2017ApJ...842...92G


Query : 2017ApJ...842...92G

2017ApJ...842...92G - Astrophys. J., 842, 92-92 (2017/June-3)

Thermal feedback in the high-mass star and cluster forming region W51.

GINSBURG A., GODDI C., KRUIJSSEN J.M.D., BALLY J., SMITH R., GALVAN-MADRID R., MILLS E.A.C., WANG K., DALE J.E., DARLING J., ROSOLOWSKY E., LOUGHNANE R., TESTI L. and BASTIAN N.

Abstract (from CDS):

High-mass stars have generally been assumed to accrete most of their mass while already contracted onto the main sequence, but this hypothesis has not been observationally tested. We present ALMA observations of a 3×1.5 pc area in the W51 high-mass star-forming complex. We identify dust continuum sources and measure the gas and dust temperature through both rotational diagram modeling of CH3OH and brightness-temperature-based limits. The observed region contains three high-mass YSOs that appear to be at the earliest stages of their formation, with no signs of ionizing radiation from their central sources. The data reveal high gas and dust temperatures (T 100 K) extending out to about 5000 au from each of these sources. There are no clear signs of disks or rotating structures down to our 1000 au resolution. The extended warm gas provides evidence that, during the process of forming, these high-mass stars heat a large volume and correspondingly large mass of gas in their surroundings, inhibiting fragmentation and therefore keeping a large reservoir available to feed from. By contrast, the more mature massive stars that illuminate compact H II regions have little effect on their surrounding dense gas, suggesting that these main-sequence stars have completed most or all of their accretion. The high luminosity of the massive protostars (L 104L), combined with a lack of centimeter continuum emission from these sources, implies that they are not on the main sequence while they accrete the majority of their mass; instead, they may be bloated and cool.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): H II regions - ISM: abundances - ISM: clouds - ISM: individual objects: W51 - stars: formation - stars: massive - stars: massive

Nomenclature: Tables 7-8: [GGK2017] ALMAmmNN (Nos 1-57). Table 8: [GGK2017] aN (Nos d2, e5), [GGK2017] e2e N=1, [GGK2017] e2e peak N=1, [GGK2017] e2ww (Nos e2nw, e2se, e2w), [GGK2017] eNmmN (Nos e1mm1, e3mm1, e8mm), [GGK2017] eWmmNa (Nos eEmm1-eEmm3, eSmm1-eSmm2, eSmm2a, eSmm3-eSmm6), [GGK2017] north N=1.

Status at CDS : All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15530 1
2 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 454 0
3 * eta Car Em* 10 45 03.545808 -59 41 03.95124 6.37 7.03 6.48 4.90 4.41 OBepec 2284 0
4 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 990 1
5 NGC 3606 GiG 11 16 15.645 -33 49 38.67   13.42   11.72   ~ 59 0
6 NAME RCW 106 GMC MoC 16 21.0 -50 30           ~ 36 0
7 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2031 1
8 W 49 SFR 19 10 20 +09 07.7           ~ 529 1
9 [OMN2000] Region 3 PoC 19 23 29.3 +14 31 38           ~ 155 0
10 OKYM W51 IRS 2 6 IR 19 23 39.816 +14 31 05.07           ~ 22 0
11 NAME W 51 North Rad 19 23 40.0 +14 30 51           ~ 147 0
12 [WBN74] W 51 IRS 2 SFR 19 23 40.05 +14 31 07.1           ~ 258 0
13 W 51e1 Rad 19 23 43.77 +14 30 25.9           ~ 118 0
14 NAME W 51 Main reg 19 23 43.8 +14 30 37           ~ 134 0
15 W 51e2 Rad 19 23 43.90 +14 30 34.8           ~ 189 0
16 [SZH2010] W51e2-E Rad 19 23 43.960 +14 30 34.56           ~ 14 0
17 W 51e8 HII 19 23 44.2 +14 30 28           ~ 35 0
18 W 51 SNR 19 23 50 +14 06.0           ~ 1191 1

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2021.09.16-23:24:55

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