GCN Circular 34059

G. Waratkar (IITB), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

We have carried out a search for X-ray candidates in Astrosat CZTI data in a 100-sec window around the trigger time of the event Fermi GBM-230619 (UTC 2023-06-19 19:25:22.3; Wood et al., GCN Circ. 34054
Not found
 
 
). We use the Event1_healpix_combined.fit map (https://zenodo.org/record/8067512) for our analysis. CZTI is a coded aperture mask instrument that has a considerable effective area for about 29% of the entire sky but is also sensitive to brighter transients from the entire sky. At the time of the event, Astrosat's nominal pointing is RA, DEC = 10:38:32.1, -10:07:25.1 (159.6337,-10.1236), which is ~72 deg away from the maximum probability location, which severely reduces the effective area of CZTI. At the time of the event, the Earth-satellite-transient angle corresponding to the maximum probability location is ~151 deg and hence is not occulted by Earth in the satellite's frame. In a time interval of 100 sec around the event, the region of the joint Fermi-LVK localisation map not occulted by Earth in the satellite's frame has a total probability of 1.0 (100%).

CZTI data were de-trended to remove orbit-wise background variation. We then searched data from the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in background count rates were estimated by using data from 5 preceding orbits. We selected confidence levels such that the probability of a false trigger in a 100-sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV.

We use a detailed mass model of the satellite to calculate the direction-dependent instrument response for points in the visible sky. We then assume the source is modeled as a power law with photon index alpha = -1, and convert our count rate upper limits to direction-dependent flux limits. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability-weighted mean over the visible sky:

0.1 s: flux limit= 2.20e-05 ergs/cm^2/s; fluence limit = 2.20e-06 ergs/cm^2
1.0 s: flux limit= 4.13e-06 ergs/cm^2/s; fluence limit = 4.13e-06 ergs/cm^2
10.0 s: flux limit= 6.35e-07 ergs/cm^2/s; fluence limit = 6.35e-06 ergs/cm^2

We also carried out a similar search for X-ray candidates in a 100-sec window around the trigger time of the event S230619bd (UTC 2023-06-19 19:25:06.4). We report that the region of localisation map bayestar.multiorder.fits,1 map (https://gracedb.ligo.org/api/superevents/S230619bd/files/S230619bd_bayestar.multiorder.fits,1) which is not occulted by Earth in the satellite's frame has a total probability of 0.62 (62%). At the time of the event, the Earth-satellite-transient angle corresponding to the maximum probability location is ~147 deg and hence is not occulted by Earth in the satellite's frame. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability-weighted mean over the visible sky for this skymap:

0.1 s: flux limit= 2.12e-05 ergs/cm^2/s; fluence limit = 2.12e-06 ergs/cm^2
1.0 s: flux limit= 4.00e-06 ergs/cm^2/s; fluence limit = 4.00e-06 ergs/cm^2
10.0 s: flux limit= 6.14e-07 ergs/cm^2/s; fluence limit = 6.14e-06 ergs/cm^2

CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.

CZTI GRB detections are reported regularly on the payload site at:
http://astrosat.iucaa.in/czti/?q=emgw