The central engine of GRB 130831A and the energy breakdown of a relativistic explosion

Pasquale, M. de; Oates, S. R.; Racusin, J. L.; Канн, Д. А.; Zhang, Bing; Pozanenko, A.; Volnova, A.; Trotter, A.; Frank, N.; Cucchiara, Antonino; Troja, E.; Sbarufatti, B.; Butler, Nathaniel R.; Schulze, S.; Cano, Z.; Page, M. J.; Castro‐Tirado, Alberto J.; Gorosabel, J.; Lien, A. Y.; Fox, O.; Littlejohns, O.; Bloom, J.; Prochaska, J. Xavier; Diego, J. A. de; González, Jesús; Richer, M. G.; Román-Zúñiga, C.; Watson, A. M.; Gehrels, N.; Moseley, H.; Kutyrev, A.; Zane, S.; Hoette, V.; Russell, R.; Rumyantsev, V.; Klunko, E.; Бурхонов, О.; Breeveld, A. A.; Reichart, D.; Haislip, J.

doi:10.1093/mnras/stv2280

Cited by 26 publications

(30 citation statements)

References 79 publications

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“…We also tried a fit with the afterglow described by a broken power-law, but found that the break time and post-break decay slope are unconstrained, while at the same time the k, s parameters hardly changed. Therefore, there is no evidence in the afterglow of a break between 0.4 and ∼ 3 days, in agreement with the lack of a break in the late X-ray light curve (De Pasquale et al 2016).…”

Section: Appendix A4: Grb 130831asupporting

confidence: 74%

“…Afterglow properties: The early optical afterglow light curve (at t 5 ks) is complex and variable, and is discussed in detail in De Pasquale et al (2016). We did not use this data for the calculation of the light curve parameters.…”

Section: Appendix A4: Grb 130831amentioning

confidence: 99%

“…In order to characterize the underlying SN component, we combined our data with that of Cano et al (2014), De Pasquale et al (2016, and Khorunzhev et al (2013). To avoid the early complex light-curve evolution, we only used data from 0.39 days onward.…”

Section: Appendix A4: Grb 130831amentioning

confidence: 99%

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Four GRB supernovae at redshifts between 0.4 and 0.8

Klose

Schmidl

Канн

et al. 2019

A&A

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Twenty years ago, GRB 980425/SN 1998bw revealed that long Gamma-Ray Bursts (GRBs) are physically associated with broad-lined type Ic supernovae. Since then more than 1000 long GRBs have been localized to high angular precision, but only in ∼ 50 cases the underlying supernova (SN) component was identified. Using the multi-channel imager GROND (Gamma-Ray Burst Optical Near-Infrared Detector) at ESO/La Silla, during the last ten years we have devoted a substantial amount of observing time to reveal and to study SN components in long-GRB afterglows.Here we report on four more GRB-SNe (associated with GRBs 071112C, 111228A, 120714B, and 130831A) which were discovered and/or followed-up with GROND and whose redshifts lie between z = 0.4 and 0.8. We study their afterglow light curves, follow the associated SN bumps over several weeks, and characterize their host galaxies. Using SN 1998bw as a template, the derived SN explosion parameters are fully consistent with the corresponding properties of the so-far known GRB-SN ensemble, with no evidence for an evolution of their properties as a function of redshift. In two cases (GRB 120714B/SN 2012eb at z = 0.398 and GRB 130831A/SN 2013fu at z = 0.479) additional Very Large Telescope (VLT) spectroscopy of the associated SNe revealed a photospheric expansion velocity at maximum light of about 40 000 and 20 000 km s −1 , respectively. For GRB 120714B, which was an intermediate-luminosity burst, we find additional evidence for a blackbody component in the light of the optical transient at early times, similar to what has been detected in some GRB-SNe at lower redshifts.

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Section: Appendix A4: Grb 130831asupporting

confidence: 74%

Section: Appendix A4: Grb 130831amentioning

confidence: 99%

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Four GRB supernovae at redshifts between 0.4 and 0.8

Klose

Schmidl

Канн

et al. 2019

A&A

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“…Since the GRB outflow still produces X-ray afterglow by the external shock during the internal plateau phase, it is expected to emerge once the X-ray emission from the magnetar wind drops below the external component. This has been seen clearly in several X-ray afterglows of both long and short GRBs (Troja et al 2007;Lyons et al 2010;Rowlinson et al 2013;Lü & Zhang 2014;Lü et al 2015;De Pasquale et al 2016;Zhang, Huang & Zong 2016). The external component typically shows a power-law (PL) decay with slope of ∼ 1 which is consistent with the prediction of the standard afterglow models (Sari, Piran & Narayan 1998;Chevalier & Li 2000).…”

