Identification and properties of the photospheric emission in GRB090902B

TL;DR

This paper analyzes the photospheric emission in GRB090902B, revealing a quasi-blackbody spectrum with a characteristic temperature and deriving key physical parameters, highlighting the dominance of photospheric emission early in the burst.

Contribution

It provides the first detailed spectral analysis of photospheric emission in GRB090902B, deriving the photospheric radius and Lorentz factor, and modeling the emission with a multi-color blackbody.

Findings

Photospheric emission dominates early in the burst.

Photospheric radius increases at higher latitudes.

Broadband emission is consistent with synchrotron radiation.

Abstract

The Fermi Gamma-ray Space Telescope observed the bright and long GRB090902B, lying at a redshift of z = 1.822. Together the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM) cover the spectral range from 8 keV to >300 GeV is covered. Here we show that the prompt burst spectrum is consistent with emission from the jet photosphere combined with non-thermal emission described by a single power-law with photon index -1.9. The photosphere gives rise to a strong quasi-blackbody spectrum which is somewhat broader than a single Planck function and has a characteristic temperature of ~290keV. We derive the photospheric radius Rph = (1.1 \pm 0.3) x 10^12 Y^{1/4} cm and the bulk Lorentz factor of the flow, which is found to vary by a factor of two and has a maximal value of Gamma = 750 Y^{1/4}. Here Y is the ratio between the total fireball energy and the energy emitted in the gamma-rays. We find that during the first quarter of the prompt phase the photospheric emission dominates, which explains the delayed onset of the observed flux in the LAT compared to the GBM. We model the photospheric emission with a multi-color blackbody and its shape indicates that the photospheric radius increases at higher latitudes. We interpret the broad band emission as synchrotron emission at R ~ 4x10^15 cm. Our analysis emphasize the importance of having high temporal resolution when performing spectral analysis on GRBs, since there is strong spectral evolution.