@unpublished{AcharyaActisAghajanietal.2013,
  author    = {Acharya, B. S. and Actis, M. and Aghajani, T. and Agnetta, G. and Aguilar, J. and Aharonian, Felix A. and Ajello, M. and Akhperjanian, A. G. and Alcubierre, M. and Aleksic, J. and Alfaro, R. and Aliu, E. and Allafort, A. J. and Allan, D. and Allekotte, I. and Amato, E. and Anderson, J. and Ang{\"u}ner, Ekrem Oǧuzhan and Antonelli, L. A. and Antoranz, P. and Aravantinos, A. and Arlen, T. and Armstrong, T. and Arnaldi, H. and Arrabito, L. and Asano, K. and Ashton, T. and Asorey, H. G. and Awane, Y. and Baba, H. and Babic, A. and Baby, N. and Baehr, J. and Bais, A. and Baixeras, C. and Bajtlik, S. and Balbo, M. and Balis, D. and Balkowski, C. and Bamba, A. and Bandiera, R. and Barber, A. and Barbier, C. and Barcelo, M. and Barnacka, Anna and Barnstedt, J{\"u}rgen and Barres de Almeida, U. and Barrio, J. A. and Basili, A. and Basso, S. and Bastieri, D. and Bauer, C. and Baushev, Anton N. and Becerra Gonzalez, J. and Becherini, Yvonne and Bechtol, K. C. and Tjus, J. Becker and Beckmann, Volker and Bednarek, W. and Behera, B. and Belluso, M. and Benbow, W. and Berdugo, J. and Berger, K. and Bernard, F. and Bernardino, T. and Bernl{\"o}hr, K. and Bhat, N. and Bhattacharyya, S. and Bigongiari, C. and Biland, A. and Billotta, S. and Bird, T. and Birsin, E. and Bissaldi, E. and Biteau, Jonathan and Bitossi, M. and Blake, S. and Blanch Bigas, O. and Blasi, P. and Bobkov, A. A. and Boccone, V. and Boettcher, Markus and Bogacz, L. and Bogart, J. and Bogdan, M. and Boisson, Catherine and Boix Gargallo, J. and Bolmont, J. and Bonanno, G. and Bonardi, A. and Bonev, T. and Bonifacio, P. and Bonnoli, G. and Bordas, Pol and Borgland, A. W. and Borkowski, Janett and Bose, R. and Botner, O. and Bottani, A. and Bouchet, L. and Bourgeat, M. and Boutonnet, C. and Bouvier, A. and Brau-Nogue, S. and Braun, I. and Bretz, T. and Briggs, M. S. and Bringmann, T. and Brook, P. and Brun, Pierre and Brunetti, L. and Buanes, T. and Buckley, J. H. and Buehler, R. and Bugaev, V. and Bulgarelli, A. and Bulik, Tomasz and Busetto, G. and Buson, S. and Byrum, K. and Cailles, M. and Cameron, R. A. and Camprecios, J. and Canestrari, R. and Cantu, S. and Capalbi, M. and Caraveo, P. A. and Carmona, E. and Carosi, A. and Carr, John and Carton, P. H. and Casanova, Sabrina and Casiraghi, M. and Catalano, O. and Cavazzani, S. and Cazaux, S. and Cerruti, M. and Chabanne, E. and Chadwick, Paula M. and Champion, C. and Chen, Andrew and Chiang, J. and Chiappetti, L. and Chikawa, M. and Chitnis, V. R. and Chollet, F. and Chudoba, J. and Cieslar, M. and Cillis, A. N. and Cohen-Tanugi, J. and Colafrancesco, Sergio and Colin, P. and Calome, J. and Colonges, S. and Compin, M. and Conconi, P. and Conforti, V. and Connaughton, V. and Conrad, Jan and Contreras, J. L. and Coppi, P. and Corona, P. and Corti, D. and Cortina, J. and Cossio, L. and Costantini, H. and Cotter, G. and Courty, B. and Couturier, S. and Covino, S. and Crimi, G. and Criswell, S. J. and Croston, J. and Cusumano, G. and Dafonseca, M. and Dale, O. and Daniel, M. and Darling, J. and Davids, I. and Dazzi, F. and De Angelis, A. and De Caprio, V. and De Frondat, F. and de Gouveia Dal Pino, E. M. and de la Calle, I. and De La Vega, G. A. and Lopez, R. de los Reyes and De Lotto, B. and De Luca, A. and de Mello Neto, J. R. T. and de Naurois, M. and de Oliveira, Y. and de Ona Wilhelmi, E. and de Souza, V. and Decerprit, G. and Decock, G. and Deil, C. and Delagnes, E. and Deleglise, G. and Delgado, C. and Della Volpe, D. and Demange, P. and Depaola, G. and Dettlaff, A. and Di Paola, A. and Di Pierro, F. and Diaz, C. and Dick, J. and Dickherber, R. and Dickinson, H. and Diez-Blanco, V. and