H2-based star formation laws in hierarchical models of galaxy formation

Xie, Lizhi; Lucia, G. De; Hirschmann, Michaela; Fontanot, Fabio; Zoldan, Anna

doi:10.1093/mnras/stx889

Cited by 70 publications

(109 citation statements)

References 140 publications

(255 reference statements)

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“…Our findings are consistent with recent literature, with models that adopt strong SN-driven winds and a multiphase treatment of gas on subkpc scales producing results that are consistent with obser-5 We note that Martindale et al (2017) partitioned the HI and H 2 content of Henriques et al (2015) in post-processing using an analytic surface-density profile and observed a similar behaviour at low mass to that obtained with our simple conversion. vation (Stevens et al 2016;Crain et al 2017;Xie et al 2017;Lagos et al 2018).…”

Section: Gas Propertiesmentioning

confidence: 99%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

112

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We have updated the Munich galaxy formation model, L-galaxies, to follow the radial distributions of stars and atomic and molecular gas in galaxy discs. We include an H 2 -based star-formation law, as well as a detailed chemical-enrichment model with explicit mass-dependent delay times for SN-II, SN-Ia and AGB stars. Information about the star formation, feedback and chemical-enrichment histories of discs is stored in 12 concentric rings. The new model retains the success of its predecessor in reproducing the observed evolution of the galaxy population, in particular, stellar mass functions and passive fractions over the redshift range 0 z 3 and mass range 8 log(M * / M ) 12, the black hole-bulge mass relation at z = 0, galaxy morphology as a function of stellar mass and the mass-metallicity relations of both stellar and gas components. In addition, its detailed modelling of the radial structure of discs allows qualitatively new comparisons with observation, most notably with the relative sizes and masses of the stellar, atomic and molecular components in discs. Good agreement is found with recent data. Comparison of results obtained for simulations differing in mass resolution by more than two orders of magnitude shows that all important distributions are numerically well converged even for this more detailed model. An examination of metallicity and surface-density gradients in the stars and gas indicates that our new model, with star formation, chemical enrichment and feedback calculated self-consistently on local disc scales, reproduces some but not all of the trends seen in recent many-galaxy IFU surveys.

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Section: Gas Propertiesmentioning

confidence: 99%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

112

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“…The model and all its upgrades are described in details in several papers (e.g. De Lucia et al 2014;Hirschmann et al 2016;Xie et al 2017;Zoldan et al 2017). We summarize here the main features that are relevant for the analysis presented in this paper.…”

Section: Simulationsmentioning

confidence: 99%

“…Previous work based on the GAEA model (e.g. Xie et al 2017;Zoldan et al 2017) adopted more conservative stellar mass limits (∼ 10 9 M for the MI, and ∼ 10 8 M for the MII). In this work, we lower the stellar mass thresholds (see table 1) in order to access lower HI masses, as the minimum HI available is connected to the stellar mass selection.…”

Section: The Hi Mass Functionmentioning

confidence: 99%

“…The most recent renditions of several independent SAMs have included prescriptions to partition the cold gas in its atomic and molecular components, based either on empirical relations or on results from sophisticated numerical simulations (e.g. Fu et al 2010;Lagos et al 2011;Kim et al 2011;Somerville & Davé 2015;Stevens et al 2017;Xie et al 2017;Zoldan et al 2017;Cora et al 2018). These models can provide reliable mock 21 cm maps, thereby helping to understand the relevant processes determining the observed 21 cm signal.…”

Section: Introductionmentioning

confidence: 99%

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The atomic hydrogen content of the post-reionization Universe

Spinelli

Zoldan

Lucia

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a comprehensive analysis of atomic hydrogen (HI) properties using a semianalytical model of galaxy formation and N-body simulations covering a large cosmological volume at high resolution. We examine the HI mass function and the HI density, characterizing both their redshift evolution and their dependence on hosting halo mass. We analyze the HI content of dark matter haloes in the local Universe and up to redshift z = 5, discussing the contribution of different galaxy properties. We find that different assembly history plays a crucial role in the scatter of this relation. We propose new fitting functions useful for constructing mock HI maps with HOD techniques. We investigate the HI clustering properties relevant for future 21 cm Intensity Mapping (IM) experiments, including the HI bias and the shot noise level. The HI bias increases with redshift and it is roughly flat on the largest scales probed. The scale dependency is found at progressively larger scales with increasing redshift, apart from a dip feature at z = 0. The shot-noise values are consistent with the ones inferred by independent studies, confirming that shot-noise will not be a limiting factor for IM experiments. We detail the contribution from various galaxy properties on the HI power spectrum and their relation to the halo bias. We find that HI poor satellite galaxies play an important role at the scales of the 1-halo term. Finally, we present the 21 cm signal in redshift space, a fundamental prediction to be tested against data from future radio telescopes such as SKA.

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“…We make use of the GAEA semi-analytic model Xie et al 2017;Hirschmann et al 2016 , which is a cosmological N-body simulation that used N = 2160 3 particles of mass m p = 8.6×10 8 h −1 M within a comoving box of size 500 3 (Mpc/h) 3 with a cosmology consistent with WMAP1 data. In particular, the values of the adopted cosmological parameters are: Ω b = 0.045, Ω m = 0.25, Ω Λ = 0.75, H 0 = 100h Mpc −1 km s −1 , h = 0.73, σ 8 = 0.9 and n s = 1.…”

Section: Cosmological Signals and Their Simulationmentioning

confidence: 99%

Impact of foregrounds on H i intensity mapping cross-correlations with optical surveys

Cunnington

Wolz

Pourtsidou

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The future of precision cosmology could benefit from cross-correlations between intensity maps of unresolved neutral hydrogen (Hi) and more conventional optical galaxy surveys. A major challenge that needs to be overcome is removing the 21cm foreground emission that contaminates the cosmological Hi signal. Using N-body simulations we simulate Hi intensity maps and optical catalogues which share the same underlying cosmology. Adding simulated foreground contamination and using state-of-the-art reconstruction techniques we investigate the impacts that 21cm foregrounds and other systematics have on these cross-correlations. We find that the impact a FASTICA 21cm foreground clean has on the cross-correlations with spectroscopic optical surveys with well-constrained redshifts is minimal. However, problems arise when photometric surveys are considered: we find that a redshift uncertainty σ z ≥ 0.04 causes significant degradation in the cross power spectrum signal. We diagnose the main root of these problems, which relates to arbitrary amplitude changes along the line-of-sight in the intensity maps caused by the foreground clean and suggest solutions which should be applicable to real data. These solutions involve a reconstruction of the line-of-sight temperature means using the available overlapping optical data along with an artificial extension to the Hi data through redshift to address edge effects. We then put these solutions through a further test in a mock experiment that uses a clustering-based redshift estimation technique to constrain the photometric redshifts of the optical sample. We find that with our suggested reconstruction, cross-correlations can be utilized to make an accurate prediction of the optical redshift distribution.

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H2-based star formation laws in hierarchical models of galaxy formation

Cited by 70 publications

References 140 publications

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

The atomic hydrogen content of the post-reionization Universe

Impact of foregrounds on H i intensity mapping cross-correlations with optical surveys

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