.2 76.4 

21 22 57 00.22 62 39 09.4 24.9 weak cont. 


23 22 57 02.63 62 41 48.7 · · · contam. from nearby star 

24 22 57 02.93 62 41 14.9 4.9 

25 22 57 04.31 62 38 21.1 · · · contam. from neighboring stars 

26 22 57 07.86 62 41 33.2 23.1 weak cont. 

27 22 57 10.82 62 40 51.0 · · · invisible cont., contam. from bright rim 

28 22 57 11.48 62 38 14.1 39.6 very weak cont. 



31 22 57 14.11 62 41 19.8 · · · double star, both show Hα emission 

32 22 57 19.38 62 40 22.5 · · · Hα ?, contam. from bright. rim 

33 22 57 27.04 62 41 07.9 6.4 

34N 22 57 04.93 62 38 23.2 14.2 

35N 22 57 05.91 62 38 18.4 10.1 

36N 22 56 36.14 62 36 45.9 · · · invisible cont. 

37N 22 56 35.29 62 39 07.8 8.1 

∗ Column revised by Ikeda et al. (2008) 

1977; Fukui 1989), followed by near-infrared and higher spatial resolution CO studies 

(Hodapp 1994; Eislöffel et al. 1996; Ladd & Hodapp 1997; Noriega-Crespo et al. 1998). 

The outflow is quite compact, and driven by the source IRAS 23011+6126, also 

known as Cep E-mm. The outflow is deeply embedded in a clump of density 10 5 cm −3 

and nearly invisible at optical wavelengths, with the exception of its southern lobe, 

which is breaking through the molecular cloud and is seen as HH 377 (Devine et al. 

1997; Noriega-Crespo 1997; Noriega-Crespo & Garnavich 2001; Ayala et al. 2000). 

Lefloch, Eislöffel & Lazareff (1996) have shown that IRAS 23011+6126 is a Class 0 

protostar. The properties of the outflow have been thoroughly analyzed by Eislöffel et 

al. (1996), Moro-Martin et al. (2001) and Smith et al. (2003). H 2 and [FeII] images 

obtained by Eislöffel et al. (1996) have shown two, almost perpendicular outflows emanating 

from Cep E, suggesting that the driving source is a Class 0 binary. Submillimeter 

and near-infrared line and continuum observations by Ladd & Hodapp (1997) led to a

84 

similar conclusion. With the assumption that the morphology of the jet results from 

precession, Terquem et al. (1999) inferred an orbital separation of 4–20 AU and disk 

radius of 1–10 AU for the binary. 

Hot molecular bullets were detected in the outflow by Hatchell, Fuller & Ladd 

(1999). A comparative study of the Cep E-mm source, in the context of other well 

known Class 0/I sources, was carried out by Froebrich et al. (2003). 

Submillimeter observations by Chini et al. (2001) and far-infrared photometry by 

Froebrich et al. (2003) resulted in L submm /L bol = 0.017 ± 0.001, an envelope mass 

M env = 7.0 M⊙, an estimated age of 3 × 10 4 yr, and an H 2 luminosity of 0.07 L⊙, 

which confirm that Cep E-mm belongs to the Class 0 objects. At a distance 2 of 730 pc, 

Cep E-mm is one of the brightest Class 0 protostars known and likely to become an 

intermediate-mass (3 M⊙) star (Moro-Martin et al. 2001; Froebrich et al. 2003). 

The Cep E outflow and its protostellar source have been observed using the three 

instruments aboard the Spitzer Space Telescope (Noriega-Crespo et al. 2004). The 

new observations have shown that the morphology of the outflow in the mid-infrared 

is remarkably similar to that of the near-infrared observations. The Cep E-mm source 

or IRAS 23011+6126 was detected in all four IRAC channels. The IRAC and MIPS 

integrated fluxes of the Cep E-mm source are consistent with the Class 0 envelope 

models. 

