The Environment of the Binary Neutron Star Merger GW170817

被引：115

作者：

Levan, A. J. ^{[1
]}

Lyman, J. D. ^{[1
]}

Tanvir, N. R. ^{[2
]}

Hjorth, J. ^{[3
]}

Mandel, I. ^{[4
,5
]}

Stanway, E. R. ^{[1
]}

Steeghs, D. ^{[1
]}

Fruchter, A. S. ^{[6
]}

Troja, E. ^{[7
,8
]}

Schroder, S. L. ^{[3
]}

Wiersema, K. ^{[2
]}

Bruun, S. H. ^{[3
]}

Cano, Z. ^{[9
]}

Cenko, S. B. ^{[8
,10
]}

de Ugarte Postigo, A. ^{[3
,9
]}

Evans, P. ^{[2
]}

Fairhurst, S. ^{[11
]}

Fox, O. D. ^{[6
]}

Fynbo, J. P. U. ^{[3
]}

Gompertz, B. ^{[1
]}

Greiner, J. ^{[12
]}

Im, M. ^{[13
,14
]}

Izzo, L. ^{[9
]}

Jakobsson, P. ^{[15
]}

Kangas, T. ^{[6
]}

Khandrika, H. G. ^{[6
]}

Lien, A. Y. ^{[8
,16
]}

Malesani, D. ^{[3
]}

O'Brien, P. ^{[2
]}

Osborne, J. P. ^{[2
]}

Palazzi, E. ^{[17
]}

Pian, E. ^{[17
]}

Perley, D. A. ^{[18
]}

Rosswog, S. ^{[19
]}

Ryan, R. E. ^{[6
]}

Schulze, S. ^{[20
]}

Sutton, P. ^{[11
]}

Thone, C. C. ^{[9
]}

Watson, D. J. ^{[3
]}

Wijers, R. A. M. J. ^{[21
]}

机构：

[1] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[2] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[3] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark

[4] Univ Birmingham, Birmingham Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England

[5] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

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

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

[8] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[9] CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain

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

[11] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[12] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85740 Garching, Germany

[13] Seoul Natl Univ, CEOU, Seoul, South Korea

[14] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea

[15] Univ Iceland, Sci Inst, Ctr Astrophys & Cosmol, Dunhagi 5, IS-107 Reykjavik, Iceland

[16] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA

[17] Inst Space Astrophys & Cosm Phys, INAF, Via Gobetti 101, I-40129 Bologna, Italy

[18] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[19] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden

[20] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-761000 Rehovot, Israel

[21] Univ Amsterdam, Anton Pannekoek Inst Astron, Postbus 94249, NL-1090 GE Amsterdam, Netherlands

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 848卷 / 02期

基金：

欧洲研究理事会; 瑞典研究理事会;

关键词：

galaxies: individual (NGC 4993); galaxies: kinematics and dynamics; stars: neutron; GAMMA-RAY BURSTS; GLOBULAR-CLUSTERS; BLACK-HOLES; GALAXIES; DISCOVERY; MODELS; RATES; GAS; ZOO;

D O I：

10.3847/2041-8213/aa905f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present Hubble Space Telescope (HST) and Chandra imaging, combined with Very Large Telescope MUSE integral field spectroscopy of the counterpart and host galaxy of the first binary neutron star merger detected via gravitational-wave emission by LIGO and Virgo, GW170817. The host galaxy, NGC 4993, is an S0 galaxy at z - 0.009783. There is evidence for large, face-on spiral shells in continuum imaging, and edge-on spiral features visible in nebular emission lines. This suggests that NGC 4993 has undergone a relatively recent (less than or similar to 1 Gyr) "dry" merger. This merger may provide the fuel for a weak active nucleus seen in Chandra imaging. At the location of the counterpart, HST imaging implies there is no globular or young stellar cluster, with a limit of a few thousand solar masses for any young system. The population in the vicinity is predominantly old with less than or similar to 1% of any light arising from a population with ages <500 Myr. Both the host galaxy properties and those of the transient location are consistent with the distributions seen for short-duration gamma-ray bursts, although the source position lies well within the effective radius (r(e) similar to 3 kpc), providing an r(e)-normalized offset that is closer than similar to 90% of short GRBs. For the long delay time implied by the stellar population, this suggests that the kick velocity was significantly less than the galaxy escape velocity. We do not see any narrow host galaxy interstellar medium features within the counterpart spectrum, implying low extinction, and that the binary may lie in front of the bulk of the host galaxy.

引用

页数：9

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