2017A&A...606L..12G


Query : 2017A&A...606L..12G

2017A&A...606L..12G - Astronomy and Astrophysics, volume 606, L12-12 (2017/10-1)

Galactocentric variation of the gas-to-dust ratio and its relation with metallicity.

GIANNETTI A., LEURINI S., KONIG C., URQUHART J.S., PILLAI T., BRAND J., KAUFFMANN J., WYROWSKI F. and MENTEN K.M.

Abstract (from CDS):

Context. The assumption of a gas-to-dust mass ratio γ is a common approach to estimate the basic properties of molecular clouds, such as total mass and column density of molecular hydrogen, from (sub)mm continuum observations of the dust. In the Milky Way a single value is used at all galactocentric radii, independently of the observed metallicity gradients. Both models and extragalactic observations suggest that this quantity increases for decreasing metallicity Z, typical of the outer regions in disks, where fewer heavy elements are available to form dust grains.
Aims. We aim to investigate the variation of the gas-to-dust ratio as a function of galactocentric radius and metallicity, to allow a more accurate characterisation of the quantity of molecular gas across the galactic disk, as derived from observations of the dust.
Methods. Observations of the optically thin C18O (2-1) transition were obtained with the APEX telescope for a sample of 23 massive and dense star-forming regions in the far outer Galaxy (galactocentric distance greater than 14kpc). From the modelling of this line and of the spectral energy distribution of the selected clumps we computed the gas-to-dust ratio and compared it to that of well-studied sources from the ATLASGAL TOP100 sample in the inner galactic disk.
Results. The gradient in γ is found to be 0.087+0.047–0.025dex/kpc (or equivalently γ∝Zexp(-1.4+0.3–1.0). The dust-to-metal ratio, decreases with galactocentric radius, which is the most common situation also for external late-type galaxies. This suggests that grain growth dominates over destruction. The predicted γ is in excellent agreement with the estimates in Magellanic clouds, for the appropriate value of Z.

Abstract Copyright: © ESO, 2017

Journal keyword(s): dust, extinction - ISM: clouds - Galaxy: disk - galaxies: ISM - submillimeter: ISM - stars: formation - stars: formation

Status at CDS : Examining the need for a new acronym.

