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The evolution of the dust and gas content in galaxies

Santini, P. and Viero, M. and Xu, K. (2014) The evolution of the dust and gas content in galaxies. Astronomy and Astrophysics, 562 . Art. No. A30. ISSN 0004-6361.

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We use deep Herschel observations taken with both PACS and SPIRE imaging cameras to estimate the dust mass of a sample of galaxies extracted from the GOODS-S, GOODS-N and the COSMOS fields. We divide the redshift–stellar mass (Mstar)–star formation rate (SFR) parameter space into small bins and investigate average properties over this grid. In the first part of the work we investigate the scaling relations between dust mass, stellar mass and SFR out to z = 2.5. No clear evolution of the dust mass with redshift is observed at a given SFR and stellar mass. We find a tight correlation between the SFR and the dust mass, which, under reasonable assumptions, is likely a consequence of the Schmidt-Kennicutt (S-K) relation. The previously observed correlation between the stellar content and the dust content flattens or sometimes disappears when considering galaxies with the same SFR. Our finding suggests that most of the correlation between dust mass and stellar mass obtained by previous studies is likely a consequence of the correlation between the dust mass and the SFR combined with the main sequence, i.e., the tight relation observed between the stellar mass and the SFR and followed by the majority of star-forming galaxies. We then investigate the gas content as inferred from dust mass measurements. We convert the dust mass into gas mass by assuming that the dust-to-gas ratio scales linearly with the gas metallicity (as supported by many observations). For normal star-forming galaxies (on the main sequence) the inferred relation between the SFR and the gas mass (integrated S-K relation) broadly agrees with the results of previous studies based on CO measurements, despite the completely different approaches. We observe that all galaxies in the sample follow, within uncertainties, the same S-K relation. However, when investigated in redshift intervals, the S-K relation shows a moderate, but significant redshift evolution. The bulk of the galaxy population at z ~ 2 converts gas into stars with an efficiency (star formation efficiency, SFE = SFR/M_gas, equal to the inverse of the depletion time) about 5 times higher than at z ~ 0. However, it is not clear what fraction of such variation of the SFE is due to an intrinsic redshift evolution and what fraction is simply a consequence of high-z galaxies having, on average, higher SFR, combined with the super-linear slope of the S-K relation (while other studies find a linear slope). We confirm that the gas fraction (f_gas = M_gas/(M_gas + M_star)) decreases with stellar mass and increases with the SFR. We observe no evolution with redshift once M_star and SFR are fixed. We explain these trends by introducing a universal relation between gas fraction, stellar mass and SFR that does not evolve with redshift, at least out to z ~ 2.5. Galaxies move across this relation as their gas content evolves across the cosmic epochs. We use the 3D fundamental f_gas–M_star–SFR relation, along with the evolution of the main sequence with redshift, to estimate the evolution of the gas fraction in the average population of galaxies as a function of redshift and as a function of stellar mass: we find that M_star ≳ 10^11 M_⊙ galaxies show the strongest evolution at z ≳ 1.3 and a flatter trend at lower redshift, while f_gas decreases more regularly over the entire redshift range probed in Mstar ≲ 10^11 M_⊙ galaxies, in agreement with a downsizing scenario.

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Additional Information:© 2014 ESO. Article published by EDP Sciences. Received 11 October 2013; Accepted 14 November 2013. Published online 03 February 2014. P.S. thanks N. Scoville for interesting and useful discussions and A. Marconi and G. Risaliti for helping with fitting routines and statistical issues. This work was supported by grant ASI I/005/11/0. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
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Subject Keywords:galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: ISM; infrared: galaxies
Record Number:CaltechAUTHORS:20140425-092036324
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Official Citation:The evolution of the dust and gas content in galaxies P. Santini, R. Maiolino, B. Magnelli, D. Lutz, A. Lamastra, G. Li Causi, S. Eales, P. Andreani, S. Berta, V. Buat, A. Cooray, G. Cresci, E. Daddi, D. Farrah, A. Fontana, A. Franceschini, R. Genzel, G. Granato, A. Grazian, E. Le Floc’h, G. Magdis, M. Magliocchetti, F. Mannucci, N. Menci, R. Nordon, S. Oliver, P. Popesso, F. Pozzi, L. Riguccini, G. Rodighiero, D. J. Rosario, M. Salvato, D. Scott, L. Silva, L. Tacconi, M. Viero, L. Wang, S. Wuyts and K. Xu A&A 562 A30 (2014) DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:45216
Deposited By: Jason Perez
Deposited On:28 Apr 2014 14:37
Last Modified:03 Oct 2019 06:28

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