Does the galaxy–halo connection vary with environment?

Dragomir, Radu; Rodríguez-Puebla, Aldo; Primack, Joel R.; Lee, Christoph T.

doi:10.1093/mnras/sty283

Cited by 40 publications

(43 citation statements)

References 87 publications

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“…We use K-corrected magnitudes at z = 0 tabulated in Blanton et al (2017). In addition, we introduce the empirical model for the E-correction at z = 0 described in Dragomir et al (2018). Finally, we derive the GSMF from the galaxy sample in Blanton et al (2017) denoted herafter as φ * (M * ).…”

Section: Appendix E: Volume Correctionsmentioning

confidence: 99%

SDSS-IV MaNGA – an archaeological view of the cosmic star formation history

Sánchez

Avila-Reese

Rodríguez-Puebla

et al. 2018

Monthly Notices of the Royal Astronomical Society

105

157

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We present the results of the archaeological analysis of the stellar populations of a sample of ∼4,000 galaxies observed by the SDSS-IV-MaNGA survey using Pipe3D. Based on this analysis we extract a sample of ∼150,000 SFRs and stellar masses that mimic a single cosmological survey covering the redshift range between z ∼0 to z ∼7. We confirm that the Star-Forming Main Sequence holds as a tight relation in this range of redshifts, evolving in both the zero-point and slope. This evolution is different for local star-forming (SFGs) and retired (RGs) galaxies, with the latter presenting a stronger evolution in the zero-point and a weaker evolution in the slope. The fraction of RGs decreases rapidly with z, particularly for RGs at z ∼ 0. We detect RGs well above z > 1, although not all of them are progenitors of local RGs. Finally, adopting the required corrections to make the survey complete in mass in a limited volume, we recover the cosmic star-formation rate (SFR), stellar mass density, and average specific SFR histories of the Universe in this wide range of look-back times. Our derivations agree with those reported by various cosmological surveys. We demonstrate that the progenitors of local RGs were more actively forming stars in the past, contributing to most of the cosmic SFR density at z > 0.5, and to most of the cosmic stellar mass density at any redshift. They suffer a general quenching in the SFR at z∼0.35. Below this redshift the progenitors of local SFGs dominate the SFR density of the Universe.

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Section: Appendix E: Volume Correctionsmentioning

confidence: 99%

SDSS-IV MaNGA – an archaeological view of the cosmic star formation history

Sánchez

Avila-Reese

Rodríguez-Puebla

et al. 2018

Monthly Notices of the Royal Astronomical Society

105

157

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“…This could still be quite expensive if the goal is efficiently creating fully nonlinear galaxy catalogues that could be directly compared to observations. One of the most promising ★ E-mail:matteo_zennaro001@ehu.eus methods in this sense is the so called sub-halo abundance matching (Conroy et al 2006;Reddick et al 2013;Chaves-Montero et al 2016;Lehmann et al 2017;Dragomir et al 2018), which exploits the substructures identified in gravity-only simulations, matching their abundance to an observed stellar-mass or luminosity functions. Recent improvements to this technique, such as the SHAMe model proposed by Contreras et al (2021b), have proven particularly reliable in reproducing hydrodynamical results at a fraction of the computational cost.…”

Section: Introductionmentioning

confidence: 99%

Priors on Lagrangian bias parameters from galaxy formation modelling

Zennaro,

Angulo,

Contreras

et al. 2021

Preprint

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We study the relations among the parameters of the hybrid Lagrangian bias expansion model, fitting biased auto and cross power spectra up to 𝑘 max = 0.7ℎ Mpc −1 . We consider ∼ 8000 halo and galaxy samples, with different halo masses, redshifts, galaxy number densities, and varying the parameters of the galaxy formation model. Galaxy samples are obtained through state-of-the-art extended subhalo abundance matching techniques and include both stellar-mass and star-formation-rate selected galaxies. All of these synthetic galaxies samples are publicly available at https://bacco.dipc.org/galpk.html. We find that the hybrid Lagrangian bias model provides accurate fits to all of our halo and galaxy samples. The coevolution relations between galaxy bias parameters, although roughly compatible with those obtained for haloes, show systematic shifts and larger scatter. We explore possible sources of this difference in terms of dependence on halo occupation and assembly bias of each sample. The bias parameter relations displayed in this work can be used as a prior for future Bayesian analyses employing the hybrid Lagrangian bias expansion model.

