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

J. HjorthDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, DenmarkAndrew J. LevanDepartment of Physics, University of Warwick, Coventry CV4 7AL, UKNial R. TanvirDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKJoe D. LymanDepartment of Physics, University of Warwick, Coventry CV4 7AL, UKRadosław WojtakDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, DenmarkSophie L. SchrøderDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, DenmarkIlya MandelBirmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UKChrista GallDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, DenmarkSofie H. BruunDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark

2017en

ABI

Annotatsiya

The historic detection of gravitational waves from a binary neutron star merger (GW170817) and its electromagnetic counterpart led to the first accurate (sub-arcsecond) localization of a gravitational-wave event. The transient was found to be ∼1000 from the nucleus of the S0 galaxy NGC 4993. We report here the luminosity distance to this galaxy using two independent methods. (1) Based on our MUSE/VLT measurement of the heliocentric redshift (zhelio = 0.009783±0.000023) we infer the systemic recession velocity of the NGC 4993 group of galaxies in the cosmic microwave background (CMB) frame to be vCMB = 3231±53 km s−1 . Using constrained cosmological simulations we estimate the line-of-sight peculiar velocity to be vpec = 307±230 km s−1 , resulting in a cosmic velocity of vcosmic = 2924±236 km s−1 (zcosmic = 0.00980±0.00079) and a distance of Dz = 40.4±3.4 Mpc assuming a local Hubble constant of H0 = 73.24± 1.74 km s−1Mpc−1 . (2) Using Hubble Space Telescope measurements of the effective radius (15. 005±1. 005) and contained intensity and MUSE/VLT measurements of the velocity dispersion, we place NGC 4993 on the Fundamental Plane (FP) of E and S0 galaxies. Comparing to a frame of 10 clusters containing 226 galaxies, this yields a distance estimate of DFP = 44.0±7.5 Mpc. The combined redshift and FP distance is DNGC4993 = 41.0±3.1 Mpc. This ‘electromagnetic’ distance estimate is consistent with the independent measurement of the distance to GW170817 as obtained from the gravitational-wave signal (DGW = 43.8 +2.9 −6.9 Mpc) and confirms that GW170817 occurred in NGC 4993.

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DOI: 10.3847/2041-8213/aa9110

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