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Spotting clusters and Hunting for extragalactic planets: a combined study of galaxy clusters in the Optical and X-ray regime.

Presentation #512.03D in the session “Galaxy Clusters Observations”.

Published onJan 11, 2021
Spotting clusters and Hunting for extragalactic planets: a combined study of galaxy clusters in the Optical and X-ray regime.

Observational studies of the distribution of galaxies in the Universe reveals inhomogeneity and structure on Mpc and larger scales. Galaxy clusters are the largest gravitationally bound structures containing a virialized assembly of galaxies; therefore, studying them is significant for understanding the constitution and assembly history of these systems and probing the large-scale structure of the Universe. The Swift AGN and cluster survey is a serendipitous X-ray survey aimed at building a large X-ray selected cluster catalog with 1200 cluster detections expected by its final release. In my thesis work, I perform an optical follow-up analysis of 348 ( out of 442) X-ray selected cluster candidates from the Swift cluster catalog using multi-band imaging from MDM 2.4m and the Pan-STARRS survey for the northern sky, and CTIO 4m and DES for the southern sky. I report the optical confirmation of 226 clusters with > 2 sigma galaxy over-density with photometric redshift estimates extending upto z~0.8. I will present the constraints on the cluster mass function and the correlations between various cluster properties for the detected SACS clusters. I will also be discussing the prospects and science case for identifying the remaining high redshift clusters with Infrared observations using NOAO/APO. Another facet of my dissertation involves using quasar microlensing to probe the intracluster region of a galaxy cluster. I employ this novel technique to exert effective constraints on planet-mass objects in two extragalactic systems, Q J0158-4325 and SDSS J1004+4112, by studying their induced microlensing signatures. Chandra observations for these two gravitationally-lensed quasars reveal variations of the emission line peak energy which can be explained as microlensing of the FeKalpha emission region surrounding the supermassive blackhole, induced by planet-mass microlenses. To corroborate this, I have performed microlensing simulations and developed an edge detection algorithm to determine the probability of caustic transiting events. Comparison with the observed rates has yielded constraints on the substellar population, with masses ranging from Lunar to Jovian mass bodies, within these galaxy or cluster scale structures. My results suggest that unbound planet-mass objects are universal in galaxies, and these are surmised to be either free-floating planets or primordial black holes. These are first-ever constraints on the substellar mass distribution in the intracluster light of a galaxy cluster. This analysis yields the most stringent limit for primordial black holes at the mass range.


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