The First Swift Ultraviolet/Optical Telescope GRB Afterglow Catalog

Roming, P. W. A.; Koch, T. S.; Oates, S. R.; Porterfield, B.; Berk, D. E. vanden; Boyd, Patricia T.; Holland, S. T.; Hoversten, E. A.; Immler, S.; Marshall, F. E.; Page, M. J.; Racusin, J. L.; Schneider, D. P.; Breeveld, A. A.; Brown, P. J.; Chester, M. M.; Cucchiara, Antonino; Pasquale, M. De; Grönwall, C.; Hunsberger, S.; Kuin, N. P. M.; Landsman, W. B.; Schady, P.; Still, M.

doi:10.1088/0004-637x/690/1/163

Cited by 135 publications

(114 citation statements)

References 41 publications

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“…In particular, the dust distribution which is based on Kann et al (2010), Schady et al (2007Schady et al ( , 2010 and Greiner et al (2011) is probably heavily skewed towards low dust environments. It hence rather resembles the sight lines towards bright and mildly extinguished afterglows as typically detected in the UV/optical range (Kann et al 2006;Schady et al 2007;Roming et al 2009). The redshift distribution is chosen to peak at the redshift interval where most of the Swift bursts originate from (z ∼ 1−4, Fynbo et al 2009), but includes a significant number of ultra-high redshift GRBs (∼1000 at z > 8) to investigate the application of photometric redshifts at these extreme values.…”

Section: Properties Of the Afterglow Mock Samplementioning

confidence: 56%

“…For GRB afterglows Swift/UVOT and GROND offer the natural data source as both instruments systematically follow-up on GRB triggers and nicely complement each others sensitivity and wavelength coverage. UVOT onboard the Swift satellite is a 30 cm space-based telescope primarily sensitive in the ultraviolet (UV) and optical range using uvw2, uvm2, uvw1, u, b, v filters, that starts observing the GRB field as quickly as ∼40 s after the trigger (Roming et al 2009). Additional optical and near-infrared (NIR) response is provided by GROND, a seven channel imager (g , r , i , z , J, H, K s simultaneously) mounted at the 2.2 m MPI/ESO telescope at the ESO/LaSilla observatory.…”

Section: Filters and Photometrymentioning

confidence: 99%

“…Using the typical GROND and UVOT detection efficiency (Roming et al 2009;Greiner et al 2011) and the most recent GRB redshift distribution ), and requesting a favorable declination for GROND observations and a Galactic latitude cut of | b |> 10 • , the presented method is applicable to around 15-30% of all GRBs detected by Swift/BAT, and 30-50% of all GRBs with a detected optical afterglow. For many (70%-90%) of the latter sources spectroscopic observations will of course be feasible and return a much more accurate redshift measurement.…”

Section: Number Statisticsmentioning

confidence: 99%

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Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Krühler

Schady

Greiner

et al. 2011

A&A

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Aims. We present a framework to obtain photometric redshifts (photo-zs) for gamma-ray burst afterglows. Using multi-band photometry from GROND and Swift/UVOT, photo-zs are derived for five GRBs for which spectroscopic redshifts are not available. Methods. We use UV/optical/NIR data and synthetic photometry based on afterglow observations and theory to derive the photometric redshifts of GRBs and their accuracy. Taking into account the afterglow synchrotron emission properties, we investigate the application of photometry to derive redshifts in a theoretical range between z ∼ 1 to z ∼ 12.Results. The measurement of photo-zs for GRB afterglows provides a quick, robust and reliable determination of the distance scale to the burst, particularly in those cases where spectroscopic observations in the optical/NIR range cannot be obtained. Given a sufficiently bright and mildly reddened afterglow, the relative photo-z accuracy η = Δz/(1 + z) is better than 10% between z = 1.5 and z ∼ 7 and better than 5% between z = 2 and z = 6. We detail the approach on 5 sources without spectroscopic redshifts observed with UVOT on-board Swift and/or GROND. The distance scale to those same afterglows is measured to be z = 4.31 +0.14 −0.15 for GRB 080825B, z = 2.13 +0.14 −0.20 for GRB 080906, z = 3.44 +0.15 −0.32 for GRB 081228, z = 2.03 +0.16 −0.14 for GRB 081230 and z = 1.28 +0.16 −0.15 for GRB 090530. Conclusions. Due to the exceptional luminosity and simple continuum spectrum of GRB afterglows, photometric redshifts can be obtained to an accuracy as good as η ∼ 0.03 over a large redshift range including robust (η ∼ 0.1) measurements in the ultra-high redshift regime (z 7). Combining the response from UVOT with ground-based observatories and in particular GROND operating in the optical/NIR wavelength regime, reliable photo-zs can be obtained from z ∼ 1.0 out to z ∼ 10, and possibly even at higher redshifts in some favorable cases, provided that these GRBs exist, are localized quickly, have sufficiently bright afterglows and are not heavily obscured.

