J/A+A/690/A322 The ACT-DR5 MCMF cluster catalog (Klein+, 2024)
The ACT-DR5 MCMF galaxy cluster catalog.
Klein M., Mohr J.J., Davies C.T.
<Astron. Astrophys. 690, A322 (2024)>
=2024A&A...690A.322K 2024A&A...690A.322K (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts ; Surveys ;
Spectra, millimetric/submm
Keywords: catalogs - galaxies: clusters: general -
galaxies: clusters: intracluster medium - cosmology: observations -
large-scale structure of Universe
Abstract:
Galaxy clusters are useful cosmological probes and interesting
astrophysical laboratories. As the cluster samples continue to grow n
size, a deeper understanding of the sample characteristics and
improved control of systematics becomes more crucial. For this
analysis we created a new and larger ACT-DR5-based thermal
Sunyaev-Zel'dovich Effect (tSZE) selected galaxy cluster catalog
with improved control over sample purity and completeness. We employ
the red sequence based cluster redshift and confirmation tool MCMF
together with optical imaging data from the Legacy Survey DR-10 and
infrared data from the WISE satellite to systematically identify true
clusters from a new cluster candidate detection run on the ACT-DR5
dataset. The resulting ACT-DR5 MCMF sample contains 6,237 clusters
with a residual contamination of 10.7%. This is an increase of 51%
compared to the previous ACT-DR5 cluster catalog, making this new
catalog the largest tSZE- selected cluster catalog to date. The
zphot>1 subsample contains 703 clusters, three times more than in the
previous ACT-DR5 catalog. Cross-matching the ACT-DR5 MCMF cluster
catalog with a deeper tSZE sample from SPTpol 500d allows us to
confirm the completeness and purity of the new ACT-DR5 MCMF sample.
Cross-matching to the two largest X-ray selected cluster samples, the
all-sky RASS MCMF and the western Galactic hemisphere survey eRASS1,
confirms the sample purity of the RASS MCMF sample and in the case of
eROSITA eRASS1 reveals that 43% of the matched clusters are designated
in eRASS1 as X-ray point sources rather than groups and clusters.
Cross-correlating the ACT-DR5 MCMF cluster catalog with ACT-DR6
lensing maps results in a 16.4 σ detection of CMB lensing around
the clusters, corresponding to the strongest signal found so far for a
galaxy cluster sample. Repeating the measurement for the z>1 cluster
subsample yields a significance of 4.3 σ, which is the strongest
CMB lensing detection in a z>1 cluster sample to date.
Description:
This is the ACT-DR5 MCMF catalog of galaxy clusters. It contains ∼50%
more clusters than the previous ACT-DR5 catalog and three times more
clusters above z=1. The catalog has an expected contamination of
10.7%, which can be easily reduced by imposing stricter upper limits
in fcont. For details see the catalog paper. The second table (A.1)
provides transformation factors to transform the old g, r, z, w1,
w2-based richness definition used in Klein+23 to the updated richness
definition of this work. Please note that residual differences between
Klein et al. (2023MNRAS.526.3757K 2023MNRAS.526.3757K, Cat. J/MNRAS/526/3757) and Klein et
al. (arXiv:2309.09908)4 richness exist due to different priors (X-ray
vs tSZE) used to calculate richnesses of the clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 558 6237 ACT-DR5 MCMF catalog of galaxy clusters
tablea1.dat 24 1501 Transformation factors
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See also:
J/MNRAS/531/3973 : SPT-SZ MCMF catalog (Klein+, 2024)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- Name Cluster name, ACT-CL JHHMM.m+DDMM
(NAME)
