Optical studies in the fields of gamma ray burst sources. 2: GRB 910219 and the detection of flashing optical counterpart

Details Optical studies in the fields of gamma ray burst sources. 2: GRB 910219 and the detection of flashing optical counterpart Optical studies in the fields of gamma ray burst sources. 2: GRB 910219 and the detection of flashing optical counterpart

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...284..839h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 284, no. 3, p. 839-852

Astronomy and Astrophysics

Astronomy

9

Astronomical Photography, Gamma Ray Astronomy, Gamma Ray Bursts, Images, Charge Coupled Devices, Error Analysis, Halos, Microdensitometers, Photographic Plates

Scientific paper

We present here the results of the analysis of the error box of the gamma ray bursts source GRB 910219 carried out on 9104 photographic plates representing 2.06 years of exposure (the most extended archival search for any particular Gamma Ray Burst Source (GRBS) position so far). One probable optical flashing candidate has been found and analyzed in detail to avoid any misinterpretation. This analysis has confirmed that the image detected on May 10, 1905, is a real object, reaching for less than or equal to 35 min the brightness of less than or equal to 5.8 mag. The image was not caused by a plate defect (brightness more than 5 mag above plate limit, presence of coma and halo like bright stars) or by a double exposure (negative blinktest). Further, the object cannot be explained as a satellite glint or aircraft flash (the plate was taken in 1905), an asteroid or comet (very bright object with lack of trailing at high ecliptic latitude, no image on adjacent plate), a novae (not found on adjacent plates), a dwarf novae (light amplitude greater than or equal to 15 mag, absent on adjacent plates) and/or a flare star (too large amplitude). The image was found to show lack of trailing and inside of the error box of GRB 910219 as provided by the WATCH experiment onboard of the GRANAT satellite. The parameters and the consequences of this optical transient candidate are presented and discussed.

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