Simbad objects: 78

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Number of rows : 78
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10529 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6555 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16507 1
4 JCMTSF J061724.0+145444 Cl* 06 17 24.30 +14 54 37.2           ~ 25 0
5 IRAS 06365-0143 * 06 39 04.0465830360 -01 46 07.205898504           ~ 4 0
6 IRAS 06375-0141 G 06 40 02.9 -01 44 44           ~ 6 0
7 IRAS 06416-0352 IR 06 44 07.6 -03 55 42           ~ 5 0
8 IRAS 06428-0257 IR 06 45 23.864 -03 01 10.11           ~ 4 0
9 IRAS 06454+0020 IR 06 48 03.2366272920 +00 17 33.415462068           ~ 6 0
10 2MASX J06494021-0332523 Y*O 06 49 40.214 -03 32 52.36           ~ 10 0
11 2MASX J06503736-0521006 G 06 50 37.3785742608 -05 20 59.774465616           ~ 15 0
12 IRAS 06520-0428 MIR 06 54 35.31288 -04 32 17.3220           ~ 8 0
13 DSH J0723.0-1455 GNe 07 23 03.6 -14 55 03           ~ 4 0
14 BRAN 33A SFR 07 30 05.219 -20 44 22.98           ~ 14 0
15 IRAS 07284-2203 IR 07 30 33.2527966536 -22 10 16.278112632           ~ 3 0
16 IRAS 07322-2336 * 07 34 22.5905554656 -23 42 39.591982224           ~ 4 0
17 2MASS J07351523-2348459 Y*? 07 35 15.24 -23 48 45.9           ~ 8 0
18 IRAS 07495-2840 IR 07 51 35.4 -28 48 01           ~ 4 0
19 IRAS 07561-3304 IR 07 58 06.1 -33 12 59           ~ 6 0
20 IRAS 08166-3810 IR 08 18 29.582 -38 19 56.70           ~ 2 0
21 IRAS 08168-3947 HII 08 18 40.043 -39 56 56.75           ~ 4 0
22 OH 301.14 -0.23 cor 12 35 35.14 -63 02 32.6           ~ 39 0
23 [HBM2005] G305.21+0.21 cor 13 11 14 -62 34.7           ~ 22 0
24 MMB G305.563+00.013 cor 13 14 26.90 -62 44 29.4           ~ 17 0
25 MMB G309.384-00.135 cor 13 47 23.98 -62 18 12.0           ~ 25 0
26 AGAL G310.014+00.387 cor 13 51 40 -61 39.4           ~ 20 0
27 MMB G313.577+00.325 cor 14 20 08.58 -60 42 00.8           ~ 22 0
28 MMB G316.640-00.087 cor 14 44 18.45 -59 55 11.5           ~ 26 0
29 MMB G326.662+00.520 cor 15 45 02.95 -54 09 03.1           ~ 17 0
30 IRAS 15437-5343 Y*O 15 47 32.73 -53 52 38.4           ~ 48 0
31 AGAL G327.393+00.199 cor 15 50 19 -53 57.1           ~ 17 0
32 OH 327.3 -0.6 cor 15 53 07.65 -54 37 06.1           ~ 49 1
33 AGAL G328.809+00.632 cor 15 55 49 -52 43.1           ~ 23 0
34 IRAS 15573-5307 cor 16 01 09.999 -53 16 02.94           ~ 37 1
35 MMB G330.953-00.182 cor 16 09 52.37 -51 54 57.6           ~ 31 0
36 OH 330.9 -0.3 cor 16 10 19.80 -52 06 07.9           ~ 32 0
37 IRAS 16124-5110 Y*O 16 16 16.46832 -51 18 25.1964           ~ 35 0
38 IRAS 16157-4957 cor 16 19 29.01 -50 04 41.3           ~ 34 0
39 MMB G332.826-00.549 cor 16 20 10.85 -50 53 14.2           ~ 32 0
40 MMB G333.135-00.431 cor 16 21 02.82 -50 35 12.0           ~ 28 0
41 [LCU2014] G333.286-00.387 cor 16 21 30.3 -50 26 48           ~ 24 0
42 AGAL G333.604-00.212 cor 16 22 09.35 -50 05 58.8           ~ 28 0
43 AGAL G337.704-00.054 cor 16 38 30 -47 00.7           ~ 22 0
44 [BE83] Maser 337.40-00.40 cor 16 38 50.52 -47 28 00.2           ~ 60 0
45 AGAL G337.916-00.477 cor 16 41 10.6 -47 08 03           ~ 31 0
46 [BE83] IR 339.62-00.12 Y*O 16 46 05.99 -45 36 43.3           ~ 41 0
47 OH 341.22 -0.21 cor 16 52 17.86 -44 26 52.3           ~ 52 0
48 AGAL G340.746-01.001 cor 16 54 03.66 -45 18 45.1           ~ 15 0
49 [PLW2012] G343.124-00.064-030.4 cor 16 58 17 -42 52.3           ~ 26 0
50 AGAL G345.718+00.817 cor 17 03.1 -40 17           ~ 20 0
51 OH 345.50 +0.35 cor 17 04 22.91 -40 44 21.7           ~ 64 0
52 MMB G345.487+00.314 cor 17 04 28.24 -40 46 28.7           ~ 28 0
53 IRAS 17016-4124 SFR 17 05 11.160 -41 29 06.00           ~ 55 0
54 Caswell CH3OH 351.16+00.70 cor 17 19 57.50 -35 57 52.8           ~ 29 0
55 AGAL G351.244+00.669 cor 17 20 17.84 -35 54 46.0           ~ 31 0
56 AGAL G351.416+00.646 cor 17 20 53 -35 47.0           ~ 26 0
57 MMB G351.581-00.353 cor 17 25 24.9262 -36 12 42.383           ~ 35 0
58 OH 351.75 -0.53 cor 17 26 42.57 -36 09 17.6           ~ 93 1
59 OH 353.41 -0.36 cor 17 30 26.18 -34 41 45.6           ~ 83 0
60 MMB G010.472+00.027 cor 18 08 38.2290 -19 51 50.262           ~ 65 1
61 MMB G010.627-00.384 cor 18 10 29.22 -19 55 41.1           ~ 46 1
62 AGAL G012.804-00.199 cor 18 14 13.34 -17 55 45.3           ~ 27 0
63 MMB G013.657-00.599 cor 18 17 24.26 -17 22 12.5           ~ 23 0
64 AGAL G015.030-00.669 cor 18 20 23 -16 11.4           ~ 23 0
65 MMB G019.884-00.534 cor 18 29 14.37 -11 50 23.0           ~ 97 1
66 AGAL G028.861+00.066 cor 18 43 46 -03 35.5           ~ 26 0
67 IRAS 18449-0115 cor 18 47 34.29 -01 12 44.5           ~ 365 0
68 AGAL G030.818-00.056 cor 18 47 47.0 -01 54 28           ~ 146 0
69 AGAL G034.411+00.234 Y*O 18 53 18.0319 +01 25 25.500           ~ 85 0
70 AGAL G034.401+00.226 cor 18 53 18.6 +01 24 40           ~ 59 1
71 [CUS2014] G034.2572+0.1535 cor 18 53 18.6449 +01 15 01.574           ~ 35 0
72 RAFGL 5542 Y*O 18 53 37.88832 +01 50 30.5844           ~ 66 0
73 AGAL G035.197-00.742 cor 18 58 12.79 +01 40 37.6           ~ 16 0
74 IRAS 18566+0408 Y*O 18 59 09.95520 +04 12 15.6240           ~ 128 0
75 BGPS G043.169+00.009 cor 19 10 14.2145 +09 06 17.697           ~ 27 0
76 AGAL G049.489-00.389 cor 19 23 44.15 +14 30 29.5           ~ 17 0
77 AGAL G053.141+00.069 cor 19 29 17.50 +17 56 24.0           ~ 26 1
78 AGAL G059.782+00.066 cor 19 43 10.83 +23 44 03.3           ~ 12 0

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2023.01.27-06:36:16

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