The molecular mass function of the local Universe

Andreani, P.; Miyamoto, Yusuke; Kaneko, Hiroyuki; Boselli, A.; Tatematsu, Ken’ichi; Saito, Kazuo; Vio, R.

doi:10.1051/0004-6361/202038675

Cited by 10 publications

(14 citation statements)

References 42 publications

(69 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The good agreement between the Hi and H2 mass functions and a single Schechter function is in contrast with the stellar mass function in the nearby Universe, which is best characterised by a double Schechter function (Baldry et al 2012). The double Schechter function, being the sum of two functions with the same M * but different α and φ * values (as in Eq.…”

Section: How Is the Cold Interstellar Medium Distributed Across The N...mentioning

confidence: 95%

“…Keres et al (2003) built a CO luminosity function and H2 mass function from the FCRAO Extragalactic CO Survey (Young et al 1995), for both a far infrared flux-limited sub-sample, and an optical B-band-selected sub-sample. To avoid the possible biases associated with the IR-or optical-flux selection, robust H2 mass functions have recently been computed using the large HRS and xCOLD GASS mass-selected samples (Andreani et al 2020, Fletcher et al 2021). In addition to the sample selection, the choice of the CO-to-H2 conversion function also has a significant impact on the H2 mass function and the best-fit Schechter function parameters (Obreschkow & Rawlings 2009, Fletcher et al 2021.…”

Section: Cold Gas Mass Functionsmentioning

confidence: 99%

“…Amongst many other measurements of ΩHI (e.g. Zwaan et al 2005), the ALFALFA survey estimates that ΩHI= (3.9 ± 0.1 ± 0.6) × 10 −4 (Jones et al 2018), while for molecular gas Fletcher et al (2021) estimate Ω mol = (7.62 ± 0.47) × 10 −5 from the xCOLD GASS sample, and Andreani et al (2020) report a value of (1.1 ± 0.4) × 10 −4 for the HRS sample. Once accounting for the presence of Helium and heavier elements by multiplying ΩHI by a factor of 1.36 (already included in Ω mol ), the total density parameter for the ISM in the nearby Universe is found to be ΩISM = 0.00061.…”

Section: How Much Hi and H 2 Is There In The Nearby Universe?mentioning

confidence: 99%

See 2 more Smart Citations

The cold interstellar medium of galaxies in the Local Universe

Saintonge¹,

Catinella²

2022

Preprint

View full text Add to dashboard Cite

The cold interstellar medium (ISM) plays a central role in the galaxy evolution process. It is the reservoir that fuels galaxy growth via star formation, the repository of material formed by these stars, and a sensitive tracer of internal and external processes that affect entire galaxies. Consequently, significant efforts have gone into systematic surveys of the cold ISM of the galaxies in the local Universe. This review discusses the resulting network of scaling relations connecting the atomic and molecular gas masses of galaxies with their other global properties (stellar masses, morphologies, metallicities, star formation activity...), and their implications for our understanding of galaxy evolution. Key take-home messages are as follows:• From a gas perspective, there are three main factors that determine the star formation rate of a galaxy: the total mass of its cold ISM, how much of that gas is molecular, and the rate at which any molecular gas is converted into stars. All three of these factors vary systematically across the local galaxy population.• The shape and scatter of both the star formation main sequence and the mass-metallicity relation are deeply linked to the availability of atomic and molecular gas.• Future progress will come from expanding our exploration of scaling relations into new parameter space (in particular the regime of dwarf galaxies), better connecting the cold ISM of large samples of galaxies with the environment that feeds them (the circumgalactic medium in particular), and understanding the impact of these large scales on the efficiency of the star formation process on molecular cloud scales.

show abstract

Section: How Is the Cold Interstellar Medium Distributed Across The N...mentioning

confidence: 95%

Section: Cold Gas Mass Functionsmentioning

confidence: 99%

Section: How Much Hi and H 2 Is There In The Nearby Universe?mentioning

confidence: 99%

See 1 more Smart Citation

The cold interstellar medium of galaxies in the Local Universe

Saintonge¹,

Catinella²

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…In this letter we compute and discuss the local molecular mass function derived from the HRS sample. CO observations are taken with single dishes and described in detail in other papers (Boselli et al 2014a,b;Andreani et al 2020). Our aim is to infer the local molecular mass density on a more solid ground which could be used as a reference to set limits to current models predicting the evolution of the molecular mass with redshift.…”

