TITLE: GCN CIRCULAR NUMBER: 38220 SUBJECT: GRB 241030A: LCO optical observation DATE: 24/11/14 16:40:32 GMT FROM: ankur ghosh at CAPP, University of Johannesburg ghosh.ankur1994@gmail.com
Ankur Ghosh, Soebur Razzaque (CAPP, University of Johannesburg), Alexander Moskvitin, Yulia Sotnikova (SAO RAS) on behalf of a larger collaboration.
We observed the field of the GRB 241030A (Klingler et al., GCN 37956; Beardmore et al., GCN 37962; Wang et al., GCN 37972; Pillera et al., GCN 37979; Ridnaia et al., GCN 37982; Ambrosi et al., GCN 37988; Wu et al., GCN 37997) using B, R filters of the 1-meter Sinistro telescope and V filter of the 0.4-m SCICAM QHY600 at the Las Cumbres Observatory Global Telescope (LCOGT) node located at Teide Observatory, Tenerife, SPAIN. The 1-m Sinistro telescope is equipped with a 4K x 4K CCD (FOV: 26 x 26 arcmin, scale: 0.39 arcsec/pixel) and the 0.4 m SCICAM QHY600 is equipped with 9576 x 6388 pixel CCD (FOV: 1.9 x 1.2 degrees, scale: 0.74 arcsec/pixel).
Observations began on October 30 2024, starting from 14.21 to 14.41 hours after the GRB trigger. We clearly detect the optical transient (OT) reported by GCNs (Klingler et al., GCN 37956; Watson et al., GCN 37957; Fernández-Rodríguez et al., GCN 37958; Zheng et al., GCN 37959; An et al., GCN 37960; Higuchi et al., GCN 37963; Qiu et al., GCN 37965; Lin et al., GCN 37966; Wu et al., GCN 37970; Breeveld & Klingler, GCN 37974; Méndez-Lapido et al., GCN 37993, Moskvitin & Goranskij, GCN 38016; Busmann et al., GCN 38019; Schneider et al., GCN 38021; Li et al., GCN 38027; Masi, GCN 38031, Yan et al., GCN 38035, Pankov et al., GCN 38105, Reguitti et al., GCN 38105) in our stacked images. Our detection is well consistent with the observation reported at the similar epoch by Moskvitin & Goranskij, GCN 38016.
Date UTstart-end t-T0 (hours) Exp (sec) Filter Magnitude 2024-10-30 19:55:20--20:05:50 14.21 2 x 300 B B = 19.52 +/- 0.14 2024-10-30 19:48:10--20:08:18 14.17 2 x 600 V V = 19.51 +/- 0.14 2024-10-30 20:07:31--20:17:59 14.41 2 x 300 R R = 19.10 +/- 0.04
The field was calibrated against nearby SDSS stars, with magnitudes converted using Lupton (2005) equations, and has not been corrected for Galactic extinction.
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