TY  - JOUR
A1  - Bersier, David
A1  - Fruchter, Andrew S.
A1  - Strolger, Louis-Gregory
A1  - Gorosabel, Javier
A1  - Levan, Andrew
A1  - Burud, Ingunn
A1  - Rhoads, James E.
A1  - Becker, Andrew C.
A1  - Cassan, Andrew C.
A1  - Chornock, Ryan
A1  - Covino, Stefano
A1  - De Jong, Roelof S.
A1  - Dominis, Dijana
A1  - Filippenko, Alexei V.
A1  - Hjorth, Jens
A1  - Holmberg, Johan
A1  - Malesani, Daniele
A1  - Mobasher, Bahram
A1  - Olsen, Kurt A. G.
A1  - Stefanon, Mauro
A1  - Castro Cerón, José María C.
A1  - Fynbo, Johan P. U.
A1  - Holland, Stephen T.
A1  - Kouveliotou, Chryssa
A1  - Pedersen, Hans-Georg
A1  - Tanvir, Nieal R.
A1  - Woosley, S. E.
T1  - Evidence for a supernova associated with the X-ray flash 020903
N2  - We present ground-based and Hubble Space Telescope optical observations of the X-ray flash ( XRF) 020903, covering 300 days. The afterglow showed a very rapid rise in the first day, followed by a relatively slow decay in the next few days. There was a clear bump in the light curve after similar to 25 days, accompanied by a drastic change in the spectral energy distribution. The light curve and the spectral energy distribution are naturally interpreted as describing the emergence and subsequent decay of a supernova ( SN), similar to SN 1998bw. At peak luminosity, the SN is estimated to be 0.8 +/- 0.1 mag fainter than SN 1998bw. This argues in favor of the existence of a SN associated with this XRF. A spectrum obtained 35 days after the burst shows emission lines from the host galaxy. We use this spectrum to put an upper limit on the oxygen abundance of the host at [O/H] <= 0.6 dex. We also discuss a possible trend between the softness of several bursts and the early behavior of the optical afterglow, in the sense that XRFs and X-ray-rich gamma- ray bursts ( GRBs) seem to have a plateau phase or even a rising light curve. This can be naturally explained in models in which XRFs are similar to GRBs but are seen off the jet axis.
Y1  - 2006
UR  - http://iopscience.iop.org/0004-637X/
U6  - https://doi.org/10.1086/502640
SN  - 0004-637X
ER  - 
TY  - JOUR
A1  - Courbin, F.
A1  - Letawe, G.
A1  - Magain, P.
A1  - Wisotzki, Lutz
A1  - Jablonka, P.
A1  - Jahnke, Knud
A1  - Kuhlbrodt, B.
A1  - Alloin, Danielle
A1  - Meylan, G.
A1  - Minniti, D.
A1  - Burud, Ingunn
T1  - On-axis spatially resolved spectroscopy of low redshift quasar host galaxies: HE 1503+0228, at z=0.135
N2  - We present the first result of a comprehensive spectroscopic study of quasar host galaxies. On-axis, spatially resolved spectra of low redshift quasars have been obtained with FORS1, mounted on the 8.2 m ESO Very Large Telescope, Antu. The spectra are spatially deconvolved using a spectroscopic version of the ``MCS deconvolution algorithm''. The algorithm decomposes two dimensional spectra into the individual spectra of the central point-like nucleus and of its host galaxy. Applied to HE 1503+0228 at z=0.135 (MB=-23.0), it provides us with the spectrum of the host galaxy between 3600 Å and 8500 Å (rest-frame), at a mean resolving power of 700. The data allow us to measure several of the important Lick indices. The stellar populations and gas ionization state of the host galaxy of HE 1503+0228 are very similar to the ones measured for normal non-AGN galaxies. Dynamical information is also available for the gas and stellar components of the galaxy. Using deconvolution and a deprojection algorithm, velocity curves are derived for emission lines, from the center up to 4arcsec away from the nucleus of the galaxy. Fitting a simple three- components mass model (point mass, spherical halo of dark matter, disk) to the position-velocity diagram, we infer a mass of M(r<1 kpc) = (2.0 +/- 0.3)x 1010 Msun within the central kiloparsec of the galaxy, and a mass integrated over 10 kpc of M(r<10 kpc) = (1.9 +/- 0.3) x 1011 Msun, with an additional 10% error due to the uncertainty on the inclination of the galaxy. This, in combination with the analysis of the stellar populations indicates that the host galaxy of HE 1503+0228, is a normal spiral galaxy. Based on observations made with ANTU/UT1 at ESO-Paranal observatory in Chile (program 65.P-0361(A)), and with the ESO 3.5 m NTT, at La Silla observatory (program 62.P-0643(B)).
Y1  - 2002
ER  - 
TY  - JOUR
A1  - Courbin, F.
A1  - Letawe, G.
A1  - Magain, P.
A1  - Wisotzki, Lutz
A1  - Jablonka, P.
A1  - Jahnke, Knud
A1  - Kuhlbrodt, B.
A1  - Alloin, Danielle
A1  - Meylan, G.
A1  - Minniti, D.
A1  - Burud, Ingunn
T1  - On-axis spatially resolved spectroscopy of low redshift quasar host galaxies: HE 1503+0228, at z=0.135
N2  - We present the first result of a comprehensive spectroscopic study of quasar host galaxies. On-axis, spatially resolved spectra of low redshift quasars have been obtained with FORS1, mounted on the 8.2 m ESO Very Large Telescope, Antu. The spectra are spatially deconvolved using a spectroscopic version of the ``MCS deconvolution algorithm''. The algorithm decomposes two dimensional spectra into the individual spectra of the central point-like nucleus and of its host galaxy. Applied to HE 1503+0228 at z=0.135 (MB=-23.0), it provides us with the spectrum of the host galaxy between 3600 Å and 8500 Å (rest-frame), at a mean resolving power of 700. The data allow us to measure several of the important Lick indices. The stellar populations and gas ionization state of the host galaxy of HE 1503+0228 are very similar to the ones measured for normal non-AGN galaxies. Dynamical information is also available for the gas and stellar components of the galaxy. Using deconvolution and a deprojection algorithm, velocity curves are derived for emission lines, from the center up to 4arcsec away from the nucleus of the galaxy. Fitting a simple three-components mass model (point mass, spherical halo of dark matter, disk) to the position-velocity diagram, we infer a mass of M(r<1 kpc) = (2.0 +/- 0.3)x 1010 Msun within the central kiloparsec of the galaxy, and a mass integrated over 10 kpc of M(r<10 kpc) = (1.9 +/- 0.3) x 1011 Msun, with an additional 10 % error due to the uncertainty on the inclination of the galaxy. This, in combination with the analysis of the stellar populations indicates that the host galaxy of HE 1503+0228, is a normal spiral galaxy. Based on observations made with ANTU/UT1 at ESO-Paranal observatory in Chile (program 65.P-0361(A)), and with the ESO 3.5 m NTT, at La Silla observatory (program 62.P-0643(B)).
Y1  - 2002
ER  -