J/ApJ/914/58 Chandra obs. of Planck ESZ & X-ray clusters (Andrade-Santos+, 2021)
Chandra observations of the Planck Early Sunyaev-Zeldovich sample: a
reexamination of masses and mass proxies.
Andrade-Santos F., Pratt G.W., Melin J.-B., Arnaud M., Jones C.,
Forman W.R., Pointecouteau E., Bartalucci I., Vikhlinin A., Murray S.S.,
Mazzotta P., Borgani S., Lovisari L., van Weeren R.J., Kraft R.P.,
David L.P., Giacintucci S.
<Astrophys. J., 914, 58 (2021)>
=2021ApJ...914...58A 2021ApJ...914...58A
ADC_Keywords: Clusters, galaxy; Intergalactic medium; X-ray sources; Redshifts
Keywords: Galaxy clusters ; Intracluster medium ; Sunyaev-Zeldovich effect
Abstract:
Using Chandra observations, we derive the YX proxy and associated
total mass measurement, M500Yx for 147 clusters with z<0.35 from
the Planck early Sunyaev-Zeldovich catalog, and for 80 clusters with
z<0.22 from an X-ray flux-limited sample. We reextract the Planck
YSZ measurements and obtain the corresponding mass proxy,
M500SZ, from the full Planck mission maps, minimizing Malmquist
bias due to observational scatter. The masses reextracted using the
more precise X-ray position and characteristic size agree with the
published PSZ2 values, but yield a significant reduction in the
scatter (by a factor of two) in the M500SZ-M500Yx relation.
The slope is 0.93±0.03, and the median ratio,
M500SZ/M500Yx=0.91±0.01, is within the expectations from
known X-ray calibration systematics. YSZ/YX is 0.88±0.02, in good
agreement with predictions from cluster structure, and implying a low
level of clumpiness. In agreement with the findings of the Planck
Collaboration, the slope of the YSZ-DA-2YX flux relation is
significantly less than unity (0.89±0.01). Using extensive
simulations, we show that this result is not due to selection effects,
intrinsic scatter, or covariance between quantities. We demonstrate
analytically that changing the YSZ-YX relation from apparent flux
to intrinsic properties results in a best-fit slope that is closer to
unity and increases the dispersion about the relation. The
redistribution resulting from this transformation implies that the
best-fit parameters of the M500SZ-M500Yx relation will be
sample-dependent.
Description:
For our investigation, we make use of the following cluster samples:
1. An SZ-selected sample of clusters derived from the first catalog of
189 objects detected in the first 10 months of the Planck survey, and
released in early 2011 (Planck Collaboration VIII 2011, VIII/88).
A Chandra X-Ray Visionary Program (PI: Jones) and High Resolution
Camera (HRC) Guaranteed Time Observations (PI: Murray) were combined
to form the Chandra-Planck Legacy Program for Massive Clusters of
Galaxies. For each of the 163 ESZ Planck clusters at z<0.35, we
obtained Chandra exposures sufficient to collect at least 10000 source
counts. Figure 1 displays a mosaic of the 147 clusters from the ESZ
sample that are used in this work. See Section 2.
2. An X-ray-selected sample of high-flux clusters.
Voevodkin & Vikhlinin (2004ApJ...601..610V 2004ApJ...601..610V) compiled a sample of the
52 X-ray-brightest clusters in the local universe by selecting the
highest-flux objects detected in the ROSAT All-sky Survey at
|b|>20° and z>0.025 --using the HIFLUGCS catalog as reference.
The sample used here is an extension of Voevodkin & Vikhlinin's (2004)
approach, where the flux limit in the 0.5-2.0keV band was lowered to
fX>7.5x10-12erg/s/cm2. We obtained a sample of 80 clusters which
all have Chandra observations. See Section 2.
