Temperature and Abundance Structure in and around the Core of the Perseus Cluster of Galaxies
Abstract
1.6 Ms of Chandra data combined from 27 observations spanning 10 years are used to produce spectra from a grid of 289 square regions in and around the core of the Perseus Cluster. The structure in the Perseus Cluster is due to a complicated system involving the central galaxy, NGC 1275 and its coincident radio jet from which bubbles of relativistic plasma are being blown, in-falling material producing a cooling flow to the core, and intracluter plasma related to Hα filaments surrounding the core. The processes involved in this system affect the X-ray emission throughout the cluster and inform the choices for models of the spectra. Spectra are expected to match that of brehmstrahlung and line emission from a hot plasma, absorbed by some amount along the line of sight to the observer. A script is used to individually analyze the spectra and produce a best fit model, providing the region's temperature, abundance with respect to solar, and column density of an intrinsic absorption column where appropriate. The galactic column density is fixed for each region from the appropriate COLDEN value. Temperature, abundance, and intrinsic column density maps are presented for the entire grid using each region as a data point. Evidence for an absorption column intrinsic to the source in addition to the galactic column is found for some regions. The base model is MEKAL emission absorbed by the galactic hydrogen column density at redshift of 0 and also absorbed by a column intrinsic to the source (i.e. at redshift of 0.0183). An exposure map and exposure-corrected image of the X-ray counts for the combined observations are presented here as well.
- Publication:
-
American Astronomical Society Meeting Abstracts #231
- Pub Date:
- January 2018
- Bibcode:
- 2018AAS...23125202D