Cold gas properties of the<i>Herschel</i>Reference Survey

Boselli, A.; Cortese, Luca; Boquien, M.

doi:10.1051/0004-6361/201322311

Cited by 148 publications

(283 citation statements)

References 112 publications

(98 reference statements)

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“…This does not prevent the nominal H i radii of the galaxies (where Σ H i = 1 M pc −2 ) from agreeing with observations for fixed H i mass, however (see Lutz et al in preparation). We compare the molecular-to-atomic ratio as a function of stellar mass for Dark Sage galaxies against data presented by Boselli et al (2014b) from the Herschel Reference Survey (Boselli et al 2010(Boselli et al , 2014a in Fig. 10.…”

Section: Caveats Discussion and Conclusionmentioning

confidence: 99%

“…Unfortunately, only limited samples of galaxies have their H2 content inferred from CO observations (e.g. Young et al 1995;Leroy et al 2009;Saintonge et al 2011a;Boselli, Cortese & Boquien 2014a), and no H2-blind survey analogous to ALFALFA currently exists (although ongoing surveys such as xCOLDGASS will help alleviate this - Saintonge et al in preparation). There is, however, a wealth of evidence, drawn primarily from these surveys, that closely connects the H2 in these galaxies to their star formation activity (e.g.…”

Section: Satellites Versus Centralsmentioning

confidence: 99%

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Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Stevens

Brown

2017

Monthly Notices of the Royal Astronomical Society

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We combine the latest spectrally stacked data of 21-cm emission from the ALFALFA survey with an updated version of the Dark Sage semi-analytic model to investigate the relative contributions of secular and environmental astrophysical processes on shaping the H i fractions and quiescence of galaxies in the local Universe. We calibrate the model to match the observed mean H i fraction of all galaxies as a function of stellar mass. Without consideration of stellar feedback, disc instabilities, and active galactic nuclei, we show how the slope and normalisation of this relation would change significantly. We find Dark Sage can reproduce the relative impact that halo mass is observed to have on satellites' H i fractions and quiescent fraction. However, the model satellites are systematically gas-poor. We discuss how this could be affected by satellite-central cross-contamination from the group-finding algorithm applied to the observed galaxies, but that it is not the full story. From our results, we suggest the anti-correlation between satellites' H i fractions and host halo mass, seen at fixed stellar mass and fixed specific star formation rate, can be attributed almost entirely to ram-pressure stripping of cold gas. Meanwhile, stripping of hot gas from around the satellites drives the correlation of quiescent fraction with halo mass at fixed stellar mass. Further detail in the modelling of galaxy discs' centres is required to solidify this result, however. We contextualise our results with those from other semi-analytic models and hydrodynamic simulations.

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Section: Caveats Discussion and Conclusionmentioning

confidence: 99%

Section: Satellites Versus Centralsmentioning

confidence: 99%

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Stevens

Brown

2017

Monthly Notices of the Royal Astronomical Society

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“…Despite the accurate aperture correction, a possible systematic bias can affect the total molecular gas determiation of the perturbed galaxies. Indeed, if this extrapolation is very accurate in isolated, unperturbed galaxies such as those used to define the H 2 -deficiency parameter (Boselli et al 2014a), this might not be the case in perturbed cluster objects. The molecular gas distribution of these cluster galaxies might be truncated because of their interaction with the cluster environment.…”