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Section: Properties Of the Afterglow Mock Samplementioning

confidence: 56%

Section: Filters and Photometrymentioning

confidence: 99%

Section: Number Statisticsmentioning

confidence: 99%

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Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Krühler

Schady

Greiner

et al. 2011

A&A

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“…Counts have been extracted in a 5 radius of aperture, and magnitudes and fluxes have been evaluated using uvotmaghist, V. 1.1. The correction for Galactic extinction has been done following Roming et al (2009), assuming E B−V = 0.104 and 0.224 for case A and B respectively, where E B−V is the difference of the total extinction in the B and V filters. The evaluation of E B−V has been done using N H = 7.79 and 16.79 × 10 20 cm −2 , for case A and B, respectively, and N H /E B−V = 7.5 × 10 21 cm −2 , as given in Jenkins & Savage (1974).…”

Section: Swift/uvotmentioning

confidence: 99%

Discovery of VHEγ-ray emission and multi-wavelength observations of the BL Lacertae object 1RXS J101015.9 − 311909

Abramowski¹,

Acero²,

Aharonian³

et al. 2012

A&A

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ABSTRACT1RXS J101015.9−311909 is a galaxy located at a redshift of z = 0.14 hosting an active nucleus (called AGN) belonging to the class of bright BL Lac objects. Observations at high (HE, E > 100 MeV) and very high (VHE, E > 100 GeV) energies provide insights into the origin of very energetic particles present in such sources and the radiation processes at work. We report on results from VHE observations performed between 2006 and 2010 with the H.E.S.S. instrument, an array of four imaging atmospheric Cherenkov telescopes. H.E.S.S. data have been analysed with enhanced analysis methods, making the detection of faint sources more significant. VHE emission at a position coincident with 1RXS J101015.9−311909 is detected with H.E.S.S. for the first time. In a total good-quality livetime of about 49 h, we measure 263 excess counts, corresponding to a significance of 7.1 standard deviations. The photon spectrum above 0.2 TeV can be described by a power-law with a photon index of Γ = 3.08 ± 0.42 stat ± 0.20 sys . The integral flux above 0.2 TeV is about 0.8% of the flux of the Crab nebula and shows no significant variability over the time reported. In addition, public Fermi/LAT data are analysed to search for high energy emission from the source. The Fermi/LAT HE emission in the 100 MeV to 200 GeV energy range is significant at 8.3 standard deviations in the chosen 25-month dataset. UV and X-ray contemporaneous observations with the Swift satellite in May 2007 are also reported, together with optical observations performed with the atom telescope located at the H.E.S.S. site. Swift observations reveal an absorbed X-ray flux of F (0.3−7) keV = 1.04 +0.04 −0.05 × 10 −11 erg cm −2 s −1 in the 0.3−7 keV range. Finally, all the available data are used to study the multi-wavelength properties of the source. The spectral energy distribution (SED) can be reproduced using a simple one-zone Synchrotron Self Compton (SSC) model with emission from a region with a Doppler factor of 30 and a magnetic field between 0.025 and 0.16 G. These parameters are similar to those obtained for other sources of this type.

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“…The UVOT repository (Roming et al 2009) gives a detailed sequence of observation times, as each of the UBV filters was used, and more than the initial 9 × 10 s exposure were taken. The time error bars in Fig.…”

Section: Other Optical Data and Upper Limitsmentioning

confidence: 99%

GRB 050502B optical afterglow: a jet-break at high redshift

Afonso

Greiner

Pian

et al. 2011

A&A

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Aims. Swift GRB 050502B is well known for the very bright flare displayed in its X-ray light curve. Despite extensive studies, however, the optical light curve has never been discussed and its redshift is unconstrained. Possible correlations between optical and X-ray data are analysed. Methods. Photometric data from TNG in the R and I bands were used to compare the optical afterglow with the X-ray light curve. The HyperZ package and a late-time VLT host observation were used to derive redshift estimates. Results. The I-band afterglow decay followed a power law of index α = 2.1 ± 0.6, after a late break at ∼1.3 × 10 5 s. The R − I colour is remarkably red and the broadband spectral index β OX = 0.9±0.1 is consistent with the X-ray spectral slope β X . Although a photometric redshift of z > 4 is the most conservative result to consider, a photometric redshift of z = 5.2 ± 0.3 is suggested with no extinction in the host, based on which an isotropic energy E γ,iso = (3.8 ± 0.7) × 10 52 erg and a jet opening angle θ ∼ 3.7 • are subsequently derived. Conclusions. The combined X-ray and optical data suggest an achromatic break, which we interpret as a jet-break. The post jet-break slope roughly obeys the closure relation for the jet's slow cooling model. Because of the afterglow's very red colour, in order for the redshift to be low (z < 1), extinction must be significantly high if present in the host. Since the optical-to-X-ray index is consistent with the X-ray spectrum, and there is no XRT evidence for excess N H , GRB 050502B was likely at high redshift.

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The First Swift Ultraviolet/Optical Telescope GRB Afterglow Catalog

Cited by 135 publications

References 41 publications

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Discovery of VHEγ-ray emission and multi-wavelength observations of the BL Lacertae object 1RXS J101015.9 − 311909

GRB 050502B optical afterglow: a jet-break at high redshift

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