The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2

By B. Magnelli, D. Lutz, A. Saintonge, S. Berta, P. Santini, M. Symeonidis, B. Altieri, P. Andreani, H. Aussel, M. B'ethermin and 31 more. 2013

180 citations recorded by the source corpus.

We study the evolution of the dust temperature of galaxies in the SFR− M∗ plane up to z ~ 2 using far-infrared and submillimetre observations from the Herschel Space Observatory taken as part of the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Starting from a sample of galaxies with reliable star-formation rates (SFRs), stellar masses (M_∗) and redshift estimates, we grid the SFR− M_∗parameter space in several redshift ranges and estimate the mean dust temperature (T_(dust)) of each SFR–M_∗ − z bin. Dust temperatures are inferred using the stacked far-infrared flux densities (100–500  μm) of our SFR–M_∗ − z bins. At all redshifts, the dust temperature of galaxies smoothly increases with rest-frame infrared luminosities (L_(IR)), specific SFRs (SSFR; i.e., SFR/M_∗), and distances with respect to the main sequence (MS) of the SFR− M_∗ plane (i.e., Δlog (SSFR)_(MS) = log [SSFR(galaxy)/SSFR_(MS)(M_∗,z)]). The T_(dust) − SSFR and T_(dust) − Δlog (SSFR)_(MS) correlations are statistically much more significant than the T_(dust) − LIR one. While the slopes of these three correlations are redshift-independent, their normalisations evolve smoothly from z = 0 and z ~ 2. We convert these results into a recipe to derive T_(dust) from SFR, M_∗ and z, valid out to z ~ 2 and for the stellar mass and SFR range covered by our stacking analysis. The existence of a strong T_(dust) − Δlog (SSFR)_(MS) correlation provides us with several pieces of information on the dust and gas content of galaxies. Firstly, the slope of the T_(dust) − Δlog (SSFR)_(MS) correlation can be explained by the increase in the star-formation efficiency (SFE; SFR/M_(gas)) with Δlog (SSFR)_(MS) as found locally by molecular gas studies. Secondly, at fixed Δlog (SSFR)_(MS), the constant dust temperature observed in galaxies probing wide ranges in SFR and M_∗ can be explained by an increase or decrease in the number of star-forming regions with comparable SFE enclosed in them. And thirdly, at high redshift, the normalisation towards hotter dust temperature of the T_(dust) − Δlog (SSFR)_(MS) correlation can be explained by the decrease in the metallicities of galaxies or by the increase in the SFE of MS galaxies. All these results support the hypothesis that the conditions prevailing in the star-forming regions of MS and far-above-MS galaxies are different. MS galaxies have star-forming regions with low SFEs and thus cold dust, while galaxies situated far above the MS seem to be in a starbursting phase characterised by star-forming regions with high SFEs and thus hot dust.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/43f6ebaee14c00714bdbba3b1cfada3a6c2a3c7f

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. R. Somerville
5. D. M. Alexander
6. D. Narayanan
7. R. Dav'e
8. E. Daddi

In Instrumentation

1. A. Dekel
2. P. Hopkins
3. L. Hernquist
4. P. V. van Dokkum
5. R. Dav'e
6. C. Conroy
7. E. Daddi
8. R. Somerville

Citations in the corpus

• AN OBJECTIVE DEFINITION FOR THE MAIN SEQUENCE OF STAR-FORMING GALAXIES (2015, background): “…studies have followed, confirming the existence of a MS, all the way to at least z ∼ 4 (Bernhard et al. 2014; Karim et al. 2011; Kashino et al. 2013; Magnelli et al. 2014; Pannella et al. 2009; Peng et al. 2010, hereafter P10; Popesso et al. 2011, 2012; Rodighiero et al. 2010, 2011, 2014; Sargent…”
• 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): “…e.g., when discussing the properties of SFGs and AGN in general (e.g., Elbaz et al. 2011, Whitaker et al. 2012, Mullaney et al. 2012b, Rosario et al. 2013), and in particular also gas and dust properties (e.g., Magdis et al. 2012b, Saintonge et al. 2012, Santini et al. 2014, Magnelli et al. 2014).”
• PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, methodology): “In comparison to the dust analysis presented in G15, which included fluxes from Magnelli et al. (2014) and analysis from Berta et al. (2016), the comparison of these three studies, based on similar data, gives an objective measure of the systematic uncertainties of the dust – SED methods and adds…”
• The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, background): “M∗ sequence (Rodighiero et al. 2010; Whitaker et al. 2012; Magnelli et al. 2014).”
• A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, background): “Some studies suggest that the MS slope varies with stellar mass so that a single power-law cannot explain the MS and a stellar mass-dependent slope is a better fit (Karim et al. 2011; Whitaker et al. 2012; Magnelli 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, background): “Magnelli et al. (2014) investigated the variations in TD derived from SED fits for stacks of galaxies at z = 1 to 2.3 from the MS to a factor 10 above the MS.”
• GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “…confirmed by the reported evolution of the IR SED shape of Main Sequence galaxies up to redshiftz ≃2 by Magdis et al. (2012) and more recently by Magnelli et al. (2014), and extended at higher redshift by Schreiber et al. (in preparation), with the median dust tem- Star formation, dust…”
• Dusty Star Forming Galaxies at High Redshift (2014, background): “Many recent works have framed analysis of new Herschel-detected DSFG populations in the context of the ‘‘Main Sequence’’ of galaxies (Elbaz et al., 2011; Rodighiero et al., 2011;Nordon et al., 2012, 2013; Sargent et al., 2012;Magnelli et al., 2014).”
• The Star Formation Main Sequence in the Hubble Space Telescope Frontier Fields (2017, background): “In recent years, however, many studies have reported evidence that the MS flattens at high masses (M ∼ 1010−11M⊙) (e.g. Magnelli et al. 2014; Whitaker et al. 2014; Schreiber et al. 2015), with the turnover mass increasing with redshift (Tasca et al. 2015; Lee et al. 2015; Tomczak et al. 2016) and…”
• COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, methodology): “For this purpose, Magnelli et al. (2014) binned the data onto a three dimensional grid in z, SFR and M* and then stacked the photometry in each bin.”
• ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “While many star-forming galaxies have measured dust temperatures of ∼25-30 K (Magnelli et al. 2014; Elbaz et al. 2011; Genzel et al. 2015), there are many faint individually detected sources which have much higher dust temperatures (Sklias et al. 2014), i.e., ∼40-50 K.”
• The confinement of star-forming galaxies into a main sequence through episodes of gas compaction, depletion and replenishment (2015, background): “G of the SFR−M? relation towards lower redshifts (Rodighiero et al. 2010; Elbaz et al. 2011; Whitaker et al. 2012; Magnelli et al. 2014; Whitaker et al. 2014; Schreiber et al. 2015).”
• The evolution of the dust and gas content in galaxies (2013, methodology): “Following Magnelli et al. (2014), if |S input − S sim|/S input > 0.5 we reject the corresponding bin9.”
• Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift (2017, methodology): “…(RJ) dust continuum emission, and applying the calibration of this technique, developed in Scoville et al. (2016) (a brief summary is provided here in Section 4 and Appendix A) (see also (Magnelli et al. 2014; Santini et al. 2014; Genzel et al. 2015; Schinnerer et al. 2016; Berta et al. 2016)).”