Compact star-forming galaxies preferentially quenched to become PSBs in<i>z</i>&lt; 1 clusters

Socolovsky, Miguel; Maltby, David T.; Hatch, N. A.; Almaini, O.; Wild, Vivienne; Hartley, W. G.; Simpson, Chris; Rowlands, Kate

doi:10.1093/mnras/sty2840

Cited by 17 publications

(18 citation statements)

References 72 publications

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“…They contain a high fraction of AGN (Wild et al 2010), and their observed properties are largely consistent with them evolving into spheroidal galaxies in several hundred Myr (Yang et al 2006;Pawlik et al 2016). Differences are found for cluster PSBs, where environmental effects such as ram-pressure stripping and weak galaxy-galaxy interactions could also be responsible for the recent shut off in star formation (Aragon-Salamanca et al 2013;Mahajan 2013;Socolovsky et al 2019). At z > 1 PSB galaxies are predominantly massive (Wild et al 2016) and highly compact (Almaini et al 2017), while at lower redshift PSBs are predominantly low mass with morphologies consistent with low-mass spheroids (Pawlik et al 2018;Maltby et al 2018).…”

Section: Introductionmentioning

confidence: 84%

Mergers, starbursts, and quenching in the simba simulation

Montero

Davé

Wild

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use the simba cosmological galaxy formation simulation to investigate the relationship between major mergers ($\lesssim$4:1), starbursts, and galaxy quenching. Mergers are identified via sudden jumps in stellar mass M* well above that expected from in situ star formation, while quenching is defined as going from specific star formation rate (sSFR) $\gt t_{\rm H}^{-1}$ to $\lt 0.2t_{\rm H}^{-1}$, where tH is the Hubble time. At z ≈ 0–3, mergers show ∼2–3× higher SFR than a mass-matched sample of star-forming galaxies, but globally represent $\lesssim 1{{\ \rm per\ cent}}$ of the cosmic SF budget. At low masses, the increase in SFR in mergers is mostly attributed to an increase in the H2 content, but for $M_*\gtrsim 10^{10.5} \,\mathrm{ M}_{\odot }$ mergers also show an elevated star formation efficiency suggesting denser gas within merging galaxies. The merger rate for star-forming galaxies shows a rapid increase with redshift, ∝(1 + z)3.5, but the quenching rate evolves much more slowly, ∝(1 + z)0.9; there are insufficient mergers to explain the quenching rate at $z\lesssim 1.5$. simba first quenches galaxies at $z\gtrsim 3$, with a number density in good agreement with observations. The quenching time-scales τq are strongly bimodal, with ‘slow’ quenchings (τq ∼ 0.1tH) dominating overall, but ‘fast’ quenchings (τq ∼ 0.01tH) dominating in M* ∼ 1010–1010.5 M$\odot$ galaxies, likely induced by simba’s jet-mode black hole feedback. The delay time distribution between mergers and quenching events suggests no physical connection to either fast or slow quenching. Hence, simba predicts that major mergers induce starbursts, but are unrelated to quenching in either fast or slow mode.

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Section: Introductionmentioning

confidence: 84%

Mergers, starbursts, and quenching in the simba simulation

Montero

Davé

Wild

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Complex molecular gas morphologies and filamentary structures have been found associated with local gas-rich BCGs (e.g., Russell et al 2016Russell et al , 2017. Several observational studies have also proposed connections between the optical morphologies and the star formation properties of distant galaxies (van der Wel et al 2014;Dimauro et al 2018Dimauro et al , 2019Socolovsky et al 2018Socolovsky et al , 2019Puglisi et al 2019;Freundlich et al 2019). Inspired by these studies we investigate the morphological properties of the 11 BCGs considered in this work, while in Sect.…”

Section: Morphological Classification Of the Bcgsmentioning

confidence: 90%

“…We compare our results with those independently found for different samples of distant galaxies. Recent studies by Socolovsky et al (2018Socolovsky et al ( , 2019 show that galaxies with high sSFR 1 Gyr −1 in dense environments at 0.5 < z < 1.0 are strongly depleted due to rapid environmental quenching, and are likely to evolve into post-starbursts (PSBs). They also tend to have larger effective radii than those in the field, possibly because the most compact star-forming galaxies are preferentially quenched in dense environments.…”