Digel, S. and Dimitrov, D. and Disset, G. and Djannati-Ata{\"i}, A. and Doert, M. and Dohmke, M. and Domainko, W. and Prester, Dijana Dominis and Donat, A. and Dorner, D. and Doro, M. and Dournaux, J-L. and Drake, G. and Dravins, D. and Drury, L. and Dubois, F. and Dubois, R. and Dubus, G. and Dufour, C. and Dumas, D. and Dumm, J. and Durand, D. and Dyks, J. and Dyrda, M. and Ebr, J. and Edy, E. and Egberts, Kathrin and Eger, P. and Einecke, S. and Eleftheriadis, C. and Elles, S. and Emmanoulopoulos, D. and Engelhaupt, D. and Enomoto, R. and Ernenwein, J-P and Errando, M. and Etchegoyen, A. and Evans, P. and Falcone, A. and Fantinel, D. and Farakos, K. and Farnier, C. and Fasola, G. and Favill, B. and Fede, E. and Federici, S. and Fegan, S. and Feinstein, F. and Ferenc, D. and Ferrando, P. and Fesquet, M. and Fiasson, A. and Fillin-Martino, E. and Fink, D. and Finley, C. and Finley, J. P. and Fiorini, M. and Firpo Curcoll, R. and Flores, H. and Florin, D. and Focke, W. and Foehr, C. and Fokitis, E. and Font, L. and Fontaine, G. and Fornasa, M. and Foerster, A. and Fortson, L. and Fouque, N. and Franckowiak, A. and Fransson, C. and Fraser, G. and Frei, R. and Albuquerque, I. F. M. and Fresnillo, L. and Fruck, C. and Fujita, Y. and Fukazawa, Y. and Fukui, Y. and Funk, S. and Gaebele, W. and Gabici, S. and Gabriele, R. and Gadola, A. and Galante, N. and Gall, D. and Gallant, Y. and Gamez-Garcia, J. and Garcia, B. and Garcia Lopez, R. and Gardiol, D. and Garrido, D. and Garrido, L. and Gascon, D. and Gaug, M. and Gaweda, J. and Gebremedhin, L. and Geffroy, N. and Gerard, L. and Ghedina, A. and Ghigo, M. and Giannakaki, E. and Gianotti, F. and Giarrusso, S. and Giavitto, G. and Giebels, B. and Gika, V. and Giommi, P. and Girard, N. and Giro, E. and Giuliani, A. and Glanzman, T. and Glicenstein, J. -F. and Godinovic, N. and Golev, V. and Gomez Berisso, M. and Gomez-Ortega, J. and Gonzalez, M. M. and Gonzalez, A. and Gonzalez, F. and Gonzalez Munoz, A. and Gothe, K. 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  title     = {Introducing the CTA concept},
  series = {Astroparticle physics},
  volume    = {43},
  journal   = {Astroparticle physics},
  number    = {2},
  publisher = {Elsevier},
  address   = {Amsterdam},
  organization    = {CTA Consortium},
  issn      = {0927-6505},
  doi       = {10.1016/j.astropartphys.2013.01.007},
  pages     = {3 -- 18},
  year      = {2013},
  abstract  = {The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project.},
  language  = {en}
}
@article{ActisAgnettaAharonianetal.2011,
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L. and Naumann, D. and Nayman, P. and Nedbal, D. and Niedzwiecki, A. and Niemiec, J. and Nikolaidis, A. and Nishijima, K. and Nolan, S. J. and Nowak, N. and O'Brien, P. T. and Ochoa, I. and Ohira, Y. and Ohishi, M. and Ohka, H. and Okumura, A. and Olivetto, C. and Ong, R. A. and Orito, R. and Orr, M. and Osborne, J. P. and Ostrowski, M. and Otero, L. and Otte, A. N. and Ovcharov, E. and Oya, I. and Ozieblo, A. and Paiano, S. and Pallota, J. and Panazol, J. L. and Paneque, D. and Panter, M. and Paoletti, R. and Papyan, G. and Paredes, J. M. and Pareschi, G. and Parsons, R. D. and Arribas, M. Paz and Pedaletti, G. and Pepato, A. and Persic, M. and Petrucci, P. O. and Peyaud, B. and Piechocki, W. and Pita, S. and Pivato, G. and Platos, L. and Platzer, R. and Pogosyan, L. and Pohl, Martin and Pojmanski, G. and Ponz, J. D. and Potter, W. and Prandini, E. and Preece, R. