Study of the excess Fe XXV line emission in the central degrees of the Galactic centre using XMM-Newton data

DOI: 
10.1051/0004-6361/202245001
Publication date: 
15/03/2023
Main author: 
Anastasopoulou, K.
IAA authors: 
Schödel, R.
Authors: 
Anastasopoulou, K.;Ponti, G.;Sormani, M. C.;Locatelli, N.;Haberl, F.;Morris, M. R.;Churazov, E. M.;Schödel, R.;Maitra, C.;Campana, S.;Di Teodoro, E. M.;Jin, C.;Khabibullin, I.;Mondal, S.;Sasaki, M.;Zhang, Y.;Zheng, X.
Journal: 
Astronomy and Astrophysics
Publication type: 
Article
Volume: 
671
Pages: 
A55
Abstract: 
The diffuse Fe XXV (6.7 keV) line emission observed in the Galactic ridge is widely accepted to be produced by a superposition of a large number of unresolved X-ray point sources. In the very central degrees of our Galaxy, however, the existence of an extremely hot (~7 keV) diffuse plasma is still under debate. In this work we measure the Fe XXV line emission using all available XMM-Newton observations of the Galactic centre (GC) and inner disc (−10° &lt; ℓ &lt; 10°, −2° &lt; b &lt; 2°). We use recent stellar mass distribution models to estimate the amount of X-ray emission originating from unresolved point sources, and find that within a region of ℓ = ±1° and b = ±0.25° the 6.7keV emission is 1.3-1.5 times in excess of what is expected from unresolved point sources. The excess emission is enhanced towards regions where known supernova remnants are located, suggesting that at least a part of this emission is due to genuine diffuse very hot plasma. If the entire excess is due to very hot plasma, an energy injection rate of at least ~6 × 10<SUP>40</SUP> erg s<SUP>−1</SUP> is required, which cannot be provided by the measured supernova explosion rate or past Sgr A<SUP>*</SUP> activity alone. However, we find that almost the entire excess we observe can be explained by assuming GC stellar populations with iron abundances ~1.9 times higher than those in the bar/bulge, a value that can be reproduced by fitting diffuse X-ray spectra from the corresponding regions. Even in this case, a leftover X-ray excess is concentrated within ℓ = ±0.3° and b = ±0.15°, corresponding to a thermal energy of ~2 × 10<SUP>52</SUP> erg, which can be reproduced by the estimated supernova explosion rate in the GC. Finally we discuss a possible connection to the observed GC Fermi-LAT excess. <P />Full Table B.1 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.cds.unistra.fr">cdsarc.cds.unistra.fr</A> (ftp://130.79.128.5) or via <A href="https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A55">https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A55</A>
Database: 
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2023A&A...671A..55A/abstract
ADS Bibcode: 
2023A&A...671A..55A
Keywords: 
Galaxy: bulge;Galaxy: center;Galaxy: disk;X-rays: general;X-rays: ISM;Astrophysics - High Energy Astrophysical Phenomena