A CS J  = 5 → 4 Mapping Survey Toward High‐Mass Star‐forming Cores Associated with Water Masers

Abstract

We have mapped 63 regions forming high-mass stars in CS J ¼ 5 ! 4 using the CSO. The CS peak position was observed in C 34 S J ¼ 5 ! 4 toward 57 cores and in 13 CS J ¼ 5 ! 4 toward the nine brightest cores. The sample is a subset of a sample originally selected toward water masers; the selection on maser sources should favor sources in an early stage of evolution. The cores are located in the first and second Galactic quadrants with an average distance of 5:3 AE 3:7 kpc and were well detected with a median peak signalto-noise ratio in the integrated intensity of 40. The integrated intensity of CS J ¼ 5 ! 4 correlates very well with the dust continuum emission at 350 lm. For 57 sufficiently isolated cores, a well-defined angular size (FWHM) was determined. The core radius (R CS ), aspect ratio [ða=bÞ obs ], virial mass (M vir ), surface density (AE), and the luminosity in the CS J ¼ 5 ! 4 line (LðCS54Þ) are calculated. The distributions of size, virial mass, surface density, and luminosity are all peaked with a few cores skewed toward much larger values than the mean. The median values, l 1/2 , are as follows: l 1/2 ðR CS Þ ¼ 0:32 pc, l 1/2 ðða=bÞ obs Þ ¼ 1:20, l 1/2 ðM vir Þ ¼ 920 M , l 1/2 ðAEÞ ¼ 0:60 g cm À2 , l 1/2 ðLðCS54ÞÞ ¼ 1:9 Â 10 À2 L , and l 1/2 ðL bol =M vir Þ ¼ 165 ðL=MÞ . We find a weak correlation between C 34 S line width and size, consistent with Dv $ R 0:3 . The line widths are much higher than would be predicted by the usual relations between line width and size determined from regions of lower mass. These regions are very turbulent. The derived virial mass agrees within a factor of 2-3 with mass estimates from dust emission at 350 lm after corrections for the density structure are accounted for. The resulting cumulative mass spectrum of cores above 1000 M can be approximated by a power law with a slope of about À0.9, steeper than that of clouds measured with tracers of lower density gas and close to that for the total masses of stars in OB associations. The median turbulent pressures are comparable to those in UCH ii regions, and the pressures at small radii are similar to those in hypercompact H ii regions (P=k $ 10 10 K cm À3 ). The filling factors for dense gas are substantial, and the median abundance of CS is about 10 À9 . The ratio of bolometric luminosity to virial mass is much higher than the value found for molecular clouds as a whole, and the correlation of luminosity with mass is tighter.

G30.79 FIR 10: a gravitationally bound infalling high-mass star-forming clump

“…Barnes et al (2008) estimated infall rates of 3 × 10 −2 M yr −1 with an infalling velocity of 0.3 km s −1 for the G286.21+0.17 molecular clump. Both regions present similar gas densities as G30.79 FIR 10 (1.9 × 10 5 cm −3 for G286.21+0.17 and 7.2 × 10 5 cm −3 for G10.47) and similar mass estimations (4.1 × 10 4 M for G286.21+0.17 and 7.3 × 10 3 M for G10.47 as estimated by Shirley et al 2003). These results are consistent with our findings where these regions appear to be in a similarly evolutionary stage.…”

Inverse dynamical population synthesis

“…indeed find that a dense initial configuration can be less dense today than another initially less dense cluster. Figure 6 shows that the constraints compare well with masses and densities of molecular clumps that have just begun to form stars (Mueller et al 2002;Shirley et al 2003;Fontani et al 2005). The masses of the clumps from these sources have been multiplied with a star-formation efficiency of one-third for comparison with the stellar masses and densities calculated here.…”

Formation of a protocluster: A virialized structure from gravoturbulent collapse

“…Larger data sets of star-forming clumps, identified as gaseous protoclusters, also exhibit a mass-size relation. Fall et al (2010) compiled the observations of Shirley et al (2003), Faúndez et al (2004), and Fontani et al (2005) in their Fig. 1, and found via least-squares regression the relation R ∝ M 0.38 .…”