Accurate flux calibration of GW170817: is the X-ray counterpart on the rise?. (arXiv:2104.13378v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Troja_E/0/1/0/all/0/1">E. Troja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+OConnor_B/0/1/0/all/0/1">B. O'Connor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryan_G/0/1/0/all/0/1">G. Ryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_L/0/1/0/all/0/1">L. Piro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_R/0/1/0/all/0/1">R. Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">B. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piran_T/0/1/0/all/0/1">T. Piran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruni_G/0/1/0/all/0/1">G. Bruni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cenko_S/0/1/0/all/0/1">S. B. Cenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eerten_H/0/1/0/all/0/1">H. van Eerten</a>
X-ray emission from the gravitational wave transient GW170817 is well
described as non-thermal afterglow radiation produced by a structured
relativistic jet viewed off-axis. We show that the X-ray counterpart continues
to be detected at 3.3 years after the merger. Such long-lasting signal is not a
prediction of the earlier jet models characterized by a narrow jet core and a
viewing angle of about 20 deg, and is spurring a renewed interest in the origin
of the X-ray emission. We present a comprehensive analysis of the X-ray dataset
aimed at clarifying existing discrepancies in the literature, and in particular
the presence of an X-ray rebrightening at late times. Our analysis does not
find evidence for an increase in the X-ray flux, but confirms a growing tension
between the observations and the jet model. Further observations at radio and
X-ray wavelengths would be critical to break the degeneracy between models.
X-ray emission from the gravitational wave transient GW170817 is well
described as non-thermal afterglow radiation produced by a structured
relativistic jet viewed off-axis. We show that the X-ray counterpart continues
to be detected at 3.3 years after the merger. Such long-lasting signal is not a
prediction of the earlier jet models characterized by a narrow jet core and a
viewing angle of about 20 deg, and is spurring a renewed interest in the origin
of the X-ray emission. We present a comprehensive analysis of the X-ray dataset
aimed at clarifying existing discrepancies in the literature, and in particular
the presence of an X-ray rebrightening at late times. Our analysis does not
find evidence for an increase in the X-ray flux, but confirms a growing tension
between the observations and the jet model. Further observations at radio and
X-ray wavelengths would be critical to break the degeneracy between models.
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