The Distance to NGC 4993: The Host Galaxy of the Gravitational-wave Event GW170817

Hjorth, J.; Levan, A. J.; Tanvir, N. R.; Lyman, J.; Wojtak, Radosław; Schröder, S.; Mandel, Ilya; Gall, C.; Bruun, S. H.

doi:10.3847/2041-8213/aa9110

Cited by 150 publications

(148 citation statements)

References 33 publications

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“…The precise distance and localization gave the follow-up with optical wide-field imagers a flying start (for a comprehensive review see Abbott et al 2017a). Coulter et al (2017a) targeted galaxies at this distance and detected a new object, SSS17a (IAU identification: AT2017gfo; Coulter et al 2017b Levan et al 2017; for a detailed discussion see also Hjorth et al 2017). 23 This discovery was confirmed by several teams including Allam et al (2017), Melandri et al (2017), Tanvir & Levan (2017a), and Yang et al (2017).…”

Section: Introductionmentioning

confidence: 50%

ALMA and GMRT Constraints on the Off-axis Gamma-Ray Burst 170817A from the Binary Neutron Star Merger GW170817

Kim

Schulze

Resmi

et al. 2017

ApJL

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Binary neutron-star mergers (BNSMs) are among the most readily detectable gravitational-wave (GW) sources with the Laser Interferometer Gravitational-wave Observatory (LIGO). They are also thought to produce short γ-ray bursts (SGRBs) and kilonovae that are powered by r-process nuclei. Detecting these phenomena simultaneously would provide an unprecedented view of the physics during and after the merger of two compact objects. Such a Rosetta Stone event was detected by LIGO/Virgo on 2017 August 17 at a distance of ∼44Mpc. We monitored the position of the BNSM with Atacama Large Millimeter/submillimeter Array (ALMA) at 338.5 GHz and the Giant Metrewave Radio Telescope (GMRT) at 1.4 GHz, from 1.4 to 44 days after the merger. Our observations rule out any afterglow more luminous than´--3 10 erg s Hz 26 1 1 in these bands, probing >2-4 dex fainter than previous SGRB limits. We match these limits, in conjunction with public data announcing the appearance of X-ray and radio emission in the weeks after the GW event, to templates of off-axis afterglows. Our broadband modeling suggests that GW170817 was accompanied by an SGRB and that the γ-ray burst (GRB) jet, powered byẼ 10 AG,iso 50 erg, had a half-opening angle of~ 20 , and was misaligned by~ 41 from our line of sight. The data are also consistent with a more collimated jet:Ẽ 10 AG,iso 51 erg, q q ~ 5 , 17. This is the most conclusive detection of an off-axis GRB afterglow and the first associated with a BNSM-GW event to date. We use the viewing angle estimates to infer the initial bulk Lorentz factor and true energy release of the burst.

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Section: Introductionmentioning

confidence: 50%

ALMA and GMRT Constraints on the Off-axis Gamma-Ray Burst 170817A from the Binary Neutron Star Merger GW170817

Kim

Schulze

Resmi

et al. 2017

ApJL

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“…So far, the only one known (by gravitational waves) host galaxy of BNS merger is NGC4993 from GW170817 event. This galaxy present a very high mass and a low star formation rates (Im et al 2017;Blanchard et al 2017;Hjorth et al 2017;Levan et al 2017;Pan et al 2017). The host galaxy of GRB150101B presented as a analogue of GRB170817A (Troja et al 2018) is also a vary massive galaxy.…”

Section: Introductionmentioning

confidence: 99%

Optimizing gravitational waves follow-up using galaxies stellar mass

Ducoin

Corre

Leroy

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a new strategy to optimise the electromagnetic follow-up of gravitational wave triggers. This method is based on the widely used galaxy targeting approach where we add the stellar mass of galaxies in order to prioritise the more massive galaxies. We crossmatched the GLADE galaxy catalog with the AllWISE catalog up to 400Mpc with an efficiency of ∼93%, and derived stellar masses using a stellar-to-mass ratio using the WISE1 band luminosity. We developed a new grade to rank galaxies combining their 3D localisation probability associated to the gravitational wave event with the new stellar mass information. The efficiency of this new approach is illustrated with the GW170817 event, which shows that its host galaxy, NGC4993, is ranked at the first place using this new method. The catalog, named Mangrove, is publicly available and the ranking of galaxies is automatically provided through a dedicated web site for each gravitational wave event.

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“…It has a measured redshift from our MUSE data of z=0.009783, corresponding to a distance of 42.5 Mpc assuming a Hubble expansion with H 69.6 0 = km s −1 and neglecting any peculiar velocity (see Hjorth et al 2017 for further details of the distance to NGC 4993). Based on photometry in 1′apertures, it has an absolute K-band magnitude of M 21.5…”

Section: Morphology and Dynamicsmentioning

confidence: 99%

The Environment of the Binary Neutron Star Merger GW170817

Levan

Lyman

Tanvir

et al. 2017

ApJL

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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 ( 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 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 3 e~k pc), providing an r e -normalized offset that is closer than 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.

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The Distance to NGC 4993: The Host Galaxy of the Gravitational-wave Event GW170817

Cited by 150 publications

References 33 publications

ALMA and GMRT Constraints on the Off-axis Gamma-Ray Burst 170817A from the Binary Neutron Star Merger GW170817

ALMA and GMRT Constraints on the Off-axis Gamma-Ray Burst 170817A from the Binary Neutron Star Merger GW170817

Optimizing gravitational waves follow-up using galaxies stellar mass

The Environment of the Binary Neutron Star Merger GW170817

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