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quel, E. and Quirrenbach, A. and Rajda, P. and Rando, R. and Rataj, M. and Raue, M. and Reimann, C. and Reimann, O. and Reimer, A. and Reimer, O. and Renaud, M. and Renner, S. and Reymond, J. -M. and Rhode, W. and Ribo, M. and Ribordy, M. and Rico, J. and Rieger, F. and Ringegni, P. and Ripken, J. and Ristori, P. and Rivoire, S. and Rob, L. and Rodriguez, S. and Roeser, U. and Romano, Patrizia and Romero, G. E. and Rosier-Lees, S. and Rovero, A. C. and Roy, F. and Royer, S. and Rudak, B. and Rulten, C. B. and Ruppel, J. and Russo, F. and Ryde, F. and Sacco, B. and Saggion, A. and Sahakian, V. and Saito, K. and Saito, T. and Sakaki, N. and Salazar, E. and Salini, A. and Sanchez, F. and Sanchez Conde, M. A. and Santangelo, Andrea and Santos, E. 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  title     = {Design concepts for the Cherenkov Telescope Array CTA an advanced facility for ground-based high-energy gamma-ray astronomy},
  series = {Experimental astronomy : an international journal on astronomical instrumentation and data analysis},
  volume    = {32},
  journal   = {Experimental astronomy : an international journal on astronomical instrumentation and data analysis},
  number    = {3},
  publisher = {Springer},
  address   = {Dordrecht},
  organization    = {CTA Consortium},
  issn      = {0922-6435},
  doi       = {10.1007/s10686-011-9247-0},
  pages     = {193 -- 316},
  year      = {2011},
  abstract  = {Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA.},
  language  = {en}
}
@article{EvansMurphyWhitmoreetal.2014,
  author    = {Evans, T. M. and Murphy, M. T. and Whitmore, J. B. and Misawa, T. and Centurion, Martin and Lopez, S. and Martins, C. J. A. P. and Molaro, P. and Petitjean, P. and Rahmani, H. and Srianand, R. and Wendt, Martin},
  title     = {The UVES Large Program for testing fundamental physics - III. Constraints on the fine-structure constant from three telescopes},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {445},
  journal   = {Monthly notices of the Royal Astronomical Society},
  number    = {1},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/stu1754},
  pages     = {128 -- 150},
  year      = {2014},
  language  = {en}
}
@article{RahmaniWendtSrianandetal.2013,
  author    = {Rahmani, H. and Wendt, Martin and Srianand, R. and Noterdaeme, P. and Petitjean, P. and Molaro, P. and Whitmore, J. B. and Murphy, M. T. and Centurion, Martin and Fathivavsari, H. and D'Odorico, S. and Evans, T. M. and Levshakov, S. A. and Lopez, S. and Martins, C. J. A. P. and Reimers, D. and Vladilo, G.},
  title     = {The UVES large program for testing fundamental physics - II. Constraints on a change in mu towards quasar HE 0027-1836},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {435},
  journal   = {Monthly notices of the Royal Astronomical Society},
  number    = {1},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/stt1356},
  pages     = {861 -- 878},
  year      = {2013},
  abstract  = {We present an accurate analysis of the H-2 absorption lines from the z(abs) similar to 2.4018 damped Ly alpha system towards HE 0027-1836 observed with the Very Large Telescope Ultraviolet and Visual Echelle Spectrograph (VLT/UVES) as a part of the European Southern Observatory Large Programme 'The UVES large programme for testing fundamental physics' to constrain the variation of proton-to-electron mass ratio, mu m(p)/m(e). We perform cross-correlation analysis between 19 individual exposures taken over three years and the combined spectrum to check the wavelength calibration stability. We notice the presence of a possible wavelength-dependent velocity drift especially in the data taken in 2012. We use available asteroids spectra taken with UVES close to our observations to confirm and quantify this effect. We consider single-and two-component Voigt profiles to model the observed