Multiwavelength observations of GRB 140629A

Hu, Y. D.; Oates, S. R.; Lipunov, V.; Zhang, Bin-Bin; Castro‐Tirado, Alberto J.; Jeong, S.; Sánchez-Ramírez, R.; Tello, J. C.; Cunniffe, R.; Gorbovskoy, E.; Caballero‐García, M. D.; Kornilov, V.; Tyurina, N.; Kuznetsov, A.; Balanutsa, P.; Gress, O.; Gorbunov, I.; Vlasenko, D.; Vladimirov, V.; Буднев, Н. М.; Balakin, F.; Ершова, О.; Krushinski, V.; Gabovich, A.; Yurkov, V.; Gorosabel, J.; Москвитин, А. С.; Burenin, R.; Соколов, В. В.; Delgado, Ismael Martínez; Guziy, S.; Fernández-García, E.; Park, I. H.

doi:10.1051/0004-6361/201834959

Cited by 6 publications

(8 citation statements)

References 133 publications

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“…Jet breaks were thought to be observed in pre-Swift observations of GRBs (e.g., [53,228,229]), however, only a few were confirmed as being achromatic [230][231][232]. While there have been some cases of confirmed achromatic jet breaks in post-Swift GRBs (e.g., GRB 050525A and GRB 140629A; [233,234]), they are small in number [186,[235][236][237], and for some GRBs, no jet break has been detected for months [238] or even years after the initial gamma-ray detection [224]. These extreme cases can pose problems for the external shock models, requiring extreme values of the physical parameters of the explosion, the emission mechanism, and the environment to explain them [224].…”

Section: Jet Breaksmentioning

confidence: 99%

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Oates

2023

Universe

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The Neil Gehrels Swift Observatory (Swift) has been in operation for 18 years. The Ultra-Violet/Optical Telescope (UVOT) onboard Swift was designed to capture the earliest optical/UV emission from gamma-ray bursts (GRBs), spanning the first few minutes to days after the prompt gamma-ray emission. In this article, we provide an overview of the long GRBs (whose prompt gamma-ray duration is >2 s) observed by the Swift/UVOT, and review the major discoveries that have been achieved by the Swift/UVOT over the last 18 years. We discuss where improvements have been made to our knowledge and understanding of the optical/UV emission, particularly the early optical/UV afterglow.

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Section: Jet Breaksmentioning

confidence: 99%

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Oates

2023

Universe

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“…In order to maximize the SNR of the optical light curves, we followed the methodology of Oates et al (2009) to combine the individual filter light curves into one single filter (Schady et al 2010;Kann et al 2010;Oates et al 2012;Roming et al 2017;Hu et al 2019). First, the ground-based photometry was converted from magnitudes to count rate using an arbitrary zero-point.…”

Section: Combined Optical Light Curvementioning

confidence: 99%

GRB 140102A: Insight into Prompt Spectral Evolution and Early Optical Afterglow Emission

Gupta,

Oates,

Pandey

et al. 2021

Preprint

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We present and perform a detailed analysis of multi-wavelength observations of GRB 140102A, an optical bright GRB with an observed reverse shock (RS) signature. Observations of this GRB were acquired with the BOOTES-4 robotic telescope, the Fermi, and the Swift missions. Time-resolved spectroscopy of the prompt emission shows that changes to the peak energy (𝐸 p ) tracks intensity and the low-energy spectral index seems to follow the intensity for the first episode, whereas this tracking behavior is less clear during the second episode. The fit to the afterglow light curves shows that the early optical afterglow can be described with RS emission and is consistent with the thin shell scenario of the constant ambient medium. The late time afterglow decay is also consistent with the prediction of the external forward shock (FS) model. We determine the properties of the shocks, Lorentz factor, magnetization parameters, and ambient density of GRB 140102A, and compare these parameters with another 12 GRBs, consistent with having RS produced by thin shells in an ISM-like medium. The value of the magnetization parameter (𝑅 B ≈ 18) indicates a moderately magnetized baryonic dominant jet composition for GRB 140102A. We also report the host galaxy photometric observations of GRB 140102A obtained with 10.4m GTC, 3.5m CAHA, and 3.6m DOT telescopes and find the host (photo 𝑧 = 2.8 +0.7 −0.9 ) to be a high mass, star-forming galaxy with a star formation rate of 20 ± 10 M yr −1 .

