Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742372.0, MPI für Astronomie / Publikationen_mpia
NIHAO VII: predictions for the galactic baryon budget in dwarf to Milky Way mass haloes
Authors:Wang, L.; Dutton, A. A.; Stinson, G. S.; Macciò, A. V.; Gutcke, T.; Kang, X.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:466
Issue / Number:4
Start Page:4858
End Page:4867
Audience:Not Specified
Abstract / Description: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 ≡ Ωbm = 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).
Free Keywords:methods: numerical; galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: spiral; cosmology: theory
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/stx066
URL:http://adsabs.harvard.edu/abs/2017MNRAS.466.4858W
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.