Cepheus F (L 1216) contains V733 Cep (Persson’s star), the only known bona fide 

FUor in the star forming regions of Cepheus, located at the coordinates 22:53:33.3, 

+62:32:23 (J 2000). The brightening of this star was discovered by Persson (2004) by 

comparing the old and new Palomar Sky Survey plates. Reipurth et al. (2007) have 

shown that the optical spectrum of Persson’s star exhibits all the features characteristic 

of FU Ori type stars. They also identified a molecular outflow associated with the star. 

At an assumed distance of 800 pc the observed apparent magnitude R ∼ 17.3 mag, 

together with the extinction A V ∼ 8 mag, estimated from the strength of the water 

vapor features in the infrared spectrum, corresponds to a luminosity of about 135 L⊙. 

The star erupted sometime between 1953 and 1984. 

Reipurth et al. (2007) identified several nebulous near-infrared sources in L 1216 

around IRAS 22151+6215 (Table 20, adopted from Reipurth et al. 2007). To the 

south of the aggregate of infrared sources containing Persson’s star there is an extended 

far-infrared source, Cep F(FIR) (Sargent et al. 1983), with a luminosity of about 

500 L⊙. Several IRAS sources can be found around this object (see Table 21, adopted 

from Reipurth et al. 2007), which most probably form an embedded cluster containing 

a Herbig Ae/Be star. A compact HII region without an obvious IRAS counterpart, 

Cep F(HII), was discovered by Harten, Thum & Felli (1981) to the south of Cep F(FIR). 

L 1211 is a class 5 dark cloud (Lynds 1962) about 1 ◦ west of Cepheus A (see Fig. 27). 

The mass of this cloud, derived from 13 CO measurements, is 1900 M⊙ (Yonekura et 

al. 1997). Its angular proximity to the group of Cepheus A-F clouds and its similar 

LSR velocity suggest that it is related to the group, and therefore lies at a similar 

distance from the Sun (725 pc, see Blaauw et al. 1959; Crawford & Barnes 1970; Sar- 

2 Throughout the literature of Cep E, the distance of 730 pc is used. This value is not an independent 

estimate for this cloud, but rounded from the 725 pc derived by Blaauw et al. (1959) and Crawford & 

Barnes (1970) for Cep OB3 (see Ladd & Hodapp 1997).

85 

Table 20. Near-infrared sources in Cep F 

around IRAS 22151+6215 (Reipurth et al. 

2007) 

ID RA(2000) Dec(2000) K ′ 

IRS 1 22 53 40.7 62 32 02 16.3 

IRS 2 22 53 41.1 62 31 56 13.7 

IRS 3 22 53 40.9 62 31 49 18.1 

IRS 4 22 53 41.0 62 31 48 17.4 

IRS 5 22 53 41.2 62 31 48 15.6 

IRS 6 22 53 43.3 62 31 46 14.2 

Table 21. IRAS sources around Cep F(FIR) (Reipurth et al. 2007) 

IRAS RA(2000) Dec(2000) 12µm 25µm 60µm 100µm L IRAS 

22507+6208 22 50 47.9 62 08 16 0.54: 1.00 12.99: 53.98 18 

22152+6201 22 51 14.1 62 01 23 1.61 4.86 13.11

86 

mm line data, the mm sources are embedded in an elongated, turbulent core of about 

150 M⊙ of mass and 0.6 pc length. Two of the millimeter sources power bipolar molecular 

outflows, another signature of their extreme youth. These outflows are referred 

to as the L1211-MMS1 and L1211-MMS4 outflows. L 1211 is included in the farinfrared 

(ISOPHOT) photometric studies of embedded objects performed by Froebrich 

et al. (2003). Table 22 lists the coordinates, millimeter fluxes and estimated masses 

of the mm-sources in L 1211, and Fig. 33 shows their appearance at different wavelengths 

(adopted from Tafalla et al. 1999). Table 23 lists the Herbig–Haro objects in 

the Cepheus OB3 molecular cloud. 

