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| Main Authors: | , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2512.06138 |
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| _version_ | 1866914473030189056 |
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| author | Nguyen-Dang, N. T. Ota, N. Okabe, N. Oguri, M. Mitsuishi, I. Reiprich, T. H. Pacaud, F. Bulbul, E. Sanders, J. S. Brüggen, M. Liu, A. Tsujita, Y. Chiu, I. Ghirardini, V. Grandis, S. Klein, M. Migkas, K. Miyatake, H. Miyazaki, S. Ramos-Ceja, M. E. |
| author_facet | Nguyen-Dang, N. T. Ota, N. Okabe, N. Oguri, M. Mitsuishi, I. Reiprich, T. H. Pacaud, F. Bulbul, E. Sanders, J. S. Brüggen, M. Liu, A. Tsujita, Y. Chiu, I. Ghirardini, V. Grandis, S. Klein, M. Migkas, K. Miyatake, H. Miyazaki, S. Ramos-Ceja, M. E. |
| contents | This is the second paper in a series exploring the X-ray properties of galaxy clusters optically selected by the Subaru Hyper Suprime-Cam (HSC) survey, using data from the SRG/eROSITA Final Equatorial-Depth Survey (eFEDS). We aim to investigate scaling relations between observable cluster properties and mass, and to study the radial X-ray profiles of a large sample of optically selected clusters. We analyze a sample of 997 CAMIRA clusters with richness $N > 15$ and redshifts of $0.1 < z < 1.3$. Using bolometric luminosities derived from count rates and a weak-lensing mass calibration, we study the $L-M$ and $N-M$ scaling relations through stacking analysis, while accounting for selection effects and redshift evolution. We also compare clusters with and without X-ray counterparts in the eFEDS catalog in terms of their scaling relations and surface brightness profiles. The best-fit $L-M$ slope ($1.56^{+0.14}_{-0.12}$) is slightly steeper than the self-similar prediction, yet remains consistent with our previous findings. The $N-M$ slope ($0.766^{+0.070}_{-0.060}$) broadly agrees with theoretical expectations and other optical samples. The data do not require any additional redshift evolution beyond the standard self-similar scaling, although current constraints on evolution remain weak. X-ray detected clusters exhibit a marginally steeper $L-M$ slope, higher central surface brightness, and more centrally concentrated X-ray profiles than undetected systems. Our results highlight systematic differences in the X-ray properties between optically and X-ray selected cluster samples. This study extends scaling relation analyses into lower mass and luminosity regimes, demonstrating the value of combining deep X-ray and optical surveys like eROSITA and Subaru HSC. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_06138 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray stacking analysis of Subaru's optically selected clusters spanning low richness regime Nguyen-Dang, N. T. Ota, N. Okabe, N. Oguri, M. Mitsuishi, I. Reiprich, T. H. Pacaud, F. Bulbul, E. Sanders, J. S. Brüggen, M. Liu, A. Tsujita, Y. Chiu, I. Ghirardini, V. Grandis, S. Klein, M. Migkas, K. Miyatake, H. Miyazaki, S. Ramos-Ceja, M. E. Cosmology and Nongalactic Astrophysics This is the second paper in a series exploring the X-ray properties of galaxy clusters optically selected by the Subaru Hyper Suprime-Cam (HSC) survey, using data from the SRG/eROSITA Final Equatorial-Depth Survey (eFEDS). We aim to investigate scaling relations between observable cluster properties and mass, and to study the radial X-ray profiles of a large sample of optically selected clusters. We analyze a sample of 997 CAMIRA clusters with richness $N > 15$ and redshifts of $0.1 < z < 1.3$. Using bolometric luminosities derived from count rates and a weak-lensing mass calibration, we study the $L-M$ and $N-M$ scaling relations through stacking analysis, while accounting for selection effects and redshift evolution. We also compare clusters with and without X-ray counterparts in the eFEDS catalog in terms of their scaling relations and surface brightness profiles. The best-fit $L-M$ slope ($1.56^{+0.14}_{-0.12}$) is slightly steeper than the self-similar prediction, yet remains consistent with our previous findings. The $N-M$ slope ($0.766^{+0.070}_{-0.060}$) broadly agrees with theoretical expectations and other optical samples. The data do not require any additional redshift evolution beyond the standard self-similar scaling, although current constraints on evolution remain weak. X-ray detected clusters exhibit a marginally steeper $L-M$ slope, higher central surface brightness, and more centrally concentrated X-ray profiles than undetected systems. Our results highlight systematic differences in the X-ray properties between optically and X-ray selected cluster samples. This study extends scaling relation analyses into lower mass and luminosity regimes, demonstrating the value of combining deep X-ray and optical surveys like eROSITA and Subaru HSC. |
| title | The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray stacking analysis of Subaru's optically selected clusters spanning low richness regime |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2512.06138 |