scholarly journals The effect of gas accretion on the radial gas metallicity profile of simulated galaxies

2020 ◽  
Vol 495 (3) ◽  
pp. 2827-2843 ◽  
Author(s):  
Florencia Collacchioni ◽  
Claudia D P Lagos ◽  
Peter D Mitchell ◽  
Joop Schaye ◽  
Emily Wisnioski ◽  
...  
Keyword(s):  
Star Formation Rate ◽  
Accretion Rate ◽  
Formation Rate ◽  
Main Property ◽  
Stellar Mass ◽  
Effective Radius ◽  
Mass Star ◽  
Hydrodynamic Simulations ◽  
Gas Accretion ◽  
Gas Fractions

ABSTRACT We study the effect of the gas accretion rate ($\dot{M}_{\rm accr}$) on the radial gas metallicity profile (RMP) of galaxies using the eagle cosmological hydrodynamic simulations, focusing on central galaxies of stellar mass M⋆ ≳ 109 M⊙ at z ≤ 1. We find clear relations between $\dot{M}_{\rm accr}$ and the slope of the RMP (measured within an effective radius), where higher $\dot{M}_{\rm accr}$ are associated with more negative slopes. The slope of the RMPs depends more strongly on $\dot{M}_{\rm accr}$ than on stellar mass, star formation rate (SFR), or gas fraction, suggesting $\dot{M}_{\rm accr}$ to be a more fundamental driver of the RMP slope of galaxies. We find that eliminating the dependence on stellar mass is essential for pinning down the properties that shape the slope of the RMP. Although $\dot{M}_{\rm accr}$ is the main property modulating the slope of the RMP, we find that it causes other correlations that are more easily testable observationally: At fixed stellar mass, galaxies with more negative RMP slopes tend to have higher gas fractions and SFRs, while galaxies with lower gas fractions and SFRs tend to have flatter metallicity profiles within an effective radius.

scholarly journals Gas accretion history of galaxies at z ~ 0 - 2: Comparison of the observational data of molecular gas with the mass evolution model of galaxies

2014 ◽  
Vol 10 (S309) ◽  
pp. 332-332
Author(s):  
Kana Morokuma ◽  
Junichi Baba ◽  
Kazuo Sorai ◽  
Nario Kuno
Keyword(s):  
Star Formation Rate ◽  
Formation Rate ◽  
Stellar Mass ◽  
Molecular Gas ◽  
Massive Galaxies ◽  
Infra Red ◽  
History Of ◽  
Gas Accretion ◽  
Mass Dependent ◽  
Gas Fractions

AbstractWe found stellar mass-dependent evolution of galactic molecular gas fractions ($f_{\rm mol}=\frac{M_{\rm mol}}{M_\star+M_{\rm mol}}$, Mmol: molecular gas mass, M*: stellar mass) where less massive galaxies have decreased fmol from z = 1 whereas massive galaxies have already had low fmol until z = 1. Comparison of the observed quantities (fmol, optical and near infra-red [NIR] colors, specific star formation rate [sSFR = SFR/M*]) with mass evolution models suggests that less massive galaxies had high fmol at z = 1 thanks to recent gas accretion.

scholarly journals The stellar mass, star formation rate and dark matter halo properties of LAEs at z ∼ 2

2018 ◽  
Vol 70 (1) ◽  
Author(s):  
Haruka Kusakabe ◽  
Kazuhiro Shimasaku ◽  
Masami Ouchi ◽  
Kimihiko Nakajima ◽  
Ryosuke Goto ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Stellar Mass ◽  
Dark Matter Halo ◽  
Mass Star

scholarly journals The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8–2.2, with HiZELS

2018 ◽  
Vol 475 (3) ◽  
pp. 3730-3745 ◽  
Author(s):  
R K Cochrane ◽  
P N Best ◽  
D Sobral ◽  
I Smail ◽  
J E Geach ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Stellar Mass ◽  
Mass Star ◽  
Galaxy Clustering

scholarly journals The Relation between Star-Formation Rate and Stellar Mass of Galaxies atz~ 1–4

2016 ◽  
Vol 33 ◽  
Author(s):  
A. Katsianis ◽  
E. Tescari ◽  
J. S. B. Wyithe
Keyword(s):  
Star Formation ◽  
Energy Distribution ◽  
Star Formation Rate ◽  
Spectral Energy Distribution ◽  
Formation Rate ◽  
Stellar Mass ◽  
Numerical Results ◽  
High Mass ◽  
Spectral Energy ◽  
Hydrodynamic Simulations

