Late evolution of the X-ray afterglow of GRB 030329

2); A. Tiengo (1; F. Tavecchio (3); G. Ghirlanda (3) ((1) IASF; G. Ghisellini (3); Merate); Milano; (2) Milano Univ.; (3) OAB; S. Mereghetti (1)

Late evolution of the X-ray afterglow of GRB 030329

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv astro-ph/0402644 v2 pith:5DXI7FZO submitted 2004-02-26 astro-ph

Late evolution of the X-ray afterglow of GRB 030329

A. Tiengo (1 , 2) , S. Mereghetti (1) , G. Ghisellini (3) , F. Tavecchio (3) , G. Ghirlanda (3) ((1) IASF , Milano; (2) Milano Univ.; (3) OAB , Merate) This is my paper

classification astro-ph

keywords x-rayburstafterglowbeendaysflatteningobservedagreement

verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

0 comments

Share X Bluesky LinkedIn Reddit HN

read the original abstract

The X-ray afterglow of the Gamma-Ray Burst GRB 030329, associated to SN2003dh at z=0.1685, has been observed with XMM-Newton 258 days after the burst explosion. A source with flux of (6.2 +/- 2.3) 10^{-16} erg cm^{-2} s^{-1} (0.5-2 keV) has been detected at the GRB position. This measurement, together with a re-analysis of the previous X-ray observations, indicates a flattening of the X-ray light curve ~40 days after the burst. This is in remarkable agreement with the scenario invoking the presence of two jets with different opening angles. The wider jet should be responsible for the observed flattening due to its transition into the non-relativistic Sedov-Taylor phase.

discussion (0)

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Early Multiwavelength Observations of AT 2026fgk: The Luminous Afterglow to Sub-luminous GRB 260310A, Identified Independently of a Gamma-ray Trigger
astro-ph.HE 2026-06 accept novelty 5.0

First blind optical identification of a z=0.153 sub-luminous GRB afterglow with Ic-BL SN, yielding a volumetric rate consistent with on-axis high-luminosity long GRBs.