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000600606 0247_ $$2arXiv$$aarXiv:2304.14482
000600606 0247_ $$2inspire$$a2655389
000600606 0247_ $$2datacite_doi$$a10.3204/PUBDB-2023-08030
000600606 037__ $$aPUBDB-2023-08030
000600606 041__ $$aEnglish
000600606 088__ $$2arXiv$$aarXiv:2304.14482
000600606 1001_ $$0P:(DE-HGF)0$$aShvartzvald, Y.$$b0$$eCorresponding author
000600606 245__ $$aULTRASAT: A wide-field time-domain UV space telescope
000600606 260__ $$c2023
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000600606 500__ $$a40 pages, 16 figures, 3 tables. Submitted to the AAS journals
000600606 520__ $$aThe Ultraviolet Transient Astronomy Satellite (ULTRASAT) is scheduled to be launched to geostationary orbit in 2026. It will carry a telescope with an unprecedentedly large field of view (204 deg$^2$) and NUV (230-290nm) sensitivity (22.5 mag, 5$\sigma$, at 900s). ULTRASAT will conduct the first wide-field survey of transient and variable NUV sources and will revolutionize our ability to study the hot transient universe: It will explore a new parameter space in energy and time-scale (months long light-curves with minutes cadence), with an extra-Galactic volume accessible for the discovery of transient sources that is $>$300 times larger than that of GALEX and comparable to that of LSST. ULTRASAT data will be transmitted to the ground in real-time, and transient alerts will be distributed to the community in $<$15 min, enabling a vigorous ground-based follow-up of ULTRASAT sources. ULTRASAT will also provide an all-sky NUV image to $>$23.5 AB mag, over 10 times deeper than the GALEX map. Two key science goals of ULTRASAT are the study of mergers of binaries involving neutron stars, and supernovae: With a large fraction ($>$50%) of the sky instantaneously accessible, fast (minutes) slewing capability and a field-of-view that covers the error ellipses expected from GW detectors beyond 2025, ULTRASAT will rapidly detect the electromagnetic emission following BNS/NS-BH mergers identified by GW detectors, and will provide continuous NUV light-curves of the events; ULTRASAT will provide early (hour) detection and continuous high (minutes) cadence NUV light curves for hundreds of core-collapse supernovae, including for rarer supernova progenitor types.
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000600606 693__ $$0EXP:(DE-H253)ULTRASAT-20211201$$5EXP:(DE-H253)ULTRASAT-20211201$$eUltraviolet Transient Astronomy Satellite$$x0
000600606 7001_ $$aWaxman, E.$$b1
000600606 7001_ $$aGal-Yam, A.$$b2
000600606 7001_ $$aOfek, E. O.$$b3
000600606 7001_ $$aBen-Ami, S.$$b4
000600606 7001_ $$0P:(DE-H253)PIP1080570$$aBerge, D.$$b5$$udesy
000600606 7001_ $$0P:(DE-H253)PIP1006050$$aKowalski, Marek$$b6$$udesy
000600606 7001_ $$0P:(DE-H253)PIP1018733$$aBühler, Rolf$$b7$$udesy
000600606 7001_ $$0P:(DE-H253)PIP1089976$$aWorm, S.$$b8$$udesy
000600606 7001_ $$aRhoads, J. E.$$b9
000600606 7001_ $$aArcavi, I.$$b10
000600606 7001_ $$aMaoz, D.$$b11
000600606 7001_ $$aPolishook, D.$$b12
000600606 7001_ $$aStone, N.$$b13
000600606 7001_ $$aTrakhtenbrot, B.$$b14
000600606 7001_ $$0P:(DE-H253)PIP1014130$$aAckermann, Markus$$b15$$udesy
000600606 7001_ $$aAharonson, O.$$b16
000600606 7001_ $$aBirnholtz, O.$$b17
000600606 7001_ $$aChelouche, D.$$b18
000600606 7001_ $$aGuetta, D.$$b19
000600606 7001_ $$aHallakoun, N.$$b20
000600606 7001_ $$aHoresh, A.$$b21
000600606 7001_ $$aKushnir, D.$$b22
000600606 7001_ $$aMazeh, T.$$b23
000600606 7001_ $$0P:(DE-H253)PIP1032718$$aNordin, J.$$b24
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000600606 7001_ $$0P:(DE-H253)PIP1092852$$aParsons, D.$$b27
000600606 7001_ $$aPe'er, A.$$b28
000600606 7001_ $$aPerets, H. B.$$b29
000600606 7001_ $$aPerdelwitz, V.$$b30
000600606 7001_ $$aPoznanski, D.$$b31
000600606 7001_ $$0P:(DE-H253)PIP1006066$$aSadeh, I.$$b32$$udesy
000600606 7001_ $$aSagiv, I.$$b33
000600606 7001_ $$aShahaf, S.$$b34
000600606 7001_ $$aSoumagnac, M.$$b35
000600606 7001_ $$aTal-Or, L.$$b36
000600606 7001_ $$0P:(DE-H253)PIP1007258$$aVan Santen, J.$$b37$$udesy
000600606 7001_ $$aZackay, B.$$b38
000600606 7001_ $$aGuttman, O.$$b39
000600606 7001_ $$aRekhi, P.$$b40
000600606 7001_ $$0P:(DE-H253)PIP1101637$$aTownsend, A.$$b41
000600606 7001_ $$aWeinstein, A.$$b42
000600606 7001_ $$aWold, I.$$b43
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