Massive Quenched Galaxies at z ∼ 0.7 Retain Large Molecular Gas Reservoirs

Suess, Katherine A.; Bezanson, Rachel; Spilker, Justin; Kriek, Mariska; Greene, Jenny E.; Feldmann, Robert; Hunt, Qiana; Narayanan, Desika

doi:10.3847/2041-8213/aa85dc

Cited by 73 publications

(114 citation statements)

References 53 publications

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“…The molecular gas contents of post-starbursts outside the local universe are essentially unconstrained. Suess et al (2017) present observations of two massive post-starburst galaxies at z ∼ 0.7, finding molecular gas masses that yield low gas fractions but depletion times of several Gyr, two orders of magnitude longer than our measurement of COSMOS 27289. Given its still rapid SFR, it may be that COSMOS 27289 will be more completely depleted of molecular gas than either of those lower-redshift post-starbursts; ALMA observations of z ∼ 2 post-starbursts are required to make a more direct comparison.…”

Section: Comparison To Probable Progenitor and Descendant Populationscontrasting

confidence: 57%

Evidence for Inside-out Galaxy Growth and Quenching of a z ∼ 2 Compact Galaxy From High-resolution Molecular Gas Imaging

Spilker

Bezanson

Weiner

et al. 2019

ApJ

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We present high spatial resolution imaging of the CO(1-0) line from the Karl G. Jansky Very Large Array (VLA) of COSMOS 27289, a massive, compact star forming galaxy at z = 2.234. This galaxy was selected to be structurally similar to z ∼ 2 passive galaxies. Our previous observations showed that it is very gas-poor with respect to typical star-forming galaxies at these redshifts, consistent with a rapid transition to quiescence as the molecular gas is depleted. The new data show that both the molecular gas fraction f H2 ≡ M H2 /M star and the molecular gas depletion time t dep ≡ M H2 /SFR are lower in the central 1-2 kpc of the galaxy and rise at larger radii ∼2-4 kpc. These observations are consistent with a scenario in which COSMOS 27289 will imminently cease star formation in the inner regions before the outskirts, i.e. inside-out quenching, the first time this phenomenon has been seen via observations of molecular gas in the high-redshift universe. We find good qualitative and quantitative agreement with a hydrodynamical simulation of galaxy quenching, in which the central suppression of molecular gas arises due to rapid gas consumption and outflows that evacuate the central regions of gas. Our results provide independent evidence for inside-out quenching of star formation as a plausible formation mechanism for z ∼ 2 quiescent galaxies.

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Section: Comparison To Probable Progenitor and Descendant Populationscontrasting

confidence: 57%

Evidence for Inside-out Galaxy Growth and Quenching of a z ∼ 2 Compact Galaxy From High-resolution Molecular Gas Imaging

Spilker

Bezanson

Weiner

et al. 2019

ApJ

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“…We caution that this is just an alternative way to look at the SFR result, as we are using the same single constraint: we use both quantities interchangeably in the following and notably in Fig.4. We assume the same SFE derived in G18 (5 × 10 −10 yr −1 ), which is lower by ×2-3 than that of typical star forming galaxies, noticing that such reduced SFE is also typical of post-starburst galaxies (Suess et al 2017). Our SFR thus converts into M mol =(1.5±0.6)×10 10 M , hence f mol ∼ 9 ± 4%.…”

Section: Discussionmentioning

confidence: 87%

“…Our SFR thus converts into M mol =(1.5±0.6)×10 10 M , hence f mol ∼ 9 ± 4%. We compare it to CO or dust-continuum-based gas fractions and upper limits (converted to Salpeter) for quiescent and post-starburst galaxies: Davis et al (2014) and Saintonge et al (2011) for local massive PEGs; Sargent et al (2015), Bezanson et al (2019), Spilker et al (2018), Zavala et al (2019), Rudnick et al (2017), Suess et al (2017), Spilker et al (2018), Hayashi et al (2018), Gobat et al (2018) for intermediate-z quiescent galaxies; Schreiber et al (2018) and Valentino et al (2020) for z∼3-4 galaxies. Despite the uncertainties, our data at z∼3 seems to disfavor the steep (1+z) 4−5 trend inferred from z = 0 to 1.5-2, suggesting a flattening in the M mol /M evolution (or equivalently, of the sSFR).…”

Section: Discussionmentioning

confidence: 99%

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The Typical Massive Quiescent Galaxy at z ∼ 3 is a Post-starburst

D’Eugenio

Daddi

Gobat

et al. 2020

ApJL

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“…passive galaxies with significant gas reservoirs (e.g. Rowlands et al 2015;Suess et al 2017;Gobat et al 2018), although in a variety of galaxy environments from isolated system to small groups. Some of the typically cited quenching processes in high-density environments are AGN feedback (e.g.…”

Section: Environmental Quenchingmentioning

confidence: 99%

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

Zavala

Casey

Scoville

et al. 2019

ApJ

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We present ALMA Band 6 (ν = 233 GHz, λ = 1.3 mm) continuum observations towards 68 'normal' star-forming galaxies within two Coma-like progenitor structures at z = 2.10 and 2.47, from which ISM masses are derived, providing the largest census of molecular gas mass in overdense environments at these redshifts. Our sample comprises galaxies with a stellar mass range of 1 × 10 9 M ⊙ − 4 × 10 11 M ⊙ with a mean M ⋆ ≈ 6 × 10 10 M ⊙ . Combining these measurements with multiwavelength observations and SED modeling, we characterize the gas mass fraction and the star formation efficiency, and infer the impact of the environment on galaxies' evolution. Most of our detected galaxies ( 70%) have star formation efficiencies and gas fractions similar to those found for coeval field galaxies and in agreement with the field scaling relations. However, we do find that the proto-clusters contain an increased fraction of massive, gas-poor galaxies, with low gas fractions (f gas 6 − 10 %) and red rest-frame ultraviolet/optical colors typical of post-starburst and passive galaxies. The relatively high abundance of passive galaxies suggests an accelerated evolution of massive galaxies in proto-cluster environments. The large fraction of quenched galaxies in these overdense structures also implies that environmental quenching takes place during the early phases of cluster assembly, even before virialization. From our data, we derive a quenching efficiency of ǫ q ≈ 0.45 and an upper limit on the quenching timescale of τ q < 1 Gyr.

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Massive Quenched Galaxies at z ∼ 0.7 Retain Large Molecular Gas Reservoirs

Cited by 73 publications

References 53 publications

Evidence for Inside-out Galaxy Growth and Quenching of a z ∼ 2 Compact Galaxy From High-resolution Molecular Gas Imaging

Evidence for Inside-out Galaxy Growth and Quenching of a z ∼ 2 Compact Galaxy From High-resolution Molecular Gas Imaging

The Typical Massive Quiescent Galaxy at z ∼ 3 is a Post-starburst

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

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