EVOLUTION OF GALAXY STELLAR MASS FUNCTIONS, MASS DENSITIES, AND MASS-TO-LIGHT RATIOS FROM z ∼ 7 TO z ∼ 4

By V. González, I. Labbé, R. Bouwens, G. Illingworth, M. Franx, M. Kriek. 2010

157 citations recorded by the source corpus.

We derive stellar masses from spectral energy distribution fitting to rest-frame optical and UV fluxes for 401 star-forming galaxies at z ∼ 4, 5, and 6 from Hubble-WFC3/IR camera observations of the Early Release Science field combined with the deep GOODS-S Spitzer/IRAC data (and include a previously published z ∼ 7 sample). A mass–luminosity relation with strongly luminosity-dependent ratios is found for the largest sample (299 galaxies) at z ∼ 4. The relation has a well-determined intrinsic sample variance of 0.5 dex. This relation is also consistent with the more limited samples at z ∼ 5–7. This z ∼ 4 mass–luminosity relation, and the well-established faint UV-luminosity functions at z ∼ 4–7, are used to derive galaxy mass functions (MFs) to masses at z ∼ 4–7. A bootstrap approach is used to derive the MFs to account for the large scatter in the relation and the luminosity function uncertainties, along with an analytical cross-check. The MFs are also corrected for the effects of incompleteness. The incompleteness-corrected MFs are steeper than previously found, with slopes αM ∼ −1.4 to −1.6 at low masses. These slopes are, however, still substantially flatter than the MFs obtained from recent hydrodynamical simulations. We use these MFs to estimate the stellar mass density (SMD) of the universe to a fixed MUV, AB  < − 18 as a function of redshift and find an SMD growth ∝(1 + z)−3.4  ±  0.8 from z ∼ 7 to z ∼ 4. We also derive the SMD from the completeness-corrected MFs to a mass limit  M☉. Such completeness-corrected MFs and the derived SMDs will be particularly important for comparisons as future MFs reach to lower masses.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/df6ff4461b0e8a7d2ae23a3db1ff94d5576f6e19

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. Volker Springel
6. C. Conroy
7. P. V. van Dokkum
8. M. Franx

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. C. Conroy
5. P. V. van Dokkum
6. R. Somerville
7. M. Franx
8. Volker Springel

