@article{da5e36975aa84d13b0b0de11c675e1d7,
title = "Nihao VII: Predictions for the galactic baryon budget in dwarf to Milky Way mass haloes",
abstract = "We use the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) galaxy formation simulations to make predictions for the baryonic budget in present day galaxies ranging from dwarf (M200 ∼ 1010 M☉) to Milky Way (M200 ∼ 1012 M☉) masses. The sample is made of 88 independent high-resolution cosmological zoom-in simulations. NIHAO galaxies reproduce key properties of observed galaxies, such as the stellar mass versus halo mass and cold gas versus stellar mass relations. Thus they make plausible predictions for the baryon budget. We present the mass fractions of stars, cold gas (T < 104 K), cool gas (104 < T < 105 K), warm-hot gas (105 < T < 5 × 106 K) and hot gas (T > 5 × 106 K), inside the virial radius, R200. Compared to the predicted baryon mass, using the dark halo mass and the universal baryon fraction, fb ≡ Ωb /Ωm = 0.15, we find that all of our haloes are missing baryons. The missing mass has been relocated past 2 virial radii, and cool gas dominates the corona at low mass (M200 ≲ 3 × 1011 M☉) while the warm-hot gas dominates at high mass (M200 ≿ 3 × 1011 M☉). Haloes of mass M200 ∼ 1010 M☉ are missing ∼90 per cent of their baryons. More massive haloes (M200 ∼ 1012 M☉) retain a higher fraction of their baryons, with ∼30 per cent missing, consistent with recent observational estimates. Moreover, these more massive haloes reproduce the observed fraction of cold, warm-hot and hot gases. The fraction of cool gas we predict (0.11 ± 0.06) is significantly lower than the observation from COS-Halos (0.3-0.47), but agrees with the alternative analysis of Stern et al. (2016).",
keywords = "Cosmology: theory, Galaxies: dwarf, Galaxies: evolution, Galaxies: formation, Galaxies: spiral, Methods: numerical",
author = "Liang Wang and Dutton, {Aaron A.} and Stinson, {Gregory S.} and Macci{\`o}, {Andrea V.} and Thales Gutcke and Xi Kang",
note = "Funding Information: We thank the two anonymous referees whose suggestions greatly improve the paper. We thank Freeke van de Voort for kindly sharing data of the FIRE simulation. GASOLINE was written by Tom Quinn and James Wadsley. Without their contribution, this paper would have been impossible. The simulations were performed on the THEO cluster of the Max-Planck-Institut f{\"u}r Astronomie and the HYDRA cluster at the Rechenzentrum in Garching; and the Milky Way supercomputer, funded by the Deutsche Forschungsgemeinschaft (DFG) through Collaborative Research Center (SFB 881) 'The Milky Way System' (subproject Z2), hosted and co-funded by the J{\"u}lich Supercomputing Center (JSC). We greatly appreciate the contributions of all these computing allocations. AAD, GSS and AVM acknowledge support through the Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject A1) of the German Research Foundation (DFG). The analysis made use of the PYNBODY package (Pontzen et al. 2013). The authors acknowledge support from the MPG-CAS through the partnership programme between the MPIA group lead by AVM and the PMO group lead by XK. LW acknowledges support of the MPG-CAS student programme. XK acknowledges the support from 973 program (No. 2015CB857003, 2013CB834900), NSFC project No.11333008 and the 'Strategic Priority Research Program the Emergence of Cosmological Structures' of the CAS (No.XD09010000). Funding Information: We thank the two anonymous referees whose suggestions greatly improve the paper. We thank Freeke van de Voort for kindly sharing data of the FIRE simulation. GASOLINE was written by Tom Quinn and James Wadsley. Without their contribution, this paper would have been impossible. The simulations were performed on the THEO cluster of the Max-Planck-Institut f{\"u}r Astronomie and the HYDRA cluster at the Rechenzentrum in Garching; and the Milky Way supercomputer, funded by the Deutsche Forschungsgemeinschaft (DFG) through Collaborative Research Center (SFB 881) {\textquoteleft}The Milky Way System{\textquoteright} (subproject Z2), hosted and co-funded by the J{\"u}lich Supercomputing Center (JSC). We greatly appreciate the contributions of all these computing allocations. AAD, GSS and AVM acknowledge support through the Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject A1) of the German Research Foundation (DFG). The analysis made use of the PYNBODY package (Pontzen et al. 2013). The authors acknowledge support from the MPG-CAS through the partnership programme between the MPIA group lead by AVM and the PMO group lead by XK. LW acknowledges support of the MPG-CAS student programme. XK acknowledges the support from 973 program (No. 2015CB857003, 2013CB834900), NSFC project No.11333008 and the {\textquoteleft}Strategic Priority Research Program the Emergence of Cosmological Structures{\textquoteright} of the CAS (No.XD09010000). Publisher Copyright: {\textcopyright} 2017 The Authors",
year = "2017",
month = may,
day = "1",
doi = "10.1093/mnras/stx066",
language = "English (US)",
volume = "466",
pages = "4858--4867",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",
}