Distance and properties of NGC 4993 as the host galaxy of a gravitational wave source, GW170817

Abstract

Recently, the optical counterpart of a gravitational wave source GW170817 has been identified in NGC 4993 galaxy. Together with evidence from observations in electromagnetic waves, the event has been suggested as a result of a merger of two neutron stars. We analyze the multi-wavelength data to characterize the host galaxy property and its distance to examine if the properties of NGC 4993 are consistent with this picture. Our analysis shows that NGC 4993 is a bulge-dominated galaxy with reff ~ 2-3 kpc and the Sersic index of n = 3-4 for the bulge component. The spectral energy distribution from 0.15 to 24 micron indicates that this galaxy has no significant ongoing star formation, the mean stellar mass of (0.3 - 1.2) times 10^11 Msun,the mean stellar age greater than ~3 Gyr, and the metallicity of about 20% to 100% of solar abundance. Optical images reveal dust lanes and extended features that suggest a past merging activity. Overall, NGC 4993 has characteristics of normal, but slightly disturbed elliptical galaxies. Furthermore, we derive the distance to NGC 4993 with the fundamental plane relation using 17 parameter sets of 7 different filters and the central stellar velocity dispersion from literature, finding an angular diameter distance of 37.7 +- 8.7 Mpc. NGC 4993 is similar to some host galaxies of short gamma-ray bursts but much different from those of long gamma-ray bursts, supporting the picture of GW170817 as a result of a merger of two NSs.

7 pages, 2 figures, 3 tables, accepted for publication in ApJL

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Cited by in corpus (7)

• Brightening X-ray Emission from GW170817/GRB170817A: Further Evidence for an Outflow
• On the Progenitor of Binary Neutron Star Merger GW170817
• Host galaxies of merging compact objects: mass, star formation rate, metallicity and colours
• Double Neutron Star Formation: Merger Times, Systemic Velocities, and Travel Distances
• Determine the Lorentz factor and the viewing angle of GRB 170817A
• Subsequent Nonthermal Emission due to the Kilonova Ejecta in GW 170817
• Binary Neutron Star (BNS) merger: What we learned from relativistic ejecta of GW/GRB~170817A