Citations in the corpus

• A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “Some studies choose to eschew using SPS models and SED fitting altogether in favor of analytical M∗/L relations (calibrated on SPS models; e.g., McCracken et al. 2010 and González et al. 2011) which can applied to a wider selection of data to get “cheap” masses (as in P09 and B12).”
• UV-CONTINUUM SLOPES AT z  ∼  4–7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR–MAGNITUDE RELATIONSHIP FOR z ⩾ 4 STAR-FORMING GALAXIES (2011, methodology): “González et al. (2011) derived these M/L ratios utilizing the HST optical + HST near-IR + Spitzer IRAC photometry for a large sample of z ∼ 4 galaxies within the CDF-South ERS field (including those sources that are not individually detected in the IRAC observations).”
• The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields (2015, methodology): “7, the relations found by Lee et al. (2012) and González et al. (2011) do not reproduce the slope of the M/L relation derived here.”
• UV-CONTINUUM SLOPES OF >4000 z ∼ 4–8 GALAXIES FROM THE HUDF/XDF, HUDF09, ERS, CANDELS-SOUTH, AND CANDELS-NORTH FIELDS (2013, background): “We have constraints on both the ages and emission line strengths of galaxies at z & 4 (e.g., Stark et al. 2009; Labbé et al. 2010; González et al. 2011; González et al. 2012; Stark 2 Leiden Observatory, Leiden University, NL-2300 RA Leiden, Netherlands 3 UCO/Lick Observatory, University of…”
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, methodology): “Other work based on semi-analytical models looked for the descendants of z≈ 2–4 galaxy populations such as sub-millimetre galaxies, Lymanbreak galaxies, and others (Guo & White 2009; González et al. 2011a, 2012).”
• The MUSE Hubble Ultra Deep Field Survey: I. Survey description, data reduction and source detection (2017, background): “…Ellis et al. 2013; Madau & Dickinson 2014; Rafelski et al. 2016; Bouwens et al. 2016; Dunlop et al. 2017), measurements of stellar mass (e.g., González et al. 2011; Grazian et al. 2015; Song et al. 2016), galaxy sizes (e.g., Oesch et al. 2010; Ono et al. 2013; van der Wel et al. 2014;…”
• THE EVOLUTION OF THE GALAXY STELLAR MASS FUNCTION AT z = 4–8: A STEEPENING LOW-MASS-END SLOPE WITH INCREASING REDSHIFT (2015, methodology): “9 are those from González et al. (2011) and Duncan et al. (2014).”
• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “On the other hand there are some differences with the LUV-selected SMFs, as LBGs samples are expected to miss quiescent and dust-obscured galaxies.”
• The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, methodology): “6 the scatter in the SFR–stellar mass relation dominates the random errors, and we adopt the scatter d log(M∗) = 0.5 dex (Gonzalez et al. 2010).”
• UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, background): “In the past, median UV–SM relations have been fit with single power-laws (e.g., González et al. 2011; Stark et al. 2013; Duncan et al. 2014; Salmon et al. 2015; Song et al. 2016).”
• Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “Observations show a very rapid rise from z = 0 → 2, and then essentially no evolution out to very high redshifts (Daddi et al. 2007; Stark et al. 2010; González et al. 2010).”
• CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, background): “…high-redshift GRB rate is substantially higher than the observedρ̇⋆(z) inferred from the abundance of UV-selected galaxies (e.g., Bouwens et al. 2010b; McLure et al. 2010), and would over-produce the observed high-redshift stellar mass density (e.g., Stark et al. 2009; González et al. 2011).”
• Evolution of galaxy stellar masses and star formation rates in the eagle simulations (2014, methodology): “At low masses, below 108 M , the data set of González et al. (2011) shows a flattening in the slope at all redshifts shown.”
• Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, unknown): “…et al. (2011) 1 < z < 3.5 0.0125 I+C Marchesini et al. (2009) 1.3 < z < 4 0.142 I+C Stark et al. (2009) z ∼ 6 0.089 I Lee et al. (2012) 3 < z < 7 0.089 I+SP+C González et al. (2011) 4 < z < 7 0.0778 I+C Duncan et al. (2014) 4 < z < 7 0.0778 C Song et al. (2015) 4 < z < 8 0.0778 I This…”
• The current status of galaxy formation (2012, background): “This result was soon followed by infrared observations that showed that stellar mass assembly favored more massive systems at earlier epochs (González et al., 2011a).”
• The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, methodology): “This rate of stellar mass growth observed is higher than observed by González et al. (2011) over the same time period but comparable to that found by Stark et al. (2013) when the large uncertainty in the z ∼ 7 SMD is taken into account.”
• GOODS–Herschel: an infrared main sequence for star-forming galaxies (2011, background): “…with a typical dispersion of 0.3 dex over a large range of redshifts:z∼0 (Brinchmann et al. 2004),z∼1 (Noeske et al. 2007, Elbaz et al. 2007),z∼2 (Daddi et al. 2007a, Pannella et al. 2009),z∼3 (Magdis et al. 2010a),z∼4 (Daddi et al. 2009, Lee et al. 2011) and even up toz∼7 (Gonzalez et al. 2011).”
• THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, background): “Recent evidence has suggested a relation with significant scatter between M1500 and stellar mass at high redshift, z & 2 (Reddy et al. 2006; Daddi et al. 2007; Stark et al. 2009; González et al. 2011; Reddy et al. 2012; Schaerer et al. 2013; Stark et al. 2013).”