H-2 absorption profiles. We use both linear regression analysis and Voigt profile fitting where Delta mu/mu is explicitly considered as an additional fitting parameter. The two-component model is marginally favoured by the statistical indicators and we get Delta mu/mu = -2.5 +/- 8.1(stat) +/- 6.2(sys) ppm. When we apply the correction to the wavelength-dependent velocity drift, we find Delta mu/mu = -7.6 +/- 8.1(stat) +/- 6.3(sys) ppm. It will be important to check the extent to which the velocity drift we notice in this study is present in UVES data used for previous Delta mu/mu measurements.},
  language  = {en}
}
@article{MolaroCenturionWhitmoreetal.2013,
  author    = {Molaro, P. and Centurion, Martin and Whitmore, J. B. and Evans, T. M. and Murphy, M. T. and Agafonova, I. I. and Bonifacio, P. and D'Odorico, S. and Levshakov, S. A. and Lopez, S. and Martins, C. J. A. P. and Petitjean, P. and Rahmani, H. and Reimers, D. and Srianand, R. and Vladilo, G. and Wendt, Martin},
  title     = {The UVES Large Program for testing fundamental physics I. Bounds on a change in alpha towards quasar HE 221-2818},
  series = {Astronomy and astrophysics : an international weekly journal},
  volume    = {555},
  journal   = {Astronomy and astrophysics : an international weekly journal},
  number    = {4},
  publisher = {EDP Sciences},
  address   = {Les Ulis},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361/201321351},
  pages     = {17},
  year      = {2013},
  abstract  = {Context. Absorption-line systems detected in quasar spectra can be used to compare the value of the fine-structure constant, alpha, measured today on Earth with its value in distant galaxies. In recent years, some evidence has emerged of small temporal and also spatial variations in alpha on cosmological scales. These variations may reach a fractional level of approximate to 10 ppm (parts per million). Aims. To test these claims we are conducting a Large Program of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high-resolution (R approximate to 60 000) and high signal-to-noise ratio (S/N approximate to 100) UVES spectra calibrated specifically for this purpose. Here we analyse the first complete quasar spectrum from this programme, that of HE 2217-2818. Methods. We applied the many multiplet method to measure alpha in five absorption systems towards this quasar: z(abs) = 0.7866, 0.9424, 1.5558, 1.6279, and 1.6919. Results. The most precise result is obtained for the absorber at z(abs) = 1.6919 where 3 Fe II transitions and Al II lambda 1670 have high S/N and provide a wide range of sensitivities to alpha. The absorption profile is complex with several very narrow features, and it requires 32 velocity components to be fitted to the data. We also conducted a range of tests to estimate the systematic error budget. Our final result for the relative variation in alpha in this system is Delta alpha/alpha = +1.3 +/- 2.4(stat) +/- 1.0(sys) ppm. This is one of the tightest current bounds on alpha-variation from an individual absorber. A second, separate approach to the data reduction, calibration, and analysis of this system yielded a slightly different result of -3.8 +/- 2.1(stat) ppm, possibly suggesting a larger systematic error component than our tests indicated. This approach used an additional 3 Fe II transitions, parts of which were masked due to contamination by telluric features. Restricting this analysis to the Fe II transitions alone and using a modified absorption profile model gave a result that is consistent with the first approach, Delta alpha/alpha = +1.1 +/- 2.6(stat) ppm. The four other absorbers have simpler absorption profiles, with fewer and broader features, and