SCUBA sub-millimeter observations of gamma-ray bursts

Smith, I. A.; Tilanus, R. P. J.; Tanvir, N. R.; Barnard, V. E.; Moriarty‐Schieven, G. H.; Frail, D. A.; Wijers, R. A. M. J.; Vreeswijk, P. M.; Rol, E.; Kouveliotou, C.

doi:10.1051/0004-6361:20053107

Cited by 22 publications

(24 citation statements)

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“…They provide "clean" measures of the source intensity, unaffected by scintillation and extinction. We have therefore been performing Target of Opportunity (ToO) sub-millimeter observations of GRB counterparts using the Sub-millimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii.Including the results shown here, SCUBA has so far performed ToO observations of 23 bursts (Smith et al 1999(Smith et al , 2000(Smith et al , 2001(Smith et al , 2005Bloom et al 1998;Galama et al 1999;Kulkarni et al 1999;Frail et al 2000Frail et al , 2002Frail et al , 2003Berger et al 2000Berger et al , 2003aYost et al 2002). A complete summary of the previous SCUBA results and the motivations for performing submillimeter observations of the afterglows and host galaxies is given in Smith et al (2005).…”

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confidence: 76%

SCUBA sub-millimeter observations of gamma-ray bursts

Smith¹,

Tilanus

Tanvir

et al. 2005

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SCUBA sub-millimeter observations of gamma-ray bursts -III. GRB 030329: the brightest sub-millimeter afterglow to date Smith, I.A.; Tilanus, R.P.J.; Tanvir, N.; Wijers, R.A.M.J.; Vreeswijk, P.; Rol, E.; Kouveliotou, C. General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. Abstract. We present all the Target of Opportunity (ToO) sub-millimeter observations of GRB 030329 taken by the Sub-millimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). This was by far the brightest sub-millimeter afterglow seen to date. The flux density at 850 µm was approximately constant up to a break that took place ∼7 days after the burst. This was consistent with being a jet break. The 850 µm results agree with those at longer wavelengths that show a brighter flux ∼7 days after the burst, right at the time of the break. No short-lived large-scale brightenings were detected in the sub-millimeter light curve. However, the 850 µm light curve may have had a drop < ∼ 16 days after the burst. The peak of the afterglow emission was at ∼90 GHz in the days before the break in the light curve. A simple modeling is consistent with the spectral indices remaining the same as the afterglow evolved, with the breaks in the spectrum moving to longer wavelengths at later times and the flux at the peak falling. No significant sub-millimeter emission was detected from the host galaxy.Key words. gamma rays: bursts -submillimeter IntroductionThe discovery of localized transients in the error boxes of gamma-ray burst (GRB) sources has led to intense multiwavelength campaigns that have revolutionized our understanding of these sources. For reviews see Van Paradijs et al. (2000) and Mészáros (2002).Sub-millimeter observations form a key element of the multiwavelength observations of the afterglow. They provide "clean" measures of the source intensity, unaffected by scintillation and extinction. We have therefore been performing Target of Opportunity (ToO) sub-millimeter observations of GRB counterparts using the Sub-millimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii.Including the results shown here, SCUBA has so far performed ToO observations of 23 bursts (Smith et al. 1999(Smith et al. , 2000(Smith et al. , 2001(Smith e...

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SCUBA sub-millimeter observations of gamma-ray bursts

Smith¹,

Tilanus

Tanvir

et al. 2005

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“…First, Smith et al (2012) simultaneously obtained an early epoch at 450 μm and 850 μm with the sub-millimetre continuum camera SCUBA-2 (Holland et al 2013) on the James Clerk Maxwell Telescope (JCMT). The 1.6-h observation began at T 0 + 41.5 min and was performed under moderate weather conditions.…”

Section: Sub-mm/mm Observationsmentioning

confidence: 99%

GRB 120422A/SN 2012bz: Bridging the gap between low- and high-luminosity gamma-ray bursts

