2011A&A...531A..26B


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.15CEST07:39:52

2011A&A...531A..26B - Astronomy and Astrophysics, volume 531A, 26-26 (2011/7-1)

High-mass star formation at high luminosities: W31 at >106 L☉.

BEUTHER H., LINZ H., HENNING Th., BIK A., WYROWSKI F., SCHULLER F., SCHILKE P., THORWIRTH S. and KIM K.-T.

Abstract (from CDS):

High-mass star formation has been a very active field over the past decade; however, most studies have targeted regions of luminosities between 104 and 105L. In contrast to that, the highest mass stars reside in clusters exceeding 105 or even 106L. We want to study the physical conditions associated with the formation of the highest mass stars. To do this, we selected the W31 star-forming complex with a total luminosity of ∼6x106L (comprised of at least two subregions) for a multiwavelength spectral line and continuum study covering wavelengths from the near- and midinfrared via (sub)mm wavelength observations to radio data in the cm regime. While the overall structure is similar among the multiwavelength continuum data, there are several intriguing differences. The 24µm emission stemming largely from small dust grains tightly follows the spatial structure of the cm emission tracing the ionized free-free emission. As a result, warm dust resides in regions that are spatially associated with the ionized hot gas (∼104K) of the HII regions. Furthermore, we find several evolutionary stages within the same complexes, ranging from infrared-observable clusters, via deeply embedded regions associated with active star formation traced by 24µm and cm emission, to at least one high-mass gas clump devoid of any such signature. The 13CO(2-1) and C18O(2-1) spectral line observations reveal kinematic breadth in the entire region with a total velocity range of approximately 90km/s. Kinematic and turbulent structures are set into context. While the average virial mass ratio for W31 is close to unity, the line width analysis indicates large-scale evolutionary differences between the southern and northern subregions (G10.2-0.3 and G10.3-0.1) of the whole W31 complex. A color-color analysis of the IRAC data also shows that the class II sources are broadly distributed throughout the entire complex, whereas the Class 0/I sources are more tightly associated with the active high-mass star-forming regions. The clump mass function - tracing cluster scales and not scales of individual stars - derived from the 875µm continuum data has a slope of 1.5±0.3, consistent with previous cloud mass functions. The highest mass and luminous stars form in highly structured and complex regions with multiple events of star formation that do not always occur simultaneously but in a sequential fashion. Warm dust and ionized gas can spatially coexist, and high-mass starless cores with low-turbulence gas components can reside in the direct neighborhood of active star-forming clumps with broad linewidths.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: early-type - stars: individual: W31 - stars: evolution - stars: massive

VizieR on-line data: <Available at CDS (J/A+A/531/A26): table1.dat table2.dat list.dat images/*>

Nomenclature: Tables 1-2: [BLH2011] 1-NN (Nos 1-73). Table 2: [BLH2011] 2-NN (Nos 1-44).

Status in Simbad:  could be processed

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2925 0
2 NAME NGC 6334-I Cl* 17 20 53.35 -35 47 01.5           ~ 255 0
3 NAME NGC 6334 I(N) smm 17 20 54 -35 45.0           ~ 119 1
4 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 316 1
5 [WC89] 010.30-0.15B HII 18 08 55.924 -20 05 54.64           ~ 28 0
6 MMB G010.299-00.146 Mas 18 08 56.0595 -20 05 59.787           ~ 45 0
7 GAL 010.30-00.15 HII 18 08 58.315 -20 05 15.27           ~ 77 0
8 GAL 010.15-00.34 HII 18 09 21.5680 -20 19 27.720           ~ 72 0
9 GAL 010.2-00.3 HII 18 09 24.6 -20 19 29           ~ 77 1
10 W 31 SFR 18 10 28.6 -19 55 51           ~ 240 0
11 W 31c HII 18 10 29.1 -19 56 05           ~ 298 0
12 IRAS 18449-0115 cor 18 47 34.4947 -01 12 40.269           ~ 291 0
13 W 49 SFR 19 10 20 +09 07.7           ~ 501 1

    Equat.    Gal    SGal    Ecl

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2019.10.15-07:39:52

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