Table 22. 

L 1211 millimeter sources 

Source RA(2000) Dec(2000) Int. flux Mass ∗ 

(mJy) (M⊙) 

MMS 1 22 46 54.5 62 01 31 45 0.3 

MMS 2 22 47 07.6 62 01 26 215 1.3 

MMS 3 22 47 12.4 62 01 37 85 0.5 

MMS 4 22 47 17.2 62 02 34 135 0.8 

∗ Assuming optically thin dust at 30 K with an opacity 

of 0.01 cm 2 g −1 

Table 23. 

Herbig–Haro objects in the Cepheus OB3 molecular clouds. 

Name RA(2000) Dec(2000) Source Cloud d Reference 

[H89] W3 22 56 08.8 +62 01 44 Cep A 700 2 

HH 168 22 56 18.0 +62 01 47 HW 2 Cep A 700 1,5 

HH 169 22 56 34.8 +62 02 36 HW 2 Cep A 700 3 

HH 174 22 56 58.5 +62 01 42 HW 2 Cep A 700 4 

HH 377 23 03 00.0 +61 42 00 IRAS 23011+6126 Cep E 700 6 

References: 1 – Gyulbudaghian, Glushkov & Denisyuk (1978); 2 – Hughes (1989); 3 – Corcoran, Ray & 

Mundt (1993); 4 – Bally et al. (1999); 5 – Hartigan, Morse & Bally (2000); 6 – Devine et al. (1997). 

6. Star Formation in Cepheus OB4 

6.1. Structure of Cep OB4 

Cep OB4 was discovered by Blanco & Williams (1959), who noticed the presence of 

16 early-type stars in a small region around (l,b)=(118. ◦ 4,+4. ◦ 7), including the cluster 

Berkeley 59. Cep OB4 is related to a dense, irregular dark cloud containing several 

emission regions, including the dense H II region S 171 (W 1) in the central part, and 

NGC 7822 to the north of S 171 (Lozinskaya, Sitnik & Toropova 1987), see Fig. 34. We 

note that in the original catalogs both W 1 (RA(J2000)=00 02 52; Dec(J2000)=+67 14, 

Westerhout 1958) and S 171 (RA(J2000)=00 04 40.3; Dec(J2000)=+67 09, Sharpless 

1959) are associated with NGC 7822, situated about one degree north of the HII region, 

according to its catalog coordinates (RA(J2000)=00 03.6; Dec(J2000)=+68 37). The 

Simbad data server also associates these objects with each other. A detailed description 

of the association and related objects was given by MacConnell (1968). He identified

42 members earlier than B8 at 845 pc. MacConnell’s UBV photometric study of the 

luminous members of Cep OB4 revealed a correlation between the luminosity and reddening 

of the stars: the O and early B stars were found only within the cloud, whereas 

later B type stars are found only outside the cloud due to the incompleteness of their 

detection. Based on the absence of supergiants, an earliest spectral type of O7 V, and 

the gravitational contraction time of a B8 star, MacConnell estimated an age between 

0.6 and 6 Myr. 

87 

BRC 2 

69 00 

NGC 7822 

68 00 

AFGL 4305 

Cepheus Loop 

Berkeley 59 

Dec(J2000) 

67 00 

S171 (W1) 

BRC 1 

AFGL 3193 

BRC 3 

66 00 

Cloud M 120.1 + 3.0 

65 00 

00 20 00 10 00 00 23 50 

RA(J2000) 

Figure 34. A large scale red photograph of the Cep OB4 region. The infrared 

sources and the radio continuum loop are indicated on the red DSS image. The HII 

region W1 is also known as S171. Star symbols show the luminous stars of Cep OB4 

(Rossano et al. 1983), and crosses mark the Hα emission stars (MacConnell 1968). 

