The Optical Afterglow of GW170817: An Off-axis Structured Jet and Deep Constraints on a Globular Cluster Origin

W. Fong, P. K. Blanchard, K. D. Alexander, J. Strader, R. Margutti, A. Hajela, V. A. Villar, Y. Wu, C. S. Ye, E. Berger, R. Chornock, D. Coppejans, P. S. Cowperthwaite, T. Eftekhari, D. Giannios, C. Guidorzi, A. Kathirgamaraju, T. Laskar, A. Macfadyen, B. D. MetzgerM. Nicholl, K. Paterson, G. Terreran, D. J. Sand, L. Sironi, P. K.G. Williams, X. Xie, J. Zrake

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Abstract

We present a revised and complete optical afterglow light curve of the binary neutron star merger GW170817, enabled by deep Hubble Space Telescope (HST) F606W observations at ≈584 days post-merger, which provide a robust optical template. The light curve spans ≈110-362 days, and is fully consistent with emission from a relativistic structured jet viewed off-axis, as previously indicated by radio and X-ray data. Combined with contemporaneous radio and X-ray observations, we find no spectral evolution, with a weighted average spectral index of , demonstrating that no synchrotron break frequencies evolve between the radio and X-ray bands over these timescales. We find that an extrapolation of the post-peak temporal slope of GW170817 to the luminosities of cosmological short gamma-ray bursts matches their observed jet break times, suggesting that their explosion properties are similar, and that the primary difference in GW170817 is viewing angle. Additionally, we place a deep limit on the luminosity and mass of an underlying globular cluster (GC) of L ≲ 6.7 × 103 L o, or M ≲ 1.3 × 104 M o, at least 4 standard deviations below the peak of the GC mass function of the host galaxy, NGC 4993. This limit provides a direct and strong constraint that GW170817 did not form and merge in a GC. As highlighted here, HST (and soon the James Webb Space Telescope) enables critical observations of the optical emission from neutron star merger jets and outflows.

Original languageEnglish
Article numberL1
JournalAstrophysical Journal Letters
Volume883
Issue number1
DOIs
Publication statusPublished - 17 Sept 2019

Funding

W. Fong P. K. Blanchard K. D. Alexander J. Strader R. Margutti A. Hajela V. A. Villar Y. Wu C. S. Ye E. Berger R. Chornock D. Coppejans P. S. Cowperthwaite T. Eftekhari D. Giannios C. Guidorzi A. Kathirgamaraju T. Laskar A. Macfadyen B. D. Metzger M. Nicholl K. Paterson G. Terreran D. J. Sand L. Sironi P. K. G. Williams X. Xie J. Zrake W. Fong P. K. Blanchard K. D. Alexander J. Strader R. Margutti A. Hajela V. A. Villar Y. Wu C. S. Ye E. Berger R. Chornock D. Coppejans P. S. Cowperthwaite T. Eftekhari D. Giannios C. Guidorzi A. Kathirgamaraju T. Laskar A. Macfadyen B. D. Metzger M. Nicholl K. Paterson G. Terreran D. J. Sand L. Sironi P. K. G. Williams X. Xie J. Zrake Center for Interdisciplinary Exploration and Research in Astrophysics and Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208-3112, USA Center for Astrophysics∣Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA Center for Cosmology and Particle Physics, New York University, 726 Broadway New York, NY 10003, USA Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USA Observatories of the Carnegie Institute for Science, 813 Santa Barbara Street, Pasadena, CA 91101-1232, USA Department of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA Dipartimento di Fisica, Universit� Ferrara, Via Paradiso 12, I-44100 Ferrara, Italy Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA Department of Physics, University of Bath, Claverton Down, Bath BA2 7AY, UK Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill EH9 3HJ, UK Birmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA American Astronomical Society, 1667 K Street NW, Suite 800, Washington, DC 20006-1681, USA Mathematical Sciences and STAG Research Centre, University of Southampton, Southampton SO17 1BJ, UK NASA Einstein Fellow. NASA Hubble Fellow. W. Fong, P. K. Blanchard, K. D. Alexander, J. Strader, R. Margutti, A. Hajela, V. A. Villar, Y. Wu, C. S. Ye, E. Berger, R. Chornock, D. Coppejans, P. S. Cowperthwaite, T. Eftekhari, D. Giannios, C. Guidorzi, A. Kathirgamaraju, T. Laskar, A. Macfadyen, B. D. Metzger, M. Nicholl, K. Paterson, G. Terreran, D. J. Sand, L. Sironi, P. K. G. Williams, X. Xie and J. Zrake 2019-09-20 2019-09-17 17:20:41 cgi/release: Article released bin/incoming: New from .zip NASA - Space Telescope Science Institute HST-GO-15606.001-A NASA - Smithsonian Astrophysical Observatory G09-20058A National Science Foundation AST-1814782 National Science Foundation AST-1909358 yes We present a revised and complete optical afterglow light curve of the binary neutron star merger GW170817, enabled by deep Hubble Space Telescope ( HST ) F606W observations at ≈584 days post-merger, which provide a robust optical template. The light curve spans ≈110–362 days, and is fully consistent with emission from a relativistic structured jet viewed off-axis, as previously indicated by radio and X-ray data. Combined with contemporaneous radio and X-ray observations, we find no spectral evolution, with a weighted average spectral index of , demonstrating that no synchrotron break frequencies evolve between the radio and X-ray bands over these timescales. We find that an extrapolation of the post-peak temporal slope of GW170817 to the luminosities of cosmological short gamma-ray bursts matches their observed jet break times, suggesting that their explosion properties are similar, and that the primary difference in GW170817 is viewing angle. Additionally, we place a deep limit on the luminosity and mass of an underlying globular cluster (GC) of L �≲�6.7�נ10 3 L ⊙ , or M �≲�1.3�נ10 4 M ⊙ , at least 4 standard deviations below the peak of the GC mass function of the host galaxy, NGC�4993. 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ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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