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A correlation between the H i 21-cm absorption strength and impact parameter in external galaxies

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 459:4 (2016) 4136-4143

Authors:

SJ Curran, SN Reeves, JR Allison, EM Sadler
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The diversity of Type II supernova versus the similarity in their progenitors

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 459:4 (2016) 3939-3962

Authors:

S Valenti, DA Howell, MD Stritzinger, ML Graham, G Hosseinzadeh, I Arcavi, L Bildsten, A Jerkstrand, C McCully, A Pastorello, AL Piro, D Sand, SJ Smartt, G Terreran, C Baltay, S Benetti, P Brown, AV Filippenko, M Fraser, D Rabinowitz, M Sullivan, F Yuan
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Spectropolarimetry of superluminous supernovae: insight into their geometry

(2016)

Authors:

C Inserra, M Bulla, SA Sim, SJ Smartt
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The Tully-Fisher Relation of COLD GASS Galaxies

(2016)

Authors:

Alfred L Tiley, Martin Bureau, Amélie Saintonge, Selcuk Topal, Timothy A Davis, Kazufumi Torii
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Corrigendum: A large light-mass component of cosmic rays at 1017-1017.5 electronvolts from radio observations.

Nature Nature Publishing Group 537:7621 (2016) 572

Authors:

S Buitink, A Corstanje, H Falcke, T Huege, A Nelles, JP Rachen, L Rossetto, P Schellart, O Scholten, S Ter Veen, S Thoudam, TNG Trinh, J Anderson, A Asgekar, IM Avruch, ME Bell, MJ Bentum, G Bernardi, P Best, A Bonafede, F Breitling, JW Broderick, WN Brouw, M Brüggen, HR Butcher, D Carbone, B Ciardi, JE Conway, F de Gasperin, E de Geus, A Deller, R-J Dettmar, G van Diepen, S Duscha, J Eislöffel, D Engels, JE Enriquez, RA Fallows, Robert P Fender, C Ferrari, W Frieswijk, MA Garrett, JM Grießmeier, AW Gunst, van van Haarlem, TE Hassall, G Heald, JWT Hessels, M Hoeft

Abstract:

In this Letter, we omitted to cite preliminary results from the low-energy extension of the Pierre Auger Observatory, as presented at the International Cosmic Ray Conference 2015 (ref. 1). Figure 1 of this Corrigendum shows measurements of the average value of Xmax for the Low Frequency Array (LOFAR), and earlier experiments using different techniques, now including the data from the Pierre Auger Observatory1 , specifically the contribution of A. Porcelli. Our values are in agreement with those of ref. 1 within systematic uncertainties.
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