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<ri:Resource created="2011-11-04T07:39:50Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>g'r'i'z'JH light curves of GRB 091127</title><shortName>J/A+A/535/A57</shortName><identifier>ivo://CDS.VizieR/J/A+A/535/A57</identifier><altIdentifier>doi:10.26093/cds/vizier.35350057</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Filgas R.</name></creator><creator><name>Greiner J.</name></creator><creator><name>Schady P.</name></creator><creator><name>Kruehler T.</name></creator><creator><name>Updike A.C.</name></creator><creator><name>Klose S.,Nardini M.</name></creator><creator><name>Kann D.A.</name></creator><creator><name>Rossi A.</name></creator><creator><name>Sudilovsky V.</name></creator><creator><name>Afonso P.M.J.</name></creator><creator><name>Clemens C.,Elliott J.</name></creator><creator><name>Nicuesa Guelbenzu A.</name></creator><creator><name>Olivares E. F.</name></creator><creator><name>Rau A.</name></creator><date role="Updated">2017-07-10T06:37:33Z</date><date role="Created">2011-11-04T07:39:50Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><description>Using high-quality, broad-band afterglow data for GRB 091127, we investigate the validity of the synchrotron fireball model for gamma-ray bursts, and infer physical parameters of the ultra-relativistic outflow. We used multi-wavelength (NIR to X-ray) follow-up observations obtained with GROND simultaneously in the g'r'i'z' JH filters and the XRT onboard the Swift satellite in the 0.3 to 10keV energy range. The resulting afterglow light curve is of excellent accuracy with relative photometric errors as low as 1%, and the spectral energy distribution is well-sampled over 5 decades in energy. 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