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“…where M 0.0 r,i is the Petrosian magnitude K+E-corrected at a rest frame z = 0, K gr,i (z) is the K-correction (see Appendix B) and E r,i = 1.1z (following Dragomir et al 2018) for the ith galaxy in the sample. For the completeness limits, we use the limiting apparent magnitude in the r-band of m lim,r = 17.77.…”

Section: A Derivation Of the Sdss Dr7 Gsmfmentioning

confidence: 99%

“…We apply K+E-corrections at a rest frame z = 0. We use the values reported in Dragomir et al (2018) for g and i bands given, respectively, by E g = 1.3 × z and E i = 1.09 × z. K-corrections are discuss in Appendix B. We applied a shift of −0.1 dex to the resulting masses from the colour-dependent mass-to-light ratios of Bell et al (2003) to be consistent with the Chabrier (2003) IMF adopted in this paper.…”

Section: A Derivation Of the Sdss Dr7 Gsmfmentioning

confidence: 99%

The bivariate gas–stellar mass distributions and the mass functions of early- and late-type galaxies at

Rodríguez-Puebla

Calette

Ávila-Reese

et al. 2020

Publ. Astron. Soc. Aust.

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We report the bivariate $\rm HI$ - and $\rm H_{2}$ -stellar mass distributions of local galaxies in addition of an inventory of galaxy mass functions, MFs, for $\rm HI$ , $\rm H_{2}$ , cold gas, and baryonic mass, separately into early- and late-type galaxies. The MFs are determined using the $\rm HI$ and $\rm H_{2}$ conditional distributions and the galaxy stellar mass function (GSMF). For the conditional distributions we use the results from the compilation presented in Calette et al. [(2018) RMxAA, 54, 443.]. For determining the GSMF from $M_{*}\sim3\times10^{7}$ to $3\times10^{12}\ \text{M}_{\odot}$ , we combine two spectroscopic samples from the Sloan Digital Sky Survey at the redshift range $0.0033<z<0.2$ . We find that the low-mass end slope of the GSMF, after correcting from surface brightness incompleteness, is $\alpha\approx-1.4$ , consistent with previous determinations. The obtained $\rm HI\,$ MFs agree with radio blind surveys. Similarly, the $\rm H_{2}\,$ MFs are consistent with CO follow-up optically-selected samples. We estimate the impact of systematics due to mass-to-light ratios and find that our MFs are robust against systematic errors. We deconvolve our MFs from random errors to obtain the intrinsic MFs. Using the MFs, we calculate cosmic density parameters of all the baryonic components. Baryons locked inside galaxies represent 5.4% of the universal baryon content, while $\sim\! 96\%$ of the $\rm HI$ and $\rm H_{2}$ mass inside galaxies reside in late-type morphologies. Our results imply cosmic depletion times of $\rm H_{2}$ and total neutral H in late-type galaxies of $\sim\!1.3$ and 7.2 Gyr, respectively, which shows that late type galaxies are on average inefficient in converting $\rm H_{2}$ into stars and in transforming $\rm HI$ gas into $\rm H_{2}$ . Our results provide a fully self-consistent empirical description of galaxy demographics in terms of the bivariate gas–stellar mass distribution and their projections, the MFs. This description is ideal to compare and/or to constrain galaxy formation models.

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Does the galaxy–halo connection vary with environment?

Cited by 40 publications

References 87 publications

SDSS-IV MaNGA – an archaeological view of the cosmic star formation history

SDSS-IV MaNGA – an archaeological view of the cosmic star formation history

Priors on Lagrangian bias parameters from galaxy formation modelling

The bivariate gas–stellar mass distributions and the mass functions of early- and late-type galaxies at

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