AbstractThe relation between the star-formation Rate and stellar mass (M⋆) of galaxies represents a fundamental constraint on galaxy formation, and has been studied extensively both in observations and cosmological hydrodynamic simulations. However, the observed amplitude of the star-formation rate—stellar mass relation has not been successfully reproduced in simulations, indicating either that the halo accretion history and baryonic physics are poorly understood/modelled or that observations contain biases. In this paper, we examine the evolution of the SFR −M⋆relation ofz~ 1–4 galaxies and display the inconsistency between observed relations that are obtained using different techniques. We employ cosmological hydrodynamic simulations from various groups which are tuned to reproduce a range of observables and compare these with a range of observed SFR −M⋆relations. We find that numerical results are consistent with observations that use Spectral Energy Distribution techniques to estimate star-formation rates, dust corrections, and stellar masses. On the contrary, simulations are not able to reproduce results that were obtained by combining only UV and IR luminosities (UV+IR). These imply star-formation rates at a fixed stellar mass that are larger almost by a factor of 5 than those of Spectral Energy Distribution measurements forz~ 1.5–4. Forz< 1.5, the results from simulations, Spectral Energy Distribution fitting techniques and IR+UV conversion agree well. We find that surveys that preferably select star-forming galaxies (e.g. by adopting Lyman-break or blue selection) typically predict a larger median/average star-formation rate at a fixed stellar mass especially for high mass objects, with respect to mass selected samples and hydrodynamic simulations. Furthermore, we find remarkable agreement between the numerical results from various authors who have employed different cosmological codes and run simulations with different resolutions. This is interesting for two reasons. (A) simulations can produce realistic populations of galaxies within representative cosmological volumes even at relatively modest resolutions. (B) It is likely that current numerical codes that rely on similar subgrid multiphase interstellar medium models and are tuned to reproduce statistical properties of galaxies, produce similar results for the SFR −M⋆relation by construction, regardless of resolution, box size and, to some extent, the adopted feedback prescriptions.

scholarly journals Signatures of Cool Gas Fueling a Star-Forming Galaxy at Redshift 2.3

Science ◽  
2013 ◽  
Vol 341 (6141) ◽  
pp. 50-53 ◽  
Author(s):  
N. Bouché ◽  
M. T. Murphy ◽  
G. G. Kacprzak ◽  
C. Péroux ◽  
T. Contini ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Accretion Rate ◽  
Formation Rate ◽  
Observational Evidence ◽  
Intergalactic Gas ◽  
Star Forming ◽  
The Galaxy ◽  
Cool Gas ◽  
Gas Accretion

Galaxies are thought to be fed by the continuous accretion of intergalactic gas, but direct observational evidence has been elusive. The accreted gas is expected to orbit about the galaxy’s halo, delivering not just fuel for star formation but also angular momentum to the galaxy, leading to distinct kinematic signatures. We report observations showing these distinct signatures near a typical distant star-forming galaxy, where the gas is detected using a background quasar passing 26 kiloparsecs from the host. Our observations indicate that gas accretion plays a major role in galaxy growth because the estimated accretion rate is comparable to the star-formation rate.

Clustering dependence of Chandra COSMOS Legacy AGN on host galaxy properties

2019 ◽  
Vol 15 (S356) ◽  
pp. 226-226
Author(s):  
Viola Allevato
Keyword(s):  
Dark Matter ◽  
Formation Rate ◽  
Stellar Mass ◽  
Active Galaxies ◽  
Host Galaxy ◽  
Mass Star ◽  
Mass Relation ◽  
Dark Matter Halos ◽  
X Ray

AbstractThe presence of a super massive BH in almost all galaxies in the Universe is an accepted paradigm in astronomy. How these BHs form and how they co-evolve with the host galaxy is one of the most intriguing unanswered problems in modern Cosmology and of extreme relevance to understand the issue of galaxy formation. Clustering measurements can powerfully test theoretical model predictions of BH triggering scenarios and put constraints on the typical environment where AGN live in, through the connection with their host dark matter halos. In this talk, I will present some recent results on the AGN clustering dependence on host galaxy properties, such as galaxy stellar mass, star formation rate and specific BH accretion rate, based on X-ray selected Chandra COSMOS Legacy Type 2 AGN. We found no significant AGN clustering dependence on galaxy stellar mass and specif BHAR for Type 2 COSMOS AGN at mean z ∼ 1.1, with a stellar - halo mass relation flatter than predicted for non active galaxies in the Mstar range probed by our sample. We also observed a negative clustering dependence on SFR, with AGN hosting halo mass increasing with decreasing SFR. Mock catalogs of active galaxies in hosting dark matter halos with logMh[Msun] > 12.5, matched to have the same X-ray luminosity, stellar mass and BHAR of COSMOS AGN predict the observed Mstar - Mh, BHAR - Mh and SFR-Mh relations, at z ∼ 1.

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