Section: Why a Local Molecular Mass Function?mentioning

confidence: 99%

“…Of the 323 galaxies 225 observations are reported in Boselli et al (2014a,b), 43 more have been targeted in January-February 2018 and 2019 with the 45 m radio telescope of the Nobeyama Radio Observatory (NRO) 1 . Observations will be fully described, analysed and discussed in a paper in preparation (Andreani et al 2020).…”

Section: The Datamentioning

confidence: 99%

The Molecular Mass function of the Local Universe

Andreani,

Miyamoto,

Kaneko

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

Aims. We construct the molecular mass function using the bivariate K-band-Mass Function (BMF) of the Herschel Reference Survey (HRS), a volume-limited sample already widely studied at the entire electromagnetic spectrum. Methods. The molecular mass function is derived from the K-band and the gas mass cumulative distribution using a copula method described in detail in our previous papers (Andreani et al. 2014(Andreani et al. , 2018.Results. The H 2 mass is relatively strong correlated with the K-band luminosity because of the tight relation between the stellar mass and the molecular gas mass within the sample with a scatter likely due to those galaxies which have lost their molecular content because of environmental effects or because of a larger gas consumption due to past star formation processes. The derived H 2 MF samples the molecular mass range from ∼ 4×10 6 M to ∼10 10 M , and when compared with theoretical models, it agrees well with the theoretical predictions at the lower end of the mass values, while at masses larger than 10 10 M the HRS sample may miss galaxies with large content of molecular hydrogen and the outcomes are not conclusive. The value of the local density of the molecular gas mass inferred from our analysis is ∼ 1.5 × 10 7 M Mpc −3 , and it is compared with the results at larger redshifts, confirming the lack of strong evolution of the molecular mass density between z=0 and z=4. Conclusions. This is the first Molecular Mass Function derived on a complete sample in the local Universe, which can be used as a reliable calibration at redshift z=0 for models aiming at predicting the evolution of the molecular mass density.

show abstract

Tracing the quenching journey across cosmic time

De Lucia,

Fontanot,

Xie

et al. 2024

A&A

View full text Add to dashboard Cite

We present the latest version of the GAlaxy Evolution and Assembly (GAEA) theoretical model of galaxy formation. Our new model now combines (i) an updated treatment of feedback from Active Galactic Nuclei (AGN), including an improved modelling of cold gas accretion on super-massive black holes and an explicit implementation of quasar winds; and (ii) a treatment for both cold and hot gas stripping from satellite galaxies. We show that our latest model version predicts specific star formation rate distributions that are in remarkable agreement with observational measurements in the local Universe. Our updated model predicts quenched fractions that are in very nice agreement with observational measurements up to $z 3-4$, and a turn-over of the number densities of quenched galaxies at low stellar masses that is in qualitative agreement with current observational estimates. We show that the main reasons for the improved behaviour with respect to previous renditions of our model are the updated treatment for satellites at low galaxy masses M sun $) and the inclusion of quasar winds at intermediate to large stellar masses ($>10^ M sun $). However, we show that the better treatment of the star formation threshold, due to our explicit partitioning of the cold gas in its atomic and molecular components, also plays an important role in suppressing excessive residual star formation in massive galaxies. While our analysis is based on a selection of quiescent galaxies that takes advantage of the information about their star formation rate, we demonstrate that the impact of a different (colour-colour) selection is not significant up to $z 3$, at least for galaxies above the completeness limits of current surveys. Our new model predicts number densities of massive quiescent galaxies at z > 3 that are the largest among recently published state-of-the-art models. Yet, our model predictions still appear to be below post-JWST observational measurements. We show that the expected cosmic variance is large, and can easily accommodate some of the most recent measurements.

show abstract

The molecular mass function of the local Universe

Cited by 10 publications

References 42 publications

The cold interstellar medium of galaxies in the Local Universe

The cold interstellar medium of galaxies in the Local Universe

The Molecular Mass function of the Local Universe

Tracing the quenching journey across cosmic time

Contact Info

Product

Resources

About