THE EVOLUTION OF INTERSTELLAR MEDIUM MASS PROBED BY DUST EMISSION: ALMA OBSERVATIONS AT z = 0.3–2

By N. Scoville, H. Aussel, K. Sheth, K. Scott, D. Sanders, R. Ivison, Adrian Pope, P. Capak, P. V. Vanden Bout, S. Manohar and 2 more. Astrophysical Journal, 2014

201 citations recorded by the source corpus.

The use of submillimeter dust continuum emission to probe the mass of interstellar dust and gas in galaxies is empirically calibrated using samples of local star-forming galaxies, Planck observations of the Milky Way, and high-redshift submillimeter galaxies. All of these objects suggest a similar calibration, strongly supporting the view that the Rayleigh–Jeans tail of the dust emission can be used as an accurate and very fast probe of the interstellar medium (ISM) in galaxies. We present ALMA Cycle 0 observations of the Band 7 (350 GHz) dust emission in 107 galaxies from z = 0.2 to 2.5. Three samples of galaxies with a total of 101 galaxies were stellar-mass-selected from COSMOS to have M* ≃ 1011 M☉: 37 at z ∼ 0.4, 33 at z ∼ 0.9, and 31 at z = 2. A fourth sample with six infrared-luminous galaxies at z = 2 was observed for comparison with the purely mass-selected samples. From the fluxes detected in the stacked images for each sample, we find that the ISM content has decreased by a factor ∼6 from 1 to 2 × 1010 M☉ at both z = 2 and 0.9 down to ∼2 × 109 M☉ at z = 0.4. The infrared-luminous sample at z = 2 shows a further ∼4 times increase in MISM compared with the equivalent non-infrared-bright sample at the same redshift. The gas mass fractions are ∼2% ± 0.5%, 12% ± 3%, 14% ± 2%, and 53% ± 3% for the four subsamples (z = 0.4, 0.9, and 2 and infrared-bright galaxies).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/45c3b8339aecbe6afa1f37a52721a38dcf2b165c

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In Astronomy and Astrophysics

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2. L. Hernquist
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5. D. M. Alexander
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In Instrumentation

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8. E. Daddi

Citations in the corpus

• Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “…to high redshift from CO and dust-based methods (corrected for selection effects) indicate a rise in mH2/(mH2 +mstar) back in cosmic time to z ∼ 2, then a plateau or possibly a slight decline (Geach et al. 2011, Genzel et al. 2014, Saintonge et al. 2013, Scoville et al. 2014, Tacconi et al. 2013).”
• Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, methodology): “This method was applied on individual galaxies at high redshift by Magdis et al. (2011, 2012a) and Scoville et al. (2014), but also on mean spectral energy distributions (SEDs) measured through a stacking analysis (Magdis et al. 2012a; Santini et al. 2014).”
• CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, background): “…de Bure interferometer (Daddi et al 2008; 2010a; D10 hereafter; Tacconi et al 2010; 2013; Geach et al 2011) and confirmed by gas mass estimates obtained via the conversion of dust masses (Magdis et al 2011; 2012; Santini et al 2014; Scoville et al 2014; Magnelli et al 2013; Genzel et al 2014).”
• Dusty Star Forming Galaxies at High Redshift (2014, methodology): “Finally, we close this subsection by noting that a number of groups have recently advocated dust mass measurements as an efficient method for deriving H2 gas masses from high-z galaxies (e.g. Magdis et al., 2012; Scoville et al., 2014).”
• ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6: ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD (2015, methodology): “We use Herschel SPIRE 350 and 500µm data which provide more reliable total submm fluxes for the extended objects at low redshift than were available from the SCUBA 850µm observations used in Scoville et al. (2014).”
• PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, unknown): “The long-wavelength dust emissivity can be estimated from a model, or calibrated from observations of sources in which gas masses are known from method 1 (e.g. Scoville et al. 2014, 2016, 2017).”
• A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, methodology): “Another method to estimate gas content is to measure the dust mass from far-infrared or submillimeter photometry and convert to gas masses using an assumed gas-to-dust ratio (e.g. Magdis et al. 2012; Santini et al. 2014; Scoville et al. 2014).”
• COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, background): “…the detection of a molecular gas mass of 10 10 M from band 7 (350 GHz) broad-band data requires only a few minutes at z~1-2 (for a 5σ detection), while a CO-based measurement (again at 5σ) requires more than one hour at z~0.6-1 and several hours at z~2 (Scoville 2013, Scoville et al. 2014) 3 .”
• An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, background): “Hence, observed 870-μm flux density should trace both the dust mass and SFR (e.g. Blain et al. 2002; Scoville et al. 2014).”
• REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “Lower conversion factors in high-redshift galaxies would bring CO-based gas mass measurements into better agreement with those estimates based on the gas-to-dust ratio technique that are systematically lower (e.g., Santini et al. 2014, Scoville et al. 2014; but see also Magdis et al. 2012b).”