Physics of the GRB 030328 afterglow and its environment

E. Maiorano, N. Masetti, E. Palazzi, S. Savaglio, E. Rol, P. M. Vreeswijk, E. Pian, P. A. Price, B. A. Peterson, M. Jelínek, L. Amati, M. I. Andersen, A. J. Castro-Tirado, J. M Castro Cerón, A. De Ugarte Postigo, F. Frontera, A. S. Fruchter, J. P U Fynbo, J. Gorosabel, A. A. HendenJ. Hjorth, B. L. Jensen, S. Klose, C. Kouveliotou, G. Masi, P. Møller, L. Nicastro, E. O. Ofek, S. B. Pandey, J. Rhoads, N. R. Tanvir, R. A M J Wijers, E. P J Van Den Heuvel

Research output: Contribution to journalArticle

13 Citations (Scopus)

Abstract

Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices α1 = 0.76 ± 0.03, α2 = 1.50 ±0.07 and a break at tb = 0.48 ±0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle θjet ∼ 3°.2. An achromatic bump starting around ∼0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-α Absorber. The optical V-band afterglow appears polarized, with P - (2.4 ±0.6)% and θ = 170° ± 7°, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope βopt = 0.47 ± 0.15, and an X-ray slope βx = 1.0 ± 0.2. Conclusions. The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium.

Original languageEnglish (US)
Pages (from-to)423-431
Number of pages9
JournalAstronomy and Astrophysics
Volume455
Issue number2
DOIs
StatePublished - Aug 2006
Externally publishedYes

Fingerprint

afterglows
gamma ray bursts
physics
homogeneous medium
spectroscopy
slopes
metal
monitoring
fireballs
extremely high frequencies
light curve
photometry
absorbers
x rays
telescopes
galaxies
expansion
decay
metals

Keywords

  • Cosmology: observations
  • Gamma rays: bursts
  • Line: identification
  • Radiation mechanisms: non-thermal

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Maiorano, E., Masetti, N., Palazzi, E., Savaglio, S., Rol, E., Vreeswijk, P. M., ... Van Den Heuvel, E. P. J. (2006). Physics of the GRB 030328 afterglow and its environment. Astronomy and Astrophysics, 455(2), 423-431. https://doi.org/10.1051/0004-6361:20054728

Physics of the GRB 030328 afterglow and its environment. / Maiorano, E.; Masetti, N.; Palazzi, E.; Savaglio, S.; Rol, E.; Vreeswijk, P. M.; Pian, E.; Price, P. A.; Peterson, B. A.; Jelínek, M.; Amati, L.; Andersen, M. I.; Castro-Tirado, A. J.; Cerón, J. M Castro; De Ugarte Postigo, A.; Frontera, F.; Fruchter, A. S.; Fynbo, J. P U; Gorosabel, J.; Henden, A. A.; Hjorth, J.; Jensen, B. L.; Klose, S.; Kouveliotou, C.; Masi, G.; Møller, P.; Nicastro, L.; Ofek, E. O.; Pandey, S. B.; Rhoads, J.; Tanvir, N. R.; Wijers, R. A M J; Van Den Heuvel, E. P J.

In: Astronomy and Astrophysics, Vol. 455, No. 2, 08.2006, p. 423-431.

