Abstract
Abstract We report on the first open-use based Atacama Large Millimeter/submm Array (ALMA) 345 GHz observation for the late afterglow phase of GRB 131030A. The ALMA observation constrained a deep limit at 17.1 d for the afterglow and host galaxy. We also identified a faint submillimeter source (ALMA J2300−0522) near the GRB 131030A position. The deep limit at 345 GHz and multifrequency observations obtained using Swift and RATIR yielded forward-shock modeling with a two-dimensional relativistic hydrodynamic jet simulation and described X-ray excess in the afterglow. The excess was inconsistent with the synchrotron self-inverse Compton radiation from the forward shock. The host galaxy of GRB 131030A and optical counterpart of ALMA J2300−0522 were also identified in the Subaru image. Based on the deep ALMA limit for the host galaxy, the 3σ upper limits of IR luminosity and the star formation rate (SFR) are estimated as LIR < 1.11 × 1011 L⊙ and SFR <18.7 (M⊙ yr−1), respectively. Although the separation angle from the burst location (3${^{\prime\prime}_{.}}$5) was rather large, ALMA J2300−0522 may be one component of the GRB 131030A host galaxy, according to previous host galaxy cases.
Highlights
Submillimeter and millimeter follow-up observations have played an essential role in identifying gamma-ray burst (GRB) afterglow and host galaxies in, for example delineating the energy scale, geometry, radiation physics, and environments of long GRBs (e.g. Frail et al 2002; Sheth et al 2003; Urata et al 2014)
We report on the first open-use based Atacama Large Millimeter/submm Array (ALMA) 345GHz observation for the late afterglow phase of GRB131030A
ALMA observed the bright submm afterglow associated with GRB110715A (∼ 5 mJy at 3.6 d) during the commissioning phase, the quality of observation was comparable with those of other smaller submm instruments
Summary
Submillimeter (submm) and millimeter (mm) follow-up observations have played an essential role in identifying gamma-ray burst (GRB) afterglow and host galaxies in, for example delineating the energy scale, geometry, radiation physics, and environments of long GRBs (e.g. Frail et al 2002; Sheth et al 2003; Urata et al 2014). Submillimeter (submm) and millimeter (mm) follow-up observations have played an essential role in identifying gamma-ray burst (GRB) afterglow and host galaxies in, for example delineating the energy scale, geometry, radiation physics, and environments of long GRBs Submm/mm follow-up observations have lagged behind X-ray, optical and cm radio observations (summaries of afterglow observations are available in de Ugarte Postigo et al 2012; Urata et al 2015a) because of the limited sensitivity of previous submm/mm facilities coupled with the higher redshift of Swift GRBs. The Atacama Large Millimeter/submm Array (ALMA) was first used in the early science phase for GRB host galaxies, and its observations have provided exceptional results (Wang et al.2012; Hatsukade et al 2014; Berger et al 2014).
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