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The Afterglows, Redshifts, and Properties of Swift Gamma-Ray Bursts | | E. Berger
; S. R. Kulkarni
; D. B. Fox
; A. M. Soderberg
; F. A. Harrison
; E. Nakar
; D. D. Kelson
; M. D. Gladders
; J. S. Mulchaey
; A. Oemler
; A. Dressler
; S. B. Cenko
; P. A. Price
; B. P. Schmidt
; D. A. Frail
; N. Morrell
; S. Gonzalez
; W. Krzeminski
; R. Sari
; A. Gal-Yam
; D.-S. Moon
; B. E. Penprase
; R. Jayawardhana
; A. Scholz
; J. Rich
; B. A. Peterson
; G. Anderson
; R. McNaught
; T. Minezaki
; Y. Yoshii
; L. L. Cowie
; K. Pimbblet
; | | Date: |
6 May 2005 | | Subject: | astro-ph | | Abstract: | We present optical, near-IR, and radio follow up of sixteen Swift bursts, including our discovery of nine afterglows and a redshift determination for three. These observations, supplemented by data from the literature, provide an afterglow recovery rate of 60% in the optical/near-IR, much higher than in previous missions (BeppoSAX, HETE-2, INTEGRAL, and IPN). The optical/near-IR afterglows of Swift events are on average 1.7 mag fainter at t=12 hr than those of previous missions. The X-ray afterglows are similarly fainter compared to those of pre-Swift bursts. In the radio the limiting factor is the VLA threshold and the detection rate for Swift bursts is similar to that for past missions. The redshift distribution of pre-Swift bursts peaked at z~1, whereas the five Swift bursts with measured redshifts are distributed evenly between 1.3 and 3.2. From these results we conclude that (i) the pre-Swift distributions were biased in favor of bright events and low redshift events, (ii) the higher sensitivity and accurate positions of Swift result in a better representation of the true burst redshift and brightness distributions (which are higher and dimmer, respectively), and (iii) as many as 1/3 of the bursts can be optically dark, as a result of a high redshift and/or dust extinction. We remark that the apparent lack of low redshift, low luminosity Swift bursts, and the lower event rate compared to pre-launch estimates (90 vs. 150 per year), are the result of a threshold that is similar to that of BATSE. In view of these inferences, afterglow observers may find it advisable to make significant changes in follow up strategies of Swift events. [abridged] | | Source: | arXiv, astro-ph/0505107 | | Services: | Forum | Review | PDF | Favorites | |
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