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“…Table 5 ofHu et al (2019) gives Γ = β + 1 = 2.040, but this is likely missing ∆Γ = 0.5 as in the first SED results of the table for the "BKP" models.A56, page 39 of 43Kann, D. A., et al: A&A, 686, A56 (2024) …”

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confidence: 99%

“…GRB 140629A, z = 2.276 ± 0.001 Data are taken from Xin et al (2018); Hu et al (2019), from GCN Circulars (Bikmaev et al 2014a;Maehara 2014;Takaki et al 2014;Kuroda et al 2014b;Perley & Cenko 2014b,a;Garnavich & Rose 2014;D'Avanzo et al 2014b;Honda et al 2014;Moskvitin et al 2014a,b;Yano et al 2014;Pandey & Kumar 2014b), as well as our own Swift UVOT data set, which expands that presented in Hu et al (2019) and also fixes errors in the upper limits presented in that work. The redshift is given by Hu et al (2019). The light curve evolution is complex.…”

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confidence: 99%

“…Using data up to 0.16 d, we find: α rise = −0.848 ± 0.097, α 1 = 1.138 ± 0.005, t b = 0.00238 ± 0.00007 d (t b = 205.6 ± 6.0 s), n = 4.34 ± 0.86 (χ 2 /d.o. f. = 1.45), with host magnitudes fixed to the values from Hu et al (2019) or estimated (they have little influence as the afterglow is far brighter than the host). After 0.16 d, the afterglow shows a bumpy structure superposed on a steepening decay, likely an achromatic jet break (Hu et al 2019), making the light curve similar to that of GRB 021004 (e.g., de Ugarte Postigo et al 2005) and GRB 060526 (Thöne et al 2010).…”

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confidence: 99%

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Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

Kann,

White,

Ghirlanda

et al. 2024

A&A

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Gamma-ray bursts (GRBs) are ideal probes of the Universe at high redshift ($z$), pinpointing the locations of the earliest star-forming galaxies and providing bright backlights with simple featureless power-law spectra that can be used to spectrally fingerprint the intergalactic medium and host galaxy during the period of reionization. Future missions such as Gamow Explorer (hereafter )\ are being proposed to unlock this potential by increasing the rate of identification of high-$z$ ($z>5$) GRBs in order to rapidly trigger observations from $6-10$ m ground telescopes, the James Webb Space Telescope (JWST), and the upcoming Extremely Large Telescopes (ELTs). was proposed to the NASA 2021 Medium-Class Explorer (MIDEX) program as a fast-slewing satellite featuring a wide-field lobster-eye X-ray telescope (LEXT) to detect and localize GRBs with arcminute accuracy, and a narrow-field multi-channel photo-$z$ infrared telescope (PIRT) to measure their photometric redshifts for $>80<!PCT!>$ of the LEXT detections using the Lyman-alpha dropout technique. We use a large sample of observed GRB afterglows to derive the PIRT sensitivity requirement. We compiled a complete sample of GRB optical--near-infrared (optical--NIR) afterglows from 2008 to 2021, adding a total of 66 new afterglows to our earlier sample, including all known high-$z$ GRB afterglows. This sample is expanded with over 2837 unpublished data points for 40 of these GRBs. We performed full light-curve and spectral-energy-distribution analyses of these afterglows to derive their true luminosity at very early times. We compared the high-$z$ sample to the comparison sample at lower redshifts. For all the light curves, where possible, we determined the brightness at the time of the initial finding chart of at different high redshifts and in different NIR bands. This was validated using a theoretical approach to predicting the afterglow brightness. We then followed the evolution of the luminosity to predict requirements for ground- and space-based follow-up. Finally, we discuss the potential biases between known GRB afterglow samples and those to be detected by We find that the luminosity distribution of high-$z$ GRB afterglows is comparable to those at lower redshift, and we therefore are able to use the afterglows of lower-$z$ GRBs as proxies for those at high $z$. We find that a PIRT sensitivity of $15\ (21 mag AB) in a 500 s exposure simultaneously in five NIR bands within 1000s of the GRB trigger will meet the mission requirements. Depending on the $z$ and NIR band, we find that between 75<!PCT!> and 85<!PCT!> of all afterglows at $z>5$ will be recovered by at $5 detection significance, allowing the determination of a robust photo-$z$. As a check for possible observational biases and selection effects, we compared the results with those obtained through population-synthesis models, and find them to be consistent. and other high-$z$ GRB missions will be capable of using a relatively modest 0.3m onboard NIR photo-$z$ telescope to rapidly identify and report high-$z$ GRBs for further follow-up by larger facilities, opening a new window onto the era of reionization and the high-redshift Universe.

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Multiwavelength observations of GRB 140629A

Cited by 6 publications

References 133 publications

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

GRB 140102A: Insight into Prompt Spectral Evolution and Early Optical Afterglow Emission

Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

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