| Name: Aratrik Basu |
| Affiliation: Indian Institute of Science Education and Research - Mohali |
| Conference ID: ASI2026_1036 |
| Title: Chandra and multiwavelength observations of NGC 4321 to study the X-ray binary population and hot gas |
| Abstract Type: Poster |
| Abstract Category: Galaxies and Cosmology |
| Author(s) and Co-Author(s) with Affiliation: Aratrik Basu(Indian Institute of Science Education and Research, Mohali - 140306, India), Smita Mathur(Ohio State University, Columbus - 43210, USA), Kulinder Pal Singh(Indian Institute of Science Education and Research, Mohali - 140306, India) |
| Abstract: NGC 4321 (M100, distance ∼ 15.2 Mpc) is a barred spiral galaxy that is a part of the PHANGS Survey (Physics at High Angular resolution in Nearby GalaxieS), which aims to study nearby (distance < 23 Mpc) galaxies in high resolution using multiwavelength data to investigate how global scaling relations behave at local, sub-galactic scales. We use archival Chandra X-ray observations of the diffuse hot gas and X-ray binary population of NGC 4321, studying them in comparison with AstroSat UVIT FUV observations and
HST archival data. We create diffuse X-ray emission maps by removing the point sources, and study the distribution of the diffuse X-ray emission against the Hα map from HST (which traces recent star formation) and the bright clumps identified in the FUV image (which traces star formation on a longer timescale), finding that the correlation is strongest in the nucleus of the galaxy where most of the X-ray gas is concentrated, along with some correlation in the southern arm. We find that the X-ray spectra of the diffuse gas in the central region and the southern spiral arm can be modelled by two-temperature thermal plasmas (kT ∼ 0.2 keV and 0.6 keV for the central region, and kT ∼ 0.2 keV and 0.8 keV for the spiral arm). We also identify ∼ 74 point sources, among which 13 have been identified in a previous study as ultra-luminous X-ray sources (ULXs). We inspect the spectra of some of these point sources as well. Further analyses will aim to investigate the energetics of the diffuse hot X-ray emitting gas in the ISM, studied in relation to star formation traced by FUV and Hα to better understand how feedback processes affect the baryon and energy cycles of galaxies. |
