GRB 020813

Polarization in the case of a smooth optical decay

J. Gorosabel, E. Rol, S. Covino, A. J. Castro-Tirado, J. M Castro Cerón, D. Lazzati, J. Hjorth, D. Malesani, M. Della Valle, S. Di Serego Alighieri, F. Fiore, A. S. Fruchter, J. P U Fynbo, G. Ghisellini, P. Goldoni, J. Greiner, G. L. Israel, L. Kaper, N. Kawai, S. Klose & 19 others C. Kouveliotou, E. Le Floc'h, N. Masetti, F. Mirabel, P. Møller, S. Ortolani, E. Palazzi, E. Pian, J. Rhoads, G. Ricker, P. Saracco, L. Stella, G. Tagliaferri, N. Tanvir, E. Van Den Heuvel, M. Vietri, P. M. Vreeswijk, R. A M J Wijers, F. M. Zerbi

Research output: Contribution to journalArticle

19 Citations (Scopus)

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 (θ) resulting from our campaign are 〈P〉 = 1.18 ± 0.10% and 〈θ〉 = 148.7° ± 23°, 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 θ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant θ rotation respect to the Keck spectropolarimetric observations performed ∼0.25 days after the GRB (Barth et al. 2003). However, 〈P〉 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 < tbreak.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 9 might be related to the smoothness of the light curve.

Original languageEnglish (US)
Pages (from-to)113-119
Number of pages7
JournalAstronomy and Astrophysics
Volume422
Issue number1
DOIs
StatePublished - Jul 2004
Externally publishedYes

Fingerprint

extremely high frequencies
light curve
polarization
linear polarization
night
decay
afterglows
gamma rays
monitoring

Keywords

  • Gamma rays: bursts
  • Techniques: photometric
  • Techniques: polarimetric

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Gorosabel, J., Rol, E., Covino, S., Castro-Tirado, A. J., Cerón, J. M. C., Lazzati, D., ... Zerbi, F. M. (2004). GRB 020813: Polarization in the case of a smooth optical decay. Astronomy and Astrophysics, 422(1), 113-119. https://doi.org/10.1051/0004-6361:20034409

GRB 020813 : Polarization in the case of a smooth optical decay. / Gorosabel, J.; Rol, E.; Covino, S.; Castro-Tirado, A. J.; Cerón, J. M Castro; Lazzati, D.; Hjorth, J.; Malesani, D.; Della Valle, M.; Di Serego Alighieri, S.; Fiore, F.; Fruchter, A. S.; Fynbo, J. P U; Ghisellini, G.; Goldoni, P.; Greiner, J.; Israel, G. L.; Kaper, L.; Kawai, N.; Klose, S.; Kouveliotou, C.; Le Floc'h, E.; Masetti, N.; Mirabel, F.; Møller, P.; Ortolani, S.; Palazzi, E.; Pian, E.; Rhoads, J.; Ricker, G.; Saracco, P.; Stella, L.; Tagliaferri, G.; Tanvir, N.; Van Den Heuvel, E.; Vietri, M.; Vreeswijk, P. M.; Wijers, R. A M J; Zerbi, F. M.

In: Astronomy and Astrophysics, Vol. 422, No. 1, 07.2004, p. 113-119.

