X-ray flux -- mass relation for $z\gtrsim 0.7$ galaxy clusters
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arXiv
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| Autori principali: | , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| author | Lyskova, Natalia Churazov, Eugene Khabibullin, Ildar Sunyaev, Rashid Gilfanov, Marat Sazonov, Sergey |
| author_facet | Lyskova, Natalia Churazov, Eugene Khabibullin, Ildar Sunyaev, Rashid Gilfanov, Marat Sazonov, Sergey |
| contents | We use a subsample of co-detections of the ACT and MaDCoWS cluster catalogs to verify the predicted relation between the observed X-ray flux $F_X$ in the 0.5-2~keV band and the cluster mass $M_{\rm 500c}$ for halos at $z>0.6-0.7$. We modify this relation by introducing a correction coefficient $η$, which is supposed to encapsulate factors associated with a particular method of flux estimation, the sample selection function, the definition of the cluster mass, etc. We show that the X-ray flux, being the most basic X-ray observable, serves as a convenient and low-cost mass indicator for distant galaxy clusters with photometric or even missing redshifts (by setting $z=1$) as long as it is known that $z\gtrsim 0.6-0.7$. The correction coefficient $η$ is $\approx 0.8$ if $M^{\rm UPP}_{\rm 500c}$ from the ACT-DR5 catalog are used as cluster masses and $η\approx 1.1$ if weak-lensing-calibrated masses $M^{\rm Cal}_{\rm 500c}$ are used instead. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_04400 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | X-ray flux -- mass relation for $z\gtrsim 0.7$ galaxy clusters Lyskova, Natalia Churazov, Eugene Khabibullin, Ildar Sunyaev, Rashid Gilfanov, Marat Sazonov, Sergey Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena We use a subsample of co-detections of the ACT and MaDCoWS cluster catalogs to verify the predicted relation between the observed X-ray flux $F_X$ in the 0.5-2~keV band and the cluster mass $M_{\rm 500c}$ for halos at $z>0.6-0.7$. We modify this relation by introducing a correction coefficient $η$, which is supposed to encapsulate factors associated with a particular method of flux estimation, the sample selection function, the definition of the cluster mass, etc. We show that the X-ray flux, being the most basic X-ray observable, serves as a convenient and low-cost mass indicator for distant galaxy clusters with photometric or even missing redshifts (by setting $z=1$) as long as it is known that $z\gtrsim 0.6-0.7$. The correction coefficient $η$ is $\approx 0.8$ if $M^{\rm UPP}_{\rm 500c}$ from the ACT-DR5 catalog are used as cluster masses and $η\approx 1.1$ if weak-lensing-calibrated masses $M^{\rm Cal}_{\rm 500c}$ are used instead. |
| title | X-ray flux -- mass relation for $z\gtrsim 0.7$ galaxy clusters |
| topic | Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.04400 |