Gas Accretion and Star Formation Rates

Alméida, J. Sánchez

doi:10.1007/978-3-319-52512-9_4

Cited by 14 publications

(1 citation statement)

References 213 publications

(232 reference statements)

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“…The FMR shows that those galaxies with larger SFR have smaller Z g . There is evidence for the FMR to hold until at least redshift 3 (e.g., Troncoso et al 2014;Sánchez Almeida 2017), but there is also dissenting views, mostly on whether the SFR is truly needed to describe the relation between M and Z g (Izotov et al 2014;de los Reyes et al 2015;Sanders et al 2015;Barrera-Ballesteros et al 2017;Sánchez et al 2013Sánchez et al , 2017Sánchez et al , 2019a. The FMR is taken as evidence for metal poor cosmic gas accretion fueling star formation (e.g., Mannucci et al 2010;Brisbin & Harwit 2012;Davé et al 2012), an observationally-elusive but fundamental physical process according to numerical simulations (e.g., Dekel et al 2009;Sánchez Almeida et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Local and global gas metallicity versus stellar age relation in MaNGA galaxies

Sánchez-Menguiano,

Almeida,

Muñoz-Tuñón

et al. 2020

Preprint

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The search for new global scaling relations linking physical properties of galaxies has a fundamental interest. Furthermore, their recovery from spatially resolved relations has been one of the spotlights of integral field spectroscopy (IFS). In this study we investigate the existence of global and local relations between stellar age (Age ) and gas-phase metallicity (Z g ). To this aim, we analyze IFS data for a sample of 736 star-forming disk galaxies from the MaNGA survey. We report a positive correlation between the global Z g and D(4000) (an indicator of stellar age), with a slope that decreases with increasing galaxy mass. Locally, a similar trend is found when analyzing the Z g and D(4000) of the star-forming regions, as well as the residuals resulting from removing the radial gradients of both parameters. The local laws have systematically smaller slopes than the global one. We ascribe this difference to random errors, that make the true slope of the Age − Z g relation to be systematically underestimated when performing a least square fitting. The explored relation is intimately linked with the already known relation between gas metallicity and star formation rate at fixed mass, both presenting a common physical origin.

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Section: Introductionmentioning

confidence: 99%

Local and global gas metallicity versus stellar age relation in MaNGA galaxies

Sánchez-Menguiano,

Almeida,

Muñoz-Tuñón

et al. 2020

Preprint

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Metal content of the circumgalactic medium around star-forming galaxies at z ∼ 2.6 as revealed by the VIMOS Ultra-Deep Survey

Méndez-Hernández

Cassata

Ibar

et al. 2022

A&A

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Context. The circumgalactic medium (CGM) is the location where the interplay between large-scale outflows and accretion onto galaxies occurs. Metals in different ionization states flowing between the circumgalactic and intergalactic mediums are affected by large galactic outflows and lowionization state inflowing gas. Observational studies on their spatial distribution and their relation with galaxy properties may provide important constraints on models of galaxy formation and evolution. Aims. The main goal of this paper is to provide new insights into the spatial distribution of the circumgalactic of star-forming galaxies at 1.5 < z < 4.5 (⟨z⟩ ∼2.6) in the peak epoch of cosmic star formation activity in the Universe. We also look for possible correlations between the strength of the low-and high-ionization absorption features (LIS and HIS) and stellar mass, star formation rate, effective radius, and azimuthal angle ϕ that defines the location of the absorbing gas relative to the galaxy disc plane. Methods. The CGM has been primarily detected via the absorption features that it produces on the continuum spectrum of bright background sources. We selected a sample of 238 close pairs from the VIMOS Ultra Deep Survey to examine the spatial distribution of the gas located around star-forming galaxies and generate composite spectra by co-adding spectra of background galaxies that provide different sight-lines across the CGM of star-forming galaxies. Results. We detect LIS (C ii and Si ii) and HIS (Si iv, C iv) up to separations ⟨b⟩ = 172 kpc and 146 kpc. Beyond this separation, we do not detect any significant signal of CGM absorption in the background composite spectra. Our Lyα, LIS, and HIS rest-frame equivalent width (W 0 ) radial profiles are at the upper envelope of the W 0 measurements at lower redshifts, suggesting a potential redshift evolution for the CGM gas content producing these absorptions. We find a correlation between C ii and C iv with star formation rate and stellar mass, as well as trends with galaxy size estimated by the effective radius and azimuthal angle. Galaxies with high star formation rate (log[SFR/(M ⊙ yr −1 )] > 1.5) and stellar mass (log[M ⋆ /M ⊙ ]>10.2) show stronger C iv absorptions compared with those low SFR (log[SFR/(M ⊙ yr −1 )] < 0.9) and low stellar mass (log[M ⋆ /M ⊙ ]<9.26). The latter population instead shows stronger C ii absorption than their more massive or more star-forming counterparts. We compute the C ii / C iv W 0 line ratio that confirms the C ii and C iv correlations with impact parameter, stellar mass, and star formation rate. We do not find any correlation with ϕ in agreement with other high-redshift studies and in contradiction to what is observed at low redshift where large-scale outflows along the minor axis forming bipolar outflows are detected. Conclusions. We find that the stronger C iv line absorptions in the outer regions of these star-forming galaxies could be explained by stronger outflows in galaxies with higher star formation rates and stellar masses that...

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Expanding on the fundamental metallicity relation in dwarf galaxies with MUSE

Bulichi,

Fahrion,

Mernier

et al. 2023

A&A

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The mass–metallicity relation (MZR) represents one of the most important scaling relations in the context of galaxy evolution, comprising a positive correlation between stellar mass and metallicity (Z). The fundamental metallicity relation (FMR) introduces a new parameter into the dependence, namely, the star formation rate (SFR). While several studies have found that Z is anti-correlated with the SFR at a fixed mass, the validity of this statement has been questioned extensively and no widely accepted consensus has been reached thus far. With this work, we investigate the FMR in nine nearby, spatially resolved, dwarf galaxies, using gas diagnostics on integral-field spectroscopic data of the Multi Unit Spectroscopic Explorer (MUSE), pushing such investigations to lower galaxy masses and higher resolutions. We find that both the MZR and FMR exhibit different behaviours within different star-forming regions of the galaxies. We find that the SFR surface-density-and-metallicity anti-correlation is tighter in the low-mass galaxies of our sample. For all the galaxies considered, we find a SFR surface-density-and-stellar-mass surface-density correlation. We propose that the main reason behind these findings is connected to the accretion mechanisms of the gas fuelling star formation, namely: low-mass, metal-poor galaxies accrete pristine gas from the intergalactic medium, while in more massive and metal-enriched systems, the gas responsible for star formation is recycled from previous star-forming episodes.

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Gas Accretion and Star Formation Rates

Cited by 14 publications

References 213 publications

Local and global gas metallicity versus stellar age relation in MaNGA galaxies

Local and global gas metallicity versus stellar age relation in MaNGA galaxies

Metal content of the circumgalactic medium around star-forming galaxies at z ∼ 2.6 as revealed by the VIMOS Ultra-Deep Survey

Expanding on the fundamental metallicity relation in dwarf galaxies with MUSE

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