The shape and scatter of the galaxy main sequence for massive galaxies at cosmic noon

Sherman, Sydney; Jogee, Shardha; Florez, Jonathan; Finkelstein, Steven L.; Ciardullo, Robin; Wold, Isak; Stevans, Matthew L.; Kawinwanichakij, Lalitwadee; Papovich, Casey; Grönwall, C.

doi:10.1093/mnras/stab1350

Cited by 13 publications

(11 citation statements)

References 92 publications

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“…the density peak in the SFR-mass plane) (Renzini & Peng 2015), or using flexible Gaussian mixture models with the number of Gaussian sub-components determined by the data (Hahn et al 2019). In the limit of wide-area surveys, these data-driven approaches can accurately measure higher-order moments of the star-forming sequence such as the width or the location of the so-called 'green valley' (Sherman et al 2021).…”

Section: Introductionmentioning

confidence: 99%

A New Census of the 0.2 < z < 3.0 Universe. I. The Stellar Mass Function

Leja

Speagle

Johnson

et al. 2020

ApJ

105

149

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There has been a long-standing factor-of-two tension between the observed star formation rate density and the observed stellar mass buildup after z ∼ 2. Recently we have proposed that sophisticated panchromatic SED models can resolve this tension, as these methods infer systematically higher masses and lower star formation rates than standard approaches. In a series of papers we now extend this analysis and present a complete, self-consistent census of galaxy formation over 0.2 < z < 3 inferred with the Prospector galaxy SED-fitting code. In this work, Paper I, we present the evolution of the galaxy stellar mass function using new mass measurements of ∼10 5 galaxies in the 3D-HST and COSMOS-2015 surveys. We employ a new methodology to infer the mass function from the observed stellar masses: instead of fitting independent mass functions in a series of fixed redshift intervals, we construct a continuity model that directly fits for the redshift evolution of the mass function. This approach ensures a smooth picture of galaxy assembly and makes use of the full, non-Gaussian uncertainty contours in our stellar mass inferences. The resulting mass function has higher number densities at a fixed stellar mass than almost any other measurement in the literature, largely owing to the older stellar ages inferred by Prospector. The stellar mass density is ∼50% higher than previous measurements, with the offset peaking at z ∼ 1. The next two papers in this series will present the new measurements of star-forming main sequence and the cosmic star formation rate density, respectively.

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Section: Introductionmentioning

confidence: 99%

A New Census of the 0.2 < z < 3.0 Universe. I. The Stellar Mass Function

Leja

Speagle

Johnson

et al. 2020

ApJ

105

149

View full text Add to dashboard Cite

show abstract

“…Understanding the nature, evolution (both with mass and redshift), and the timescales associated with this scatter is a currently active area of research (e.g. Speagle et al 2014, Matthee & Schaye 2019, Berti et al 2021, Sherman et al 2021.…”

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confidence: 99%

The cold interstellar medium of galaxies in the Local Universe

Saintonge¹,

Catinella²

2022

Preprint

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The cold interstellar medium (ISM) plays a central role in the galaxy evolution process. It is the reservoir that fuels galaxy growth via star formation, the repository of material formed by these stars, and a sensitive tracer of internal and external processes that affect entire galaxies. Consequently, significant efforts have gone into systematic surveys of the cold ISM of the galaxies in the local Universe. This review discusses the resulting network of scaling relations connecting the atomic and molecular gas masses of galaxies with their other global properties (stellar masses, morphologies, metallicities, star formation activity...), and their implications for our understanding of galaxy evolution. Key take-home messages are as follows:• From a gas perspective, there are three main factors that determine the star formation rate of a galaxy: the total mass of its cold ISM, how much of that gas is molecular, and the rate at which any molecular gas is converted into stars. All three of these factors vary systematically across the local galaxy population.• The shape and scatter of both the star formation main sequence and the mass-metallicity relation are deeply linked to the availability of atomic and molecular gas.• Future progress will come from expanding our exploration of scaling relations into new parameter space (in particular the regime of dwarf galaxies), better connecting the cold ISM of large samples of galaxies with the environment that feeds them (the circumgalactic medium in particular), and understanding the impact of these large scales on the efficiency of the star formation process on molecular cloud scales.

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“…It is not dominated by IR-bright (i.e., in dust continuum) submm galaxies (SMGs). The ALPINE galaxies are mainly located on or near the main sequence (e.g., Rodighiero et al 2011;Gruppioni et al 2013;Donnari et al 2019;Sherman et al 2021) in the SFR versus stellar mass (M star ) relation observed at these redshifts (Speagle et al 2014;Pearson et al 2018). It is mostly dominated by UVselected galaxies (see Table 1 in with about 62% of the sample identified with the dropout technique, that is LBGs and 28% that are Lyman α emitters which were selected with narrow bands.…”

Section: The Sample Of Studied Galaxiesmentioning

confidence: 99%

The ALMA-ALPINE [CII] survey

Burgarella

Bogdanoska

Nanni

et al. 2022

A&A

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Star-forming galaxies are composed of various types of galaxies. However, the luminosity functions at z 4 -5 suggest that most galaxies have a relatively low stellar mass (log M star ∼ 10) and a low dust attenuation (A FUV ∼ 1.0). The physical properties of these objects are quite homogeneous. We used an approach where we combined their rest-frame far-infrared and submillimeter emissions and utilized the universe and the redshift as a spectrograph to increase the amount of information in a collective way. From a subsample of 27 ALMA-detected galaxies at z > 4.5, we built an infrared spectral energy distribution composite template. It was used to fit, with CIGALE, the 105 galaxies (detections and upper limits) in the sample from the far-ultraviolet to the far-infrared. The derived physical parameters provide information to decipher the nature of the dust cycle and of the stellar populations in these galaxies. The derived IR composite template is consistent with the galaxies in the studied sample. A delayed star formation history with τ main = 500 Myrs is slightly favored by the statistical analysis as compared to a delayed with a final burst or a continuous star formation history. The position of the sample in the star formation rate (SFR) versus M star diagram is consistent with previous papers. The redshift evolution of the log M star versus A FUV relation is in agreement with an evolution in redshift of this relation. This evolution is necessary to explain the cosmic evolution of the average dust attenuation of galaxies. Evolution is also observed in the L dust / L FUV (IRX) versus UV slope β FUV diagram: younger galaxies have bluer β FUV . We modeled the shift of galaxies in the IRX versus the β FUV diagram with the mass-weighted age as a free parameter, and we provide an equation to make predictions. The large sample studied in this paper is generally consistent with models that assume rapid dust formation from supernovae and removal of dust by outflows and supernovae blasts. However, we find that high mass dusty star-forming galaxies cannot be explained by the models.

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The shape and scatter of the galaxy main sequence for massive galaxies at cosmic noon

Cited by 13 publications

References 92 publications

A New Census of the 0.2 < z < 3.0 Universe. I. The Stellar Mass Function

A New Census of the 0.2 < z < 3.0 Universe. I. The Stellar Mass Function

The cold interstellar medium of galaxies in the Local Universe

The ALMA-ALPINE [CII] survey

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