SCUBA observations of galaxies with metallicity measurements: a new method for determining the relation between submillimetre luminosity and dust mass

By A. James, L. Dunne, S. Eales, M. Edmunds. 2002

177 citations recorded by the source corpus.

Using a new technique, we have determined a value for the constant of proportionality between submillimetre emission and dust mass, the dust mass‐absorption coefficient (κd) at 850 µm. Our method has an advantage over previous methods in that we avoid assumptions about the properties of dust in the interstellar medium. Our only assumption is that the fraction of metals incorporated in the dust (e) in galaxies is a universal constant. To implement our method, we require objects that have submillimetre and far-infrared flux measurements as well as gas mass and metallicity estimates. We present data for all the galaxies with suitable measurements, including new submillimetre maps for five galaxies. We find κ850 = 0.07 ± 0.02 m 2 kg −1 . We have also been able to use our sample to investigate our assumption that e is a universal constant. We find no evidence that e is different for dwarf and giant galaxies, and show that the scatter in e from galaxy to galaxy is apparently quite small.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/694f722b8f56dd63352c5705165bac0279f1e182

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

ISM properties in low-metallicity environments II. The dust spectral energy distribution of NGC 1569 (2003, background): “James et al. (2002) calculated dust masses for galaxies from the submillimeter emission, assuming that the fraction of metals incorporated in the dust in galaxies is a universal constant.”
An Overview of the Dwarf Galaxy Survey (2013, background): “James et al. (2002), who did a similar study using some ground-based 850 μm observations, include a few low metallicity galaxies in their large sample and find a flatter trend of the D/G at lower metallicities that needs to be tested for a larger range of metallicities, particularly for lower…”
Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, background): “This reference trend between G/D and metallicity seems consistent with the observations of galaxies with near-solar metallicities (e.g., James et al. 2002; Draine et al. 2007; Bendo et al. 2010; Magrini et al. 2011).”
A Herschel view of the far-infrared properties of submillimetre galaxies (2012, background): “To allow direct comparison with Kovács et al. (2010), we adoptedκ850 = 0.15 m2 kg−1 at ν0 = c/850µm (Dunne et al. 2003), even though the exact value of this parameter is still under active discussion (e.g., Hildebrand 1983; Krügel et al. 1990; Sodroski et al.1997; James et al. 2002).”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “…as a function of metallicity or galaxy stellar mass (Issa, MacLaren & Wolfendale 1990; Lisenfeld & Ferrara 1998; Hirashita, Tajiri & Kamaya 2002; James et al. 2002; Hunt, Bianchi & Maiolino 2005; Draine et al. 2007; Engelbracht et al. 2008; Galametz et al. 2011; Magrini et al. 2011; Rémy-Ruyer…”
Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, methodology): “The restricted sample is presented in Table 1 and gathers subsamples of the James et al. (2002), Draine et al. (2007), Galliano et al. (2008) and Galametz et al. (2009) samples.”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, result): “James et al. (2002) compared models to dust masses estimated from IR and submillimeter observations and argued that the fraction of the metals condensed into dust grains appeared to be the same in dwarf and giant galaxies, i.e., dust-to-gas mass ratios consistent with equation (13), for 8:1PAOP9:0.”
Planckintermediate results (2016, methodology): “However, using a different approach, James et al. (2002) found κ850 = (0.07 ± 0.02) m2 kg−1, nearly a factor of 2 higher.”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, methodology): “The value of κ used here is based on that measured in the diffuse ISM of the Milky Way (Boulanger et al. 1996; Sodroski et al. 1997; Planck Collaboration 2011a) and also on nearby galaxies by James et al. (2002).”
WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST MASS (2010, methodology): “We have assumed 40% of the metals are in dust (Dwek 1998; James et al. 2002).”
The evolution of the dust and gas content in galaxies (2013, methodology): “As suggested by previous studies, focused either on local (e.g., Draine et al. 2007; Leroy et al. 2011; Smith et al. 2012; Corbelli et al. 2012; Sandstrom et al. 2013), z < 0.5 (e.g., James et al. 2002) or high-z galaxies (e.g., Zafar & Watson 2013; Chen et al. 2013, Cresci et al., in prep.)”
RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, background): “Indeed, a correlation has been widely shown between the dustto-gas ratio and the gas-phase oxygen abundance (e.g. Lisenfeld & Ferrara 1998; Edmunds 2001; James et al. 2002; Hirashita et al. 2002; D07).”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, methodology): “The dust distribution is determined by projecting the total gasphase metal density in the GADGET-2 simulations on to a 3D adaptive mesh refinement grid assuming a dust-to-metal ratio of 0.4 (Dwek 1998; James et al. 2002).”