Preprint Logo P4 March
1997


To be published in:
Astrophysical Journal

HST confirmation of the lensed quasar J03.13+

J. Surdej1,*, J.-F. Claeskens1,**, M. Remy1, S. Refsdal2, B. Pirenne3, A. Prieto4, Ch Vanderriest5


1 Institut d'Astrophysique et de Géophysique - Université de Liège, Avenue de Cointe 5, 4000 Liège, Belgium
2 Hamburger Sternwarte, Gojenbergsweg 112, D-21029, Germany
3 ST-ECF, c/o ESO, Karl-Schwarzschild Str. 2, D-85748 Garching bei München, Germany
4 MPI für Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching bei München, Germany
5 Observatoire de Meudon, Place Jules Janssen 5, F-92195 Meudon PRINCIPAL CEDEX

* Directeur de Recherches FNRS, Belgium
** Aspirant FNRS, Belgium

+ Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS 5-26555.


Abstract

     In order to definitively prove the claim by Claeskens et al. (1996) that J03.13 is a doubly imaged quasar, WFPC2 direct imaging and FOS spectroscopy of this compact system have been obtained with HST. These textbook case observations clearly show that J03.13 consists of two point-like images separated by 0.849" ± 0.001" with a magnitude difference of 2.14 ± 0.03 in V and I. We see no trace of a lensing galaxy. From the FOS observations, we find that J03.13 A and B have identical spectra within the measurement uncertainties. The data also show that spectroscopic contamination of B by A is negligible. We do confirm the redshift z = 2.545 for J03.13 A and B (emission-lines due to Ly- 1025 and OVI 1031, 1037 are also detected), first derived from an unresolved groud-based spectrum of the two components by Claeskens et al. We also find that the absorption line system at z = 2.344 (CIV and Ly-) is present in the spectra of A and B. On the contrary, the absorption line system at z = 1.085 (MgII) is only present in the spectrum of J03.13 A. if this latter system is associated with the lens, we may expect that image A consists of two radially merging images with a very small angular separation. From the WFPC2 imagery, we can rule out the presence of a third component fainter than A by up to 5.2 mag. with an angular separation 0.13".

Key Words
gravitational lensing - quasars: individual: J03.13 - Techniques: image processing

Files
Article: hstj03.ps.gz (59339 bytes): HTTP FTP (ftp://vela.astro.ulg.ac.be/preprints/)


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