Garrotxa Cosmological Simulations of Milky Way-Sized Galaxies: General Properties, Hot-Gas Distribution, and Missing Baryons

Roca-Fàbrega, S.; Valenzuela, O.; Colín, Pedro; Figueras, F.; Krongold, Y.; Velázquez, Héctor; Avila-Reese, Vladimir; Ibarra-Medel, H.

doi:10.3847/0004-637x/824/2/94

Cited by 32 publications

(53 citation statements)

References 144 publications

(242 reference statements)

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“…We find, in agreement with our previous studies (e.g., González-Samaniego et al 2014), nearly flat circular velocity curves. However, contrary to our re-sults on the low-mass galaxies González-Samaniego et al 2014), and to some degree also on the MW-sized galaxy of Roca-Fàbrega et al (2016), here our predicted M s /M vir values agree with those determined by semi-empirical methods.…”

Section: Introductioncontrasting

confidence: 99%

“…The aim of this work is to introduce a new suite of zoom-in Milky Way (MW) sized simulations run with the N-body + Hydrodynamic ART code (Kravtsov 2003) and with the SF and stellar feedback prescription implemented for the first time in (Colín et al 2010, see also Avila-Reese et al 2011a), and used recently in Roca-Fàbrega et al (2016) for the "Garrotxa" simulations. Here we use the same n SF and ǫ SF values as in the latter paper.…”

Section: Introductionmentioning

confidence: 99%

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Cosmological Simulations of Milky Way-Sized Galaxies

Colín

Avila-Reese

Roca-Fàbrega

et al. 2016

ApJ

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We introduce a new set of eight Milky Way-sized cosmological simulations performed using the AMR code ART + Hydrodynamics in a ΛCDM cosmology. The set of zoom-in simulations covers present-day virial masses that range from 8.3 × 10 11 M ⊙ to 1.56 × 10 12 M ⊙ and is carried out with our simple but effective deterministic star formation (SF) and "explosive" stellar feedback prescriptions. The work is focused on showing the goodness of the simulated set of "field" Milky Way-sized galaxies. To this end, we compare some of the predicted physical quantities with the corresponding observed ones. Our results are as follows. (a) In agreement with some previous works, we found circular velocity curves that are flat or slightly peaked. (b) All simulated galaxies with a significant disk component are consistent with the observed Tully-Fisher, radius-mass, and cold gas-stellar mass correlations of latetype galaxies. (c) The disk-dominated galaxies have stellar specific angular momenta in agreement with those of late-type galaxies, with values around 10 3 km/s/kpc. (d) The SF rates at z = 0 of all runs but one are comparable to those estimated for the star-forming galaxies. (e) The two most spheroid-dominated galaxies formed in halos with late active merger histories and late bursts of SF, but the other run that ends also as dominated by an spheroid, never had major mergers. (f) The simulated galaxies lie in the semi-empirical stellar-to-halo mass correlation of local central galaxies, and those that end up as disk dominated, evolve mostly along the low-mass branch of this correlation. Moreover, the baryonic and stellar mass growth histories of these galaxies are proportional to their halo mass growth histories since the last 6.5-10 Gyr. (g) Within the virial radii of the simulations, ≈ 25 − 50% of the baryons are missed; the amount of gas in the halo is similar to the one in stars in the galaxy, and most of this gas is in the warm-hot phase. (h) The z ∼ 0 vertical gas velocity dispersion profiles, σ z (r), are nearly flat and can be mostly explained by the kinetic energy injected by stars. The average values of σ z increase at higher redshifts, following roughly the shape of the SF history.

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Section: Introductioncontrasting

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Cosmological Simulations of Milky Way-Sized Galaxies

Colín

Avila-Reese

Roca-Fàbrega

et al. 2016

ApJ

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“…At smaller scales, one uses either extrapolations of the density profile matching at larger scales or the results from cosmological simulations. We use density profiles from state-of-the-art N-body þ hydrodynamics simulations of Milky Way-like galaxies in the lambda cold dark matter (ΛCDM) cosmology: Mollitor et [20]), and Garrotxa (GARR [21]). For comparison to Ref.…”

Section: Dm-halo Profilementioning

confidence: 99%

Analysis of the very inner Milky Way dark matter distribution and gamma-ray signals

et al. 2016

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We analyze the possibility that the HESS γ-ray source at the Galactic center could be explained as the secondary flux produced by annihilation of TeV dark matter (DM) particles with locally enhanced density, in a region spatially compatible with the HESS observations themselves. We study the inner 100 pc considering (i) the extrapolation of several density profiles from state-of-the-art N-body þ hydrodynamics simulations of Milky Way-like galaxies, (ii) the DM spike induced by the black hole, and (iii) the DM particles scattering off by bulge stars. We show that in some cases the DM spike may provide the enhancement in the flux required to explain the cutoff in the HESS J1745-290γ-ray spectra as TeV DM. In other cases, it may help to describe the spatial tail reported by HESS II at angular scales ≲0.54°toward Sgr A Ã .

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“…Meanwhile, a significant computational effort is underway by cosmological simulators to understand the origin of oxygen in the hot circumgalactic gas: Stinson et al (2013);Suresh, et al (2015); Liang, Kravtsov & Agertz (2016); Roca-Fabrega et al (2016);Oppenheimer, et al (2016); Sokolowska et al (2016) etc. In these studies most of the circumgalactic oxygen is provided by supernova-driven galactic winds from the central galaxy.…”

Section: Introductionmentioning

confidence: 99%

Circumgalactic Oxygen Absorption and Feedback

Mathews

Prochaska

2017

ApJL

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OVI absorption in quasar spectra caused by intervening circumgalactic atmospheres suggests a downturn in the atmospheric column density in sightlines passing beyond about 100 kpc from central star-forming galaxies. This turnover supports the hypothesis that the oxygen originates in the central galaxies. When converted into oxygen space density using an Abel integral inversion, the OVI columns require > ∼ 10 9 M of oxygen concentrated near 100 kpc. Circumgalactic gas within this radius cools in less than 1 Gyr and radiates ∼ 10 42.2 erg s −1 overall. The feedback power necessary to maintain such oxygen-rich atmospheres for many Gyrs cannot be easily supplied by galactic supernovae. However, massive central black holes in star-forming galaxies may generate sufficient accretion power and intermittent shock waves at r ∼ 100 kpc to balance circumgalactic radiation losses in late-type L galaxies. The relative absence of OVI absorption observed in early-type, passive L galaxies may arise from enhanced AGN feedback from their more massive central black holes.

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Garrotxa Cosmological Simulations of Milky Way-Sized Galaxies: General Properties, Hot-Gas Distribution, and Missing Baryons

Cited by 32 publications

References 144 publications

Cosmological Simulations of Milky Way-Sized Galaxies

Cosmological Simulations of Milky Way-Sized Galaxies

Analysis of the very inner Milky Way dark matter distribution and gamma-ray signals

Circumgalactic Oxygen Absorption and Feedback

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