Fifty-one dense cores associated with water masers were mapped at 350 lm. These cores are very luminous, 10 3 < L bol =L < 10 6 , indicative of the formation of massive stars. Dust continuum contour maps, radial intensity profiles, and photometry are presented for these sources. The submillimeter dust emission peak is, on average, nearly coincident with the water maser position. The spectral energy distributions and normalized radial profiles of dust continuum emission were modeled for 31 sources using a one-dimensional dust radiative transfer code, assuming a power-law density distribution in the envelope, n ¼ n f ðr=r f Þ Àp . The bestfit density power-law exponent, p, ranged from 0.75 to 2.5 with hpi ¼ 1:8 AE 0:4, similar to the mean value found recently by Beuther and coworkers in a large sample of massive star-forming regions. The mean value of p is also comparable to that found in regions forming only low-mass stars, but hn f i is over 2 orders of magnitude greater for the massive cores. The mean p is incompatible with a logatropic sphere (p ¼ 1), but other star formation models cannot be ruled out. Different mass estimates are compared and mean masses of gas and dust are reported within a half-power radius determined from the dust emission, hlog Mð< r dec Þi ¼ 2:0 AE 0:6, and within a radius where the total density exceeds 10 4 cm À3 , hlog Mð< r n Þi ¼ 2:5 AE 0:6. Evolutionary indicators commonly used for low-mass star formation, such as T bol and L bol /L smm , may have some utility for regions forming massive stars. Additionally, for comparison with extragalactic star formation studies, the luminosity-to-dust mass ratio is calculated for these sources, hL bol =M D i ¼ 1:4 Â 10 4 L /M , with a method most parallel to that used in studies of distant galaxies. This ratio is similar to that seen in high-redshift starburst galaxies.

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ABSTRACT. We have conducted a search for Ha emission-line stars within the Ðeld containing the reÑection nebula NGC 2626 and the associated dark cloud DC 259.9[0.0. Thirty-two Ha stars, most of them newly discovered, have been identiÐed. Magnitudes and colors for these stars are listed. Some are found to be variable and are possible T Tauri stars. Changes between 1991 and 1999 in the brightness and appearance of a small reÑection nebula in the region are shown. These are caused by an unevenly obscured young stellar object which is the probable source of IRAS 08337[4028 and the Herbig-Haro object HH 132. The overall morphology of the small nebula is strikingly similar to that of the well-studied HH 46È47 conÐguration, but the NGC 2626 region is at about twice the distance.