Multicolor Shallow Decay and Chromatic Breaks in the GRB 050319 Optical Afterglow

Huang, K. Y.; Urata, Y.; Kuo, P. H.; Ip, Wing-Huen; Ioka, Kunihito; Aoki, Tsutomu; Chen, C. W.; Chen, W. P.; Isogai, M.; Lin, H. C.; Makishima, Kazuo; Mito, Hiroyuki; Miyata, Takashi; Nakada, Y.; Nishiura, S.; Onda, K.; Qiu, Y.; Soyano, Takao; Tamagawa, Toru; Tarusawa, K.; Tashiro, M.; Yoshioka, T.

doi:10.1086/510737

Cited by 37 publications

(22 citation statements)

References 32 publications

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“…Vreeswijk et al (2008a). (1) Huang et al (2007); (2) Kamble et al (2007); (3) Woźniak et al (2005); (4) Cobb & Bailyn (2005); (5) Rosenberg & Garnavich (2005); (6) Flasher et al (2005); (7) Yanagisawa et al (2005); (8) Homewood et al (2005); (9) Mirabal et al (2005); (10) Pandey et al (2006); (11) Macomb et al (2005); (12) Cenko et al (2006b); (13) Durig & Price (2005); (14) Jakobsson et al (2005b); (15) Andreev & Pozanenko (2005); (16) Henych et al (2005); (17) Piranomonte et al (2005); (18) D'Elia et al (2005); (19) Alatalo et al (2006); (20) Curran et al (2007); (21) Stanek et al (2007); (22) Woźniak et al (2006); (23) Molinari et al (2007); (24) Nysewander et al (2006); (25) …”

Section: Xrt Datamentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

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The composition and amount of interstellar dust within gamma-ray burst (GRB) host galaxies is of key importance when addressing selection effects in the GRB redshift distribution, and when studying the properties of their host galaxies. As well as the implications for GRB research, probing the dust within the high-z hosts of GRBs also contributes to our understanding of the conditions of the interstellar medium and star-formation in the distant Universe. Nevertheless, the physical properties of dust within GRB host galaxies continues to be a highly contended issue. In this paper we explore the mean extinction properties of dust within the host galaxies of a sample of 17 GRBs with total host galaxy visual extinction A V < 1 ( A V = 0.4), covering a redshift range z = 0.7−3.1. We find the average host extinction curve to have an ultraviolet slope comparable to that of the LMC, but with little evidence of a 2175 Å dust extinction feature as observed along Milky Way and LMC sightlines. We cannot at present rule out the presence of a 2175 Å feature, and both the standard SMC and LMC extinction curves also provide good fits to our data. However, we can reject an extinction curve that has a UV slope as flat as the mean Milky Way extinction curve, whilst also having a 2175 Å feature as prominent as seen in the mean Milky Way extinction curve. This is in contrast to the clear detection of a 2175 Å bump and the flatter extinction curves of some more heavily extinguished GRBs (A V > 1), which may be indicative of there being a dependence between dust abundance and the wavelength dependence of dust extinction, as has been previously speculated.

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Section: Xrt Datamentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

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show abstract

“…It was also observed by ground-based telescopes RAPTOR (Wozniak et al 2005), and ROTSE-III (Quimby et al 2006a) just 27.1 s after the Swift trigger. The optical AG was followed later with a number of ground-based telescopes (Huang et al 2007 and references therein). An absorption redshift, z = 3.24, was measured with the Nordic Optical Telescope (Jakobsson et al 2006).…”

Section: Grbs With Complex Chromatic Light Curvesmentioning

confidence: 99%

THE DIVERSE BROADBAND LIGHT CURVES OFSWIFTGAMMA-RAY BURSTS REPRODUCED WITH THE CANNONBALL MODEL

Dado

Dar

Rújula

2009

ApJ

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Two radiation mechanisms, inverse Compton scattering (ICS) and synchrotron radiation (SR), suffice within the Cannonball (CB) model of long gamma-ray bursts (LGRBs) and X-ray flashes (XRFs) to provide a very simple and accurate description of their observed prompt emission and afterglows (AGs). Simple as they are, the two mechanisms and the burst environment generate the rich structure of the light curves at all frequencies and times. This is demonstrated for 33 selected Swift LGRBs and XRFs, which are well sampled from early until late time and faithfully represent the entire diversity of the broadband light curves of Swift LGRBs and XRFs. Their prompt gamma-ray and X-ray emission is dominated by ICS of "glory" light. During their fast decline phase, ICS is taken over by SR, which dominates their broadband AG. The pulse shape and spectral evolution of the gamma-ray peaks and the early-time X-ray flares, and even the delayed optical "humps" in XRFs, are correctly predicted. The "canonical" and noncanonical X-ray light curves and the chromatic behavior of the broadband AGs are well reproduced. In particular, in canonical X-ray light curves, the initial fast decline and rapid softening of the prompt emission, the transition to the plateau phase, the subsequent gradual steepening of the plateau to an asymptotic power-law decay, and the transition from chromatic to achromatic behavior of the light curves agree well with those predicted by the CB model. The Swift earlytime data on XRF 060218 are inconsistent with a blackbody emission from a shock breakout through a stellar envelope. Instead, they are well described by ICS of glory light by a jet breaking out from SN2006aj.

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“…Thus, these results indicate that the X-ray afterglow could have an origin that was distinct from that of the optical afterglow (e.g. Huang et al 2007;Troja et al 2007). …”

Section: Forward Shock Radiation and X-ray Excessmentioning

confidence: 69%

ALMA and RATIR observations of GRB 131030A

Huang

Urata

Takahashi

et al. 2017

Publications of the Astronomical Society of Japan

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We report on the first open-use based Atacama Large Millimeter/submm Array (ALMA) 345-GHz observation for the late afterglow phase of GRB131030A. The ALMA observation constrained a deep limit at 17.1 d for the afterglow and host galaxy. We also identified a faint submillimeter source (ALMAJ2300-0522) near the GRB131030A position. The deep limit at 345 GHz and multifrequency observations obtained using Swift and RATIR yielded forward shock modeling with a two-dimensional relativistic hydrodynamic jet simulation and described X-ray excess in the afterglow. The excess was inconsistent with the synchrotron self-inverse Compton radiation from the forward shock. The host galaxy of GRB131030A and optical counterpart of ALMAJ2300-0522 were also identified in the SUBARU image. Based on the deep ALMA limit for the host galaxy, the 3-σ upper limits of IR luminosity and the star formation rate (SFR) is estimated as L IR < 1.11 × 10 11 L ❡ t and SFR< 18.7 (M ❡ t yr −1 ), respectively. Although the separation angle from the burst location (3. ′′ 5) was rather large, ALMAJ2300-0522 may be one component of the GRB131030A host galaxy, according to previous host galaxy cases.

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Multicolor Shallow Decay and Chromatic Breaks in the GRB 050319 Optical Afterglow

Cited by 37 publications

References 32 publications

The dust extinction curves of gamma-ray burst host galaxies

The dust extinction curves of gamma-ray burst host galaxies

THE DIVERSE BROADBAND LIGHT CURVES OFSWIFTGAMMA-RAY BURSTS REPRODUCED WITH THE CANNONBALL MODEL

ALMA and RATIR observations of GRB 131030A

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