Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component
Abstract
For the first ~3 yrs after the binary neutron star merger event GW 170817, the radio and X-ray radiation has been dominated by emission from a structured relativistic off-axis jet propagating into a low-density medium with n < 0.01 cm-3. We report on observational evidence for an excess of X-ray emission at δt > 900 days after the merger. With Lx ≈ 5 × 1038 erg s-1 at 1234 days, the recently detected X-ray emission represents a ≥ 3.2σ (Gaussian equivalent) deviation from the universal post-jet-break model that best fits the multiwavelength afterglow at earlier times. In the context of JetFit afterglow models, current data represent a departure with statistical significance ≥ 3.1σ, depending on the fireball collimation, with the most realistic models showing excesses at the level of ≥ 3.7σ. A lack of detectable 3 GHz radio emission suggests a harder broadband spectrum than the jet afterglow. These properties are consistent with the emergence of a new emission component such as synchrotron radiation from a mildly relativistic shock generated by the expanding merger ejecta, i.e., a kilonova afterglow. In this context, we present a set of ab initio numerical relativity binary neutron star (BNS) merger simulations that showmore »
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- Northwestern Univ., Evanston, IL (United States)
- Univ. of California, Berkeley, CA (United States)
- Columbia Univ., New York, NY (United States); Flatiron Institute, New York, NY (United States)
- Max Planck Institute for Gravitational Physics, Potsdam (Germany); Univ. of Potsdam (Germany)
- California Institute of Technology (CalTech), Pasadena, CA (United States)
- Pennsylvania State Univ., University Park, PA (United States)
- Univ. of Ferrara (Italy); Istituto Nazionale di Fisica Nucleare (INFN), Ferrara (Italy); Istituto Nazionale di Astrofisica (INAF), Bologna (Italy)
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
- New York Univ. (NYU), NY (United States). Center for Cosmology and Particle Physics
- Purdue Univ., West Lafayette, IN (United States)
- Univ. of Oxford (United Kingdom); Rhodes Univ., Makhanda (South Africa); South African Radio Astronomy Observatory, Cape Town (South Africa)
- Columbia Univ., New York, NY (United States)
- Northwestern Univ., Evanston, IL (United States); Univ. of Warwick, Coventry (United Kingdom)
- Radboud Univ., Nijmegen (Netherlands)
- California State University, Sacramento, CA (United States)
- New York Univ. (NYU), NY (United States)
- Univ. of Birmingham (United Kingdom)
- Univ. of Southampton (United Kingdom)
- Clemson Univ., SC (United States)
- Friedrich Schiller Univ., Jena (Germany)
- Las Cumbres Observatory, Goleta, CA (United States); Univ. of California, Santa Barbara, CA (United States)
- Space Telescope Science Institute, Baltimore, MD (United States)
- Univ. of Arizona, Tucson, AZ (United States). Steward Observatory
- Publication Date:
- Research Org.:
- Pennsylvania State Univ., University Park, PA (United States); NASA
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP)
- OSTI Identifier:
- 1865195
- Grant/Contract Number:
- SC0021177; AST-1909796; AST-1944985; G09-20058A; 15606; 80NSSC19K1422
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal. Letters
- Additional Journal Information:
- Journal Volume: 927; Journal Issue: 1; Journal ID: ISSN 2041-8205
- Publisher:
- IOP Publishing
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; gamma ray bursts; neutron stars; gravitational wave sources; X-ray transient sources; radio transient sources
Citation Formats
Hajela, A., Margutti, R., Bright, J. S., Alexander, K. D., Metzger, B. D., Nedora, V., Kathirgamaraju, A., Margalit, B., Radice, D., Guidorzi, C., Berger, E., MacFadyen, A., Giannios, D., Chornock, R., Heywood, I., Sironi, L., Gottlieb, O., Coppejans, D., Laskar, T., Cendes, Y., Duran, R. Barniol, Eftekhari, T., Fong, W., McDowell, A., Nicholl, M., Xie, X., Zrake, J., Bernuzzi, S., Broekgaarden, F. S., Kilpatrick, C. D., Terreran, G., Villar, V. A., Blanchard, P. K., Gomez, S., Hosseinzadeh, G., Matthews, D. J., and Rastinejad, J. C. Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component. United States: N. p., 2022.
Web. doi:10.3847/2041-8213/ac504a.
