The X-ray invisible Universe. A look into the haloes undetected by eROSITA

Journal
Date Issued
2024
Author(s)
Popesso, P.
•
•
Bulbul, E.
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Merloni, A.
•
Comparat, J.
•
Clerc, N.
•
Igo, Z.
•
Liu, A.
•
Driver, S.
•
Salvato, M.
•
Brusa, M.
•
Bahar, Y. E.
•
Malavasi, N.
•
•
Robotham, A.
•
Liske, J.
•
DOI
Abstract
The paper presents the analysis of optically selected GAMA groups and clusters in the SRG/eROSITA X-ray map of eROSITA Final Equatorial Depth Survey, in the halo mass range 1013-5 × 1014 M⊙ and at z < 0.2. All X-ray detections have a clear GAMA counterpart, but most of the GAMA groups in the halo mass range 1013-1014 M⊙ remain undetected. We compare the X-ray surface brightness profiles of the eROSITA detected groups with the mean stacked profile of the undetected low-mass haloes at fixed halo mass. Overall, we find that the undetected groups exhibit less concentrated X-ray surface brightness, dark matter, and galaxy distributions with respect to the X-ray-detected haloes. The mean gas mass fraction profiles are consistent in the two samples within 1.5σ, indicating that the gas follows the dark matter profile. The low-mass concentration and the magnitude gap indicate that these systems are young. They reside with a higher probability in filaments while X-ray-detected groups favour the nodes of the Cosmic Web. Because of the lower central emission, the undetected systems tend to be X-ray underluminous at fixed halo mass and to lie below the LX-Mhalo relation. Interestingly, the X-ray-detected systems inhabiting the nodes scatter the less around the relation, while those in filaments tend to lie below it. We do not observe any strong relationship between the system X-ray appearance and the active galactic nucleus (AGN) activity. We cannot exclude the role of the past AGN feedback in affecting the gas distribution over the halo lifetime. However, the data suggests that the observed differences might be related to the halo assembly bias.
Volume
527
Issue
1
Start page
895
Uri
Url
Issn Identifier
0035-8711
Ads BibCode
2024MNRAS.527..895P
Rights
open.access
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