Star Forming Regions in Cepheus

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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.
Page 1 and 2: Handbook of Star Forming Regions Vo
Page 3 and 4: note that the LDN coordinates, deri
Page 5 and 6: Table 1.: List of clouds catalogued
Page 7 and 8: Table 1.: Continued. Cloud name RA(
Page 17 and 18: 17 Table 2. Cloud groups in Cepheus
Page 19 and 20: 19 Table 3. Distance measured for t
Page 21 and 22: 21 300 l=180 o Loop III - old super
Page 23 and 24: We find these objects in statistica
Page 25 and 26: Class 0 object, L 1157-mm, with L b
Page 27 and 28: long) Herbig-Haro flow, HH 315, con
Page 29 and 30: GF 9-6 and GF 9-7 are most likely r
Page 31 and 32: Table 7.: Pre-main sequence stars i
Page 33 and 34: Table 7.: Pre-main sequence stars i
Page 35 and 36: 35 Figure 9. 13 CO contours of the
Page 37 and 38: 37 Figure 10. Hα + [SII] image of
Page 39 and 40: associated with a low-luminosity (2
Page 41 and 42: 41 Figure 12. An optical image of N
Page 43 and 44: 43 66 14 GGD 33a,b V350 Cep 66 12 6
Page 45: 45 Table 8. Embedded YSOs in NGC 71
Page 49 and 50: stars that are spread over a large
Page 51 and 52: M) pre-main sequence members of Tr
Page 53 and 54: 53 Table 10. uncertain. B. Other cl
Page 55 and 56: Moriarty-Schieven et al. (1996) hav
Page 57 and 58: 57 Figure 18. Hα emission stars in
Page 59 and 60: are. About 5% of the mass of the gl
Page 61 and 62: 61 HH 778 HH 777 IRS HH 777 HH 780
Page 63 and 64: cluded in a high angular resolution
Page 65 and 66: gions associated with the Cepheus B
Page 67 and 68: 67 Figure 23. Optical and NIR image
Page 69 and 70: 69 Table 14. Position of far-infrar
Page 71 and 72: from IRS 3, while the source of the
Page 73 and 74: 73 Figure 25. Left: 100 µm optical
Page 75 and 76: 75 4 Cep F V733 Cep Galactic latitu
Page 77 and 78: 77 62 50 HD 217486 62 45 Dec(J2000)
Page 79 and 80: 79 Figure 31. VLA map at 6 cm of Ce
Page 81 and 82: Torrelles et al. (2007) report SMA
Page 83 and 84: 83 Table 19. et al. 2002) Hα emiss
Page 85 and 86: 85 Table 20. Near-infrared sources
Page 87 and 88: 42 members earlier than B8 at 845 p
Page 89 and 90: 89 Figure 35. Hα emission stars di
Page 91 and 92: 91 Table 25. Hα emission stars ass
Page 93 and 94: Ayala, S., Noriega-Crespo, A., Garn
Page 95 and 96: Elmegreen, D. M. & Elmegreen, B. G.
Page 97 and 98:
Hoogerwerf, R., de Bruijne, J. H. J
Page 99 and 100:
Minchin, N. R., Krause, D., Stutzki
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101 Rouan, D., Lena, P. J., Puget,
Page 103 and 104:
103 Velusamy, T., Langer, W. D., &
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Star Forming Regions in Cepheus

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