Hintze Centre for Astrophysical Surveys

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JINGLE, a JCMT legacy survey of dust and gas for galaxy evolution studies - I. Survey overview and first results

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 481:3 (2018) 3497-3519

Authors:

Amelie Saintonge, Christine D Wilson, Ting Xiao, Lihwai Lin, Ho Seong Hwang, Tomoka Tosaki, Martin Bureau, Phillip J Cigan, Christopher JR Clark, David L Clements, Ilse De Looze, Thavisha Dharmawardena, Yang Gao, Walter K Gear, Joshua Greenslade, Isabella Lamperti, Jong Chul Lee, Cheng Li, Michal J Michalowski, Angus Mok, Hsi-An Pan, Anne E Sansom, Mark Sargent, Matthew WL Smith, Thomas Williams, Chentao Yang, Ming Zhu, Gioacchino Accurso, Pauline Barmby, Elias Brinks, Nathan Bourne, Toby Brown, Aeree Chung, Eun Jung Chung, Anna Cibinel, Kristen Coppin, Jonathan Davies, Timothy A Davis, Steve Eales, Lapo Fanciullo, Taotao Fang, Yu Gao, David HW Glass, Haley L Gomez, Thomas Greve, Jinhua He, Luis C Ho, Feng Huang, Hyunjin Jeong, Xuejian Jiang, Qian Jiao, Francisca Kemper, Ji Hoon Kim, Minjin Kim, Taehyun Kim, Jongwan Ko, Xu Kong, Kevin Lacaille, Cedric G Lacey, Bumhyun Lee, Joon Hyeop Lee, Wing-Kit Lee, Karen Masters, Se-Heon Oh, Padelis Papadopoulos, Changbom Park, Sung-Joon Park, Harriet Parsons, Kate Rowlands, Peter Scicluna, Jillian M Scudder, Ramya Sethuram, Stephen Serjeant, Yali Shao, Yun-Kyeong Sheen, Yong Shi, Hyunjin Shim, Connor MA Smith, Kristine Spekkens, An-Li Tsai, Aprajita Verma, Sheona Urquhart, Giulio Violino, Serena Viti, David Wake, Junfeng Wang, Jan Wouterloot, Yujin Yang, Kijeong Yim, Fangting Yuan, Zheng Zheng
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SPIRITS 16tn in NGC 3556: A Heavily Obscured and Low-luminosity Supernova at 8.8 Mpc

ASTROPHYSICAL JOURNAL 863:1 (2018) ARTN 20

Authors:

Jacob E Jencson, Mansi M Kasliwal, Scott M Adams, Howard E Bond, Ryan M Lau, Joel Johansson, Assaf Horesh, Kunal P Mooley, Robert Fender, Kishalay De, Donal O'Sullivan, Frank J Masci, Ann Marie Cody, Nadia Blagorodnova, Ori D Fox, Robert D Gehrz, Peter A Milne, Daniel A Perley, Nathan Smith, Schuyler D Van Dyk
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The KMOS Redshift One Spectroscopic Survey (KROSS): the origin of disc turbulence in z ≈ 1 star-forming galaxies

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 474:4 (2018) 5076-5104

Authors:

HL Johnson, CM Harrison, AM Swinbank, AL Tiley, JP Stott, RG Bower, Ian Smail, AJ Bunker, D Sobral, OJ Turner, P Best, M Bureau, M Cirasuolo, MJ Jarvis, G Magdis, RM Sharples, J Bland-Hawthorn, B Catinella, L Cortese, SM Croom, C Federrath, K Glazebrook, SM Sweet, JJ Bryant, M Goodwin, IS Konstantopoulos, JS Lawrence, AM Medling, MS Owers, S Richards
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WISDOM Project - III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 473:3 (2018) 3818-3834

Authors:

Timothy A Davis, Martin Bureau, Kyoko Onishi, Freeke van de Voort, Michele Cappellari, Satoru Iguchi, Lijie Liu, Eve V North, Marc Sarzi, Mark D Smith
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A radio counterpart to a neutron star merger

Science American Association for the Advancement of Science 358:6370 (2017) 1579-1583

Authors:

G Hallinan, A Corsi, KP Mooley, K Hotokezaka, E Nakar, MM Kasliwal, DL Kaplan, DA Frail, ST Myers, T Murphy, K De, D Dobie, James Allison, KW Bannister, V Bhalerao, P Chandra, TE Clarke, S Giacintucci, AYQ Ho, A Horesh, NE Kassim, E Lenc, FJ Lockman, C Lynch, D Nichols, S Nissanke, N Palliyaguru, T Piran, J Rana, EM Sadler, LP Singer

Abstract:

Gravitational waves have been detected from a binary neutron star merger event, GW170817. The detection of electromagnetic radiation from the same source has shown that the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Earth. We report the detection of a counterpart radio source that appears 16 days after the event, allowing us to diagnose the energetics and environment of the merger. The observed radio emission can be explained by either a collimated ultrarelativistic jet, viewed off-axis, or a cocoon of mildly relativistic ejecta. Within 100 days of the merger, the radio light curves will enable observers to distinguish between these models, and the angular velocity and geometry of the debris will be directly measurable by very long baseline interferometry.
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