adsabs/AstroCLIMB huggingface dataset:
Paper: 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
Authors: A. Hajela, R. Margutti, J. S. Bright, K. D. Alexander, B. D. Metzger, V. Nedora, A. Kathirgamaraju, B. Margalit, D. Radice, C. Guidorzi, E. Berger, A. MacFadyen, D. Giannios, R. Chornock, I. Heywood, L. Sironi, O. Gottlieb, D. Coppejans, T. Laskar, Y. Cendes, R. Barniol Duran, T. Eftekhari, W. Fong, A. McDowell, M. Nicholl, X. Xie, J. Zrake, S. Bernuzzi, F. S. Broekgaarden, C. D. Kilpatrick, G. Terreran, V. A. Villar, P. K. Blanchard, S. Gomez, G. Hosseinzadeh, D. J. Matthews, J. C. Rastinejad
Figure caption: Left panel: nonthermal emission from GW 170817 across the electromagnetic spectrum and best-fitting universal post-jet-break model, as explained in Section 4, with t start = 196 days. Right panel: nonthermal emission from GW 170817 and best-fitting jet-afterglow model computed with JetFit for n = 0.01 cm−3, ϵ  e  = 0.1, and γ B = 12 fixed. In both panels, empty symbols were not included in the fitting procedure but are shown here for completeness adopting a flux calibration consistent with the afterglow models. Colored bands identify the 68% flux confidence interval. The gray empty square symbol is the peak pixel value within one synthesized beam at the location of GW 170817 at 3 GHz from Balasubramanian et al. (2021). The bottom subplots show the difference between observations and the best-fitting models as derived from the model posteriors, and expressed in units of 1σ data uncertainties for displaying purposes.
Paper: 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
Authors: A. Hajela, R. Margutti, J. S. Bright, K. D. Alexander, B. D. Metzger, V. Nedora, A. Kathirgamaraju, B. Margalit, D. Radice, C. Guidorzi, E. Berger, A. MacFadyen, D. Giannios, R. Chornock, I. Heywood, L. Sironi, O. Gottlieb, D. Coppejans, T. Laskar, Y. Cendes, R. Barniol Duran, T. Eftekhari, W. Fong, A. McDowell, M. Nicholl, X. Xie, J. Zrake, S. Bernuzzi, F. S. Broekgaarden, C. D. Kilpatrick, G. Terreran, V. A. Villar, P. K. Blanchard, S. Gomez, G. Hosseinzadeh, D. J. Matthews, J. C. Rastinejad
Figure caption: Top panel: universal post-jet-break model distributions. Expected 1 keV flux density distributions at 939.31 and 1234.11 days (histograms in color) are derived from fitting the post-peak multiwavelength afterglow of GW 170817 in the post-jet-break regime with F  ν  ∝ ν −β  t −α  (where β = (p − 1)/2 and α = p) in the time range t start < δ t < 900 days for a variety of choices of t start. Bottom panel: JetFit model distributions. Expected 1 keV flux density distributions at 939.31 and 1234.11 days (histograms in color) derived from the fitting of the multiwavelength afterglow of GW 170817 in the time range 2 < δ t < 900 days using the code JetFit (using different values of γ B). Both panels: the vertical blue thick line and shaded area show the observed X-ray flux density at the corresponding epoch and ±1σ confidence range, respectively, for which the flux calibration was performed by conservatively assuming a jet-afterglow spectrum (Sections 2.2–4).