A Tale of Two Transients: GW 170104 and GRB 170105A

Bhalerao, V.; Kasliwal, M. M.; Bhattacharya, Dipankar; Corsi, A.; Aarthy, E.; Adams, S. M.; Blagorodnova, N.; Cantwell, T.; Cenko, S. Bradley; Fender, R. P.; Frail, D. A.; Itoh, R.; Jencson, J.; Kawai, N.; Kong, Albert; Kupfer, Thomas; Kutyrev, A.; Mao, J.; Mate, Sujay; Mithun, N. P. S.; Mooley, K. P.; Perley, D.; Perrott, Y. C.; Quimby, R.; Rao, A. R.; Singer, L. P.; Sharma, V.; Titterington, D.; Troja, E.; Vadawale, S.; Vibhute, A.; Vedantham, H. K.; Veilleux, Sylvain

doi:10.3847/1538-4357/aa81d2

Cited by 40 publications

(32 citation statements)

References 56 publications

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“…This was classified as a regular long GRB (GRB170105) with an optical afterglow that could also be independently found in the ATLAS follow-up observations of GW170104 (ATLAS17aeu; Bhalerao et al 2017;Melandri et al 2017;Stalder et al 2017;Tonry et al 2017). INTEGRAL observations contributed to the triangulation, which allowed for establishing the association between GRB170105 and ATLAS17aeu (Svinkin et al 2017a).…”

Section: Integral Observations Of Gw170104mentioning

confidence: 71%

INTEGRAL Observations of GW170104

Savchenko

Ferrigno

Bozzo

et al. 2017

ApJL

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INTEGRAL Observations of GW170104Savchenko Document VersionPublisher's PDF, also known as Version of record Link back to DTU Orbit Citation (APA): Savchenko, V., Ferrigno, C., Bozzo, E., Bazzano, A., Brandt, S., Chenevez, J., ... Ubertini, P. (2017 AbstractWe used data from the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) to set upper limits on the γ-ray and hard X-ray prompt emission associated with the gravitational-wave event GW170104, discovered by the Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo collaboration. The unique omnidirectional viewing capability of the instruments on board INTEGRAL allowed us to examine the full 90% confidence level localization region of the LIGO trigger. Depending on the particular spectral model assumed and the specific position within this region, the upper limits inferred from the INTEGRAL observations range from F γ =1.9×10ergcm −2 (75 keV-2 MeV energy range). This translates into a ratio between the prompt energy released in γ-rays along the direction to the observer and the gravitational-wave energy of E γ /E GW <2.6×10 . Using the INTEGRAL results, we cannot confirm the γ-ray proposed counterpart to GW170104 by the Astro-Rivelatore Gamma a Immagini Leggero (AGILE) team with the mini-Calorimeter (MCAL) instrument. The reported flux of the AGILE/MCAL event, E2, is not compatible with the INTEGRAL upper limits within most of the 90% LIGO localization region. There is only a relatively limited portion of the sky where the sensitivity of the INTEGRAL instruments was not optimal and the lowest-allowed fluence estimated for E2 would still be compatible with the INTEGRAL results. This region was also observed independently by Fermi/Gamma-ray Burst Monitor and AstroSAT, from which, as far as we are aware, there are no reports of any significant detection of a prompt high-energy event.

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Section: Integral Observations Of Gw170104mentioning

confidence: 71%

INTEGRAL Observations of GW170104

Savchenko

Ferrigno

Bozzo

et al. 2017

ApJL

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“…AstroSat CZTI is one of the most sensitive instruments for detecting short duration high energy transients (see for example Bhalerao et al 2017b). Our limits on 41 bursts out of 64 that occurred in our search period are consistent with the operational expectations of being sensitive to about half the events, the rest being lost to Earth-occultation and SAA transits.…”

Section: Discussionmentioning

confidence: 99%

“…CZTI has detected over two hundred GRBs 3 . For transients with a clear detection, CZTI data can yield spectra (Rao et al 2016), polarisation (Vadawale et al 2015;Chattopadhyay et al 2017) and localisation (Rao et al 2016;Bhalerao et al 2017b). a Modules with more than 1000 counts in one second are flagged as noisy, and suppressed for that one second duration.…”

Section: Introductionmentioning

confidence: 99%

Prompt X-Ray Emission from Fast Radio Bursts—Upper Limits with AstroSat

Anumarlapudi

Bhalerao

Tendulkar

et al. 2020

ApJ

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Fast Radio Bursts (FRBs) are short lived (∼ msec), energetic transients (having a peak flux density of ∼ Jy) with no known prompt emission in other energy bands. We present results of a search for prompt X-ray emissions from 41 FRBs using the Cadmium Zinc Telluride Imager (CZTI) on AstroSat which continuously monitors ∼ 70% of the sky. Our searches on various timescales in the 20-200 keV range, did not yield any counterparts in this hard X-ray band. We calculate upper limits on hard X-ray flux, in the same energy range and convert them to upper bounds for η: the ratio X-ray to radio fluence of FRBs. We find η ≤ 10 8−10 for hard X-ray emission. Our results will help constrain the theoretical models of FRBs as the models become more quantitative and nearer, brighter FRBs are discovered.

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“…For example, iPTF14yb and ATLAS17aeu (Bhalerao et al 2017;Stalder et al 2017) were optical afterglows to GRBs identified via fading broadband afterglow emission; in both cases, the "parent" GRB was identified only later (ibid). Then there is the curious PTF11agg (Cenko et al 2013), which had no identified high-energy counterpart but had other characteristic features of a GRB afterglow: a rapidly fading optical source, a long-lived scintillating radio counterpart, and coincidence with a dwarf galaxy with an estimated redshift of 0.5z3.0.…”

Section: Introductionmentioning

confidence: 99%

iPTF Archival Search for Fast Optical Transients

Kulkarni

Nugent

et al. 2018

ApJL

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There has been speculation about a class of relativistic explosions with an initial Lorentz factor Γ init smaller than that of classical gamma-ray bursts (GRBs). These "dirty fireballs" would lack prompt GRB emission but could be pursued via their optical afterglow, appearing as transients that fade overnight. Here we report a search for such transients (that fade by 5-σ in magnitude overnight) in four years of archival photometric data from the intermediate Palomar Transient Factory (iPTF). Our search criteria yielded 50 candidates. Of these, two were afterglows to GRBs that had been found in dedicated follow-up observations to triggers from the Fermi GRB Monitor. Another (iPTF14yb) was a GRB afterglow discovered serendipitously. Eight were spurious artifacts of reference image subtraction, and one was an asteroid. The remaining 38 candidates have red stellar counterparts in external catalogs. The photometric and spectroscopic properties of the counterparts identify these transients as strong flares from M dwarfs of spectral type M3-M7 at distances of d≈0.15-2.1 kpc; three counterparts were already spectroscopically classified as late-type M stars. With iPTF14yb as the only confirmed relativistic outflow discovered independently of a high-energy trigger, we constrain the all-sky rate of transients that peak at m=18 and fade by Δm=2 mag in Δt=3 hr to be 680 yr 1 -, with a 68% confidence interval of 119 2236 yr 1 --. This implies that the rate of visible dirty fireballs is at most comparable to that of the known population of long-duration GRBs.

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A Tale of Two Transients: GW 170104 and GRB 170105A

Cited by 40 publications

References 56 publications

INTEGRAL Observations of GW170104

INTEGRAL Observations of GW170104

Prompt X-Ray Emission from Fast Radio Bursts—Upper Limits with AstroSat

iPTF Archival Search for Fast Optical Transients

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