LARgE Survey – I. Dead monsters: the massive end of the passive galaxy stellar mass function at cosmic noon

Arcila-Osejo, Liz; Sawicki, Marcin; Arnouts, S.; Golob, Anneya; Moutard, T.; Sorba, Robert

doi:10.1093/mnras/stz1169

Cited by 10 publications

(36 citation statements)

References 91 publications

(196 reference statements)

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“…We note that for a typical UMPEG with M UMPEG ≈ 10 11.6 M , satellites of 1:5.5 mass ratio have stellar masses M sat = 0.18×M UMPEG ≈ 10 10.8 , which is similar to the characteristic Schechter mass of M * ∼ 10 10.6−10.8 for quiescent z∼1.6 galaxies (indicated with the arrow in Fig. 4; Arcila-Osejo & Sawicki 2013;Ilbert et al 2013;Muzzin et al 2013a;Tomczak et al 2014;Arcila-Osejo et al 2019). Consequently, our "low-mass" UMPEG satellites are in fact very massive themselves.…”

Section: Masses Of Umpeg Satellitesmentioning

confidence: 58%

“…The detailed description of our catalogs and sample selection is given in Arcila-Osejo et al (2019) so here we only summarize the key details.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

“…In the modern cosmic structure formation framework, dark matter halos form from initial density perturbations via gravitational collapse (White & Rees 1978) and subsequently grow bottom-up via hierarchical merging (White & Frenk 1991;Kauffmann & White 1993). Today, the most massive of these halos host galaxy clusters, at the centres of which reside Brightest Cluster Galaxies (BCGs) -ultramassive galaxies that are among the most extreme, most massive galaxies in the present-day Universe (stellar masses Passively Evolving Galaxies (UMPEGs; M > 10 11.5 M ), while very rare have -however -been found at z > 1 (e.g., Marchesini et al 2014;Arcila-Osejo et al 2019), with a handful of examples spectroscopically confirmed out to z∼4 (Onodera et al 2012;Belli et al 2016;Kado-Fong et al 2017;Stockmann et al 2020;Forrest et al 2019). If they formed as single objects through intense bursts of star formation, UMPEG progenitors must have had star formation rates (SFRs) of several hundred M /yr (e.g., Arcila-Osejo et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…Today, the most massive of these halos host galaxy clusters, at the centres of which reside Brightest Cluster Galaxies (BCGs) -ultramassive galaxies that are among the most extreme, most massive galaxies in the present-day Universe (stellar masses Passively Evolving Galaxies (UMPEGs; M > 10 11.5 M ), while very rare have -however -been found at z > 1 (e.g., Marchesini et al 2014;Arcila-Osejo et al 2019), with a handful of examples spectroscopically confirmed out to z∼4 (Onodera et al 2012;Belli et al 2016;Kado-Fong et al 2017;Stockmann et al 2020;Forrest et al 2019). If they formed as single objects through intense bursts of star formation, UMPEG progenitors must have had star formation rates (SFRs) of several hundred M /yr (e.g., Arcila-Osejo et al 2019). Moreover, UMPEGs are very strongly clustered (Cheema et al 2020), suggesting that they are associated with the high-z progenitors of present-day massive galaxy clusters; UMPEGs could therefore be the direct, main-branch progenitors of some of the present-day BCGs.…”

Section: Introductionmentioning

confidence: 99%

“…An alternative approach to testing the merger scenario is to identify BCG progenitors in a way that is less dependent on assumptions inherent in galaxy abundance matching, whether corrected or not using hierarchical merger trees. In (Arcila-Osejo et al 2019) we used wide-area imaging to identify a population of z ∼ 1.6 UMPEGs, and their extremely strong clustering (r 0 = 29.77 ± 2.75 h −1 Mpc) suggests that they are associated with halos of mass M halo ∼ 10 14.1 h −1 M . Under the assumption of smooth halo mass growth, these z∼1.6 halos are likely to be the progenitors of present-day massive (M halo ∼ 10 15 M ) galaxy clusters (Cheema et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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LARgE survey – III. Environments of ultra-massive passive galaxies at cosmic noon: BCG progenitors growing through mergers

Sawicki

Arcila-Osejo

Golob

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the environments of a sample of 61 extremely rare z∼1.6 Ultra-Massive Passively Evolving Galaxies (UMPEGs: stellar masses M > 10 11.5 M ) which -based on clustering analysis presented in Cheema et al. (2020) -appear to be associated with very massive (M halo ∼10 14.1 h −1 M ) dark matter halos that are likely to be the progenitors of z∼0 massive (Coma-and Virgo-like) galaxy clusters. We find that UMPEGs on average have fewer than one satellite galaxy with mass ratio M sat :M UMPEG ≥1:5 (i.e., M sat > ∼ 10 10.8 M ) within 0.5 Mpc; the large mass gap that we observe between the typical UMPEG and its most massive satellite implies that the z∼1.6 UMPEGs assembled through major mergers. Using observed satellite counts with merger timescales from the literature, we estimate the growth rate due to mergers with mass ratio of ≥ 1:4 to be ∼13% Gyr −1 (with a ∼2× systematic uncertainty). This relatively low growth rate is unlikely to significantly affect the shape of the massive end of the stellar mass function, whose evolution must instead be driven by the quenching of new cohorts of ultra-massive star-forming galaxies. However, this growth rate is high enough that, if sustained to z∼0, the typical z∼1.6 M UMPEG = 10 11.6 M UMPEG can grow into a M ≈ 10 12 M brightest cluster galaxy (BCG) of a present-day massive galaxy cluster. Our observations favour a scenario in which our UMPEGs are main-branch progenitors of some of the present-day BCGs that have first assembled through major mergers at high redshifts and grown further through (likely minor) merging at later times.

