Table 5: Coordinates for all sources discussed (taken from MSX  data). Comment descriptions include: massive young stellar object candidate (MYSO); compact ${\rm H~{\scriptstyle {II}}}$  regions ( ${\rm H~{\scriptstyle {II}}}$); bright stellar object (S); tip of a filamentary feature (T); molecular condensation (MC); cluster (C); diffuse $K_{\rm s}$-band emission (DE); red object in 2MASS  images (R) and any additional nomenclature. The divisions in the table separate the MYSO, the compact ${\rm H~{\scriptstyle {II}}}$  regions, the sources that most likely correspond to evolved stars, the source displaying an extremely red colour in 2MASS  images, and the molecular condensations. Fluxes for these sources are given in Rathborne (2003).
Source Coordinates Comments
  $\alpha_{\footnotesize {J2000}}$ $\delta_{\footnotesize {J2000}}$  
G287.87-1.36 10 44 17.9 -60 27 46 MYSO; B0-star
      IRAS 10423-6011
G287.52-0.41 10 45 20.9 -59 27 28 ${\rm H~{\scriptstyle {II}}}$; O8.5-star
      IRAS 10434-5911
G287.84-0.82 10 45 53.6 -59 57 10 ${\rm H~{\scriptstyle {II}}}$; MC; C;
      OB-cluster;
      IRAS 10439-5941
G287.88-0.93 10 46 00.9 -60 05 12 ${\rm H~{\scriptstyle {II}}}$; T; B0-star
      IRAS 10441-5949
G287.57-0.91 10 43 51.1 -59 55 23 ${\rm H~{\scriptstyle {II}}}$; T
G287.51-0.49 10 44 59.0 -59 31 24 ${\rm H~{\scriptstyle {II}}}$; DE
G287.22-0.53 10 42 49.2 -59 25 27 ${\rm H~{\scriptstyle {II}}}$; DE
G287.47-0.54a 10 44 32.8 -59:33:20 ${\rm H~{\scriptstyle {II}}}$; DE
G287.63-0.72b 10 45 01.1 -59 47 06 ${\rm H~{\scriptstyle {II}}}$; DE
      IRAS 10430-5931
G287.75-0.66 10 46 01.2 -59 46 58 ${\rm H~{\scriptstyle {II}}}$; DE
G287.76-0.87 10 45 22.3 -59 58 23 ${\rm H~{\scriptstyle {II}}}$
G287.68-1.09 10 43 57.2 -60 08 25 ${\rm H~{\scriptstyle {II}}}$
G287.73-1.01 10 44 34.6 -60 05 36 S; HD 93222
G287.80-0.56 10 46 46.8 -59 43 25 S
G287.86-0.82 10 46 13.9 -59 58 41 R
G287.73-0.92 10 44 45.4 -59 59 16 MC
G287.93-0.99 10 45 56.1 -60 08 50 MC; C?
G288.07-0.80 10 47 35.4 -60 02 51 MC
a Source N4 from Rathborne et al. (2002).
b Identified by Megeath et al. (1996).


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