Section: Introductionsupporting

confidence: 72%

Search for the signatures of a new-born black hole from the collapse of a supra-massive millisecond magnetar in short GRB light curves

Zhang

Lei

Zhang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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'Internal plateau' followed by a sharp decay is commonly seen in short gamma-ray burst (GRB) light curves. The plateau component is usually interpreted as the dipole emission from a supra-massive magnetar, and the sharp decay may imply the collapse of the magnetar to a black hole (BH). Fall-back accretion onto the new-born BH could produce long-lasting activities via the Blandford-Znajek (BZ) process. The magnetic flux accumulated near the BH would be confined by the accretion disks for a period of time. As the accretion rate decreases, the magnetic flux is strong enough to obstruct gas infall, leading to a magnetically-arrested disk (MAD). Within this scenario, we show that the BZ process could produce two types of typical X-ray light curves: type I exhibits a long-lasting plateau, followed by a power-law decay with slopes ranging from 5/3 to 40/9; type II shows roughly a single power-law decay with slope of 5/3. The former requires low magnetic filed strength, while the latter corresponds to relatively high values. We search for such signatures of the new-born BH from a sample of short GRBs with an internal plateau, and find two candidates: GRB 101219A and GRB 160821B, corresponding to type II and type I light curve, respectively. It is shown that our model can explain the data very well.

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“…7 Currently, our optical telescopes range in size from 14 to 40 inches, and span four continents. Originally envisioned for gammaray burst follow-up (Reichart et al 2005, Haislip et al 2006, Dai et al 2007, Updike et al 2008, Nysewander et al 2009, Cenko et al 2011, Cano et al 2011, Bufano et al 2012, Jin et al 2013, Morgan et al 2014, Martin-Carrillo et al 2014, Friis et al 2015, De Pasquale et al 2016, Bardho et al 2016, Melandri et al 2017), Skynet has also been used to study gravitational-wave sources (Abbott et al 2017a, 2017b, blazars (Osterman Meyer et al 2008, Liu et al 2017, Goyal et al 2017, supernovae (Foley et al 2010, Pignata et al 2011, Valenti et al 2011, Pastorello et al 2013, Milisavljevic et al 2013, Maund et al 2013, Stritzinger et al 2014, Inserra et al 2014, Takats et al 2014, Dall'Ora et al 2014, Folatelli et al 2014, Barbarino et al 2015, de Jaeger et al 2016, Gutierrez et al 2016, Tartaglia et al 2017, Prentice et al 2018, supernova remnants (Trotter et al 2017), novae (Schaefer et al ...…”

Section: Introductionmentioning

confidence: 99%

Skynet Algorithm for Single-dish Radio Mapping. I. Contaminant-cleaning, Mapping, and Photometering Small-scale Structures

Martin

Reichart

Dutton

et al. 2019

ApJS

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We present a single-dish mapping algorithm with a number of advantages over traditional techniques.(1) Our algorithm makes use of weighted modeling, instead of weighted averaging, to interpolate between signal measurements. This smooths the data, but without blurring the data beyond instrumental resolution. Techniques that rely on weighted averaging blur point sources sometimes as much as 40%.(2) Our algorithm makes use of local, instead of global, modeling to separate astronomical signal from instrumental and/or environmental signal drift along the telescope's scans. Other techniques, such as basket weaving, model this drift with simple functional forms (linear, quadratic, etc.) across the entirety of scans, limiting their ability to remove such contaminants. (3) Our algorithm makes use of a similar, local modeling technique to separate astronomical signal from radio-frequency interference (RFI), even if only continuum data are available. (4) Unlike other techniques, our algorithm does not require data to be collected on a rectangular grid or regridded before processing. (5) Data from any number of observations, overlapping or not, may be appended and processed together. (6) Any pixel density may be selected for the final image. We present our algorithm, and evaluate it using both simulated and real data. We are integrating it into the image-processing library of the Skynet Robotic Telescope Network, which includes optical telescopes spanning four continents, and now also Green Bank Observatory's 20-meter diameter radio telescope in West Virginia. Skynet serves hundreds of professional users, and additionally tens of thousands of students, of all ages. Default data products are generated on the fly, but will soon be customizable after the fact.

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The central engine of GRB 130831A and the energy breakdown of a relativistic explosion

Cited by 26 publications

References 79 publications

Four GRB supernovae at redshifts between 0.4 and 0.8

Four GRB supernovae at redshifts between 0.4 and 0.8

Search for the signatures of a new-born black hole from the collapse of a supra-massive millisecond magnetar in short GRB light curves

Skynet Algorithm for Single-dish Radio Mapping. I. Contaminant-cleaning, Mapping, and Photometering Small-scale Structures

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