Section: The Datamentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

et al. 2014

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The Herschel Reference Survey is a complete volume-limited, K-band-selected sample of nearby objects including Virgo cluster and isolated objects. Using a recent compilation of Hi and CO data for this sample we study the effects of the cluster environment on the molecular gas content of spiral galaxies. With the subsample of unperturbed field galaxies, we first identify the stellar mass as the scaling variable that traces the total molecular gas mass of galaxies better. We show that, on average, Hi-deficient galaxies are significantly offset (4σ) from the M(H 2 ) vs. M star relation for Hi-normal galaxies. We use the M(H 2 ) vs. M star scaling relation to define the H 2 -deficiency parameter as the difference, on logarithmic scale, between the expected and observed molecular gas mass for a galaxy of given stellar mass. The H 2 -deficiency parameter shows a weak and scattered relation with the Hi-deficiency parameter, here taken as a proxy for galaxy interactions with the surrounding cluster environment. We also show that, as for the atomic gas, the extent of the molecular disc decreases with increasing Hi-deficiency. All together, these results show that cluster galaxies have, on average, a lower molecular gas content than similar objects in the field. Our analysis indicates that ram pressure stripping is the physical process responsible for this molecular gas deficiency. The slope of the H 2 − de f vs. Hi − de f relation is less than unity, while the D(Hi)/D(i) vs. Hi − de f relation is steeper than the D(CO)/D(i) vs. Hi − de f relation, thereby indicating that the molecular gas is removed less efficiently than the atomic gas. This result can be understood if the atomic gas is distributed on a relatively flat disc that is more extended than the stellar disc. It is thus less anchored to the gravitational potential well of the galaxy than the molecular gas phase, which is distributed on an exponential disc with a scalelength r CO 0.2r 24.5 (g). There is a clear trend between the NUV-i colour index, which is a proxy for the specific star formation activity, and the H 2 -deficiency parameter, which suggests that molecular gas removal quenches the activity of star formation. This causes galaxies migrate from the blue cloud to the green valley and, eventually, to the red sequence. The total gas-consumption timescale of gas deficient cluster galaxies is comparable to that of isolated, unperturbed systems. The total gas depletion timescale determined by considering the recycled fraction is τ gas,R 3.0−3.3 Gyr, which is significantly larger than the typical timescale for total gas removal in a ram pressure stripping process, indicated by recent hydrodynamical simulations to be τ RP 1.5 Gyr. The comparison of these timescales suggests that ram pressure, rather than a simple stop of the infall of pristine gas from the halo, will be the dominant process driving the future evolution of these cluster galaxies.

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“…CO data were retrieved from nine studies Daddi et al 2010;Geach et al 2011;Saintonge et al 2011a;Bauermeister et al 2013;Tacconi et al 2013;Boselli et al 2014;Bothwell et al 2014;Morokuma-Matsui et al 2015) to cover a wide range of redshifts and stellar masses. We adopted the Galactic conversion factor of αCO = 4.35 M⊙(K km s −1 pc 2 ) −1 (including the contribution of helium; Bolatto et al 2013) for all the sample galaxies 2 considered in this study to estimate the molecular gas mass as where L ′ CO represents the luminosity of the 12 CO(J = 1−0) line in units of K km s −1 pc 2 .…”

Section: Measurement Of Molecular Gas Mass From Comentioning

confidence: 99%

Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

Morokuma-Matsui¹,

Baba²

2015

Mon. Not. R. Astron. Soc.

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We investigate the redshift evolution of the molecular gas mass fraction (f mol = M mol M⋆+M mol , where M mol is molecular gas mass and M ⋆ is stellar mass) of galaxies in the redshift range of 0 < z < 2 as a function of the stellar mass by combining CO literature data. We observe a stellar-mass dependence of the f mol evolution where massive galaxies have largely depleted their molecular gas at z = 1, whereas the f mol value of less massive galaxies drastically decreases from z = 1. We compare the observed M ⋆ −f mol relation with theoretical predictions from cosmological hydrodynamic simulations and semi-analytical models for galaxy formation. Although the theoretical studies approximately reproduce the observed mass dependence of f mol evolution, they tend to underestimate the f mol values, particularly of less massive (< 10 10 M ⊙ ) and massive galaxies (> 10 11 M ⊙ ) when compared with the observational values. Our result suggests the importance of the feedback models which suppress the star formation while simultaneously preserving the molecular gas in order to reproduce the observed M ⋆ − f mol relation.

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Cold gas properties of theHerschelReference Survey

Cited by 148 publications

References 112 publications

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Cold gas properties of theHerschelReference Survey

Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

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