@article{HeinmuellerPetitjeanLedouxetal.2006,
  author    = {Heinm{\"u}ller, Janine and Petitjean, Patrick and Ledoux, Cedric and Caucci, Sara and Srianand, Raghunathan},
  title     = {Kinematics and star formation activity in the z(abs)=2.03954 damped Lyman-alpha system towards PKS 0458-020},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361:20053910},
  year      = {2006},
  abstract  = {We present UVES observations of the log N(H I) = 21.7 damped Lyman-alpha system at z(abs) = 2.03954 towards the quasar PKS 0458-020. Hi Lyman-alpha emission is detected in the center of the damped Lyman-alpha absorption trough. Metallicities are derived for Mg II, Si II, P II, Cr II, Mn II, Fe II and Zn II and are found to be -1.21 +/- 0.12, - 1.28 +/- 0.20, -1.54 +/- 0.11, -1.66 +/- 0.10, -2.05 +/- 0.11, -1.87 +/- 0.11, -1.22 +/- 0.10, respectively, relative to solar. The depletion factor is therefore of the order of [Zn/Fe] = 0.65. We observe metal absorption lines to be blueshifted compared to the Lyman-alpha emission up to a maximum of similar to 100 and 200 km s(-1) for low and high- ionization species respectively. This can be interpreted either as the consequence of rotation in a large (similar to 7 kpc) disk or as the imprint of a galactic wind. The star formation rate (SFR) derived from the Lyman-alpha emission, 1.6 M-circle dot yr(-1), is compared with that estimated from the observed C II* absorption. No molecular hydrogen is detected in our data, yielding a molecular fraction log f < -6.52. This absence of H-2 can be explained as the consequence of a high ambient UV flux which is one order of magnitude larger than the radiation field in the ISM of our Galaxy and originates in the observed emitting region},
  language  = {en}
}
@article{KubasCassanBeaulieuetal.2005,
  author    = {Kubas, Daniel and Cassan, A. and Beaulieu, Jean-Philippe and Coutures, C. and Dominik, M. and Albrow, Michael D. and Brillant, Stephane and Caldwell, John A. R. and Dominis, Dijana and Donatowicz, J. and Fendt, Christian and Fouque, P. and Jorgensen, Uffe Grae and Greenhill, John and Hill, K. and Heinm{\"u}ller, Janine and Horne, Keith and Kane, Stephen R. and Marquette, Jean-Baptiste and Martin, Ralph and Menzies, J. W. and Pollard, K. R. and Sahu, K. C. and Vinter, C. and Wambsganss, Joachim and Watson, R. and Williams, A. and Thurl, C.},
  title     = {Full characterization of binary-lens event OGLE-2002-BLG-069 from PLANET observations},
  issn      = {0004-6361},
  year      = {2005},
  abstract  = {We analyze the photometric data obtained by PLANET and OGLE on the caustic-crossing binary-lens microlensing event OGLE-2002-BLG-069. Thanks to the excellent photometric and spectroscopic coverage of the event, we are able to constrain the lens model up to the known ambiguity between close and wide binary lenses. The detection of annual parallax in combination with measurements of extended-source effects allows us to determine the mass, distance and velocity of the lens components for the competing models. While the model involving a close binary lens leads to a Bulge- Disc lens scenario with a lens mass of M = (0.51 ± 0.15) M-\&ODOT; and distance of D-L = (2.9 ± 0.4) kpc, the wide binary lens solution requires a rather implausible binary black-hole lens ( M \&GSIM; 126 M-\&ODOT;). Furthermore we compare current state-of-the-art numerical and empirical models for the surface brightness profile of the source, a G5III Bulge giant. We find that a linear limb-darkening model for the atmosphere of the source star is consistent with the data whereas a PHOENIX atmosphere model assuming LTE and with no free parameter does not match our observations},
  language  = {en}
}
@article{WisotzkiSchechterBradtetal.2002,
  author    = {Wisotzki, Lutz and Schechter, P. L. and Bradt, H. V. and Heinm{\"u}ller, Janine and Reimers, Dieter},
  title     = {HE 0435-1223 : a wide separation quadruple QSO and gravitational lens},
  year      = {2002},
  abstract  = {We report the discovery of a new gravitationally lensed QSO, at a redshift z = 1.689, with four QSO components in a cross-shaped arrangement around a bright galaxy. The maximum separation between images is 2farcs 6, enabling a reliable decomposition of the system. Three of the QSO components have g =~ 19.6, while component A is about 0.6 mag brighter. The four components have nearly identical colours, suggesting little if any dust extinction in the foreground galaxy. The lensing galaxy is prominent in the i band, weaker in r and not detected in g. Its spatial profile is that of an elliptical galaxy with a scale length of ~ 12 kpc. Combining the measured colours and a mass model for the lens, we estimate a most likely redshift range of 0.3 < z < 0.4. Predicted time delays between the components are la 10 days. The QSO shows evidence for variability, with total g band magnitudes of 17.89 and 17.71 for two epochs separated by ~ 2 months. However, the relative fluxes of the components did not change, indicating that the variations are intrinsic to the QSO rather than induced by microlensing. Based in part on observations obtained with the Baade 6.5-m telescope of the Magellan Consortium. Also based in part on observations collected at the European Southern Observatory, La Silla, Chile.},
  language  = {en}
}