Chandra and Hubble Space Telescope observations of dark gamma-ray bursts and their host galaxies. Issue 3 (15th April 2019)

• Record Type: Journal Article
• Authors: Chrimes, A A; Levan, A J; Stanway, E R; Lyman, J D; Fruchter, A S; Jakobsson, P; O'Brien, P; Perley, D A; Tanvir, N R; Wheatley, P J; Wiersema, K
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 486:Issue 3(2019)
• Page Start: 3105
• Page End: 3117
• Publication Date: 2019-04-15
• Subjects: gamma-ray burst: general -- galaxies: high-redshift -- galaxies: ISM -- galaxies: photometry -- galaxies: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz1039
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We present a study of 21 dark gamma-ray burst (GRB) host galaxies, predominantly using X-ray afterglows obtained with the Chandra X-Ray Observatory ( CXO ) to precisely locate the burst in deep Hubble Space Telescope ( HST ) imaging of the burst region. The host galaxies are well-detected in F160W in all but one case and in F606W imaging in 60 per cent of cases. We measure magnitudes and perform a morphological analysis of each galaxy. The asymmetry, concentration, and ellipticity of the dark burst hosts are compared against the host galaxies of optically bright GRBs. In agreement with other studies, we find that dark GRB hosts are redder and more luminous than the bulk of the GRB host population. The distribution of projected spatial offsets for dark GRBs from their host galaxy centroids is comparable to that of optically bright bursts. The dark GRB hosts are physically larger, more massive and redder, but are morphologically similar to the hosts of bright GRBs in terms of concentration and asymmetry. Our analysis constrains the fraction of high redshift ( z > 5) GRBs in the sample to 14 per cent, implying an upper limit for the whole long-GRB population of ≤4.4 per cent. If dust is the primary cause of afterglow darkening amongst dark GRBs, the measured extinction may require a clumpy dust component in order to explain the observed offset and ellipticity distributions.