Lozinskaya et al. (1987) studied the morphology and kinematics of the H II regions 

associated with Cep OB4 based on monochromatic images of the [OIII], [NII], 

[SII] and Hα lines, and found two expanding shells: one shell, of radius ∼0. ◦ 7, connects 

NGC 7822 and S 171. Most Cep OB4 members are located inside this shell; their en-

88 

ergy input into the interstellar medium can account for its observed size and expansion 

velocity of 10 km s −1 . The other shell, of radius ∼1. ◦ 5, is centered on S 171 and has an 

expansion velocity of ∼30–40 km s −1 ; it may be the result of a supernova explosion or 

of the stellar wind of a massive star that so far has escaped detection. 

Olano et al. (2006) found that the space distribution and kinematics of the interstellar 

matter in the region of Cep OB4 suggest the presence of a big expanding 

shell, centered on (l,b) ∼ (122 ◦ ,+10 ◦ ). Assuming a distance of 800 pc for the center 

they derived a radius of some 100 pc, expansion velocity of 4 km s −1 , and HI mass of 

9.9 × 10 4 M⊙ for the Cepheus OB4 Shell, whose approximate position is plotted in 

Fig. 1. 

Only 19 of the 42 classical members of Cep OB4 are listed in the Hipparcos Catalog 

(de Zeeuw et al. 1999). This may be caused by a combination of crowding effects 

and the large extinction toward Cep OB4, A V > 3 mag (MacConnell 1968). Based 

on their proper motions and parallaxes, three MacConnell stars (HIP 117724, 118192, 

118194) are not associated with Cep OB4. De Zeeuw et al. (1999) found that the 

Hipparcos parallaxes of the other classical members are consistent with a distance of 

800–1000 pc. 

Rossano, Grayzeck & Angerhofer (1983) mapped the Cep OB4 region in the 6 cm 

transition of H 2 CO, and detected neutral gas at the velocities −13, −7, and −1 km s −1 . 

They established that Cep OB4 consisted of two kinematically distinct components, 

W1 west and W1 east, and a loop-shaped, optically thin, thermal shell, the Cep Loop. 

They modeled the observed morphology and kinematics as follows. The association 

Cep OB4 consists of two subgroups with differing ages and kinematic properties. The 

older, dispersed, subgroup extends over an area about 4 degrees (60 pc) in diameter, 

clustered towards the Cep Loop. The younger subgroup, the young cluster Berkeley 59, 

extends over an area of 15 ′ (about 4 pc) in diameter, located along the southern edge of 

the Cep Loop. The average velocity of the OB stars of the older subgroup is −6 km s −1 . 

Thus Rossano et al. (1983) propose that the gas component at −7 km s −1 represents the 

undisturbed gas associated with the star forming region. Beginning with a cloud complex 

having a velocity of −7 km s −1 , star formation occurred near the center of what is 

now the Cep Loop. The Cep Loop was subsequently formed by this first generation of 

OB stars. Expansion of the Cep Loop into a cloud to the north resulted in collisional 

excitation of the HII region NGC 7822. In the south, expansion of the Cep Loop resulted 

in fragmentation of the remainder of the original dark complex producing clouds 

at −13 and −1 km s −1 . Berkeley 59 was formed in this environment. Ionization of the 

clouds surrounding Berkeley 59 has resulted in ionized gas at each velocity component. 

Ionization is now occurring most actively in a −1 km s −1 cloud west of Be 59. Okada 

et al. (2003) studied the photodissociation region associated with S 171 using mid- to 

far-infrared spectroscopy using the ISO SWS, LWS, and PHT-S instruments. Gahm et 

al. (2006) investigated the structure and velocity of an elephant trunk associated with 

NGC 7822. Figure 34, based on Fig. 1 of Rossano et al. (1983), shows a large scale red 

photograph of the Cep OB4 region. The infrared sources and the radio continuum loop 

are indicated. Star symbols show the luminous stars of Cep OB4, and crosses mark the 

Hα emission stars. 