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Section: Masses Of Umpeg Satellitesmentioning

confidence: 58%

“…The detailed description of our catalogs and sample selection is given in Arcila-Osejo et al (2019) so here we only summarize the key details.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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LARgE survey – III. Environments of ultra-massive passive galaxies at cosmic noon: BCG progenitors growing through mergers

Sawicki

Arcila-Osejo

Golob

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The miniJPAS survey

Rodríguez‐Martín

Delgado

Martínez-Solaeche

et al. 2022

A&A

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The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is a photometric survey that is poised to scan several thousands of square degrees of the sky. It will use 54 narrow-band filters, combining the benefits of low-resolution spectra and photometry. Its offshoot, miniJPAS, is a 1 deg 2 survey that uses J-PAS filter system with the Pathfinder camera. In this work, we study mJPC2470-1771, the most massive cluster detected in miniJPAS. We survey the stellar population properties of the members, their star formation rates (SFR), star formation histories (SFH), the emission line galaxy (ELG) population, spatial distribution of these properties, and the ensuing effects of the environment. This work shows the power of J-PAS to study the role of environment in galaxy evolution. We used a spectral energy distribution (SED) fitting code to derive the stellar population properties of the galaxy members: stellar mass, extinction, metallicity, (u − r) res and (u − r) int colours, mass-weighted age, the SFH that is parametrised by a delayed-τ model (τ, t 0 ), and SFRs. We used artificial neural networks for the identification of the ELG population via the detection of the Hα, [NII], Hβ, and [OIII] nebular emission. We used the Ew(Hα)-[NII] (WHAN) and [OIII]/Hα-[NII]/Hα (BPT) diagrams to separate them into individual star-forming galaxies and AGNs. We find that the fraction of red galaxies increases with the cluster-centric radius; and at 0.5 R 200 the red and blue fractions are both equal. The redder, more metallic, and more massive galaxies tend to be inside the central part of the cluster, whereas blue, less metallic, and less massive galaxies are mainly located outside of the inner 0.5 R 200 . We selected 49 ELG, with 65.3 % of the them likely to be star-forming galaxies, dominated by blue galaxies, and 24 % likely to have an AGN (Seyfert or LINER galaxies). The rest are difficult to classify and are most likely composite galaxies. These latter galaxies are red, and their abundance decreases with the cluster-centric radius; in contrast, the fraction of star-forming galaxies increases outwards up to R 200 . Our results are compatible with an scenario in which galaxy members were formed roughly at the same epoch, but blue galaxies have had more recent star formation episodes, and they are quenching out from within the cluster centre. The spatial distribution of red galaxies and their properties suggest that they were quenched prior to the cluster accretion or an earlier cluster accretion epoch. AGN feedback or mass might also stand as an obstacle in the quenching of these galaxies.

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The CAVITY project: The spatially resolved stellar population properties of galaxies in voids

Conrado,

González Delgado,

García-Benito

et al. 2024

A&A

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The Universe is shaped as a web-like structure, formed by clusters, filaments, and walls that leave large low number-density volumes in between named voids. Galaxies in voids have been found to be of a later type, bluer, less massive, and to have a slower evolution than galaxies in denser environments (filaments and walls). However, the effect of the void environment on their stellar population properties is still unclear. We aim to address this question using 118 optical integral field unit datacubes from the Calar Alto Void Integral-field Treasury surveY (CAVITY), observed with the PMAS/PPaK spectrograph at the 3.5m telescope at the Calar Alto Observatory (Almería, Spain). We fitted their spectra from $3750 to $7000 with the non-parametric full spectral fitting code STARLIGHT to estimate their stellar population properties: stellar mass, stellar mass surface density, age, star formation rate (SFR), and specific star formation rate (sSFR). We analysed the results through the global properties, assessing the behaviour of the whole galaxy, and the spatially resolved information, by obtaining the radial profiles from the 2D maps up to the 2 half-light radius of each stellar population property. The results were examined with respect to their morphological type and stellar mass. Then, we compared them with a control sample of galaxies in filaments and walls, selected from the CALIFA survey and analysed following the same procedure. To make a fair comparison between the samples, we selected a twin filament galaxy for each void galaxy of the same morphological type and closest stellar mass, to match the void galaxy sample as much as possible in morphology and mass. Key findings from our global and spatially resolved analysis include void galaxies having a slightly higher half-light radius (HLR), lower stellar mass surface density, and younger ages across all morphological types, and slightly elevated SFR and sSFR (only significant enough for Sas). Many of these differences appear in the outer parts of spiral galaxies (HLR > 1), where discs are younger and exhibit a higher sSFR compared to galaxies in filaments and walls, indicative of less evolved discs. This trend is also found for early-type spirals, suggesting a slower transition from star-forming to quiescent states in voids. Our analysis indicates that void galaxies, influenced by their surroundings, undergo a more gradual evolution, especially in their outer regions, with a more pronounced effect for low-mass galaxies. We find that below a certain mass threshold, environmental processes play a more influential role in galactic evolution.

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LARgE Survey – I. Dead monsters: the massive end of the passive galaxy stellar mass function at cosmic noon

Cited by 10 publications

References 91 publications

LARgE survey – III. Environments of ultra-massive passive galaxies at cosmic noon: BCG progenitors growing through mergers

LARgE survey – III. Environments of ultra-massive passive galaxies at cosmic noon: BCG progenitors growing through mergers

The miniJPAS survey

The CAVITY project: The spatially resolved stellar population properties of galaxies in voids

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