Constraining the rate of GRB visible afterglows  with the
CFHTLS very wide survey

Malacrino, F.; Atteia, J. L.; Boër, M.; Klotz, A.; Veillet, Christian; Cuillandre, Jean-Charles

doi:10.1051/0004-6361:20066912

Cited by 25 publications

(23 citation statements)

References 18 publications

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“…Up until today the quest for their discovery has resulted in upper (θ jet ∼ < 22 • Levinson et al 2002) or lower (θ jet ∼ > 0.8 • Soderberg et al 2006b) limits on the GRB opening angles. Some peculiar transients in past surveys could have been genuine OAs both in the optical (Rau et al 2006;Zou et al 2007;Malacrino et al 2007) and radio (for a recent reveiw on blind surveys see Murphy et al 2013) regime, but none have been confirmed so far. The evolution of the OA lightcurve differs from that of a normal afterglow before reaching its peak flux.…”

Section: Pos(aaska14)052mentioning

confidence: 99%

The SKA View of Gamma-Ray Bursts

Burlon¹,

Ghirlanda²,

Horst³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Gamma-ray bursts (GRBs) are some of the most extreme events in the Universe. As well as providing a natural laboratory for investigating fundamental physical processes, they might trace the cosmic star formation rate up to extreme redshifts and probe the composition of the intergalactic medium over most of the Universe's history. Radio observations of GRBs play a key part in determining their physical properties, but currently they are largely limited to follow-up observations of γ-ray-detected objects. The SKA will significantly increase our ability to study GRB afterglows, following up several hundred objects in the high frequency bands already in the "early science" implementation of the telescope. SKA1-MID Bands 4 (4 GHz) and 5 (9.2 GHz) will be particularly suited to the detection of these transient phenomena. The SKA will trace the peak of the emission, sampling the thick-to-thin transition of the evolving spectrum, and follow-up the afterglow down to the time the ejecta slow down to non-relativistic speeds. The full SKA will be able to observe the afterglows across the non-relativistic transition, for ∼ 25% of the whole GRB population. This will allow us to get a significant insight into the true energy budget of GRBs, probe their surrounding density profile, and the shock microphysics. The SKA will also be able to routinely detect the elusive "orphan afterglow" emission, from the population of GRBs whose jets are not pointed towards the Earth. We expect that a deep all-sky survey such as SKA1-SUR will see around 300 orphan afterglows every week. We predict these detection to be ∼ > 1000 when the full SKA telescope will be operational.Advancing Astrophysics with the Square Kilometre Array

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Section: Pos(aaska14)052mentioning

confidence: 99%

The SKA View of Gamma-Ray Bursts

Burlon¹,

Ghirlanda²,

Horst³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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“…The Deep Lensing Survey (DLS; Becker et al 2004) provides a (less constraining) limit of 5.2 deg −2 day −1 for transients with typical duration of a few ksec and 19.5 < R < 23.4. Malacrino et al (2007) obtained a more stringent upper limit from the CFHTLS Very Wide survey: excluding that the three transient they find are GRBs (Malacrino et al 2007), an upper limit of 0.24 deg −2 yr −1 down to R = 23 can be placed. The ROTSE-III and CFHTLS limits are shown in Fig.…”

Section: Optical Surveysmentioning

confidence: 99%

“…Despite specific studies designed to search for OAs in X-ray surveys (Grindlay 1999;Greiner et al 2000), in optical surveys (Vreeswijk 2002;Rau et al 2006;Malacrino et al 2007;Rau et al 2007), and in the radio band (Levinson et al 2002;Gal-Yam et al 2006;Bannister et al 2011;Bell et al 2011;Bower & Saul 2011;Croft et al 2010;Frail et al 2012;Carilli et al 2003;Matsumura et al 2009;Lazio et al 2010), no OA have been conclusively detected so far.…”

Section: Introductionmentioning

confidence: 99%

Unveiling the population of orphanγ-ray bursts

Ghirlanda

Salvaterra

Campana

et al. 2015

A&A

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Gamma-ray bursts (GRBs) are detectable in the γ-ray band if their jets are oriented toward the observer. However, for each GRB with a typical θ jet , there should be ∼2/θ 2 jet bursts whose emission cone is oriented elsewhere in space. These off-axis bursts can eventually be detected when, due to the deceleration of their relativistic jets, the beaming angle becomes comparable to the viewing angle. Orphan afterglows (OAs) should outnumber the current population of bursts detected in the γ-ray band even if they have not been conclusively observed so far at any frequency. We compute the expected flux of the population of orphan afterglows in the mm, optical, and X-ray bands through a population synthesis code of GRBs and the standard afterglow emission model. We estimate the detection rate of OAs with ongoing and forthcoming surveys. The average duration of OAs as transients above a given limiting flux is derived and described with analytical expressions: in general OAs should appear as daily transients in optical surveys and as monthly/yearly transients in the mm/radio band. We find that ∼2 OA yr −1 could already be detected by Gaia and up to 20 OA yr −1 could be observed by the ZTF survey. A larger number of 50 OA yr −1 should be detected by LSST in the optical band. For the X-ray band, ∼26 OA yr −1 could be detected by the eROSITA. For the large population of OA detectable by LSST, the X-ray and optical follow up of the light curve (for the brightest cases) and/or the extensive follow up of their emission in the mm and radio band could be the key to disentangling their GRB nature from other extragalactic transients of comparable flux density.

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“…If GRB jets are highly beamed, off-axis GRBs and their subsequent orphan afterglow are a natural prediction. Thus, various wide-field searches have looked for them in the optical and radio wavelengths (e.g., Levinson et al 2002;Malacrino et al 2007), but none has been detected at high significance. Along the same vein, specifically Soderberg et al (2006b) and Soderberg et al (2010b) targeted as part of their survey 143 SN Ib/c (including SN Ic-bl) for late-time VLA observations to search for off-axis GRB afterglows, but none of their objects showed evidence for bright, late-time radio emission that could be attributed to off-axis jets coming into our line of sight, until 2009.…”

Section: Search For Off-axis Grbsmentioning

confidence: 99%

Stellar Forensics with the Supernova‐GRB Connection

Modjaz¹

2011

Reviews in Modern Astronomy

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Long-duration gamma-ray bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) are amongst nature's most magnificent explosions. While GRBs launch relativistic jets, SNe Ib/c are core-collapse explosions whose progenitors have been stripped of their hydrogen and helium envelopes. Yet for over a decade, one of the key outstanding questions is which conditions lead to each kind of explosion and death in massive stars. Determining the fates of massive stars is not only a vibrant topic in itself, but also impacts using GRBs as star formation indicators over distances of up to 13 billion light-years and for mapping the chemical enrichment history of the universe. This article reviews a number of comprehensive observational studies that probe the progenitor environments, their metallicities and the explosion geometries of SN with and without GRBs, as well as the emerging field of SN environmental studies. Furthermore, it discusses SN 2008D/XRT 080109 which was discovered serendipitously with the Swift satellite via its X-ray emission from shock breakout, and which has generated great interest amongst both observers and theorists while illustrating a novel technique for stellar forensics. The article concludes with an outlook on how the most promising venues of research -with the many existing and upcoming large-scale surveys such as the Palomar Transient Factory and LSST -will shed new light on the diverse deaths of massive stars.

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Constraining the rate of GRB visible afterglows with the CFHTLS very wide survey

Cited by 25 publications

References 18 publications

The SKA View of Gamma-Ray Bursts

The SKA View of Gamma-Ray Bursts

Unveiling the population of orphanγ-ray bursts

Stellar Forensics with the Supernova‐GRB Connection

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