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

被引：18

作者：

Shvartzvald, Y. ^{[1
]}

Waxman, E. ^{[1
]}

Gal-Yam, A. ^{[1
]}

Ofek, E. O. ^{[1
]}

Ben-Ami, S. ^{[1
]}

Berge, D. ^{[2
,3
]}

Kowalski, M. ^{[2
,3
]}

Buehler, R. ^{[2
]}

Worm, S. ^{[2
]}

Rhoads, J. E. ^{[4
]}

Arcavi, I. ^{[5
,6
]}

Maoz, D. ^{[5
]}

Polishook, D. ^{[7
]}

Stone, N. ^{[8
]}

Trakhtenbrot, B. ^{[5
]}

Ackermann, M. ^{[2
]}

Aharonson, O. ^{[9
,10
]}

Birnholtz, O. ^{[11
]}

Chelouche, D. ^{[12
,13
]}

Guetta, D. ^{[14
]}

Hallakoun, N. ^{[1
]}

Horesh, A. ^{[8
]}

Kushnir, D. ^{[1
]}

Mazeh, T. ^{[5
]}

Nordin, J. ^{[3
]}

Ofir, A. ^{[9
]}

Ohm, S. ^{[2
]}

Parsons, D. ^{[2
]}

Peer, A. ^{[11
]}

Perets, H. B. ^{[15
,16
]}

Perdelwitz, V. ^{[9
]}

Poznanski, D. ^{[5
]}

Sadeh, I. ^{[2
]}

Sagiv, I. ^{[17
]}

Shahaf, S. ^{[1
]}

Soumagnac, M. ^{[11
]}

Tal-Or, L. ^{[14
,18
]}

Van Santen, J. ^{[2
]}

Zackay, B. ^{[1
]}

Guttman, O. ^{[1
]}

Rekhi, P. ^{[1
]}

Townsend, A. ^{[3
]}

Weinstein, A. ^{[19
]}

Wold, I. ^{[4
]}

机构：

[1] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel

[2] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

[3] Humboldt Univ, Humboldt Universitzau Berlin, D-12489 Berlin, Germany

[4] Goddard Space Flight Ctr, NASA, Greenbelt, MD 20771 USA

[5] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[6] CIFAR Azrieli Global Scholars Program, CIFAR, Toronto, ON, Canada

[7] Weizmann Inst Sci, Fac Phys, Rehovot, Israel

[8] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel

[9] Weizmann Inst Sci, Rehovot, Israel

[10] Planetary Sci Inst, Honolulu, HI 96822 USA

[11] Bar Ilan Univ, Dept Phys, R Ramat Gan, Israel

[12] Univ Haifa, Fac Nat Sci, Dept Phys, Haifa, Israel

[13] Univ Haifa, Haifa Res Ctr Theoret Phys & Astrophys, Haifa, Israel

[14] Ariel Univ, Dept Phys, IL-40700 Ariel, Israel

[15] Technion Israel Inst Technol, Phys Dept, IL-3200002 Haifa, Israel

[16] Open Univ Israel, Dept Nat Sci, 1 Univ Rd,POB 808, IL-4353701 Raanana, Israel

[17] ElOp Elbit Syst Ltd, Rehovot, Israel

[18] Ariel Univ, Astrophys Geophys & Space Sci Res Ctr, IL-40700 Ariel, Israel

[19] Tufts Univ, Medford, MA 02155 USA

来源：

ASTROPHYSICAL JOURNAL | 2024年 / 964卷 / 01期

基金：

以色列科学基金会; 欧洲研究理事会;

关键词：

TIDAL DISRUPTION EVENTS; NEUTRON-STAR MERGER; DIGITAL SKY SURVEY; ZWICKY TRANSIENT FACILITY; ACTIVE GALACTIC NUCLEI; SUPERNOVA SHOCK BREAKOUT; CHANGING-LOOK QUASAR; OPTICAL CONTINUUM EMISSION; GALAXY-EVOLUTION-EXPLORER; RADIATION MEDIATED SHOCKS;

D O I：

10.3847/1538-4357/ad2704

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 deg2) and near-ultraviolet (NUV; 230-290 nm) sensitivity (22.5 mag, 5 sigma, 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.

引用

页数：29

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