Hajela, A., Margutti, R., Bright, J. S., Alexander, K. D., Metzger, B. D., Nedora, V., Kathirgamaraju, A., Margalit, B., Radice, D., Guidorzi, C., Berger, E., MacFadyen, A., Giannios, D., Chornock, R., Heywood, I., Sironi, L., Gottlieb, O., Coppejans, D., Laskar, T., Cendes, Y., Duran, R. Barniol, Eftekhari, T., Fong, W., McDowell, A., Nicholl, M., Xie, X., Zrake, J., Bernuzzi, S., Broekgaarden, F. S., Kilpatrick, C. D., Terreran, G., Villar, V. A., Blanchard, P. K., Gomez, S., Hosseinzadeh, G., Matthews, D. J., & Rastinejad, J. C. Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component. United States. https://doi.org/10.3847/2041-8213/ac504a
Hajela, A., Margutti, R., Bright, J. S., Alexander, K. D., Metzger, B. D., Nedora, V., Kathirgamaraju, A., Margalit, B., Radice, D., Guidorzi, C., Berger, E., MacFadyen, A., Giannios, D., Chornock, R., Heywood, I., Sironi, L., Gottlieb, O., Coppejans, D., Laskar, T., Cendes, Y., Duran, R. Barniol, Eftekhari, T., Fong, W., McDowell, A., Nicholl, M., Xie, X., Zrake, J., Bernuzzi, S., Broekgaarden, F. S., Kilpatrick, C. D., Terreran, G., Villar, V. A., Blanchard, P. K., Gomez, S., Hosseinzadeh, G., Matthews, D. J., and Rastinejad, J. C. Tue .
"Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component". United States. https://doi.org/10.3847/2041-8213/ac504a. https://www.osti.gov/servlets/purl/1865195.
@article{osti_1865195,
title = {Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component},
author = {Hajela, A. and Margutti, R. and Bright, J. S. and Alexander, K. D. and Metzger, B. D. and Nedora, V. and Kathirgamaraju, A. and Margalit, B. and Radice, D. and Guidorzi, C. and Berger, E. and MacFadyen, A. and Giannios, D. and Chornock, R. and Heywood, I. and Sironi, L. and Gottlieb, O. and Coppejans, D. and Laskar, T. and Cendes, Y. and Duran, R. Barniol and Eftekhari, T. and Fong, W. and McDowell, A. and Nicholl, M. and Xie, X. and Zrake, J. and Bernuzzi, S. and Broekgaarden, F. S. and Kilpatrick, C. D. and Terreran, G. and Villar, V. A. and Blanchard, P. K. and Gomez, S. and Hosseinzadeh, G. and Matthews, D. J. and Rastinejad, J. C.},
abstractNote = {For the first ~3 yrs after the binary neutron star merger event GW 170817, the radio and X-ray radiation has been dominated by emission from a structured relativistic off-axis jet propagating into a low-density medium with n < 0.01 cm-3. We report on observational evidence for an excess of X-ray emission at δt > 900 days after the merger. With Lx ≈ 5 × 1038 erg s-1 at 1234 days, the recently detected X-ray emission represents a ≥ 3.2σ (Gaussian equivalent) deviation from the universal post-jet-break model that best fits the multiwavelength afterglow at earlier times. In the context of JetFit afterglow models, current data represent a departure with statistical significance ≥ 3.1σ, depending on the fireball collimation, with the most realistic models showing excesses at the level of ≥ 3.7σ. A lack of detectable 3 GHz radio emission suggests a harder broadband spectrum than the jet afterglow. These properties are consistent with the emergence of a new emission component such as synchrotron radiation from a mildly relativistic shock generated by the expanding merger ejecta, i.e., a kilonova afterglow. In this context, we present a set of ab initio numerical relativity binary neutron star (BNS) merger simulations that show that an X-ray excess supports the presence of a high-velocity tail in the merger ejecta, and argues against the prompt collapse of the merger remnant into a black hole. Radiation from accretion processes on the compact-object remnant represents a viable alternative. Neither a kilonova afterglow nor accretion-powered emission have been observed before, as detections of BNS mergers at this phase of evolution are unprecedented},
doi = {10.3847/2041-8213/ac504a},
journal = {The Astrophysical Journal. Letters},
number = 1,
volume = 927,
place = {United States},
year = {Tue Mar 08 00:00:00 EST 2022},
month = {Tue Mar 08 00:00:00 EST 2022}
}
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