Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/25898
 Title: GRB 020813: Polarization in the case of a smooth optical decay Authors: Gorosabel, J.Castro-Tirado, A. J.Gorosabel, J.Cerón, J. M. C.Fruchter, A. S.Rhoads, J.Rol, E.Kaper, L.Van Den Heuvel EWijers, R. A. M. J.Covino, S.Ghisellini, G.Saracco, P.Tagliaferri, G.Zerbi, F. M.Lazzati, D.Hjorth, J.Malesani, D.Della Valle MDi Serego Alighieri SFiore, F.Israel, G. L.Stella, L.Fynbo, J. P. U.Goldoni, P.Le Floc'h EMirabel, F.Greiner, J.Kawai, N.Klose, S.Kouveliotou, C.Masetti, N.Palazzi, E.Møller, P.Ortolani, S.Pian, E.Ricker, G.Tanvir, N.Vietri, M.Vreeswijk, P. M. First Published: Jul-2004 Publisher: EDP Sciences for European Southern Observatory (ESO) Citation: Astronomy & Astrophysics, 2004, 422 (1), pp. 113-119 Abstract: We present the results of a VLT polarimetric monitoring campaign of the GRB 020813 optical afterglow carried out in three nights, from 0.88 to 4.20 days after the gamma-ray event. The mean values of the degree of linear polarization ( P) and its position angle ( $\theta$) resulting from our campaign are $\langle P\rangle=1.18 \pm 0.10 \%$ and $\langle \theta\rangle = 148.7^{\circ} \pm 2.3^{\circ}$ , after correcting for Galactic interstellar polarization. Our VLT data set is most naturally described by a constant degree of linear polarization and position angle, nonetheless a slow $\theta$ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant $\theta$ rotation respect to the Keck spectropolarimetric observations performed ~0.25 days after the GRB (Barth et al. 2003). However, $\langle P\rangle$ is a factor of two lower than the polarization degree measured from Keck. Additionally, the VLT polarization data allowed us to construct an accurate V-band light curve. The V-band photometric data revealed a smooth light curve with a break located between the last Keck and our first VLT polarimetric measurement, $0.33 < t_{{\rm break}, V} < 0.88$ days after the GRB. The typical magnitude fluctuations of the VLT V-band lightcurve are 0.003 mag, 0.010 mag and 0.016 mag for our three observing nights, respectively. We speculate that the stability of $\theta$ might be related to the smoothness of the light curve. DOI Link: 10.1051/0004-6361:20034409 ISSN: 0004-6361 Links: http://hdl.handle.net/2381/25898http://www.aanda.org/articles/aa/abs/2004/28/aa0409/aa0409.html Version: Publisher Version Status: Peer-reviewed Type: Journal Article Rights: Copyright © 2004 ESO. Reproduced with permission from Astronomy & Astrophysics, © ESO. Appears in Collections: Published Articles, Dept. of Physics and Astronomy

Files in This Item:
File Description SizeFormat