6.2. Low and Intermediate Mass Star Formation in Cep OB4 

MacConnell (1968) found 24 Hα emission-line (named as MacC H1–H24) objects 

within the dark cloud in the region of Cep OB4, some of which may be T Tauri stars.

89 

Figure 35. Hα emission stars discovered by Ogura et al. (2002) in BRC 1 (left) 

and BRC 2 (right) associated with S 171. The position of the IRAS source associated 

with the cloud is shown by a pair of thick tick marks. 

Cohen & Kuhi (1976) obtained optical spectrophotometry and infrared photometry of 

some MacC H stars, determined their spectral types and luminosities, as well as masses 

and ages using Iben’s (1965) pre-main sequence evolutionary tracks. They identified 

four new nebulous stars in the same field (MC 1–MC 4), three of which have shown Hα 

emission. Table 24 lists the Hα emission stars found by MacConnell, and nebulous Hα 

emission stars reported by Cohen & Kuhi (1976), supplemented by the spectral types 

determined by Cohen & Kuhi (1976). 

Sharma et al. (2007) obtained slitless spectroscopy and JH photometry for Berkeley 

59. They identified 9 Hα emission stars, whose location in the J/J−H colormagnitude 

diagram indicates that they may be pre-main sequence stars. The age of the 

cluster was estimated from the turn-off and turn-on points and is found to lie between 

about 1 and 4 million years. Pandey et al. (2008) present UBV I C CCD photometry 

of Be 59 with the aim to study the star formation scenario in the cluster. Using slitless 

spectroscopy, they have identified 48 Hα emission stars in the region of Be 59. 