Research output: Contribution to journalArticle

Maiorano, E, Masetti, N, Palazzi, E, Savaglio, S, Rol, E, Vreeswijk, PM, Pian, E, Price, PA, Peterson, BA, Jelínek, M, Amati, L, Andersen, MI, Castro-Tirado, AJ, Cerón, JMC, De Ugarte Postigo, A, Frontera, F, Fruchter, AS, Fynbo, JPU, Gorosabel, J, Henden, AA, Hjorth, J, Jensen, BL, Klose, S, Kouveliotou, C, Masi, G, Møller, P, Nicastro, L, Ofek, EO, Pandey, SB, Rhoads, J, Tanvir, NR, Wijers, RAMJ & Van Den Heuvel, EPJ 2006, 'Physics of the GRB 030328 afterglow and its environment', Astronomy and Astrophysics, vol. 455, no. 2, pp. 423-431. https://doi.org/10.1051/0004-6361:20054728
Maiorano E, Masetti N, Palazzi E, Savaglio S, Rol E, Vreeswijk PM et al. Physics of the GRB 030328 afterglow and its environment. Astronomy and Astrophysics. 2006 Aug;455(2):423-431. https://doi.org/10.1051/0004-6361:20054728
Maiorano, E. ; Masetti, N. ; Palazzi, E. ; Savaglio, S. ; Rol, E. ; Vreeswijk, P. M. ; Pian, E. ; Price, P. A. ; Peterson, B. A. ; Jelínek, M. ; Amati, L. ; Andersen, M. I. ; Castro-Tirado, A. J. ; Cerón, J. M Castro ; De Ugarte Postigo, A. ; Frontera, F. ; Fruchter, A. S. ; Fynbo, J. P U ; Gorosabel, J. ; Henden, A. A. ; Hjorth, J. ; Jensen, B. L. ; Klose, S. ; Kouveliotou, C. ; Masi, G. ; Møller, P. ; Nicastro, L. ; Ofek, E. O. ; Pandey, S. B. ; Rhoads, J. ; Tanvir, N. R. ; Wijers, R. A M J ; Van Den Heuvel, E. P J. / Physics of the GRB 030328 afterglow and its environment. In: Astronomy and Astrophysics. 2006 ; Vol. 455, No. 2. pp. 423-431.
@article{5056bf9d692e456095972e89159bf02f,
title = "Physics of the GRB 030328 afterglow and its environment",
abstract = "Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices α1 = 0.76 ± 0.03, α2 = 1.50 ±0.07 and a break at tb = 0.48 ±0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle θjet ∼ 3°.2. An achromatic bump starting around ∼0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-α Absorber. The optical V-band afterglow appears polarized, with P - (2.4 ±0.6){\%} and θ = 170° ± 7°, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope βopt = 0.47 ± 0.15, and an X-ray slope βx = 1.0 ± 0.2. Conclusions. The discussion of the results in the context of the {"}fireball model{"} shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium.",
keywords = "Cosmology: observations, Gamma rays: bursts, Line: identification, Radiation mechanisms: non-thermal",
author = "E. Maiorano and N. Masetti and E. Palazzi and S. Savaglio and E. Rol and Vreeswijk, {P. M.} and E. Pian and Price, {P. A.} and Peterson, {B. A.} and M. Jel{\'i}nek and L. Amati and Andersen, {M. I.} and Castro-Tirado, {A. J.} and Cer{\'o}n, {J. M Castro} and {De Ugarte Postigo}, A. and F. Frontera and Fruchter, {A. S.} and Fynbo, {J. P U} and J. Gorosabel and Henden, {A. A.} and J. Hjorth and Jensen, {B. L.} and S. Klose and C. Kouveliotou and G. Masi and P. M{\o}ller and L. Nicastro and Ofek, {E. O.} and Pandey, {S. B.} and J. Rhoads and Tanvir, {N. R.} and Wijers, {R. A M J} and {Van Den Heuvel}, {E. P J}",
year = "2006",
month = "8",
doi = "10.1051/0004-6361:20054728",
language = "English (US)",
volume = "455",
pages = "423--431",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "2",

}

TY - JOUR

T1 - Physics of the GRB 030328 afterglow and its environment

AU - Maiorano, E.

AU - Masetti, N.

AU - Palazzi, E.

AU - Savaglio, S.

AU - Rol, E.

AU - Vreeswijk, P. M.

AU - Pian, E.

AU - Price, P. A.

AU - Peterson, B. A.

AU - Jelínek, M.

AU - Amati, L.

AU - Andersen, M. I.

AU - Castro-Tirado, A. J.

AU - Cerón, J. M Castro

AU - De Ugarte Postigo, A.

AU - Frontera, F.

AU - Fruchter, A. S.

AU - Fynbo, J. P U

AU - Gorosabel, J.

AU - Henden, A. A.

AU - Hjorth, J.

AU - Jensen, B. L.

AU - Klose, S.

AU - Kouveliotou, C.

AU - Masi, G.

AU - Møller, P.

AU - Nicastro, L.

AU - Ofek, E. O.

AU - Pandey, S. B.

AU - Rhoads, J.

AU - Tanvir, N. R.

AU - Wijers, R. A M J

AU - Van Den Heuvel, E. P J

PY - 2006/8

Y1 - 2006/8

N2 - Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices α1 = 0.76 ± 0.03, α2 = 1.50 ±0.07 and a break at tb = 0.48 ±0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle θjet ∼ 3°.2. An achromatic bump starting around ∼0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-α Absorber. The optical V-band afterglow appears polarized, with P - (2.4 ±0.6)% and θ = 170° ± 7°, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope βopt = 0.47 ± 0.15, and an X-ray slope βx = 1.0 ± 0.2. Conclusions. The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium.

AB - Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices α1 = 0.76 ± 0.03, α2 = 1.50 ±0.07 and a break at tb = 0.48 ±0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle θjet ∼ 3°.2. An achromatic bump starting around ∼0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-α Absorber. The optical V-band afterglow appears polarized, with P - (2.4 ±0.6)% and θ = 170° ± 7°, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope βopt = 0.47 ± 0.15, and an X-ray slope βx = 1.0 ± 0.2. Conclusions. The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium.

KW - Cosmology: observations

KW - Gamma rays: bursts

KW - Line: identification

KW - Radiation mechanisms: non-thermal

UR - http://www.scopus.com/inward/record.url?scp=33748422834&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33748422834&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20054728

DO - 10.1051/0004-6361:20054728

M3 - Article

AN - SCOPUS:33748422834

VL - 455

SP - 423

EP - 431

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 2

ER -