The evolution of the gas fraction of quiescent galaxies modeled as a consequence of their creation rate

Gobat, R.; Magdis, G.; D’Eugenio, Chiara; Valentino, F.

doi:10.1051/0004-6361/202039593

Cited by 13 publications

(9 citation statements)

References 51 publications

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“…We thus conclude that completely dry mergers cannot dominate the late evolution of galaxies, and that additional in-situ stellar mass growth, even in the most massive galaxies, should occur during and/or in between mergers to maintain a flat or increasing 𝜎 𝑎 𝑝 [𝑀 * , 𝑧]. This conclusion is consistent with the declining, but still non-zero, star formation histories inferred in massive galaxies (e.g., Buchan & Shankar 2016;Leja et al 2019;Grylls et al 2020a, and references therein) and with the presence of substantial amounts of gas in massive galaxies at intermediate epochs (e.g., Gobat et al 2018Gobat et al , 2020.…”

Section: The Role Of (Dry) Mergerssupporting

confidence: 64%

The weak dependence of velocity dispersion on disc fractions, mass-to-light ratio, and redshift: implications for galaxy and black hole evolution

Marsden

Shankar

Bernardi

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Velocity dispersion (σ) is a key driver for galaxy structure and evolution. We here present a comprehensive semi-empirical approach to compute σ via detailed Jeans modelling assuming both a constant and scale-dependent mass-to-light ratio M*/L. We compare with a large sample of local galaxies from MaNGA and find that both models can reproduce the Faber-Jackson (FJ) relation and the weak dependence of σ on bulge-to-total ratio B/T (for B/T ≳ 0.25). The dynamical-to-stellar mass ratio within R ≲ Re can be fully accounted for by a gradient in M*/L. We then build velocity dispersion evolutionary tracks σap[M*, z] (within an aperture) along the main progenitor dark matter haloes assigning stellar masses, effective radii and Sérsic indices via a variety of abundance matching and empirically motivated relations. We find: 1) clear evidence for downsizing in σap[M*, z] along the progenitor tracks; 2) at fixed stellar mass σ∝(1 + z)0.2 − 0.3 depending on the presence or not of a gradient in M*/L. We extract σap[M*, z] from the TNG50 hydrodynamic simulation and find very similar results to our models with constant M*/L. The increasing dark matter fraction within Re tends to flatten the σap[M*, z] along the progenitors at z ≳ 1 in constant M*/L models, while σap[M*, z] have a steeper evolution in the presence of a stellar gradient. We then show that a combination of mergers and gas accretion are likely responsible for the constant or increasing σap[M*, z] with time. Finally, our σap[M*, z] are consistent with a nearly constant and steep Mbh − σ relation at z ≲ 2, with black hole masses derived from the LX − M* relation.

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Section: The Role Of (Dry) Mergerssupporting

confidence: 64%

The weak dependence of velocity dispersion on disc fractions, mass-to-light ratio, and redshift: implications for galaxy and black hole evolution

Marsden

Shankar

Bernardi

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…4. Here we estimated the median gas fraction of the whole population of QGs as a function of redshift by assuming only the QG production rate from stellar mass functions, an initial gas fraction (constant with redshift) of ∼10% immediately following quenching, and a closed-box consumption with a time scale of ∼2 Gyr after that (Gobat et al 2020). The track derived in this manner reproduces our data well, especially when considering that the latter are likely slightly biased towards dustier objects at lower redshift (see Fig.…”

Section: Discussionmentioning

confidence: 99%

“…The dotted blue line (blue shaded region) corresponds to the best fit (scatter) to the 0.0 < z < 1.0 M dust /M * data of QGs, with a functional form of M dust /M * ∝ (1 + z) 5.0 . The bold, dashed purple line (shaded region) depicts the evolution (scatter) of M dust /M * (and of f gas ) as derived from the progenitor bias analysis ofGobat et al (2020), which is discussed in Sects. 5.2 and 6.…”