21- 35 F15.11 deg RAdeg Right ascension (J2000) from ACT
(RADEG)
37- 51 F15.11 deg DEdeg Declination (J2000) from ACT (DECDEG)
53- 69 F17.14 --- SNR Signal-to-noise ratio, optimized over
all filter scales (SNR)
71- 87 A17 --- Template Name of the optimal matched filter
template for this cluster (TEMPLATE)
89- 95 A7 --- TileName Name of the ACT map tile in which the
cluster was found (TILENAME)
97-113 F17.14 --- fixedSNR Signal-to-noise ratio at the reference
2.4 arcmin filter scale (FIXED_SNR)
115-132 F18.15 10-4 YC Central Comptonization parameter of the
optimal matched filter (Y_C)
134-150 F17.15 10-4 e_YC Uncertainty on column YC (ERRYC)
152-168 F17.15 10-4 fixedYC Central Comptonization parameter of the
optimal matched filter using measured
at the reference filter scale of
2.4 arcmin (FIXEDYC)
170-186 F17.15 10-4 e_fixedYC Uncertainty on column fixedYC
(FIXEDERRY_C)
188-204 F17.15 --- z1C Redshift of the best optical
counterpart (Z1COMB)
206-224 F19.15 --- z2C ?=-99 Redshift of the second best
counterpart (Z2COMB)
226-242 F17.13 --- L1C Richness of the best counterpart
(L1COMB)
244-263 F20.15 --- L2C ?=-99 Richness of the second best
counterpart (L2COMB)
265-282 F18.14 --- e_L1C Uncertainty on column L1C (EL1COMB)
284-302 F19.14 --- e_L2C []?=-99.9 Uncertainty on L2COMB
(EL2COMB)
304-320 F17.15 --- e_z1C Uncertainty on column z1C (EZ1COMB)
322-338 F17.15 --- e_z2C ?=- Uncertainty on column z2C
(EZ2COMB)
340-356 F17.15 --- fcont1C ?=-99.9 Contamination estimator fcont
of best counter part (FCONT1_COMB)
358-374 F17.15 --- fcont2C Contamination estimator fcont of
second best counter part
(FCONT2_COMB)
376-387 E12.6 Msun M500-1C tSZE-based estimate of M500c using z1C
corresponding to M500c in Hilton et
al. (2021ApJS..253....3H 2021ApJS..253....3H,
Cat. J/APJS/253/3) (M5001COMB)
389-405 F17.15 10+14Msun E_M500-1C Positive uncertainty to M500-1C
(M5001COMB_ERRPLUS)
407-423 F17.15 10+14Msun e_M500-1C Negative uncertainty to M500-1C
(M5001COMB_ERRMINUS)
425-436 E12.6 Msun M500-2C ?=-95.791 tSZE-based estimate of M500c
using z2C (M5002COMB)
438-455 F18.15 --- fcont1CSNR45 ?=99.9 Contamination estimator fcont
of best counterpart for SNR>4.5 samp
(FCONT1COMBSNR45)
457-474 F18.15 --- fcont2CSNR45 ?=99.9 Contamination estimator fcont
of second best counterpart for SNR>4
(FCONT2COMBSNR45)
476-487 E12.6 Msun M500-1CCAL tSZE-based estimate of M500c using z1C
rescaled with an calibration factor
of 0.71 (M5001COMB_CAL)
489-505 F17.15 10+14Msun E_M500-1CCAL Negative uncertainty to M500-1CCAL
(M5001COMBCALERRMINUS)
507-523 F17.15 10+14Msun e_M500-1CCAL Positive uncertainty to M500-1CCAL
(M5001COMBCALERRPLUS)
525-536 E12.6 Msun M500-2CCAL ?=-1.34917e+02 tSZE-based estimate of
M500c using z2C rescaled with an
calibration factor of 0.71
(M5002COMB_CAL)
538-556 F19.15 --- zsp1 ?=-99 Spectroscopic redshift for the
best optical counterpart (ZSPEC1)
558 I1 --- zspType [0/3] Type of spec-z (ZSPECTYPE) (1)
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Note (1): Type of spec-z as follows:
0 = no reliable spectroscopic redshift
1 = spectroscopic redshift from Literature
2 = spectroscopic redshift from >2 galaxies
3 = spectroscopic redshift from ≤2 galaxies from which one is the BCG
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 F5.3 --- z Redshift (Z)
7- 24 F18.16 --- GRZW1W2toGRZW1 Transformation from g,r,z,w1,w2
(Klein et al., 2023MNRAS.526.3757K 2023MNRAS.526.3757K)
richness to g,r,z,w1 richness
(GRZW1W2TOGRZW1)
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Acknowledgements:
Matthias Klein, matthias.klein(at)physik.lmu.de
(End) Patricia Vannier [CDS] 08-Sep-2024