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PreviewIssue DateTitleAuthor(s)
2013Erratum: 3 to 12 millimetre studies of dense gas towards the western rim of supernova remnant rx j1713.7-3946Maxted, N.; Rowell, G.; Dawson, B.; Burton, M.; Nicholas, B.; Fukui, Y.; Walsh, A.; Kawamura, A.; Horachi, H.; Sano, H.
2010GRB 081008: From burst to afterglow and the transition phase in betweenRowell, G.
201112mm line survey of the dense molecular gas towards the W28 field TeV gamma-ray sourcesNicholas, B.; Rowell, G.; Burton, M.; Walsh, A.; Fukui, Y.; Kawamura, A.; Longmore, S.; Keto, E.
2010H.E.S.S. observations of massive stellar clustersOhm, S.; Horns, D.; Reimer, O.; Hinton, J.; Rowell, G.; de Ona Wilhelmi, E.; Fernandes, M.; Acero, F.; Marcowith, A.; High Energy Phenomena in Massive Stars Conference (2009 : Jaén, Spain)
2010Constraints on the cosmic ray diffusion coefficient in the W28 region from gamma-ray observationsGabici, S.; Casanova, S.; Aharonian, F.; Rowell, G.; Société Française d’Astronomie et d’Astrophysique (2010 : Marseille, France)
2011The ground-based large-area wide-angle γ-ray and cosmic-ray experiment HiSCORETluczykont, M.; Hampf, D.; Horns, D.; Kneiske, T.; Eichler, R.; Nachtigall, R.; Rowell, G.
2014The carbon inventory in a quiescent, filamentary molecular cloud in G328Burton, M.; Ashley, M.; Braiding, C.; Storey, J.; Kulesa, C.; Hollenbach, D.; Wolfire, M.; Gluck, C.; Rowell, G.
2012A study of dense molecular gas towards galactic TeV γ-ray sourcesde Wilt, P.; Rowell, G.; Dawson, B.; Walsh, A.; Burton, M.; Brooks, K.; Rathborne, J.; Aharonian, F.; International Meeting on High Energy Gamma-Ray Astronomy (5th : 9-13 July 2012 : Heidelberg, Germany)
2012Dense gas towards the RXJ1713.7-3946 supernova remnantMaxted, N.; Rowell, G.; Dawson, B.; Burton, M.; Fukui, Y.; Walsh, A.; Kawamura, A.; Sano, H.; Lazendic, J.; International Meeting on High Energy Gamma-Ray Astronomy (5th : 2012 : Heidelberg, Germany)
2014HESS J1640-465 - an exceptionally luminous TeV γ-ray supernova remnantAbramowski, A.; de Wilt, P.; Dickinson, H.; Maxted, N.; Mayer, M.; Rowell, G.