xGASS: passive discs do not host unexpectedly large reservoirs of cold atomic hydrogen

Cortese, Luca; Catinella, Barbara; Cook, Robin H. W.; Janowiecki, Steven

doi:10.1093/mnrasl/slaa032

Cited by 27 publications

(16 citation statements)

References 27 publications

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“…In contrast, truly passive spirals like the N U V -selected red spirals in our sample are expected to be gas poor, in terms of both atomic gas (e.g. Cortese 2012;Cortese et al 2020) and molecular gas (e.g. Luo et al 2020).…”

Section: Radial Gradientsmentioning

confidence: 86%

Star formation histories of massive red spiral galaxies in the local universe

Zhou,

Li,

Hao

et al. 2020

Preprint

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We investigate the star formation histories (SFHs) of massive red spiral galaxies with stellar mass M * > 10 10.5 M , and make comparisons with blue spirals and red ellipticals of similar masses. We make use of the integral field spectroscopy from the SDSS-IV/DR15 MaNGA sample, and estimate spatially resolved SFHs and stellar population properties of each galaxy by applying a Bayesian spectral fitting code to the MaNGA spectra. We consider three different SFH models: an unparameterized stepwise SFH, a Γ model with a single star formation episode, and a model of Γ+B in which an additional burst is added to the Γ model to allow two episodes of star formation. We find that massive red spirals are similar to red ellipticals in both SFHs and present-day stellar populations. Both types of galaxies have experienced only one major star formation episode at early times, and the result is independent of the adopted SFH model. On average, more than half of their present-day stellar mass were formed >10 Gyrs ago, and more than 90% of the mass were formed > 6 Gyrs ago. The two types of galaxies show similarly flat profiles in a variety of stellar population parameters: old stellar ages indicated by D4000 (the spectral break at around 4000 Å), high stellar metallicities, large Mgb/Fe ratios indicative of fast formation, and little stellar dust attenuation. In contrast, The SFHs of blue spirals cannot be modelled with a single episode of star formation. Although they formed the majority of stars in their central regions also >10 Gyrs ago, both the central and outer disk have been continuously forming stars over a long timescale. Radial profiles of stellar population parameters reveal young populations and ongoing star formation in their outer regions. Our results strongly suggest that massive red spirals share common processes of formation (and possibly quenching) with massive red ellipticals in the sense that both types were formed at z > 2 through a fast formation process, and that massive red spirals are not evolutionary remnants of their blue counterparts. Possible mechanisms for the formation and quenching of massive red spirals are discussed.

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Section: Radial Gradientsmentioning

confidence: 86%

Star formation histories of massive red spiral galaxies in the local universe

Zhou,

Li,

Hao

et al. 2020

Preprint

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“…Recently Zhang et al (2019) claimed that even "quiescent" massive disk galaxies have an Hi content comparable to their star-forming counterparts. However, Cortese et al (2020) countered this claim by analyzing the SFRs used by Zhang et al (2019). They found that the SFRs used by Zhang et al (2019) were systematically low, thus the galaxies they considered quiescent were in fact star forming.…”

