The eROSITA Final Equatorial-Depth Survey (eFEDS) Optical confirmation, redshifts, and properties of the cluster and group catalog

Klein, M.; Oguri, M.; Mohr, J. J.; Grandis, S.; Ghirardini, V.; Liu, T.; Liu, A.; Bulbul, E.; Wolf, J.; Comparat, J.; Ramos-Ceja, M. E.; Buchner, J.; Chiu, I.; Clerc, N.; Merloni, A.; Miyatake, H.; Miyazaki, S.; Okabe, N.; Ota, N.; Pacaud, F.; Salvato, M. und Driver, S. P. (2022): The eROSITA Final Equatorial-Depth Survey (eFEDS) Optical confirmation, redshifts, and properties of the cluster and group catalog. In: Astronomy & Astrophysics, Bd. 661, A4

Abstract

Context. In 2019, the eROSITA telescope on board the Russian-German satellite Spectrum-Roentgen-Gamma (SRG) began to perform a deep all-sky X-ray survey with the aim of identifying similar to 100 000 clusters and groups over the course of four years. As part of its performance verification phase, a similar to 140 deg(2) survey, called eROSITA Final Equatorial-Depth Survey (eFEDS), was performed. With a depth typical of the all-sky survey after four years, it allows tests of tools and methods as well as improved predictions for the all-sky survey. Aims. As part of this effort, a catalog of 542 X-ray selected galaxy group and cluster candidates was compiled. In this paper we present the optical follow-up, with the aim of providing redshifts and cluster confirmation for the full sample. Furthermore, we aim to provide additional information on the dynamical state, richness, and optical center of the clusters. Finally, we aim to evaluate the impact of optical cluster confirmation on the purity and completeness of the X-ray selected sample. Methods. We used optical imaging data from the Hyper Suprime-Cam Subaru Strategic Program and from the Legacy Survey to identify optical counterparts to the X-ray detected cluster candidates. We make use of the multi-component matched filter cluster confirmation tool (MCMF), as well as of the optical cluster finder CAMIRA to derive cluster redshifts and richnesses. MCMF provided the probabilities with which an optical structure would be a chance superposition with the X-ray candidate. These probabilities were used to identify the best optical counterpart as well as to confirm an X-ray candidate as a cluster. The impact of this confirmation process on catalog purity and completeness was estimated using optical to X-ray scaling relations as well as simulations. The resulting catalog was furthermore matched with public group and cluster catalogs. Optical estimators of the cluster dynamical state were constructed based on density maps of the red-sequence galaxies at the cluster redshift. Results. By providing redshift estimates for all 542 candidates, we construct an optically confirmed sample of 477 clusters and groups with a residual contamination of 6%. Of these, 470 (98.5%) are confirmed using MCMF, and 7 systems are added through cross-matching with spectroscopic group catalogs. Using observable-to-observable scaling and the applied confirmation threshold, we predict that 8 +/- 2 real systems have been excluded with the MCMF cut required to build this low-contamination sample. This number agrees well with the 7 systems found through cross-matching that were not confirmed with MCMF. The predicted redshift and mass distribution of this catalog agree well with simulations. Thus, we expect that these 477 systems include >99% of all true clusters in the candidate list. Using an MCMF-independent method, we confirm that the catalog contamination of the confirmed subsample is 6 +/- 3%. Application of the same method to the full candidate list yields 17 +/- 3%, consistent with estimates coming from the fraction of confirmed systems of similar to 17% and with expectations from simulations of similar to 20%. We also present a sample of merging cluster candidates based on the derived estimators of the cluster dynamical state.

• Dokumententyp: Zeitschriftenartikel
• Fakultät: Physik
• Themengebiete: 500 Naturwissenschaften und Mathematik > 530 Physik
• ISSN: 0004-6361
• Sprache: Englisch
• DFG: Gefördert durch die Deutsche Forschungsgemeinschaft (DFG) - 390783311