Enabling kilonova science with Nancy Grace Roman Space Telescope

被引：11

作者：

Andreoni, Igor ^{[1
,2
,3
]}

Coughlin, Michael W. ^{[4
]}

Criswell, Alexander W. ^{[4
]}

Bulla, Mattia ^{[5
,6
,7
]}

Toivonen, Andrew ^{[4
]}

Singer, Leo P. ^{[8
]}

Palmese, Antonella ^{[9
]}

Burns, E. ^{[10
]}

Gezari, Suvi ^{[11
,12
]}

Kasliwal, Mansi M. ^{[13
]}

Kiendrebeogo, R. Weizmann ^{[4
,14
,15
]}

Mahabal, Ashish ^{[13
]}

Moriya, Takashi J. ^{[16
,17
]}

Rest, Armin ^{[18
,19
]}

Scolnic, Dan ^{[20
]}

Simcoe, Robert A.

Soon, Jamie ^{[22
]}

Stein, Robert ^{[13
,21
]}

Travouillon, Tony ^{[23
]}

机构：

[1] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[2] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[3] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA

[4] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[5] Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy

[6] INFN, Sez Ferrara, Via Saragat 1, I-44122 Ferrara, Italy

[7] INAF, Osservatorio Astron Abruzzo, Via Mentore Maggini snc, I-64100 Teramo, Italy

[8] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Code 661, Greenbelt, MD 20771 USA

[9] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA

[10] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

[11] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[12] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA

[13] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[14] Univ Joseph KI ZERBO, Lab Phys & Chim Environm, Ouagadougou, Burkina Faso

[15] Univ Cote Azur, Artemis, Observ Cote Azur, Blvd Observ, F-06304 Nice, France

[16] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[17] Monash Univ, Fac Sci, Sch Phys & Astron, Clayton, Vic 3800, Australia

[18] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[19] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[20] Duke Univ, Dept Phys, Durham, NC 27708 USA

[21] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[22] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia

[23] Australian Natl Univ, Adv Instrumentat & Technol Ctr, Res Sch Astron & Astrophys, Mt Stromlo Observ,Cotter Rd, Weston, Australia

来源：

ASTROPARTICLE PHYSICS | 2024年 / 155卷

基金：

美国国家科学基金会;

关键词：

Surveys; Gravitational waves; Kilonova; Multi-messenger; Neutron stars; NEUTRON-STAR MERGERS; EQUATION-OF-STATE; GAMMA-RAY BURST; RADIOACTIVELY POWERED EMISSION; TRANSIENT FACILITY SEARCHES; INFRARED LIGHT CURVES; GRAVITATIONAL-WAVE; ELECTROMAGNETIC COUNTERPART; HUBBLE CONSTANT; MULTIMESSENGER CONSTRAINTS;

D O I：

10.1016/j.astropartphys.2023.102904

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Binary neutron star mergers and neutron star-black hole mergers are multi-messenger sources that can be detected in gravitational waves and in electromagnetic radiation. The low electron fraction of neutron star merger ejecta favors the production of heavy elements such as lanthanides and actinides via rapid neutron capture (r-process). The decay of these unstable nuclei powers an infrared-bright transient called a "kilonova". The discovery of a population of kilonovae will allow us to determine if neutron star mergers are the dominant sites for r-process element nucleosynthesis, constrain the equation of state of nuclear matter, and make independent measurements of the Hubble constant. The Nancy Grace Roman Space Telescope (Roman) will have a unique combination of depth, near-infrared sensitivity, and wide field of view. These characteristics will enable Roman's discovery of GW counterparts that will be missed by optical telescopes, such as kilonova that are associated with large distances, high lanthanide fractions, high binary mass-ratios, large dust extinction in the line of sight, or that are observed from equatorial viewing angles. In preparation for Roman's launch and operations, our analysis suggests to (i) make available a rapid (similar to 1 week) Target of Opportunity mode for GW follow-up; (ii) include observations of the High Latitude Time-Domain survey footprint in at least two filters (preferably the F158 and F213 filters) with a cadence of less than or similar to 8 days; (iii) operate in synergy with Rubin Observatory. Following these recommendations, we expect that 1-6 kilonovae can be identified by Roman via target of opportunity observations of well localized (A < 10 deg(2), 90% C.I.) neutron star mergers during 1.5 years of the LIGO-Virgo-KAGRA fifth (or similar to 4-21 in during the sixth) observing run. A sample of 5-40 serendipitously discovered kilonovae can be collected in a 5-year high latitude survey.

引用

页数：15

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