Query : 2017A&A...602A..68O

2017A&A...602A..68O - Astronomy and Astrophysics, volume 602A, 68-68 (2017/6-1)

Molecular gas, dust, and star formation in galaxies. I. Dust properties and scalings in ∼1600 nearby galaxies.


Abstract (from CDS):

Context. Dust and its emission is increasingly being used to constrain the evolutionary stage of a galaxy. A comprehensive characterization of dust, best achieved in nearby bright galaxies, is thus a highly useful resource.
Aims. We aim to characterize the relationship between dust properties (mass, luminosity, and temperature) and their relationships with galaxy-wide properties (stellar, atomic, and molecular gas mass, and star formation mode). We also aim to provide equations to accurately estimate dust properties from limited observational datasets.
Methods. We assemble a sample of 1630 nearby (z<0.1) galaxies - over a large range of stellar masses (M*), star formation rates (SFR) and specific star formation rates (sSFR=SFR/M*) - for which comprehensive and uniform multi-wavelength observations are available from WISE, IRAS, Planck, and/or SCUBA. The characterization of dust emission comes from spectral energy distribution (SED) fitting using Draine & Li (2007ApJ...657..810D) dust models, which we parametrize using two components (warm at 45-70K and cold at 18-31K). The subsample of these galaxies with global measurements of CO and/or HI are used to explore the molecular and/or atomic gas content of the galaxies.
Results. The total infrared luminosity (LIR), dust mass (Mdust), and dust temperature of the cold component (Tcold) form a plane that we refer to as the dust plane. A galaxy's sSFR drives its position on the dust plane: starburst (high sSFR) galaxies show higher LIR, Mdust, and Tcold compared to main sequence (typical sSFR) and passive galaxies (low sSFR). Starburst galaxies also show higher specific dust masses (Mdust/M*) and specific gas masses (Mgas/M*). We confirm earlier findings of an anti-correlation between the dust to stellar mass ratio and M*. We also find different anti-correlations depending on sSFR; the anti-correlation becomes stronger as the sSFR increases, with the spread due to different cold dust temperatures. The dust mass is more closely correlated with the total gas mass (atomic plus molecular) than with the individual atomic and molecular gas masses. Our comprehensive multiwavelength data allows us to define several equations to accurately estimate LIR, Mdust, and Tcold from one or two monochromatic luminosities in the infrared and/or sub-millimeter.
Conclusions. It is possible to estimate the dust mass and infrared luminosity from a single monochromatic luminosity within the Rayleigh-Jeans tail of the dust emission, with errors of 0.12 and 0.20dex, respectively. These errors are reduced to 0.05 and 0.10dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM∝Mdust0.7). For galaxies with stellar masses 8.5<log(M*/M)<11.9, the conversion factor between the single monochromatic luminosity at 850µm and the total ISM mass (α850µm) shows a large scatter (rms=0.29dex) and a weak correlation with the LIR. The star formation mode of a galaxy shows a correlation with both the gas mass and dust mass: the dustiest (high Mdust/M*) galaxies are gas-rich and show the highest SFRs.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: ISM - galaxies: photometry - galaxies: star formation - infrared: ISM - submillimeter: galaxies - submillimeter: galaxies

Simbad objects: 6

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Number of rows : 6
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10530 1
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16507 1
3 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2872 4
4 NAME Super Antennae Sy2 19 31 21.4272801984 -72 39 21.442847832   17.39 16.37 14.65   ~ 289 2
5 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2425 2
6 NAME South America H2G 22 51 49.307 -17 52 23.96   16.97       ~ 314 3

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