Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

Grylls, Philip; Shankar, Francesco; Leja, Joel; Menci, Nicola; Moster, Benjamin P.; Behroozi, Peter; Zanisi, Lorenzo

doi:10.1093/mnras/stz2956

Cited by 21 publications

(25 citation statements)

References 77 publications

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“…In most previous studies, M step was chosen to be at the median or mean stellar mass of the SN Ia sample, or arbitrarily chosen at some location (e.g., 10 10 M ; Sullivan et al 2010). There is little physical motivation for this choice, although we note that 10 10 M lies just below the knee in the galaxy-mass/halo-mass relation (∼ 3x10 10 M at low redshift, Kauffmann et al 2003), the point at which galaxies transform from 'star-formation-dominated SN-regulated', to 'accretion-dominated AGN-regulated' growth (Silk 2011(Silk , 2013Taylor et al 2017;Grylls et al 2020). This galaxy-halo connection is known to have effects on galaxy properties (for a review, see Wechsler & Tinker 2018).…”

Section: Sn Derived Parametersmentioning

confidence: 98%

The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Kelsey

Sullivan

Smith

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Analyses of Type Ia supernovae (SNe Ia) have found puzzling correlations between their standardized luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey 3-yr spectroscopically confirmed cosmological sample, obtaining photometry in a series of ‘local’ apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U − R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3σ in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 ± 0.018 mag; ∼0.03 mag greater than the largest global stellar mass step in our sample (0.070 ± 0.017 mag). When splitting at the sample median, differences between local and global U − R steps are small, both ∼0.08 mag, but are more significant than the global stellar mass step (0.057 ± 0.017 mag). We split the data into sub-samples based on SN Ia light-curve parameters: stretch (x1) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U − R, for both local and global measurements, of ∼0.14 mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U − R rms scatter as low as 0.084 ± 0.017 mag for blue (c < 0) SNe Ia in locally blue U − R environments.

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Section: Sn Derived Parametersmentioning

confidence: 98%

The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Kelsey

Sullivan

Smith

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Baugh 2006;Benson 2012;Linke et al 2020) and even empirical methods in which physical constraints are taken entirely from observations (e.g. Yang et al 2012;Moster et al 2020;Grylls et al 2020). We are now able to simulate the physics of galaxy formation and, to some extent, link galaxy properties to the host halo properties.…”

Section: Introductionmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA)

Sureshkumar

Durkalec

Pollo

et al. 2021

A&A

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Context. Galaxies are biased tracers of the underlying network of dark matter. The strength of this bias depends on various galaxy properties, as well as on redshift. One of the methods used to study these dependences of the bias are measurements of galaxy clustering. Such studies are made using galaxy samples from various catalogues -frequently bearing their own problems related to sample selection methods. It is therefore crucial to understand how sample choice influences the clustering measurements, and which galaxy property is the most direct tracer of the galaxy environment. Aims. We investigate how different galaxy properties -luminosities in u, g, r, J, K-bands, stellar mass, star formation rate and specific star formation rate trace the environment in the local universe. We also study the effect of survey flux limits on galaxy clustering measurements. Methods. We measure the two-point correlation function (2pCF) and marked correlation functions (MCFs) using the aforementioned properties as marks. We use nearly stellar-mass-complete galaxy sample in the redshift range 0.1 < z < 0.16 from the Galaxy And Mass Assembly (GAMA) survey with a flux limit of r < 19.8. Further, we impose a brighter flux limit of r < 17.8 to our sample and repeat the measurements to study how this affects galaxy clustering analysis. We compare our results to measurements from the Sloan Digital Sky Survey (SDSS) with flux limits of r < 17.8 and r < 16.8. Results. We show that the stellar mass is the most direct tracer of galaxy environment, the K-band luminosity being a good substitute, although such a proxy sample misses close pairs of evolved, red galaxies. We also show that the u-band luminosity can be a proxy of star formation rate in the context of galaxy clustering. We observe an effect of the survey flux limit on clustering studies -samples with a higher flux limit (smaller magnitude) miss some information about close pairs of starburst galaxies.

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“…Similarly to Grylls et al (2020), in the previous Sections we made use of toy models where only these two parameters are changed to explore their impact on the sizes of MGs. 2020) (in the wo latter cases the masses have been shifted by 0.15 dex to account for M/L differences with our SDSS data, see Grylls et al 2019a). Note that the data points were retrieved from the Schechter fits provided in the two studies, extrapolated in our mass range.…”

Section: The Sizes Of Mgs As Effective Constraints To the Galaxy-halo Connectionmentioning

confidence: 92%

“…Due to their flexibility and relatively lower number of free parameters, semi-empirical models have become a popular route to study the mass assembly, star formation, and merger histories of galaxies (e.g., Conroy & Wechsler 2009;Hopkins et al 2010a,b;Behroozi et al 2013;Moster et al 2013;Shankar et al 2013;Gu et al 2016;Matthee et al 2017;Rodríguez-Puebla et al 2017;Lapi et al 2018a;Chen et al 2020;Grylls et al 2019aGrylls et al , 2020O'Leary et al 2021). The main ingredient in semi-empirical models is the input stellar mass-halo mass (SMHM) relation, which is extracted from the cumulative equivalence between the number densities of the stellar mass and (sub)halo mass functions (e.g., Vale & Ostriker 2006;Shankar et al 2006;Guo et al 2011;Dutton et al 2010;Firmani & Avila-Reese 2010;Leauthaud et al 2012;Rodríguez-Puebla et al 2013;Mandelbaum et al 2016;Pillepich et al 2018;Behroozi et al 2019;Moster et al 2018;Kravtsov et al 2018;Erfanianfar et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

Zanisi

Shankar

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The mean size ( effective radius Re) of Massive Galaxies (MGs, Mstar > 1011.2M⊙) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g., mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass-halo mass (SMHM) relations with varying high-mass slopes and scatters σSMHM in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically-motivated, constant and linear relationship between Re and the host dark matter halo radius Rh. We find that: 1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; 2) the numbers of compact MGs grow steadily until z ≳ 2 and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; 3) a time-independent scatter σSMHM is consistent with a scenario in which compact starforming MGs transition into quiescent MGs in a few 108yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the starforming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution.

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Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL steel.

Cited by 21 publications

References 77 publications

The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Galaxy and Mass Assembly (GAMA)

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

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