The ages of these YSOs range between

90 

Table 24. Data for the Hα emission stars found by MacConnell (1968) and Cohen 

& Kuhi (1976) in the region of Cep OB4 

Name Other name RA(2000) Dec(2000) V B−V U−B Type Remarks 

H1 HBC 742 23 52 33.0 68 25 55 14.97 1.47 +0.27 B8eα 

H2 23 41 45.0 66 39 36 12.47 1.1 −0.09 1 

H3 HBC 319, Blanco 1 23 54 26.6 66 54 17 14.50 1.09 −0.15 K2 2,20 

H4 HBC 321n, Blanco 3 23 58 41.4 66 26 11 14.67 1.96: A9eα 3 

H5 HBC 322, Blanco 4 23 59 20.2 66 23 10 15.80 1.75: K5 4,20 

H6 23 59 12.0 66 22 16 16.79 pT 

H7 Blanco 5 0 00 57.3 66 28 53 16.68 0.97 pT 5 

H8 Blanco 11 0 15 21.6 65 45 32 17.33 0.60: pT 6 

H9 Blanco 10 0 13 29.1 65 35 59 14.96 1.28: +0.72: K4 7,20 

H10 Blanco 9 0 12 54.4 65 34 09 14.72 1.51: +0.52: K4 8,20 

H11 Blanco 7 0 07 06.1 65 40 15 16.83 0.92: pT 

H12 0 07 03.1 65 38 37 16.23 1.12: F: 9,20 

H13 Blanco 8 0 07 18.4 65 36 42 16.77 0.87: pT 10 

H14 23 41 24.8 65 40 40 15.74 

H15 GG 179 0 17 35.0 65 16 08 12.12 1.04 −0.10 11 

H16 Sh 118 0 07 20.2 64 57 21 13.79 1.17 −0.36 12 

H17 0 04 52.2 65 05 49 13.49 0.83 −0.12 13 

H18 HBC 323, Blanco 6 0 02 13.0 64 54 22 14.21 1.29: +0.02: K7 14,20 

H19 HBC 320, Blanco 2 23 57 34.3 64 54 21 14.21 1.29: +0.02: K3 15,20 

H20 GG 162 23 50 02.3 64 41 41 12.23 

H21 0 06 40.6 65 34 52 11.55 0.49 +0.32 16 

H22 MWC 1085 23 52 12.4 67 10 07 9.96 0.53 −0.22 B3e 17 

H23 AS 517 23 57 33.9 66 25 54 10.37 0.70 +0.01 B5e 18 

H24 AS 2 0 12 58.9 66 19 19 10.68 0.77 +0.25 B5e 19 

MC1 0 06 57.9 65 37 21 14.6 A5 20 

MC2 0 35 57.5 66 19 15 14.1 A2 20 

MC3 0 16 35.0 65 43 20 16.8 K5 20 

MC4 0 16 42.0 65 44 20 14.4 K4 20 

sH15 0 13 23.9 65 35 20 13.6 K1 20 

Remarks: (1) Faint, blue continuum; could be Be. (2) Probable Ca II infrared emission; suspected var. in 

B. (3) LkHa 259; probably not T Tauri type. (4) Found independently by Herbig (unpublished); probable 

Ca II infrared emission; var. in B and V. (5) Found independently by Herbig (unpublished). (6) Suspected 

var. in B (no filter) and V. (8) Found independently by Herbig (unpublished); probable var. in V. (7) 

Found independently by Herbig (unpublished); probable var. in V. (8) Found independently by Herbig 

(unpublished); probable var. in V. (9) Near-red nebulosity; probable Ca II infrared emission; var. in V. 

(10) Var. in V. (11) Faint, blue continuum; could be Be. (12) Known planetary nebula, Sh 118. (13) 

Faint, blue continuum; could be Be. (14) Var. in U and V. (15) Var. in U and V. (16) New Be star; 

spectral type about B8, very broad Balmer lines, particularly Hζ and Hη. (17) Known Be star; No. 30 of 

MacConnell’s Table 3. (18) Known Be star; No. 33 of MacConnell’s Table 3. (19) Known Be star; No. 

32 of MacConnell’s Table 3. (20) Spectral type from Cohen & Kuhi (1976) 

(2008). Table 25 lists the coordinates and Hα equivalent widths (revised by Ikeda et al. 

2008) of these stars, and Fig. 35 shows the finding charts. 

The bright rimmed cloud BRC 2 contains a compact cluster of Hα emission stars. 

The S 171 cluster was observed by the IRAC on board the Spitzer Space Telescope 

(Megeath et al. 2004). The cluster of young stars is situated near the edge of the cloud 

with a dense group of five Class I sources at the northern apex of the cluster. This morphology 

suggests that star formation is triggered by a photoevaporation-driven shock 

wave propagating into the cloud, as first proposed for this region by Sugitani et al.

91 

Table 25. Hα emission stars associated with bright rimmed clouds of S 171 and 

NGC 7822 (Ogura et al. 2002; Ikeda et al. 2008). 

N RA(J2000) Dec(J2000) EW(Hα) Remarks 

BRC 1 

1 23 59 42.50 67 22 27.8 · · · invisible cont., contam. from nearby star 

2 23 59 43.72 67 25 50.0 26.6 weak cont. 


4 23 59 47.61 67 23 11.2 · · · Hα ?, invisible cont. 

5 23 59 47.98 67 23 06.9 · · · Hα ?, weak cont. 

6 23 59 52.75 67 25 37.5 32.6 weak cont. 

BRC 2 

1 00 03 51.03 68 33 15.8 · · · Hα ? 


3 00 03 54.52 68 33 44.6 · · · contam. from nearby stars 

4 00 03 54.98 68 32 42.8 145.7 very weak cont. 

5 00 03 57.12 68 33 46.7 15.6 

6 00 03 57.35 68 33 23.0 99.6 

7 00 03 58.33 68 34 06.5 13.1 

8 00 03 59.12 68 32 47.3 18.2 

9 00 04 01.70 68 34 13.8 2.8 

10 00 04 01.81 68 34 00.0 14.0 

11 00 04 01.80 68 34 37.4 5.5 

12 00 04 01.88 68 34 34.5 21.2 

13 00 04 02.32 68 31 36.2 · · · Hα ? 