offer transitions with a narrower range of sensitivities to alpha. They therefore provide looser bounds on Delta alpha/alpha at the greater than or similar to 10 ppm precision level. Conclusions. The absorbers towards quasar HE 2217-2818 reveal no evidence of any variation in alpha at the 3-ppm precision level (1 sigma confidence). If the recently reported 10-ppm dipolar variation in alpha across the sky is correct, the expectation at this sky position is (3.2-5.4) +/- 1.7 ppm depending on dipole model used. Our constraint of Delta alpha/alpha = +1.3 +/- 2.4(stat) +/- 1.0(sys) ppm is not inconsistent with this expectation.},
  language  = {en}
}
@article{BonifacioRahmaniWhitmoreetal.2014,
  author    = {Bonifacio, P. and Rahmani, H. and Whitmore, J. B. and Wendt, Martin and Centurion, Martin and Molaro, P. and Srianand, R. and Murphy, M. T. and Petitjean, P. and Agafonova, I. I. and Evans, T. M. and Levshakov, S. A. and Lopez, S. and Martins, C. J. A. P. and Reimers, D. and Vladilo, G.},
  title     = {Fundamental constants and high-resolution spectroscopy},
  series = {Astronomische Nachrichten = Astronomical notes},
  volume    = {335},
  journal   = {Astronomische Nachrichten = Astronomical notes},
  number    = {1},
  publisher = {Wiley-VCH},
  address   = {Weinheim},
  issn      = {0004-6337},
  doi       = {10.1002/asna.201312005},
  pages     = {83 -- 91},
  year      = {2014},
  language  = {en}
}
@article{BoucheFinleySchroetteretal.2016,
  author    = {Bouche, Nicolas and Finley, H. and Schroetter, I. and Murphy, M. T. and Richter, Philipp and Bacon, Roland and Contini, Thierry and Richard, J. and Wendt, Martin and Kamann, S. and Epinat, Benoit and Cantalupo, Sebastiano and Straka, Lorrie A. and Schaye, Joop and Martin, C. L. and Peroux, C. and Wisotzki, Lutz and Soto, K. and Lilly, S. and Carollo, C. M. and Brinchmann, Jarle and Kollatschny, W.},
  title     = {POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z similar to 1 GALAXY-QUASAR PAIR TOWARD SDSS J1422-0001},
  series = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  volume    = {820},
  journal   = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0004-637X},
  doi       = {10.3847/0004-637X/820/2/121},
  pages     = {1872 -- 1882},
  year      = {2016},
  abstract  = {We use a background quasar to detect the presence of circumgalactic gas around a z = 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7 +/- 2.0. M-circle dot yr(-1), with no companion down to 0.22 M-circle dot yr(-1) (5 sigma) within 240 h(-1) kpc ("30"). Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle alpha of only 15 degrees), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold-flow disk" extending at least 12 kpc (3 x R-1/2). We estimate the mass accretion rate M-in to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H (I) column density of log N-H (I)/cm(-2) similar or equal to 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the low-ionization lines (e.g., Zn II, Cr II, Ti II, MnII, Si II), the accreting material appears to be enriched to about 0.4 Z(circle dot) (albeit with large uncertainties: log Z/Z(circle dot) = -0.4 +/- 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 +/- 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II* emission.},
  language  = {en}
}
@article{CrightonProchaskaMurphyetal.2019,
  author    = {Crighton, Neil H. M. and Prochaska, J. Xavier and Murphy, Michael T. and Worseck, Gabor and Smith, Britton D.},
  title     = {Imprints of the first billion years},
  series = {Monthly notices of the Royal Astronomical Society},
  volume    = {482},
  journal   = {Monthly notices of the Royal Astronomical Society},
  number    = {2},
