Deep Chandra observations will provide the needed superior angular resolution to perform this study, and will �definitively constrain the presence of X-ray emission from a persistent source such as an AGN (Fig. 1). If the Chandra observations yield a detection, we will be able to pinpoint the source of the emission to &lt; 0:500 precision and trace it to a galaxy in our HST imaging. This would also allow us to subtract the AGN contribution from the early X-ray emission for a proper re-analysis of the data. If detected, it will most likely originate from the host galaxy itself, as the expected number of sources from X-ray number counts with FX > 2:5 10-15 erg s-1 cm-2 (the limit of our proposed Chandra observations, see next section) within a random 500-radius region is only 2:4x10-3 (Bauer et al., 2004). If the Chandra observations yield a non-detection, this would rule out a persistent AGN, and would significantly strengthen the claim that the excess originates from the central engine. Such an observation would be a milestone in GRB studies, as the nature of the central engine and its impact on the electromagnetic emission is a decades-long open question.
|Effective start/end date||2/17/20 → 2/16/22|
- Smithsonian Astrophysical Observatory (GO0-21041X//NAS803060)
- National Aeronautics and Space Administration (GO0-21041X//NAS803060)
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