14 00 04 02.65 68 34 26.6 24.9 

15 00 04 04.69 68 33 49.3 25.8 weak cont. 

16 00 04 04.59 68 34 52.2 23.0 

17 00 04 05.28 68 33 56.0 136.6 very weak cont. 

18 00 04 05.26 68 33 53.1 50.4 

19 00 04 05.66 68 33 44.3 94.5 


21 00 04 07.60 68 33 25.1 12.8 

22 00 04 11.66 68 33 25.4 46.7 

23 00 04 13.97 68 32 21.8 85.7 weak cont. 

24 00 04 14.71 68 32 49.1 42.1 

25 00 04 15.18 68 33 02.0 16.1 

26 00 04 15.41 68 34 05.5 26.6 very weak cont. 

27 00 04 21.66 68 30 59.6 · · · Hα ? 

28 00 04 25.36 68 32 31.0 12.3 weak cont. 

29 00 04 29.99 68 31 19.9 · · · Hα ? 

30N 00 03 59.88 68 33 41.7 1.4 

(1991). In addition to the stars in the cluster, Spitzer detected six Class II and two 

Class I objects spread throughout the molecular cloud. The presence of these stars 

suggests that a distributed mode of star formation is also occurring in the cloud. 

A new generation of low mass stars has been born in the molecular clouds in 

the neighborhood of the young luminous stars. Yang et al. (1990) reported on the 

discovery of a molecular cloud in Cep OB4. The cloud M 120.1+3.0, appearing dense 

and filamentary, is composed of two parts. Each of the two parts has a size of 6 pc×1 pc, 

and a mass of 800 M⊙. The cloud is associated with 12 low luminosity (L < 20 L⊙) 

IRAS sources, and the locations of the sources show remarkable coincidence with the 

distribution of the dense molecular gas. Two molecular outflows have been discovered 

towards two IRAS sources, IRAS 00213+6530 and IRAS 00259+6510. The results 

indicate that low-mass star formation took place recently in the cloud.

92 

7. Cepheus OB6 

The nearby association Cep OB6 first appeared in the literature in 1999. De Zeeuw 

et al. (1999) identified this moving group of 27 stars in the Hipparcos data base. The 

stars show a modest concentration at (l,b)≈ (104. ◦ 0, −0. ◦ 5). The final sample contains 

20 stars, 6 B, 7 A, 1 F, 2 G and 3 K type in the area 110 ◦ < l < 110 ◦ , and −2 ◦ < 

b < +2 ◦ . The brightest member is the K1Ib supergiant ζ Cep (HIP 109492). The 

color–magnitude diagram is very narrow, and strengthens the evidence that these stars 

form a moving group, that is, an old OB association. The earliest spectral type is B5III, 

suggesting an age of some 50 million years. The mean distance of the association is 

270 ±12 pc. The supergiant δ Cephei, the archetype of Cepheid variables, also belongs 

to Cep OB6. Makarov (2007) during his study of the Galactic orbits of nearby stars 

found that a few members of the AB Dor moving group were in conjunction with the 

coeval Cepheus OB6 association 38 Myr ago. He proposed that the AB Dor nucleus 

formed 38 Myr ago during a close passage of, or encounter with, the Cepheus OB6 

cloud, which may have triggered formation of the latter association as well. No younger 

subgroup of Cep OB 6 has been identified. 

Acknowledgments. This work was supported by the Hungarian OTKA grant 

T049082. We are grateful to Jeong-Eun Lee for sending us the results on L 1251 B 

before publication, to Miklós Rácz for his help with some figures, to László Szabados 

for a careful reading of the manuscript, and to Tom Megeath for the data in Table 17. 

We thank Giovanni Benintende, Richard Gilbert, John Bally, Robert Gendler, and Davide 

De Martin for the use of figures 6, 8, 10, 12, and 16, respectively. Bo Reipurth’s 

referee report led to an enormous improvement of this chapter. We used the Simbad 

and ADS data bases throughout this work. 

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