  publisher = {Oxford Univ. Press},
  address   = {Oxford},
  issn      = {0035-8711},
  doi       = {10.1093/mnras/sty2762},
  pages     = {1456 -- 1470},
  year      = {2019},
  abstract  = {Lyman limit systems (LLSs) trace the low-density circumgalactic medium and the most dense regions of the intergalactic medium, so their number density and evolution at high-redshift, just after reionization, are important to constrain. We present a survey for LLSs at high redshifts, z(LLS) = 3.5-5.4, in the homogeneous data set of 153 optical quasar spectra at z similar to 5 from the Giant Gemini GMOS survey. Our analysis includes detailed investigation of survey biases using mock spectra which provide important corrections to the raw measurements. We estimate the incidence of LLSs per unit redshift at z approximate to 4.4 to be l(z) = 2.6 +/- 0.4. Combining our results with previous surveys at z(LLS) < 4, the best-fit power-law evolution is l(z) = l(*)[(1 + z)/4](alpha) with l* = 1.46 +/- 0.11 and alpha = 1.70 +/- 0.22 (68 per cent confidence intervals). Despite hints in previous z(LLS) < 4 results, there is no indication for a deviation from this single power-law soon after reionization. Finally, we integrate our new results with previous surveys of the intergalactic and circumgalactic media to constrain the hydrogen column density distribution function, f(N-HI, X), over 10 orders ofmagnitude. The data at z similar to 5 are not well-described by the f(N-HI, X) model previously reported for z similar to 2-3 (after re-scaling) and a 7-pivot model fitting the full z similar to 2-5 data set is statistically unacceptable. We conclude that there is significant evolution in the shape of f(N-HI, X) over this similar to 2-billion-year period.},
  language  = {en}
}
@article{RichterKrauseFechneretal.2011,
  author    = {Richter, Philipp and Krause, F. and Fechner, Cora and Charlton, Jane C. and Murphy, M. T.},
  title     = {The neutral gas extent of galaxies as derived from weak intervening Ca II absorbers},
  series = {Astronomy and astrophysics : an international weekly journal},
  volume    = {528},
  journal   = {Astronomy and astrophysics : an international weekly journal},
  number    = {4},
  publisher = {EDP Sciences},
  address   = {Les Ulis},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361/201015566},
  pages     = {22},
  year      = {2011},
  abstract  = {We present a systematic study of weak intervening CaII absorbers at low redshift (z < 0.5), based on the analysis of archival high-resolution (R >= 45 000) optical spectra of 304 quasars and active galactic nuclei observed with VLT/UVES. Along a total redshift path of Delta z approximate to 100 we detected 23 intervening CaII absorbers in both the CaII H \& K lines, with rest frame equivalent widths W-r,W-3934 = 15-799 m angstrom and column densities log N(CaII) = 11.25-13.04 (obtained by fitting Voigt-profile components). We obtain a bias-corrected number density of weak intervening CaII absorbers of dN/dz = 0.117 +/- 0.044 at < z(abs)> = 0.35 for absorbers with log N(CaII) >= 11.65 (W-r,W-3934 >= 32 m angstrom). This is similar to 2.6 times the value obtained for damped Lyman alpha absorbers (DLAs) at low redshift. All CaII absorbers in our sample show associated absorption by other low ions such as MgII and FeII; 45 percent of them have associated NaI absorption. From ionization modelling we conclude that intervening CaII absorption with log N(CaII) >= 11.5 arises in DLAs, sub-DLAs and Lyman-limit systems (LLS) at HI column densities of log N(HI) >= 17.4. Using supplementary HI information for nine of the absorbers we find that the CaII/HI ratio decreases strongly with increasing HI column density, indicating