TY  - JOUR
A1  - Richter, Philipp
A1  - Fox, Andrew J.
A1  - Ben Bekhti, Nadya
A1  - Murphy, M. T.
A1  - Bomans, Dominik J.
A1  - Frank, S.
T1  - High-resolution absorption spectroscopy of the circumgalactic medium of the Milky Way
JF  - Astronomische Nachrichten = Astronomical notes
KW  - Galaxy: halo
KW  - Galaxy: structure
KW  - quasars: absorption lines
KW  - techniques: spectroscopic
Y1  - 2014
U6  - https://doi.org/10.1002/asna.201312013
SN  - 0004-6337
SN  - 1521-3994
VL  - 335
IS  - 1
SP  - 92
EP  - 98
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
TY  - JOUR
A1  - Fox, Andrew J.
A1  - Wakker, Bart P.
A1  - Barger, Kathleen A.
A1  - Hernandez, Audra K.
A1  - Richter, Philipp
A1  - Lehner, Nicolas
A1  - Bland-Hawthorn, Joss
A1  - Charlton, Jane C.
A1  - Westmeier, Tobias
A1  - Thom, Christopher
A1  - Tumlinson, Jason
A1  - Misawa, Toru
A1  - Howk, J. Christopher
A1  - Haffner, L. Matthew
A1  - Ely, Justin
A1  - Rodriguez-Hidalgo, Paola
A1  - Kumari, Nimisha
T1  - The COS/UVES absorption survey of the magellanic stream. III. Ionization, total mass, and inflow rate onto the milky way
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - Dynamic interactions between the two Magellanic Clouds have flung large quantities of gas into the halo of the Milky Way. The result is a spectacular arrangement of gaseous structures, including the Magellanic Stream, the Magellanic Bridge, and the Leading Arm (collectively referred to as the Magellanic System). In this third paper of a series studying the Magellanic gas in absorption, we analyze the gas ionization level using a sample of 69 Hubble Space Telescope/Cosmic Origins Spectrograph sightlines that pass through or within 30 degrees of the 21 cm emitting regions. We find that 81% (56/69) of the sightlines show UV absorption at Magellanic velocities, indicating that the total cross-section of the Magellanic System is approximate to 11,000 deg(2), or around one-quarter of the entire sky. Using observations of the Si III/Si II ratio together with Cloudy photoionization modeling, we calculate the total gas mass (atomic plus ionized) of the Magellanic System to be approximate to 2.0 x 10(9) M-circle dot (d/55 kpc)(2), with the ionized gas contributing around three times as much mass as the atomic gas. This is larger than the current-day interstellar H I mass of both Magellanic Clouds combined, indicating that they have lost most of their initial gas mass. If the gas in the Magellanic System survives to reach the Galactic disk over its inflow time of similar to 0.5-1.0 Gyr, it will represent an average inflow rate of similar to 3.7-6.7 M-circle dot yr(-1), potentially raising the Galactic star formation rate. However, multiple signs of an evaporative interaction with the hot Galactic corona indicate that the Magellanic gas may not survive its journey to the disk fully intact and will instead add material to (and cool) the corona.
KW  - Galaxy: evolution
KW  - Galaxy: halo
KW  - ISM: abundances
KW  - Magellanic Clouds
KW  - quasars: absorption lines
Y1  - 2014
U6  - https://doi.org/10.1088/0004-637X/787/2/147
SN  - 0004-637X
SN  - 1538-4357
VL  - 787
IS  - 2
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
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  -