TY  - JOUR
A1  - Nuza, Sebastian E.
A1  - Parisi, Florencia
A1  - Scannapieco, Cecilia
A1  - Richter, Philipp
A1  - Gottloeber, Stefan
A1  - Steinmetz, Matthias
T1  - The distribution of gas in the Local Group from constrained cosmological simulations: the case for Andromeda and the Milky Way galaxies
JF  - Monthly notices of the Royal Astronomical Society
N2  - We study the gas distribution in the Milky Way and Andromeda using a constrained cosmological simulation of the Local Group (LG) within the context of the CLUES (Constrained Local UniversE Simulations) project. We analyse the properties of gas in the simulated galaxies at z = 0 for three different phases: 'cold', 'hot' and H i, and compare our results with observations. The amount of material in the hot halo (M-hot a parts per thousand 4-5 x 10(10) M-aS (TM)), and the cold (M-cold(r a parts per thousand(2) 10 kpc) a parts per thousand 10(8) M-aS (TM)) and H i components displays reasonable agreement with observations. We also compute the accretion/ejection rates together with the H i (radial and all-sky) covering fractions. The integrated H i accretion rate within r = 50 kpc gives similar to 0.2-0.3 M-aS (TM) yr(-1), i.e. close to that obtained from high-velocity clouds in the Milky Way. We find that the global accretion rate is dominated by hot material, although ionized gas with T a parts per thousand(2) 10(5) K can contribute significantly too. The net accretion rates of all material at the virial radii are 6-8 M-aS (TM) yr(-1). At z = 0, we find a significant gas excess between the two galaxies, as compared to any other direction, resulting from the overlap of their gaseous haloes. In our simulation, the gas excess first occurs at z similar to 1, as a result of the kinematical evolution of the LG.
KW  - methods: numerical
KW  - Galaxy: halo
KW  - intergalactic medium
KW  - Local Group
KW  - large-scale structure of Universe
Y1  - 2014
U6  - https://doi.org/10.1093/mnras/stu643
SN  - 0035-8711
SN  - 1365-2966
VL  - 441
IS  - 3
SP  - 2593
EP  - 2612
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Damle, Mitali
A1  - Sparre, Martin
A1  - Richter, Philipp
A1  - Hani, Maan H.
A1  - Nuza, Sebastian
A1  - Pfrommer, Christoph
A1  - Grand, Robert J. J.
A1  - Hoffman, Yehuda
A1  - Libeskind, Noam
A1  - Sorce, Jenny
A1  - Steinmetz, Mathias
A1  - Tempel, Elmo
A1  - Vogelsberger, Mark
A1  - Wang, Peng
T1  - Cold and hot gas distribution around the Milky-Way – M31 system in the HESTIA simulations
JF  - Monthly notices of the royal astronomical society
N2  - Recent observations have revealed remarkable insights into the gas reservoir in the circumgalactic medium (CGM) of galaxy haloes. In this paper, we characterise the gas in the vicinity of Milky Way and Andromeda analogues in the hestia (High resolution Environmental Simulations of The Immediate Area) suite of constrained Local Group (LG) simulations. The hestia suite comprise of a set of three high-resolution arepo-based simulations of the LG, run using the Auriga galaxy formation model.
For this paper, we focus only on the 𝑧 = 0 simulation datasets and generate mock skymaps along with a power spectrum analysis to show that the distributions of ions tracing low-temperature gas (H i and Si iii) are more clumpy in comparison to warmer gas tracers (O vi, O vii and O viii). We compare to the spectroscopic CGM observations of M31 and low-redshift galaxies.
hestia under-produces the column densities of the M31 observations, but the simulations are consistent with the observations of low-redshift galaxies. A possible explanation for these findings is that the spectroscopic observations of M31 are contaminated by gas residing in the CGM of the Milky Way.
KW  - software: data analysis
KW  - software: simulations
KW  - Galaxy: evolution
KW  - galaxies: evolution
KW  - galaxies: Local Group
Y1  - 2022
U6  - https://doi.org/10.1093/mnras/stac663
SN  - 0035-8711
SN  - 1365-2966
VL  - 512
SP  - 3717
EP  - 3737
PB  - Oxford Univ. Press
CY  - Oxford
ER  -