MUFASA: The strength and evolution of galaxy conformity in various tracers

We investigate galaxy conformity using the Mufasa cosmological hydrodynamical simulation. We show a bimodal distribution in galaxy colour with radius, albeit with too many low-mass quenched satellite galaxies compared to observations. Mufasa produces conformity in observed properties such as colour, sSFR, and Hi content; i.e neighbouring galaxies have similar properties. We see analogous trends in other properties such as in environment, stellar age, H2 content, and metallicity. We intro- duce quantifying conformity using S(R), measuring the relative difference in upper and lower quartile properties of the neighbours.We show that low-mass and non-quenched haloes have weak conformity (S(R) < 0.5) extending to large projected radii R in all properties, while high-mass and quenched haloes have strong conformity (S(R) ~ 1) that diminishes rapidly with R and disappears at R & 1 Mpc. S(R) is strongest for environment in low-mass haloes, and sSFR (or colour) in high-mass haloes, and is dominated by one-halo conformity with the exception of Hi in small haloes. Metal- licity shows a curious anti-conformity in massive haloes. Tracking the evolution of conformity for z = 0 galaxies back in time shows that conformity broadly emerges as a late-time (z < 1) phenomenon. However, for fixed halo mass bins, conformity is fairly constant with redshift out to z > 2. These trends are consistent with the idea that strong conformity only emerges once haloes grow above Mufasa’s quenching mass scale of ~ 1012M⊙. A quantitative measure of conformity in various properties, along with its evolution, thus represents a new and stringent test of the impact of quenching on environment within current galaxy formation models.ScopusIS

Hallazgo de un manuscrito sobre el "balsamo de Malats"

El autor halló en un libro de "Medicina y Cirugía Humana" de 1753, un manuscrito anónimo del famoso Bálsamo de Malats. Estimado en la primera mitad del 1800. Dos variantes. Se adjuntan las fotocopias, que ha traducido del catalán antiguo. Comparando la fórmula del Bálsamo con otras publicaciones de 1820

Non-thermal pressure in the outskirts of Abell 2142

Clumping and turbulence are expected to affect the matter accreted on to the outskirts of galaxy clusters. To determine their impact on the thermodynamic properties of Abell 2142, we perform an analysis of the X-ray temperature data from XMM-Newton via our SuperModel, a state-of-the-art tool for investigating the astrophysics of the intracluster medium already tested on many individual clusters (since Cavaliere, Lapi & Fusco-Femiano 2009). Using the gas density profile corrected for clumpiness derived by Tchernin et al. (2016), we find evidence for the presence of a non-thermal pressure component required to sustain gravity in the cluster outskirts of Abell 2142, that amounts to about 30 per cent of the total pressure at the virial radius. The presence of the non-thermal component implies the gas fraction to be consistent with the universal value at the virial radius and the electron thermal pressure profile to be in good agreement with that inferred from the SZ data. Our results indicate that the presence of gas clumping and of a non-thermal pressure component are both necessary to recover the observed physical properties in the cluster outskirts. Moreover, we stress that an alternative method often exploited in the literature (included Abell 2142) to determine the temperature profile kBT = Pe/nebasing on a combination of the Sunyaev-Zel'dovich (SZ) pressure Peand of the X-ray electron density nedoes not allow us to highlight the presence of non-thermal pressure support in the cluster outskirts

A galaxy–halo model for multiple cosmological tracers

archiveprefix: arXiv primaryclass: astro-ph.GA slaccitation: %%CITATION = ARXIV:1610.08948;%%archiveprefix: arXiv primaryclass: astro-ph.GA slaccitation: %%CITATION = ARXIV:1610.08948;%%archiveprefix: arXiv primaryclass: astro-ph.GA slaccitation: %%CITATION = ARXIV:1610.08948;%