a column-density-dependent dust depletion of Ca. The observed column density distribution function of CaII absorption components follows a relatively steep power law, f(N) proportional to N-beta, with a slope of -beta = -1.68, which again points towards an enhanced dust depletion in high column density systems. The relatively large cross section of these absorbers together with the frequent detection of CaII absorption in high-velocity clouds (HVCs) in the halo of the Milky Way suggests that a considerable fraction of the intervening CaII systems trace (partly) neutral gas structures in the halos and circumgalactic environment of galaxies (i.e., they are HVC analogs). Based on the recently measured detection rate of CaII absorption in the Milky Way HVCs we estimate that the mean (projected) CaII covering fraction of galaxies and their gaseous halos is < f(c,CaII)> = 0.33. Using this value and considering all galaxies with luminosities L >= 0.05 L-star we calculate that the characteristic radial extent of (partly) neutral gas clouds with log N(HI) >= 17.4 around low-redshift galaxies is R-HVC approximate to 55 kpc.},
  language  = {en}
}
@article{BenBekhtiWinkelRichteretal.2012,
  author    = {Ben Bekhti, Nadya and Winkel, B. and Richter, P. and Kerp, J. and Klein, U. and Murphy, M. T.},
  title     = {An absorption-selected survey of neutral gas in the Milky Way halo New results based on a large sample of Ca II, Na I, and H I spectra towards QSOs},
  series = {Astronomy and astrophysics : an international weekly journal},
  volume    = {542},
  journal   = {Astronomy and astrophysics : an international weekly journal},
  number    = {2},
  publisher = {EDP Sciences},
  address   = {Les Ulis},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361/201118673},
  pages     = {17},
  year      = {2012},
  abstract  = {Aims. We aim at analysing systematically the distribution and physical properties of neutral and mildly ionised gas in the Milky Way halo, based on a large absorption-selected data set. Methods. Multi-wavelength studies were performed combining optical absorption line data of Ca II and Na I with follow-up H I 21-cm emission line observations along 408 sight lines towards low-and high-redshift QSOs. We made use of archival optical spectra obtained with UVES/VLT. H I data were extracted from the Effelsberg-Bonn H I survey and the Galactic All-Sky survey. For selected sight lines we obtained deeper follow-up observations using the Effelsberg 100-m telescope. Results. Ca II (Na I) halo absorbers at intermediate and high radial velocities are present in 40-55\% (20-35\%) of the sightlines, depending on the column density threshold chosen. Many halo absorbers show multi-component absorption lines, indicating the presence of sub-structure. In 65\% of the cases, absorption is associated with H I 21-cm emission. The Ca II (Na I) column density distribution function follows a power-law with a slope of beta approximate to -2.2 (-1.4). Conclusions. Our absorption-selected survey confirms our previous results that the Milky Way halo is filled with a large number of neutral gas structures whose high column density tail represents the population of common H I high-and intermediate-velocity clouds seen in 21-cm observations. We find that Na I/Ca II column density ratios in the halo absorbers are typically smaller than those in the Milky Way disc, in the gas in the Magellanic Clouds, and in damped Lyman a systems. The small ratios (prominent in particular in high-velocity components) indicate a lower level of Ca depletion onto dust grains in Milky Way halo absorbers compared to gas in discs and inner regions of galaxies.},
  language  = {en}
}