J/A+A/653/A135 ACT/MaDCoWS clusters co-detections (Orlowski-Scherer+, 2021)
Atacama Cosmology Telescope measurements of a large sample of candidates from
the Massive and Distant Clusters of WISE Survey.
Sunyaev-Zeldovich effect confirmation of MaDCoWS candidates using ACT.
Orlowski-scherer J., Di Mascolo L., Bhandarkar T., Manduca A.,
Mroczkowski T., Amodeo S., Battaglia N., Brodwin M., Choi S.K., Devlin M.,
Dicker S., Dunkley J., Gonzalez A.H., Han D., Hilton M., Huffenberger K.,
Hughes J.P., Macinnis A., Knowles K., Koopman B.J., Lowe I., Moodley K.,
Nati F., Niemack M.D., Page L.A., Partridge B., Romero C., Salatino M.,
Schillaci A., Sehgal N., Sifon C., Staggs S., Stanford S.A., Thornton R.,
Vavagiakis E.M., Wollack E.J., Xu Z., Zhu N.
<Astron. Astrophys., 653, A135-135 (2021)>
=2021A&A...653A.135O 2021A&A...653A.135O (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts
Keywords: large-scale structure of Universe - cosmic background radiation -
submillimeter: galaxies - radio continuum: galaxies -
galaxies: clusters: general - galaxies: clusters: intracluster medium
Abstract:
Galaxy clusters are an important tool for cosmology, and their
detection and characterization are key goals for current and future
surveys. Using data from the Wide-field Infrared Survey Explorer
(WISE), the Massive and Distant Clusters of WISE Survey (MaDCoWS)
located 2839 significant galaxy overdensities at redshifts
0.7≤z≤1.5, which included extensive follow-up imaging from the
Spitzer Space Telescope to determine cluster richnesses. Concurrently,
the Atacama Cosmology Telescope (ACT) has produced large area
millimeter-wave maps in three frequency bands along with a large
catalog of Sunyaev-Zeldovich (SZ)-selected clusters as part of its
Data Release 5 (DR5).
We aim to verify and characterize MaDCoWS clusters using measurements
of, or limits on, their thermal SZ effect signatures. We also use
these detections to establish the scaling relation between SZ mass and
the MaDCoWS-defined richness.
Using the maps and cluster catalog from DR5, we explore the scaling
between SZ mass and cluster richness. We do this by comparing
cataloged detections and extracting individual and stacked SZ signals
from the MaDCoWS cluster locations. We use complementary radio survey
data from the Very Large Array, submillimeter data from Herschel, and
ACT 224GHz data to assess the impact of contaminating sources on the
SZ signals from both ACT and MaDCoWS clusters. We use a hierarchical
Bayesian model to fit the mass-richness scaling relation, allowing for
clusters to be drawn from two populations: one, a Gaussian centered on
the mass-richness relation, and the other, a Gaussian centered on zero
SZ signal.
We find that MaDCoWS clusters have submillimeter contamination that is
consistent with a gray-body spectrum, while the ACT clusters are
consistent with no submillimeter emission on average. Additionally,
the intrinsic radio intensities of ACT clusters are lower than those
of MaDCoWS clusters, even when the ACT clusters are restricted to the
same redshift range as the MaDCoWS clusters. We find the best-fit ACT
SZ mass versus MaDCoWS richness scaling relation has a slope of
p1=1.84-0.14+0.15, where the slope is defined as
Mλ∝λ15p1 and λ15 is the richness.
We also find that the ACT SZ signals for a significant fraction (∼57%)
of the MaDCoWS sample can statistically be described as being drawn
from a noise-like distribution, indicating that the candidates are
possibly dominated by low-mass and unvirialized systems that are below
the mass limit of the ACT sample. Further, we note that a large
portion of the optically confirmed ACT clusters located in the same
volume of the sky as MaDCoWS are not selected by MaDCoWS, indicating
that the MaDCoWS sample is not complete with respect to SZ selection.
Finally, we find that the radio loud fraction of MaDCoWS clusters
increases with richness, while we find no evidence that the
submillimeter emission of the MaDCoWS clusters evolves with richness.
We conclude that the original MaDCoWS selection function is not well
defined and, as such, reiterate the MaDCoWS collaboration's
recommendation that the sample is suited for probing cluster and
galaxy evolution, but not cosmological analyses. We find a best-fit
mass-richness relation slope that agrees with the published MaDCoWS
preliminary results. Additionally, we find that while the approximate
level of infill of the ACT and MaDCoWS cluster SZ signals (1-2%) is
subdominant to other sources of uncertainty for current generation
experiments, characterizing and removing this bias will be critical
for next-generation experiments hoping to constrain cluster masses at
the sub-percent level.
Description:
MaDCoWS cluster catalog (Gonzalez et al., 2019ApJS..240...33G 2019ApJS..240...33G, Cat.
J/ApJS/240/33) and the catalog and maps from ACT (Hilton et al.,
2021ApJS..253....3H 2021ApJS..253....3H) co-detections.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 77 96 *ACT/MaDCoWS Co-detections
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Note on tablec1.dat: These cluster co-detections were made following the
analysis described in Sect. 3.
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See also:
J/ApJS/240/33 : MaDCoWS. I. Catalog of z∼1 galaxy clusters (Gonzalez+, 2019)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- ACT ACT name (ACT-CL JHHMM/m+DDMM)
21- 25 F5.3 --- zACT ACT redshift
27- 31 F5.3 --- e_zACT ?=- ACT redshift error
33- 36 A4 --- f_zACT [spec phot] ACT z Type
38- 41 F4.2 10+14Msun M500-SZ ?=- Mass within an overdensity 500 times
the critical density
43- 46 F4.2 10+14Msun E_M500-SZ ?=- Error on M500-SZ (upper value)
48- 51 F4.2 10+14Msun e_M500-SZ ?=- Error on M500-SZ (lower value)
53- 66 A14 --- MaDCoWS MaDCoWS Name, MOO JHHMM+DDMM
68- 72 F5.3 --- zMaDCoWS ?=- MaDCoWS redshift
74- 75 I2 --- lambda15 ?=- Richness (1)
77 I1 --- e_lambda15 ?=- Richness error
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Note (1): Richness (lambda15) values are those reported by Gonzalez et al.
(2019ApJS..240...33G 2019ApJS..240...33G, Cat. J/ApJS/240/33). Note that some clusters do not
have a 15 value associated with them, as Gonzalez et al.
(2019ApJS..240...33G 2019ApJS..240...33G, Cat. J/ApJS/240/33) did not report richness values for
clusters with for clusters with low partial IRAC data.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Dec-2021