TY  - JOUR
A1  - Wendt, Martin
T1  - Constraints on variations of m(p)/m(e) based on UVES observations of H-2
JF  - Astronomische Nachrichten = Astronomical notes
N2  - This article summarizes the latest results on the proton-to-electron mass ratio derived from H-2 observations at high redshift in the light of possible variations of fundamental physical constants. The focus lies on UVES observations of the past years as enormous progress was achieved since the first positive results on / were published. With the better understanding of systematics, dedicated observation runs, and numerous approaches to improve wavelength calibration accuracy, all current findings are in reasonable good agreement with no variation and provide an upper limit of / < 1 x 10(-5) for the redshift range of 2 < z < 3. ((
KW  - cosmology: observations
KW  - early Universe
KW  - quasars: absorption lines
Y1  - 2014
U6  - https://doi.org/10.1002/asna.201312008
SN  - 0004-6337
SN  - 1521-3994
VL  - 335
IS  - 1
SP  - 106
EP  - 112
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
TY  - JOUR
A1  - Bonifacio, P.
A1  - Rahmani, H.
A1  - Whitmore, J. B.
A1  - Wendt, Martin
A1  - Centurion, Martin
A1  - Molaro, P.
A1  - Srianand, R.
A1  - Murphy, M. T.
A1  - Petitjean, P.
A1  - Agafonova, I. I.
A1  - Evans, T. M.
A1  - Levshakov, S. A.
A1  - Lopez, S.
A1  - Martins, C. J. A. P.
A1  - Reimers, D.
A1  - Vladilo, G.
T1  - Fundamental constants and high-resolution spectroscopy
JF  - Astronomische Nachrichten = Astronomical notes
KW  - atomic processes
KW  - cosmology: observations
KW  - elementary particles
KW  - line: formation
KW  - quasars: absorption lines
KW  - techniques: spectroscopic
Y1  - 2014
U6  - https://doi.org/10.1002/asna.201312005
SN  - 0004-6337
SN  - 1521-3994
VL  - 335
IS  - 1
SP  - 83
EP  - 91
PB  - Wiley-VCH
CY  - Weinheim
ER  - 
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  - Evans, T. M.
A1  - Murphy, M. T.
A1  - Whitmore, J. B.
A1  - Misawa, T.
A1  - Centurion, Martin
A1  - Lopez, S.
A1  - Martins, C. J. A. P.
A1  - Molaro, P.
A1  - Petitjean, P.
A1  - Rahmani, H.
A1  - Srianand, R.
A1  - Wendt, Martin
T1  - The UVES Large Program for testing fundamental physics - III. Constraints on the fine-structure constant from three telescopes
JF  - Monthly notices of the Royal Astronomical Society
KW  - intergalactic medium
KW  - quasars: absorption lines
KW  - quasars: individual: HS 1549+1919
KW  - cosmology: miscellaneous
KW  - cosmology: observations
Y1  - 2014
U6  - https://doi.org/10.1093/mnras/stu1754
SN  - 0035-8711
SN  - 1365-2966
VL  - 445
IS  - 1
SP  - 128
EP  - 150
PB  - Oxford Univ. Press
CY  - Oxford
ER  -