2010A&A...520A..50S


Query : 2010A&A...520A..50S

2010A&A...520A..50S - Astronomy and Astrophysics, volume 520, A50-50 (2010/9-2)

The molecular environment of the galactic star forming region G19.61-0.23.

SANTANGELO G., TESTI L., LEURINI S., WALMSLEY C.M., CESARONI R., BRONFMAN L., CAREY S., GREGORINI L., MENTEN K.M., MOLINARI S., NORIEGA-CRESPO A., OLMI L. and SCHULLER F.

Abstract (from CDS):

Although current facilities allow the study of Galactic star formation at high angular resolution, our current understanding of the high-mass star-formation process is still very poor. In particular, we still need to characterize the properties of clouds giving birth to high-mass stars in our own Galaxy and use them as templates for our understanding of extragalactic star formation. We present single-dish (sub)millimeter observations of gas and dust in the Galactic high-mass star-forming region G19.61-0.23, with the aim of studying the large-scale properties and physical conditions of the molecular gas across the region. The final aim is to compare the large-scale (about 100pc) properties with the small-scale (about 3pc) properties and to consider possible implications for extragalactic studies. We have mapped CO isotopologues in the J=1-0 transition using the FCRAO-14m telescope and the J=2-1 transition using the IRAM-30m telescope. We have also used APEX 870µm continuum data from the ATLASGAL survey and FCRAO supplementary observations of the 13CO J=1-0 line from the BU-FCRAO Galactic Ring Survey, as well as the Spitzer infrared Galactic plane surveys GLIMPSE and MIPSGAL to characterize the star-formation activity within the molecular clouds. We reveal a population of molecular clumps in the 13CO(1-0) emission, for which we derived the physical parameters, including sizes and masses. Our analysis of the 13CO suggests that the virial parameter (ratio of kinetic to gravitational energy) varies over an order of magnitude between clumps that are unbound and some that are apparently ``unstable''. This conclusion is independent of whether they show evidence of ongoing star formation. We find that the majority of ATLASGAL sources have MIPSGAL counterparts with luminosities in the range 104-5x104L and are presumably forming relatively massive stars. We compare our results with previous extragalactic studies of the nearby spiral galaxies M31 and M33; and the blue compact dwarf galaxy Henize 2-10. We find that the main giant molecular cloud surrounding G19.61-0.23 has physical properties typical for Galactic GMCs and which are comparable to the GMCs in M31 and M33. However, the GMC studied here shows smaller surface densities and masses than the clouds identified in Henize 2-10 and associated with super star cluster formation.

Abstract Copyright:

Journal keyword(s): ISM: molecules - ISM: individual objects: G19.61-0.23 - radio continuum: ISM - stars: formation

Nomenclature: Fig. 3, Table 2: [STL2010] Cloud N (Nos 1-4). Fig. A.2, Table 3: [STL2010] coNN (Nos co1-co19). Fig. 4, Tables 4-5: [STL2010] CNN (Nos C1-C14).

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 M 31 AGN 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 12474 1
2 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 5764 1
3 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1230 3
4 NAME Rosette Molecular Cloud MoC 06 34.7 +04 02           ~ 260 0
5 NAME Maddalena Cloud MoC 06 48.1 -03 52           ~ 93 0
6 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 559 3
7 M 82 AG? 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5780 6
8 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33 13.47 ~ 1348 4
9 [STL2010] C9 MoC 18 27 05.36 -11 54 54.3           ~ 1 0
10 [STL2010] C8 MoC 18 27 14.08 -11 53 23.5           ~ 1 0
11 [STL2010] co6 MoC 18 27 17.01 -12 02 03.0           ~ 1 0
12 [STL2010] co7 MoC 18 27 17.03 -11 53 41.4           ~ 1 0
13 [STL2010] co9 MoC 18 27 22.07 -11 54 47.6           ~ 1 0
14 [STL2010] co12 MoC 18 27 23.49 -11 49 08.2           ~ 1 0
15 [STL2010] co11 MoC 18 27 24.62 -11 46 40.3           ~ 1 0
16 [STL2010] co13 MoC 18 27 27.60 -11 53 19.2           ~ 1 0
17 [STL2010] co19 MoC 18 27 28.11 -12 02 32.0           ~ 1 0
18 [STL2010] co8 MoC 18 27 29.61 -11 53 12.0           ~ 1 0
19 [STL2010] co10 MoC 18 27 34.05 -11 45 26.1           ~ 1 0
20 [STL2010] co15 MoC 18 27 35.66 -11 50 22.0           ~ 1 0
21 [STL2010] co1 MoC 18 27 37.63 -11 56 15.7           ~ 1 0
22 GAL 019.61-00.23 HII 18 27 38.0 -11 56 42           ~ 155 0
23 [STL2010] co16 MoC 18 27 41.68 -11 47 39.9           ~ 1 0
24 [STL2010] co2 MoC 18 27 43.21 -11 56 52.7           ~ 1 0
25 [STL2010] co4 MoC 18 27 45.22 -11 53 18.7           ~ 1 0
26 [STL2010] C4 MoC 18 27 50.42 -11 51 45.7           ~ 1 0
27 [STL2010] co3 MoC 18 27 51.73 -11 51 57.7           ~ 1 0
28 [STL2010] C3 MoC 18 27 55.43 -11 52 39.7           ~ 1 0
29 [STL2010] co18 MoC 18 28 02.29 -11 54 25.9           ~ 1 0
30 [STL2010] co14 MoC 18 28 18.23 -11 39 54.2           ~ 1 0
31 [STL2010] co5 MoC 18 28 25.15 -11 47 12.6           ~ 1 0
32 [STL2010] co17 MoC 18 28 30.14 -11 41 02.6           ~ 1 0

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2023.11.28-11:10:23

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