Schulze

Malesani

Cucchiara

et al. 2014

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Context. At low redshift, a handful of gamma-ray bursts (GRBs) have been discovered with luminosities that are substantially lower (L iso < ∼ 10 48.5 erg s −1 ) than the average of more distant ones (L iso > ∼ 10 49.5 erg s −1 ). It has been suggested that the properties of several low-luminosity (low-L) GRBs are due to shock break-out, as opposed to the emission from ultrarelativistic jets. This has led to much debate about how the populations are connected. Aims. The burst at redshift z = 0.283 from 2012 April 22 is one of the very few examples of intermediate-L GRBs with a γ-ray luminosity of L iso ∼ 10 49.6−49.9 erg s −1 that have been detected up to now. With the robust detection of its accompanying supernova SN 2012bz, it has the potential to answer important questions on the origin of low-and high-L GRBs and the GRB-SN connection. Methods. We carried out a spectroscopy campaign using medium-and low-resolution spectrographs with 6-10-m class telescopes, which covered a time span of 37.3 days, and a multi-wavelength imaging campaign, which ranged from radio to X-ray energies over a duration of ∼270 days. Furthermore, we used a tuneable filter that is centred at Hα to map star-formation in the host and the surrounding galaxies. We used these data to extract and model the properties of different radiation components and fitted the spectral energy distribution to extract the properties of the host galaxy. Results. Modelling the light curve and spectral energy distribution from the radio to the X-rays revealed that the blast wave expanded with an initial Lorentz factor of Γ 0 ∼ 50, which is a low value in comparison to high-L GRBs, and that the afterglow had an exceptionally low peak luminosity density of < ∼ 2 × 10 30 erg s −1 Hz −1 in the sub-mm. Because of the weak afterglow component, we were able to recover the signature of a shock break-out in an event that was not a genuine low-L GRB for the first time. At 1.4 hr after the burst, the stellar envelope had a blackbody temperature of k B T ∼ 16 eV and a radius of ∼7 × 10 13 cm (both in the observer frame). The accompanying SN 2012bz reached a peak luminosity of M V = −19.7 mag, which is 0.3 mag more luminous than SN 1998bw. The synthesised nickel mass of 0.58 M , ejecta mass of 5.87 M , and kinetic energy of 4.10 × 10 52 erg were among the highest for GRB-SNe, which makes it the most luminous spectroscopically confirmed SN to date. Nebular emission lines at the GRB location were visible, which extend from the galaxy nucleus to the explosion site. The host and the explosion site had close-to-solar metallicity. The burst occurred in an isolated star-forming region with an SFR that is 1/10 of that in the galaxy's nucleus. Conclusions. While the prompt γ-ray emission points to a high-L GRB, the weak afterglow and the low Γ 0 were very atypical for such a burst. Moreover, the detection of the shock break-out signature is a new quality for high-L GRBs. So far, shock break-outs were exclusively detected for low-L GRBs, while GRB 120422A had an intermediate...

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“…The AG was not detected at radio or sub-mm wavelengths Smith et al 2013). A redshift of z = 0.479 was measured with Gemini-North (Cucchiara & Perley 2013).…”

Section: Grb 130831amentioning

confidence: 86%

“…The AG was not detected at radio (Laskar et al 2012) down to 3σ upper limits of 39 mJy and 58 mJy, at 5.8 and 21.8 GHz, respectively. The AG was not detected either at sub-mm wavelengths (350 GHz, with rms of 1.8 mJy; Smith et al 2012) An estimate of the isotropic energy release in γ-rays (1-10 4 keV, restframe) is E iso,γ = 2.3 +0.3 −1.5 × 10 52 erg, while the peak energy E p ≈ 310.6 keV 2 . The probability that GRB 120729A arises from a collapsar ) based on T 90 alone is 99.996 ± 0.001% (BAT) and 98.225 ± 1.004% (GBM).…”

Section: Grb 120729amentioning

confidence: 98%

A trio of gamma-ray burst supernovae:

Cano

Postigo

Pozanenko

et al. 2014

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We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t − t 0 = 16.1 d, which covers rest-frame 3000-6250 Å. Based on Fe  λ5169 and Si  λ6355, our spectrum indicates an unusually low expansion velocity of ∼4000-6350 km s −1 , the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Mészáros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 × 10 15 G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs.

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SCUBA sub-millimeter observations of gamma-ray bursts

Cited by 22 publications

References 76 publications

SCUBA sub-millimeter observations of gamma-ray bursts

SCUBA sub-millimeter observations of gamma-ray bursts

GRB 120422A/SN 2012bz: Bridging the gap between low- and high-luminosity gamma-ray bursts

A trio of gamma-ray burst supernovae:

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