Research output: Contribution to journalArticle

Gorosabel, J, Rol, E, Covino, S, Castro-Tirado, AJ, Cerón, JMC, Lazzati, D, Hjorth, J, Malesani, D, Della Valle, M, Di Serego Alighieri, S, Fiore, F, Fruchter, AS, Fynbo, JPU, Ghisellini, G, Goldoni, P, Greiner, J, Israel, GL, Kaper, L, Kawai, N, Klose, S, Kouveliotou, C, Le Floc'h, E, Masetti, N, Mirabel, F, Møller, P, Ortolani, S, Palazzi, E, Pian, E, Rhoads, J, Ricker, G, Saracco, P, Stella, L, Tagliaferri, G, Tanvir, N, Van Den Heuvel, E, Vietri, M, Vreeswijk, PM, Wijers, RAMJ & Zerbi, FM 2004, 'GRB 020813: Polarization in the case of a smooth optical decay', Astronomy and Astrophysics, vol. 422, no. 1, pp. 113-119. https://doi.org/10.1051/0004-6361:20034409
Gorosabel J, Rol E, Covino S, Castro-Tirado AJ, Cerón JMC, Lazzati D et al. GRB 020813: Polarization in the case of a smooth optical decay. Astronomy and Astrophysics. 2004 Jul;422(1):113-119. https://doi.org/10.1051/0004-6361:20034409
Gorosabel, J. ; Rol, E. ; Covino, S. ; Castro-Tirado, A. J. ; Cerón, J. M Castro ; Lazzati, D. ; Hjorth, J. ; Malesani, D. ; Della Valle, M. ; Di Serego Alighieri, S. ; Fiore, F. ; Fruchter, A. S. ; Fynbo, J. P U ; Ghisellini, G. ; Goldoni, P. ; Greiner, J. ; Israel, G. L. ; Kaper, L. ; Kawai, N. ; Klose, S. ; Kouveliotou, C. ; Le Floc'h, E. ; Masetti, N. ; Mirabel, F. ; Møller, P. ; Ortolani, S. ; Palazzi, E. ; Pian, E. ; Rhoads, J. ; Ricker, G. ; Saracco, P. ; Stella, L. ; Tagliaferri, G. ; Tanvir, N. ; Van Den Heuvel, E. ; Vietri, M. ; Vreeswijk, P. M. ; Wijers, R. A M J ; Zerbi, F. M. / GRB 020813 : Polarization in the case of a smooth optical decay. In: Astronomy and Astrophysics. 2004 ; Vol. 422, No. 1. pp. 113-119.
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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 (θ) resulting from our campaign are 〈P〉 = 1.18 ± 0.10{\%} and 〈θ〉 = 148.7° ± 23°, 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 θ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant θ rotation respect to the Keck spectropolarimetric observations performed ∼0.25 days after the GRB (Barth et al. 2003). However, 〈P〉 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 < tbreak.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 9 might be related to the smoothness of the light curve.",
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author = "J. Gorosabel and E. Rol and S. Covino and Castro-Tirado, {A. J.} and Cer{\'o}n, {J. M Castro} and D. Lazzati and J. Hjorth and D. Malesani and {Della Valle}, M. and {Di Serego Alighieri}, S. and F. Fiore and Fruchter, {A. S.} and Fynbo, {J. P U} and G. Ghisellini and P. Goldoni and J. Greiner and Israel, {G. L.} and L. Kaper and N. Kawai and S. Klose and C. Kouveliotou and {Le Floc'h}, E. and N. Masetti and F. Mirabel and P. M{\o}ller and S. Ortolani and E. Palazzi and E. Pian and J. Rhoads and G. Ricker and P. Saracco and L. Stella and G. Tagliaferri and N. Tanvir and {Van Den Heuvel}, E. and M. Vietri and Vreeswijk, {P. M.} and Wijers, {R. A M J} and Zerbi, {F. M.}",
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TY - JOUR

T1 - GRB 020813

T2 - Polarization in the case of a smooth optical decay

AU - Gorosabel, J.

AU - Rol, E.

AU - Covino, S.

AU - Castro-Tirado, A. J.

AU - Cerón, J. M Castro

AU - Lazzati, D.

AU - Hjorth, J.

AU - Malesani, D.

AU - Della Valle, M.

AU - Di Serego Alighieri, S.

AU - Fiore, F.

AU - Fruchter, A. S.

AU - Fynbo, J. P U

AU - Ghisellini, G.

AU - Goldoni, P.

AU - Greiner, J.

AU - Israel, G. L.

AU - Kaper, L.

AU - Kawai, N.

AU - Klose, S.

AU - Kouveliotou, C.

AU - Le Floc'h, E.

AU - Masetti, N.

AU - Mirabel, F.

AU - Møller, P.

AU - Ortolani, S.

AU - Palazzi, E.

AU - Pian, E.

AU - Rhoads, J.

AU - Ricker, G.

AU - Saracco, P.

AU - Stella, L.

AU - Tagliaferri, G.

AU - Tanvir, N.

AU - Van Den Heuvel, E.

AU - Vietri, M.

AU - Vreeswijk, P. M.

AU - Wijers, R. A M J

AU - Zerbi, F. M.

PY - 2004/7

Y1 - 2004/7

N2 - 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 (θ) resulting from our campaign are 〈P〉 = 1.18 ± 0.10% and 〈θ〉 = 148.7° ± 23°, 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 θ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant θ rotation respect to the Keck spectropolarimetric observations performed ∼0.25 days after the GRB (Barth et al. 2003). However, 〈P〉 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 < tbreak.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 9 might be related to the smoothness of the light curve.

AB - 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 (θ) resulting from our campaign are 〈P〉 = 1.18 ± 0.10% and 〈θ〉 = 148.7° ± 23°, 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 θ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant θ rotation respect to the Keck spectropolarimetric observations performed ∼0.25 days after the GRB (Barth et al. 2003). However, 〈P〉 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 < tbreak.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 9 might be related to the smoothness of the light curve.

KW - Gamma rays: bursts

KW - Techniques: photometric

KW - Techniques: polarimetric

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