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dc.contributorSchool of Physics, University of New South Wales, Sydney, NSW 2052, Australia; Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG, Northern Ireland, UK
dc.contributorAustralian Astronomical Observatory, 105 Delhi Road, North Ryde, NSW 2113, Australia
dc.contributorCentre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Mail Number H29, Hawthorn, VIC 3122, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Sydney, NSW 2006, Australia
dc.contributorAustralian National University, Canberra, ACT 2611, Australia
dc.contributorPurple Mountain Observatory, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China
dc.contributorSchool of Astronomy and Space Science, Nanjing University, Nanjing 210008, China
dc.contributorNanjing Institute of Astronomical Optics & Technology, Chinese Academy of Sciences, 188 Bancang Street, Nanjing 210042, China
dc.contributorSchool of Physics, University of New South Wales, Sydney, NSW 2052, Australia
dc.contributorCentre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Mail Number H29, Hawthorn, VIC 3122, Australia
dc.contributorPurple Mountain Observatory, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China; Texas A&M University, College Station, Texas 77843, USA
dc.contributor.authorBurton, Michael G.
dc.contributor.authorZheng, Jessica
dc.contributor.authorMould, Jeremy
dc.contributor.authorCooke, Jeff
dc.contributor.authorIreland, Michael
dc.contributor.authorUddin, Syed Ashraf
dc.contributor.authorZhang, Hui
dc.contributor.authorYuan, Xiangyan
dc.contributor.authorLawrence, Jon
dc.contributor.authorAshley, Michael C. B.
dc.contributor.authorWu, Xuefeng
dc.contributor.authorCurtin, Chris
dc.contributor.authorWang, Lifan
dc.date.accessioned2024-02-21T11:03:33Z
dc.date.available2024-02-21T11:03:33Z
dc.date.issued2016-09-01T00:00:00Z
dc.identifier.doi10.1017/pasa.2016.38
dc.identifier.doi10.48550/arXiv.1608.02345
dc.identifier.other2016arXiv160802345B
dc.identifier.otherastro-ph.IM
dc.identifier.otherastro-ph.GA
dc.identifier.other2016PASA...33...47B
dc.identifier.other10.48550/arXiv.1608.02345
dc.identifier.other10.1017/pasa.2016.38
dc.identifier.otherarXiv:1608.02345
dc.identifier.other2016arXiv160802345B
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1874
dc.description.abstractThe high Antarctic plateau provides exceptional conditions for infrared observations on account of the cold, dry and stable atmosphere above the ice surface. This paper describes the scientific goals behind the first program to examine the time-varying universe in the infrared from Antarctica - the Kunlun Infrared Sky Survey (KISS). This will employ a 50cm telescope to monitor the southern skies in the 2.4μmK <SUB>dark</SUB> window from China's Kunlun station at Dome A, on the summit of the Antarctic plateau, through the uninterrupted 4-month period of winter darkness. An earlier paper discussed optimisation of the K <SUB>dark</SUB> filter for sensitivity (Li et al. 2016). This paper examines the scientific program for KISS. We calculate the sensitivity of the camera for the extrema of observing conditions that will be encountered. We present the parameters for sample surveys that could then be carried out for a range of cadences and sensitivities. We then discuss several science programs that could be conducted with these capabilities, involving star formation, brown dwarfs and hot Jupiters, exoplanets around M dwarfs, the terminal phases of stellar evolution, fast transients, embedded supernova searches, reverberation mapping of AGN, gamma ray bursts and the detection of the cosmic infrared background.
dc.publisherPublications of the Astronomical Society of Australia
dc.titleScientific Goals of the Kunlun Infrared Sky Survey (KISS)
dc.typearticle
dc.source.journalPASA
dc.source.journalPASA...33
dc.source.volume33
refterms.dateFOA2024-02-21T11:03:33Z
dc.identifier.bibcode2016PASA...33...47B


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