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

G. Orellana, N. M. Nagar, D. Elbaz, P. Calderón-Castillo, R. Leiton, E. Ibar, B. Magnelli, E. Daddi, H. Messias, P. Cerulo, R. Slater

Resultado de la investigación: Article

3 Citas (Scopus)

Resumen

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 (2007, ApJ, 657, 810) dust models, which we parametrize using two components (warm at 45-70 K and cold at 18-31 K). 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 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM ∞ Mdust 0.7). For galaxies with stellar masses 8.5 < log(M/M) < 11.9, the conversion factor between the single monochromatic luminosity at 850 μm and the total ISM mass (α850 μm) shows a large scatter (rms = 0.29 dex) 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.

Idioma originalEnglish
Número de artículoA68
PublicaciónAstronomy and Astrophysics
Volumen602
DOI
EstadoPublished - 1 jun 2017
Publicado de forma externa

Huella dactilar

molecular gases
star formation
dust
galaxies
scaling
gas
luminosity
monatomic gases
star formation rate
stellar mass
gases
temperature
estimates
Wide-field Infrared Survey Explorer
M stars
starburst galaxies
atomic weights
Infrared Astronomy Satellite
spectral energy distribution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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Orellana, G., Nagar, N. M., Elbaz, D., Calderón-Castillo, P., Leiton, R., Ibar, E., ... Slater, R. (2017). Molecular gas, dust, and star formation in galaxies: I. Dust properties and scalings in ~ 1600 nearby galaxies. Astronomy and Astrophysics, 602, [A68]. https://doi.org/10.1051/0004-6361/201629009
Orellana, G. ; Nagar, N. M. ; Elbaz, D. ; Calderón-Castillo, P. ; Leiton, R. ; Ibar, E. ; Magnelli, B. ; Daddi, E. ; Messias, H. ; Cerulo, P. ; Slater, R. / Molecular gas, dust, and star formation in galaxies : I. Dust properties and scalings in ~ 1600 nearby galaxies. En: Astronomy and Astrophysics. 2017 ; Vol. 602.
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abstract = "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 (2007, ApJ, 657, 810) dust models, which we parametrize using two components (warm at 45-70 K and cold at 18-31 K). 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 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM ∞ Mdust 0.7). For galaxies with stellar masses 8.5 < log(M∗/M⊙) < 11.9, the conversion factor between the single monochromatic luminosity at 850 μm and the total ISM mass (α850 μm) shows a large scatter (rms = 0.29 dex) 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.",
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Orellana, G, Nagar, NM, Elbaz, D, Calderón-Castillo, P, Leiton, R, Ibar, E, Magnelli, B, Daddi, E, Messias, H, Cerulo, P & Slater, R 2017, 'Molecular gas, dust, and star formation in galaxies: I. Dust properties and scalings in ~ 1600 nearby galaxies', Astronomy and Astrophysics, vol. 602, A68. https://doi.org/10.1051/0004-6361/201629009

Molecular gas, dust, and star formation in galaxies : I. Dust properties and scalings in ~ 1600 nearby galaxies. / Orellana, G.; Nagar, N. M.; Elbaz, D.; Calderón-Castillo, P.; Leiton, R.; Ibar, E.; Magnelli, B.; Daddi, E.; Messias, H.; Cerulo, P.; Slater, R.

En: Astronomy and Astrophysics, Vol. 602, A68, 01.06.2017.

Resultado de la investigación: Article

TY - JOUR

T1 - Molecular gas, dust, and star formation in galaxies

T2 - I. Dust properties and scalings in ~ 1600 nearby galaxies

AU - Orellana, G.

AU - Nagar, N. M.

AU - Elbaz, D.

AU - Calderón-Castillo, P.

AU - Leiton, R.

AU - Ibar, E.

AU - Magnelli, B.

AU - Daddi, E.

AU - Messias, H.

AU - Cerulo, P.

AU - Slater, R.

PY - 2017/6/1

Y1 - 2017/6/1

N2 - 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 (2007, ApJ, 657, 810) dust models, which we parametrize using two components (warm at 45-70 K and cold at 18-31 K). 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 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM ∞ Mdust 0.7). For galaxies with stellar masses 8.5 < log(M∗/M⊙) < 11.9, the conversion factor between the single monochromatic luminosity at 850 μm and the total ISM mass (α850 μm) shows a large scatter (rms = 0.29 dex) 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.

AB - 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 (2007, ApJ, 657, 810) dust models, which we parametrize using two components (warm at 45-70 K and cold at 18-31 K). 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 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM ∞ Mdust 0.7). For galaxies with stellar masses 8.5 < log(M∗/M⊙) < 11.9, the conversion factor between the single monochromatic luminosity at 850 μm and the total ISM mass (α850 μm) shows a large scatter (rms = 0.29 dex) 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.

KW - Galaxies: ISM

KW - Galaxies: photometry

KW - Galaxies: star formation

KW - Infrared: ISM

KW - Submillimeter: galaxies

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