The massive end of the luminosity and stellar mass functions and clustering from CMASS to SDSS: evidence for and against passive evolution

Bernardi, Mariangela; Meert, A.; Sheth, Ravi K.; Huertas-Company, M.; Maraston, Claudia; Shankar, Francesco; Vikram, V.

doi:10.1093/mnras/stv2487

Cited by 42 publications

(54 citation statements)

References 36 publications

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“…We note that the resulting z=0.37 stellar mass function after this correction is in remarkable good agreement with the z=0.1 stellar mass function by . Our result also matches the findings by Bernardi et al (2016), who showed that, by making use of the BOSS sample, the stellar mass function shows negligible number density evolution up to z˜0.5.…”

Section: Highsupporting

confidence: 92%

Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

Grylls

Shankar

Leja

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Observational systematics complicate comparisons with theoretical models limiting understanding of galaxy evolution. In particular, different empirical determinations of the stellar mass function imply distinct mappings between the galaxy and halo masses, leading to diverse galaxy evolutionary tracks. Using our state-of-the-art STatistical sEmi-Empirical modeL, steel, we show fully self-consistent models capable of generating galaxy growth histories that simultaneously and closely agree with the latest data on satellite richness and star-formation rates at multiple redshifts and environments. Central galaxy histories are generated using the central halo mass tracks from state-of-the-art statistical dark matter accretion histories coupled to abundance matching routines. We show that too flat high-mass slopes in the input stellar-masshalo-mass relations as predicted by previous works, imply non-physical stellar mass growth histories weaker than those implied by satellite accretion alone. Our best-fit models reproduce the satellite distributions at the largest masses and highest redshifts probed, the latest data on star formation rates and its bi-modality in the local Universe, and the correct fraction of ellipticals. Our results are important to predict robust and self-consistent stellar-mass-halo-mass relations and to generate reliable galaxy mock catalogues for the next generations of extra-galactic surveys such as Euclid and LSST.

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Section: Highsupporting

confidence: 92%

Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

Grylls

Shankar

Leja

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The details of light profile fitting can have a significant impact on the inferred stellar masses of CMASS galaxies, however. Bernardi et al (2016) demonstrate that the Sérsic profile fits increase the magnitudes of the brightest end of the CMASS galaxy distribution, increasing the abundance of galaxies at M M 10 11.7 *   relative to that derived using cmodel magnitudes. This would change our constraints on the stellar-to-halo mass relation (SHMR) at the very massive endhalo masses above M 10 14  -but would not significantly change our constraints on M log * s , because most of the constraining power on that quantity is at smaller galaxy masses.…”

Section: The Cmass Samplementioning

confidence: 64%

The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe

Tinker

Brownstein

Guo

et al. 2017

ApJ

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We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen et al. clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of M * for galaxies with M log 11.4 *  , correcting for incompleteness at the low-mass end of our measurements. Using the abundance matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b M * ( ) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, . This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.

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“…This framework can also be extended to higher redshift using upcoming cosmological surveys, such as the Extended Baryon Oscillation Spectroscopic Survey (eBOSS, Dawson et al 2016). Although the general view is that the massive RS population evolves in a way that approximates that of a passively evolving galaxy population at z 1 (see, e.g., Cool et al 2008;Tojeiro et al 2012;Maraston et al 2013;Montero-Dorta et al 2016a,b), a detailed characterization has not emerged, and discrepancies with the passive-evolution scenario have been reported (see, e.g., Bernardi et al 2016). The importance of a VDF-based constraint resides in the fact that is independent of SPS models.…”

Section: Discussionmentioning

confidence: 99%

“…The importance of a VDF-based constraint resides in the fact that is independent of SPS models. In addition, the VDF is related to the total mass of galaxies, which provides a different angle to the study of massive galaxy evolution, to be combined with the evolution of the red SMF (see, e.g., Pozzetti et al 2010;Moustakas et al 2013;Bernardi et al 2016) and the red/RS LF (see, e.g., Wake et al 2006;Cool et al 2008;Loveday et al 2012;Montero-Dorta et al 2016a;Bernardi et al 2016).…”

Section: Discussionmentioning

confidence: 99%

A direct measurement of the high-mass end of the velocity dispersion function at z ∼ 0.55 from SDSS-III/BOSS

Montero-Dorta

Bolton

Shu

2017

Monthly Notices of the Royal Astronomical Society

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We report the first direct spectroscopic measurement of the velocity dispersion function (VDF) for the high-mass red sequence (RS) galaxy population at redshift z ∼ 0.55. We achieve high precision by using a sample of 600,000 massive galaxies with spectra from the Baryon Oscillation Spectroscopic Survey (BOSS) of the third Sloan Digital Sky Survey (SDSS-III), covering stellar masses M * 10 11 M ⊙ . We determine the VDF by projecting the joint probability-density function (PDF) of luminosity L and velocity dispersion σ, i.e. p(L, σ), defined by our previous measurements of the RS luminosity function and L − σ relation for this sample. These measurements were corrected from red-blue galaxy population confusion, photometric blurring, incompleteness and selection effects within a forward-modeling framework that furthermore correctly accommodates the low spectroscopic signal-to-noise ratio of individual BOSS spectra. Our z ∼ 0.55 RS VDF is in overall agreement with the z ∼ 0 early-type galaxy (ETG) VDF at log 10 σ 2.47, however the number density of z = 0.55 RS galaxies that we report is larger than that of z = 0 ETG galaxies at 2.35 log 10 σ 2.47. The extrapolation of an intermediate-mass L-σ relation towards the high-mass end in previous low-z works may be responsible for this disagreement. Evolutionary interpretation of this comparison is also subject to differences in the way the respective samples are selected; these differences can be mitigated in future work by analyzing z = 0 SDSS data using the same framework presented in this paper. We also provide the sample PDF for the RS population (i.e. uncorrected for incompleteness), which is a key ingredient for gravitational lensing analyses using BOSS.

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The massive end of the luminosity and stellar mass functions and clustering from CMASS to SDSS: evidence for and against passive evolution

Cited by 42 publications

References 36 publications

Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe

A direct measurement of the high-mass end of the velocity dispersion function at z ∼ 0.55 from SDSS-III/BOSS

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