The XMM Cluster Survey: An independent demonstration of the fidelity of the eFEDS galaxy cluster data products and implications for future studies

Turner, DJ ORCID: 0000-0001-9658-1396, Giles, PA ORCID: 0000-0003-4937-8453, Romer, AK, Wilkinson, R ORCID: 0000-0002-3908-7313, Upsdell, EW ORCID: 0000-0003-0628-7201, Klein, M, Viana, PTP ORCID: 0000-0003-1572-8531, Hilton, M ORCID: 0000-0002-8490-8117, Bhargava, S, Collins, CA, Mann, RG, Sahlén, M ORCID: 0000-0003-0973-4804 and Stott, JP ORCID: 0000-0002-1679-9983 (2022) The XMM Cluster Survey: An independent demonstration of the fidelity of the eFEDS galaxy cluster data products and implications for future studies. Monthly Notices of the Royal Astronomical Society, 517 (1). pp. 657-674. ISSN 0035-8711

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Abstract

We present the first comparison between properties of clusters of galaxies detected by the eROSITA Final Equatorial-Depth Survey (eFEDS) and the XMM Cluster Survey (XCS). We have compared, in an ensemble fashion, properties from the eFEDS X-ray cluster catalogue with those from the Ultimate XMM eXtragaLactic (XXL) survey project (XXL-100-GC). We find the redshift and temperature (TX) distributions to be similar, with a larger proportion of clusters above 4 keV in the XXL-100-GC sample; fractional temperature uncertainties are significantly larger in eFEDS compared to XXL. We find 62 eFEDS cluster candidates with XMM data (eFEDS-XMM sample); 10 do not have good enough XMM data to confirm or deny, 11 are classed as sample contaminants, and 4 have their X-ray flux contaminated by another source. The majority of eFEDS-XMM sources have longer XMM exposures than eFEDS, and most eFEDS positions are within 100 kpc of XCS positions. Our eFEDS-XCS sample of 37 clusters is used to calculate minimum sample contamination fractions of ∼18 and ∼9 per cent in the eFEDS X-ray and optically confirmed samples, respectively, in general agreement with eFEDS findings. We directly compare 29 X-ray luminosities (LX) measured by eFEDS and XCS, finding excellent agreement. Eight clusters have a TX measured by XCS and eFEDS, and we find that XMM temperatures are 25 ± 9 per cent larger than their eROSITA counterparts. Finally, we construct LX-TX scaling relations based on eFEDS and XCS measurements, which are in tension; the tension is decreased when we measure a third scaling relation with calibrated XCS temperatures.

Item Type:	Article
Uncontrolled Keywords:	0201 Astronomical and Space Sciences; Astronomy & Astrophysics
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press (OUP)
Date of acceptance:	26 August 2022
Date of first compliant Open Access:	19 June 2023
Date Deposited:	19 Jun 2023 11:23
Last Modified:	04 Jul 2025 18:15
DOI or ID number:	10.1093/mnras/stac2463
URI:	https://researchonline.ljmu.ac.uk/id/eprint/19930

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