Mr. Irfan

Founder Member:   

Mr. Irfan (M.Sc. Physics, B.Ed.)

Citations – 05
h-index – 1
i10-index – 1

Main Research Areas: 

Galaxy groups and clusters (using X-ray, radio & optical observations), Study of AGN feedback in the hot gas environment via X-ray cavities, shocks, cold fronts, gas sloshing, cluster dynamics, metal enrichment, the study of X-ray point sources, cluster merging systems, radio halos and relics, quenching and triggering star formation by AGN activity etc., and co-evolution of SMBH and galaxies.

Biography:

Mr. Irfan obtained an M.Sc. in Physics from the School of Physical Sciences, Swami Ramanand Teerth Marathwada University, Nanded, in 20??. She is a final year PhD Astrophysics student at the same university. 

Research description

Her research interests are in galaxy groups and clusters. This study is based on multiwavelength data. Currently, involved in the following research topics:

  1. Feedback from active galactic nuclei (AGN):

The issue of AGN feedback is not yet fully understood. Despite extensive discussions in the literature, it is still not clear how an AGN transfers its power to the diffuse ambient plasma. Recently, there has been great interest in the process of “AGN feedback”, its role in galaxy formation, and the possibility that AGN feedback solves the over-cooling problem. Key issues include the effect of AGN feedback in regulating the cooling of the intra-cluster medium, how AGNs are fuelled in groups and clusters, and the physics of the balance between heating and cooling process in the cores of groups and clusters. I am currently involved studies of samples of groups and clusters that that aims to improve our understanding of AGN feedback processes.

  1. Investigation of X-ray cavities:

X-ray cavities have been detected in a large number of clusters, and are expected to arise due to AGN feedback. However, little information is available is on X-ray cavities at high redshifts, and it is not clear if and how AGN heating evolves across time. According to cosmological simulations, currently black holes are in the “radio mode” of accretion (i.e. a mechanical mode), which involves accretion at sub-Eddington rates and the driving of powerful outflows, whereas at earlier times ( z >> 1), the “quasar mode” (i.e. a radiative mode) dominates, corresponding to a merger-driven phase where the black hole grows rapidly. I am trying to investigate when and how this transition occurs in high-redshift systems.

 

 

Last Updated on August 20, 2022 by Sonkamble Satish