J/A+A/661/A14 Properties of eFEDS shear-selected clusters (Ramos-Ceja+, 2022)
The eROSITA Final Equatorial-Depth Survey (eFEDS). A complete census of X-ray
properties of Subaru Hyper Suprime-Cam weak lensing shear-selected clusters
in the eFEDS footprint.
Ramos-Ceja M.E., Oguri M., Miyazaki S., Ghirardini V., Chiu I., Okabe N.,
Liu A., Schrabback T., Akino D., Bahar Y.E., Bulbul E., Clerc N.,
Comparat J., Grandis S., Klein M., Lin Y.-T., Merloni A., Mitsuishi I.,
Miyatake H., More S., Nandra K., Nishizawa A.J., Ota N., Pacaud F.,
Reiprich T.H., Sanders J.S.
<Astron. Astrophys., 661, A14 (2022)>
=2022A&A...661A..14R 2022A&A...661A..14R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Redshifts
Keywords: galaxies: clusters: general - large-scale structure of Universe -
galaxies: clusters: intracluster medium - X-rays: galaxies: clusters
Abstract:
The eFEDS survey is a proof-of-concept mini-survey designed to
demonstrate the survey science capabilities of SRG/eROSITA. It covers
an area of 140deg2 where ∼540 galaxy clusters have been detected
out to a redshift of 1.3. The eFEDS field is partly embedded in the
Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) S19A data
release, which covers ∼510deg2, containing approximately 36 million
galaxies. This galaxy catalogue has been used to construct a sample of
∼180 shear-selected galaxy clusters. The common area to both surveys
covers about 90deg2, making it an ideal region to study galaxy
clusters selected in different ways.
The aim of this work is to investigate the effects of selection
methods in the galaxy cluster detection by comparing the X-ray
selected, eFEDS, and the shear-selected, HSC-SSP S19A, galaxy cluster
samples. There are 25 shear-selected clusters in the eFEDS footprint.
The relation between X-ray bolometric luminosity and weak-lensing mass
is investigated (Lbol-M relation), comparing this relation derived
from a shear-selected cluster sample to the relation obtained from an
X-ray selected sample. Moreover, the dynamical state of the
shear-selected clusters is investigated and compared to the X-ray
selected sample using X-ray morphological parameters and galaxy
distribution. Results. The normalisation of the Lbol-M relation of
the X-ray selected and shear-selected samples is consistent within
1σ-. Moreover, the dynamical state and merger fraction of the
shear-selected clusters is not different from the X-ray selected ones.
Four shear-selected clusters are undetected in X-rays. A close
inspection reveals that one is the result of projection effects, while
the other three have an X-ray flux below the ultimate eROSITA
detection limit. Finally, 43% of the shear-selected clusters lie in
superclusters.Conclusions. Our results indicate that the scaling
relation between X-ray bolometric luminosity and true cluster mass of
the shear-selected cluster sample is consistent with the eFEDS sample.
There is no significant population of X-ray underluminous clusters,
indicating that X-ray selected cluster samples are complete and can be
used as an accurate cosmological probe.
Description:
The shear-selected galaxy cluster sample studied in this paper is
taken from Oguri et al. (2021PASJ...73..817O 2021PASJ...73..817O).
Table 1 shows the calibrated weak-lensing mass, M500, of the
shear-selected clusters in the common area between the HSC GAMA09H and
eFEDS fields.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 25 Properties of the shear-selected clusters
within the eFEDS footprint
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See also:
J/A+A/661/A1 : The eFEDS X-ray catalogs (V7.4) (Brunner+, 2022)
J/A+A/661/A2 : Galaxy clusters and groups in eFEDS (Liu+, 2022)
J/A+A/661/A11 : eFEDS. Masses of galaxy clusters and groups (Chui+, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- Categ [UPN] Category (1)
3- 18 A16 --- eFEDS eFEDS name (JHHMMSS.s+DDMMSS)
20- 24 F5.3 --- zMCMF ? MCMF redshift
26- 31 F6.2 10+35W Lbol Bolometric luminosity
33- 37 F5.2 10+35W E_Lbol Error on Lbol (upper value)
39- 43 F5.2 10+35W e_Lbol Error on Lbol (lower value)
45- 47 I3 --- ID ID in Oguri et al. (2021PASJ...73..817O 2021PASJ...73..817O)
49- 53 F5.3 --- z Redshift
55- 58 F4.2 10+14Msun M500 Mass M500
60- 63 F4.2 10+14Msun E_M500 Error on M500 (upper value)
65- 68 F4.2 10+14Msun e_M500 Error on M500 (lower value)
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Note (1): Categories as follows:
U = unique
P = primary
N = nonmatches. Weak-lensing peaks not matched to an eFEDS cluster have
no corresponding eFEDS ID and redshift.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 24-Aug-2022