Статья

ULTRASAT: A Wide-field Time-domain UV Space Telescope

Yossi ShvartzvaldDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]Eli WaxmanDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]A. Gal‐YamDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]E. O. OfekDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]Sagi Ben-AmiDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]D. BergeDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyM. KowalskiDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyR. BühlerDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyS. D. WormDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyJ. E. RhoadsNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAIair ArcaviCIFAR Azrieli Global Scholars program, CIFAR, Toronto, CanadaDan MaozSchool of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, IsraelD. PolishookFaculty of Physics, Weizmann Institute of Science, Rehovot 7610001, IsraelNicholas C. StoneRacah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, IsraelBenny TrakhtenbrotSchool of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, IsraelM. AckermannDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyO. AharonsonHelen Kimmel Center for Planetary Science, Weizmann Institute of Science, Rehovot, IsraelO. BirnholtzDepartment of Physics, Bar-Ilan University, Ramat-Gan 52900, IsraelDoron CheloucheDepartment of Physics, Faculty of Natural Sciences, University of Haifa, Haifa 3498838, IsraelD. GuettaDepartment of Physics, Ariel University, Ariel, IL-40700, IsraelN. HallakounDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]A. HoreshRacah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, IsraelDoron KushnirDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]T. MazehSchool of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, IsraelJ. NordinInstitut fur Physik, Humboldt-Universitzäu Berlin, D-12489 Berlin, GermanyA. OfirHelen Kimmel Center for Planetary Science, Weizmann Institute of Science, Rehovot, IsraelS. OhmDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyD. ParsonsDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyAsaf Pe’erDepartment of Physics, Bar-Ilan University, Ramat-Gan 52900, IsraelH. B. PeretsDepartment of Natural Sciences, The Open University of Israel, 1 University Road, P.O. Box 808, Raanana 4353701, IsraelV. PerdelwitzHelen Kimmel Center for Planetary Science, Weizmann Institute of Science, Rehovot, IsraelD. PoznanskiSchool of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, IsraelI. SadehDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyIlan SagivElOp—Elbit Systems Ltd., Rehovot, IsraelS. ShahafDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]Maayane T. SoumagnacDepartment of Physics, Bar-Ilan University, Ramat-Gan 52900, IsraelL. Tal-OrAstrophysics Geophysics And Space Science Research Center, Ariel University, Ariel 40700, IsraelJ. Van SantenDeutsches Elektronen Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, GermanyBarak ZackayDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]O. GuttmanDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]Param RekhiDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel; [email protected]A. TownsendInstitut fur Physik, Humboldt-Universitzäu Berlin, D-12489 Berlin, GermanyA. WeinsteinTufts University, Medford, MA 02155, USAIsak WoldNASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

2024en

ABI

Аннотация

Abstract The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is scheduled to be launched to geostationary orbit in 2027. It will carry a telescope with an unprecedentedly large field of view (204 deg 2 ) and near-ultraviolet (NUV; 230–290 nm) sensitivity (22.5 mag, 5 σ , at 900 s). 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 timescale (months-long light curves with minutes cadence), with an extragalactic volume accessible for the discovery of transient sources that is >300 times larger than that of the Galaxy Evolution Explorer (GALEX) and comparable to that of the Vera Rubin Observatory’s Legacy Survey of Space and Time. ULTRASAT data will be transmitted to the ground in real time, and transient alerts will be distributed to the community in <15 minutes, enabling 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 gravitational-wave (GW) detectors beyond 2026, ULTRASAT will rapidly detect the electromagnetic emission following binary neutron star/neutron star–black hole mergers identified by GW detectors, and will provide continuous NUV light curves of the events. ULTRASAT will provide early (hour) detection and continuous high-cadence (minutes) NUV light curves for hundreds of core-collapse supernovae, including for rarer supernova progenitor types.

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Идентификаторы

DOI: 10.3847/1538-4357/ad2704

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Цитирований: 3Использованных источников: 0

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