A Search for Untriggered GRB Afterglows with ROTSE‐III

Rykoff, E. S.; Aharonian, F.; Akerlof, C.; Alatalo, Katherine; Ashley, M. C. B.; Güver, T.; Horns, D.; Kehoe, R.; Kızıloğlu, Ü.; McKay, Timothy A.; Özel, M. E.; Phillips, A.; Quimby, R.; Schaefer, Bradley E.; Smith, D. A.; Swan, H.; Vestrand, W. T.; Wheeler, J. C.; Wren, J.; Yost, S. A.

doi:10.1086/432832

Cited by 57 publications

(82 citation statements)

References 25 publications

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“…Among past searches for orphan afterglows in the optical, Rykoff et al (2005) used the Robotic Optical Transients Search Experiment III (ROTSE-III). Over a period of 1.5 year, they identified no credible GRB afterglow.…”

Section: Optical Surveysmentioning

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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Section: Optical Surveysmentioning

confidence: 99%

Unveiling the population of orphanγ-ray bursts

Ghirlanda

Salvaterra

Campana

et al. 2015

A&A

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“…These transients brighten over the course of several days or even weeks, depending on the observing band and viewing angle. Identifying orphan afterglows in large area surveys, such as Rykoff et al (2005), has proven difficult, but a GW trigger may help distinguish orphan afterglows from other EM variability.…”

Section: Stellar Core Collapsementioning

confidence: 99%

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

Abadie

Abbott

et al. 2012

A&A

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Article published by EDP Sciences A124, page 1 of 15 A&A 539, A124 (2012) ABSTRACT Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations. Methods. During two observing periods (Dec. 17, 2009 to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010, a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly.Results. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ∼50% or better probability with a few pointings of wide-field telescopes.

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“…Searches have been made of OAs by both X-ray surveys (Grindlay 1999;Greiner et al 2000) and optical searches (Becker et al 2004;Rykoff et al 2005;Rau et al 2006;Malacrino et al 2007). The purpose of the present paper is to calculate the Pop III.2 GRB OA rate that might be detected by the Gaia mission (for more details about Gaia, see, e.g., Perryman et al 2001;Lindegren 2009).…”

Section: Introductionmentioning

confidence: 99%

Searching for the first stars with theGaiamission

Krone-Martins¹,

Ishida²,

Ciardi³

2012

A&A

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Aims. We construct a theoretical model to predict the number of orphan afterglows (OA) from gamma-ray bursts (GRBs) triggered by primordial metal-free (Pop III) stars expected to be observed by the Gaia mission. In particular, we consider primordial metal-free stars that were affected by radiation from other stars (Pop III.2) as a possible target. Methods. We use a semi-analytical approach that includes all relevant feedback effects to construct cosmic star formation history and its connection with the cumulative number of GRBs. The OA events are generated using the Monte Carlo method, and realistic simulations of Gaia's scanning law are performed to derive the observation probability expectation. Results. We show that Gaia can observe up to 2.28 ± 0.88 off-axis afterglows and 2.78 ± 1.41 on-axis during the five-year nominal mission. This implies that a nonnegligible percentage of afterglows that may be observed by Gaia (∼10%) could have Pop III stars as progenitors.

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A Search for Untriggered GRB Afterglows with ROTSE‐III

Cited by 57 publications

References 25 publications

Unveiling the population of orphanγ-ray bursts

Unveiling the population of orphanγ-ray bursts

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

Searching for the first stars with theGaiamission

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