B. O'Connor (GWU/UMD), E. Troja (Tor Vergata),
on behalf of a larger collaboration:
The Chandra X-ray Observatory (CXO) carried out observations of GW170817
starting at 1671 d post-merger (ObsIDs: 25733, 25734; PI: Troja) for 59.4
an additional epoch was performed starting at 1734 d (ObsID: 25527) for
The data were re-processed and the astrometry corrected following Troja et
2020, MNRAS, 4, 5643. In the 0.5-8 keV energy range we measure 2 counts
a 1" aperture centered on the X-ray position. A background contribution
of about 0.85 counts was estimated from adjacent source-free regions.
Following Kraft, Burrows, and Nousek (1991), we derive a 95% upper limit of
<5.5 source counts, yielding a rate of <6E-5 cts/s in the combined 95.8 ks.
This corresponds to a 0.3-10 keV flux limit of 1.3E-15 erg/cm2/s for a
power-law with photon index of 1.585. This limit is comparable to the value
measured at 1234 d (1.6E-15 erg/cm2/s; Troja et al. 2022, MNRAS, 510, 1902),
and does not show evidence for a rebrightening of the X-ray emission.
By combining this new epoch with the CXO observations acquired in
December 2021 at 1575 d (Hajela et al. 2021, GCN 31231), we obtain
a weak (3-sigma) detection with an average count-rate of 3E-05 cts/s,
and a 0.3-10 keV flux of ~0.6E-15 erg/cm2/s.
An updated light curve can be found at this link:
We thank the Chandra staff for scheduling these observations.