Section: Compactness and Quenchingmentioning

confidence: 99%

Molecular gas in distant brightest cluster galaxies

Castignani

Combes

Salomé

et al. 2020

A&A

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Brightest cluster galaxies (BCGs) are excellent laboratories to study galaxy evolution in dense Mpc-scale environments. We have observed in CO(1→0), CO(2→1), CO(3→2), or CO(4→3), with the IRAM-30m, 18 BCGs at z ∼ 0.2 − 0.9 that are drawn from the Cluster Lensing And Supernova survey with Hubble (CLASH) survey. Our sample includes RX1532, which is our primary target, being among the BCGs with the highest star formation rate (SFR 100 M /yr) in the CLASH sample. We unambiguously detected both CO(1→0) and CO(3→2) in RX1532, yielding a large reservoir of molecular gas, M H 2 = (8.7 ± 1.1) × 10 10 M , and a high level of excitation r 31 = 0.75 ± 0.12. A morphological analysis of the Hubble Space Telescope I-band image of RX1532 reveals the presence of clumpy substructures both within and outside the half-light radius r e = (11.6 ± 0.3) kpc, similarly to those found independently both in ultraviolet and in H α in previous work. We tentatively detected CO(1→0) or CO(2→1) in four other BCGs, with molecular gas reservoirs in the range M H 2 = 2 × 10 10−11 M . For the remaining 13 BCGs we set robust upper limits of M H 2 /M 0.1, which are among the lowest molecular gas to stellar mass ratios found for distant ellipticals and BCGs. By comparison with distant cluster galaxies observed in CO our study shows that RX1532 (M H 2 /M = 0.40 ± 0.05) belongs to the rare population of star forming and gas-rich BCGs in the distant universe. By using available X-ray based estimates of the central intra-cluster medium entropy, we show that the detection of large reservoirs of molecular gas M H 2 10 10 M in distant BCGs is possible when the two conditions are met: i) high SFR and ii) low central entropy, which favors the condensation and the inflow of gas onto the BCGs themselves, similarly to what has been previously found for some local BCGs.

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mentioning

confidence: 91%

Mergers, Starbursts, and Quenching in the Simba Simulation

Montero,

Davé,

Wild

et al. 2019

Preprint

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We use the Simba cosmological galaxy formation simulation to investigate the relationship between major mergers ( < ∼ 4:1), starbursts, and galaxy quenching. Mergers are identified via sudden jumps in stellar mass M * well above that expected from in situ star formation, while quenching is defined as going from specific star formation rate sSFR> t −1 H to sSFR< 0.2t −1 H , where t H is the Hubble time. At z ≈ 0 − 3, mergers show ∼ ×2 − 3 higher SFR than a mass-matched sample of star-forming galaxies, but globally represent < ∼ 1% of the cosmic SF budget. At low masses, the increase in SFR in mergers is mostly attributed to an increase in the H 2 content, but for M * > ∼ 10 10.5 M mergers also show an elevated star formation efficiency suggesting denser gas within merging galaxies. The merger rate for star-forming galaxies shows a rapid increase with redshift ∝ (1 + z) 3.5 , but the quenching rate evolves much more slowly, ∝ (1 + z) 0.9 ; there are insufficient mergers to explain the quenching rate at z < ∼ 1.5. Simba first quenches galaxies at z > ∼ 3, with a number density in good agreement with observations. The quenching timescales τ q are strongly bimodal, with 'slow' quenchings (τ q ∼ 0.1t H ) dominating overall, but 'fast' quenchings (τ q ∼ 0.01t H ) dominating in M * ∼ 10 10 − 10 10.5 M galaxies, likely induced by Simba's jet-mode black hole feedback. The delay time distribution between mergers and quenching events suggests no physical connection to either fast or slow quenching. Hence, Simba predicts that major mergers induce starbursts, but are unrelated to quenching in either fast or slow mode.

show abstract

Compact star-forming galaxies preferentially quenched to become PSBs inz< 1 clusters

Cited by 17 publications

References 72 publications

Mergers, starbursts, and quenching in the simba simulation

Mergers, starbursts, and quenching in the simba simulation

Molecular gas in distant brightest cluster galaxies

Mergers, Starbursts, and Quenching in the Simba Simulation

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