Section: The Relation Between Molecular and Atomic Gasmentioning

confidence: 99%

Scaling relations and baryonic cycling in local star-forming galaxies

Hunt

Tortora

Ginolfi

et al. 2020

A&A

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Assessments of the cold-gas reservoir in galaxies are a cornerstone for understanding star-formation processes and the role of feedback and baryonic cycling in galaxy evolution. Here we exploit a sample of 392 galaxies (dubbed MAGMA, Metallicity and Gas for Mass Assembly), presented in a recent paper, to quantify molecular and atomic gas properties across a broad range in stellar mass, Mstar, from ∼107 − 1011 M⊙. First, we find the metallicity (Z) dependence of the conversion factor for CO luminosity to molecular H2 mass αCO to be shallower than previous estimates, with αCO ∝ (Z/Z⊙)−1.55. Second, molecular gas mass MH2 is found to be strongly correlated with Mstar and star-formation rate (SFR), enabling predictions of MH2 good to within ∼0.2 dex; analogous relations for atomic gas mass MHI and total gas mass Mgas are less accurate, ∼0.4 dex and ∼0.3 dex, respectively. Indeed, the behavior of atomic gas mass MHI in MAGMA scaling relations suggests that it may be a third, independent variable that encapsulates information about the circumgalactic environment and gas accretion. If Mgas is considered to depend on MHI, together with Mstar and SFR, we obtain a relation that predicts Mgas to within ∼0.05 dex. Finally, the analysis of depletion times and the scaling of MHI/Mstar and MH2/Mstar over three different mass bins suggests that the partition of gas and the regulation of star formation through gas content depends on the mass regime. Dwarf galaxies (Mstar ≲ 3 × 109 M⊙) tend to be overwhelmed by (H I) accretion, and despite short τH2 (and thus presumably high star-formation efficiency), star formation is unable to keep up with the gas supply. For galaxies in the intermediate Mstar “gas-equilibrium” bin (3 × 109 M⊙ ≲ Mstar ≲3 × 1010 M⊙), star formation proceeds apace with gas availability, and H I and H2 are both proportional to SFR. In the most massive “gas-poor, bimodality” regime (Mstar ≳ 3 × 1010 M⊙), H I does not apparently participate in star formation, although it generally dominates in mass over H2. Our results confirm that atomic gas plays a key role in baryonic cycling, and is a fundamental ingredient for current and future star formation, especially in dwarf galaxies.

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“…As discussed in Z19, using different SFR estimators may produce different results. Cortese et al (2020) show that utilizing the SFRs calculated from UV and IR photometry will lead to different conclusions. To address this concern, we repeat all analysis in this paper by using the SFRs derived from the SED fitting of UV, optical, and mid-IR bands (GSWLC-M2 catalog; Salim et al 2016;Salim et al 2018).…”

Section: The Effect Of Using Alternative Sfr Estimatormentioning

confidence: 97%

Mass and Environment as Drivers of Galaxy Evolution. IV. On the Quenching of Massive Central Disk Galaxies in The Local Universe

Zhang,

Peng,

et al. 2021

Preprint

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The phenomenological study of evolving galaxy populations has shown that star forming galaxies can be quenched by two distinct processes: mass quenching and environment quenching (Peng et al. 2010). To explore the mass quenching process in local galaxies, we study the massive central disk galaxies with stellar mass above the Schechter characteristic mass. In Zhang et al. (2019), we showed that during the quenching of the massive central disk galaxies as their star formation rate (SFR) decreases, their molecular gas mass and star formation efficiency drop rapidly, but their H i gas mass remains surprisingly constant. To identify the underlying physical mechanisms, in this work we analyze the change during quenching of various structure parameters, bar frequency, and active galactic nucleus (AGN) activity. We find three closely related facts. On average, as SFR decreases in these galaxies:(1) they become progressively more compact, indicated by their significantly increasing concentration index, bulge-to-total mass ratio, and central velocity dispersion, which are mainly driven by the growth and compaction of their bulge component; (2) the frequency of barred galaxies increases dramatically, and at a given concentration index the barred galaxies have a significantly higher quiescent fraction than unbarred galaxies, implying that the galactic bar may play an important role in mass quenching; and (3) the "AGN" frequency increases dramatically from 10% on the main sequence to almost 100% for the most quiescent galaxies, which is mainly driven by the sharp increase of LINERs. These observational results lead to a self-consistent picture of how mass quenching operates.

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xGASS: passive discs do not host unexpectedly large reservoirs of cold atomic hydrogen

Cited by 27 publications

References 27 publications

Star formation histories of massive red spiral galaxies in the local universe

Star formation histories of massive red spiral galaxies in the local universe

Scaling relations and baryonic cycling in local star-forming galaxies

Mass and Environment as Drivers of Galaxy Evolution. IV. On the Quenching of Massive Central Disk Galaxies in The Local Universe

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