most citedDetection of Thermal Emission from an Extrasolar Planet

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astro-ph200516 cited

Multi-Wavelength Studies of the Optically Dark Gamma-Ray Burst 001025A

K. Pedersen, K. Hurley, J. Hjorth +18

We identify the fading X-ray afterglow of GRB 001025A from XMM-Newton observations obtained 1.9-2.3 days, 2 years, and 2.5 years after the burst. The non-detection of an optical co…

astro-ph2005

The Opacity of Spiral Galaxy Disks: dust opacity from calibrated counts of distant galaxies

B. W. Holwerda, R. A. Gonzalez, Ronald J. Allen +1

The opacity of foreground spiral disks can be probed from the number of distant galaxies seen through them. To calibrate this number for effects other than the dust extinction, Gon…

astro-ph200579 cited

Gamma-Ray Burst Selected High Redshift Galaxies: Comparison to Field Galaxy Populations to z~3

C. J. Conselice, P. M. Vreeswijk, A. S. Fruchter +6

We study the internal structural properties of 37 long duration gamma-ray burst (GRB) host galaxies imaged with the Hubble Space Telescope. Fitting exponential disk and r^1/4 model…

astro-ph2005131 cited

Definitive Identification of the Transition between Small- to Large-Scale Clustering for Lyman Break Galaxies

M Ouchi, T. Hamana, K. Shimasaku +9

We report angular correlation function (ACF) of Lyman Break Galaxies (LBGs) with unprecedented statistical quality on the basis of 16,920 LBGs at z=4 detected in the 1 deg^2 sky of…

astro-ph2005126 cited

On the nature of nearby GRB/SN host galaxies

J. Sollerman, G. Ostlin, J. P. U. Fynbo +3

We present and discuss optical diagnostics of the low redshift (z<0.2) galaxies that are known to have hosted supernovae associated with gamma-ray bursts (GRBs). The three galaxies…

astro-ph200595 cited

Ly-alpha and UV emission from high-redshift GRB hosts: To what extent do GRBs trace star formation?

P. Jakobsson, G. Bjornsson, J. P. U. Fynbo +9

We report the result of a search for Ly-alpha emission from the host galaxies of the gamma-ray bursts (GRBs) 030226 (z = 1.986), 021004 (z = 2.335) and 020124 (z = 3.198). We find…