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confidence: 99%

The interstellar medium of quiescent galaxies and its evolution with time

Magdis

Gobat

Valentino

et al. 2021

A&A

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We characterise the basic far-IR properties and the gas mass fraction of massive (⟨log(M*/M⊙)⟩ ≈ 11.0) quiescent galaxies (QGs) and explore how these evolve from z = 2.0 to the present day. We use robust, multi-wavelength (mid- to far-IR and sub-millimetre to radio) stacking ensembles of homogeneously selected and mass complete samples of log(M*/M⊙)≳10.8 QGs. We find that the dust to stellar mass ratio (Mdust/M*) rises steeply as a function of redshift up to z ∼ 1.0 and then remains flat at least out to z = 2.0. Using Mdust as a proxy of gas mass (Mgas), we find a similar trend for the evolution of the gas mass fraction (fgas), with z > 1.0 QGs having fgas ≈ 7.0% (for solar metallicity). This fgas is three to ten times lower than that of normal star-forming galaxies (SFGs) at their corresponding redshift but ≳3 and ≳10 times larger compared to that of z = 0.5 and local QGs. Furthermore, the inferred gas depletion time scales are comparable to those of local SFGs and systematically longer than those of main sequence galaxies at their corresponding redshifts. Our analysis also reveals that the average dust temperature (Td) of massive QGs remains roughly constant (⟨Td⟩ = 21.0 ± 2.0 K) at least out to z ≈ 2.0 and is substantially colder (ΔTd ≈ 10 K) compared to that of SFGs. This motivated us to construct and release a redshift-invariant template IR SED, that we used to make predictions for ALMA observations and to explore systematic effects in the Mgas estimates of massive, high-z QGs. Finally, we discuss how a simple model that considers progenitor bias can effectively reproduce the observed evolution of Mdust/M* and fgas. Our results indicate universal initial interstellar medium conditions for quenched galaxies and a large degree of uniformity in their internal processes across cosmic time.

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“…Since dust is destroyed over time in QGs (e.g., Smercina et al 2018;Whitaker et al 2021b), its low concentration in MRG-0138 is therefore unsurprising. For example, a depletion time for dust of ∼1.7 Gyr (Michałowski et al 2019;Gobat et al 2020) would imply that the initial dust mass after quenching was higher by at least a factor 2. This mirrors the anticorrelation between f gas and stellar mass seen in the local Universe (e.g., Young et al 2011;Saintonge et al 2017;Tacconi et al 2018Tacconi et al , 2020Liu et al 2019;Saintonge & Catinella 2022).…”

Section: Resultsmentioning

confidence: 99%

The uncertain interstellar medium of high-redshift quiescent galaxies: Impact of methodology

Gobat

D’Eugenio

Liu

et al. 2022

A&A

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How much gas and dust is contained in high-redshift quiescent galaxies (QGs) is currently an open question with relatively few and contradictory answers, as well as important implications for our understanding of the nature of star formation quenching processes at cosmic noon. Here we revisit far-infrared (FIR) observations of the REQUIEM-ALMA sample of six z = 1.6 − 3.2 QGs strongly lensed by intermediate-redshift galaxy clusters. We measured their continuum emission using priors obtained from high resolution near-infrared (NIR) imaging, as opposed to focusing on point-source extraction, converted it into dust masses using a FIR dust emission model derived from statistical samples of QGs, and compared the results to those of the reference work. We find that, while at least the most massive sample galaxy is indeed dust-poor, the picture is much more nuanced than previously reported. In particular, these more conservative constraints remain consistent with high dust fractions in early QGs. We find that these measurements are very sensitive to the adopted extraction method and conversion factors: the use of an extended light model to fit the FIR emission increases the flux of detections by up to 50% and the upper limit by up to a factor 6. Adding the FIR-to-dust conversion, this amounts to an order of magnitude difference in dust fraction, casting doubts on the power of these data to discriminate between star formation quenching scenarios. Unless these are identified by other means, mapping the dust and gas in high-redshift QGs will continue to require somewhat costly observations.

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The evolution of the gas fraction of quiescent galaxies modeled as a consequence of their creation rate

Cited by 13 publications

References 51 publications

The weak dependence of velocity dispersion on disc fractions, mass-to-light ratio, and redshift: implications for galaxy and black hole evolution

The weak dependence of velocity dispersion on disc fractions, mass-to-light ratio, and redshift: implications for galaxy and black hole evolution

The interstellar medium of quiescent galaxies and its evolution with time

The uncertain interstellar medium of high-redshift quiescent galaxies: Impact of methodology

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