Throughout this paper, we assume a standard ΛCDM cosmology with
H0=70km/s/Mpc, ΩM=0.3, and ΩΛ=0.7. The
variables M500 and R500 are the total mass within R500 and the
radius corresponding to a total density contrast Δ=500 as
compared to ρc(z), the critical density of the universe at the
cluster redshift. The SZ flux is characterized by Y500SZ (in
square arcminutes), or simply YSZ. The quantity DA2YSZ is then
the spherically integrated Compton parameter within R500 (in square
megaparsecs), where DA is the angular diameter distance of the
cluster. All uncertainties are quoted at the 1σ (68% confidence)
level.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 162 147 Cluster masses using SZ and X-ray proxies
for the clusters in the Planck ESZ (see VIII/88)
sample
table2.dat 163 80 Cluster masses using SZ and X-ray proxies
for the clusters in the X-ray (see
Voevodkin & Vikhlinin 2004ApJ...601..610V 2004ApJ...601..610V) sample
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
VIII/88 : Planck Early Release Compact Source Catalogue (Planck, 2011)
VIII/91 : Planck Catalog of Compact Sources Release 1 (Planck, 2013)
J/ApJ/511/65 : Einstein images of galaxy clusters (Jones & Forman, 1999)
J/A+A/536/A8 : Planck early results. VIII. ESZ sample. (Planck+, 2011)
J/A+A/575/A30 : HIFLUGCS XMM/Chandra cross-calibration (Schellenberger+, 2015)
J/A+A/594/A27 : Planck Sunyaev-Zeldovich sources (PSZ2) (Planck+, 2016)
J/ApJ/843/76 : Cool-core clusters with Chandra obs. (Andrade-Santos+, 2017)
J/MNRAS/469/3738 : Complete sample of galaxy clusters (Schellenberger+, 2017)
J/MNRAS/468/3322 : CoMaLit. V. Mass forecasting with proxies (Sereno+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- PLCKESZ Cluster identifier (GLLL.ll+BB.bb)
15- 16 I2 h RAh Hour of Right Ascension (J2000)
18- 19 I2 min RAm Minute of Right Ascension (J2000)
21- 26 F6.3 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 39 F5.2 arcsec DEs Arcsecond of Declination (J2000)
41- 45 F5.3 --- z [0.017/0.35] Spectroscopic redshift
47- 51 F5.2 10+14Msun M500YX [2/17.6] Mass derived using Yx
53- 56 F4.2 10+14Msun e_M500YX [0.2/2.1] Uncertainty in M500YX
58- 62 F5.2 10+14Msun M500PSX [2/16.3] Mass re-derived using Ysz with
X-ray center & size
64- 67 F4.2 10+14Msun e_M500PSX [0.1/0.6] Uncertainty in M500PSX
69- 73 F5.2 10+14Msun M500PSZ2 [1.9/16.2] Mass from PSZ2 catalog
75- 78 F4.2 10+14Msun e_M500PSZ2 [0.05/0.6] Uncertainty in M500PSZ2
80- 84 F5.2 Mpc2 YX-Mpc2 [1/44.7] Yx value in Mpc squared
86- 89 F4.2 Mpc2 e_YX-Mpc2 [0.16/8.5] Lower uncertainty in YX-Mpc2
91- 94 F4.2 Mpc2 E_YX-Mpc2 [0.17/9.2] Upper uncertainty in YX-Mpc2
96- 103 F8.2 arcmin2 YX-Arc2 [63/13793] Yx value in arcmin squared
105- 111 F7.2 arcmin2 e_YX-Arc2 [10/2109] Lower uncertainty in YX-Arc2
113- 119 F7.2 arcmin2 E_YX-Arc2 [11/2257] Upper uncertainty in YX-Arc2
121- 125 F5.2 Mpc2 YSZ-Mpc2 [0.9/41.4] Ysz value in Mpc squared
127- 130 F4.2 Mpc2 e_YSZ-Mpc2 [0.1/1.6] Lower uncertainty in YSZ-Mpc2
132- 135 F4.2 Mpc2 E_YSZ-Mpc2 [0.1/1.6] Upper uncertainty in YSZ-Mpc2
137- 143 F7.2 arcmin2 YSZ-Arc2 [65/8451] Ysz value in arcmin squared
145- 150 F6.2 arcmin2 e_YSZ-Arc2 [8.9/300] Lower uncertainty in YSZ-Arc2
152- 157 F6.2 arcmin2 E_YSZ-Arc2 [8.9/300] Upper uncertainty in YSZ-Arc2
159- 162 F4.2 --- rmax [0.45/2.11] Maximum radius, R500 (1)
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Note (1): Where the emission integral is computed, in units of R500.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Cluster identifier (GLLL.ll+BB.bb)
16- 17 I2 h RAh Hour of Right Ascension (J2000)
19- 20 I2 min RAm Minute of Right Ascension (J2000)
22- 27 F6.3 s RAs Second of Right Ascension (J2000)
29 A1 --- DE- Sign of the Declination (J2000)
30- 31 I2 deg DEd Degree of Declination (J2000)
33- 34 I2 arcmin DEm Arcminute of Declination (J2000)
36- 40 F5.2 arcsec DEs Arcsecond of Declination (J2000)
42- 46 F5.3 --- z [0.027/0.22] Spectroscopic redshift
48- 52 F5.2 10+14Msun M500YX [1.2/17.6] Mass derived using Yx
54- 57 F4.2 10+14Msun e_M500YX [0.1/2.1] Uncertainty in M500YX
59- 63 F5.2 10+14Msun M500PSX [1/16.3] Mass re-derived using Ysz with
X-ray center & size
65- 68 F4.2 10+14Msun e_M500PSX [0.1/0.5] Uncertainty in M500PSX
70- 74 F5.2 10+14Msun M500PSZ2 [1/16.2] Mass from PSZ2 catalog
76- 80 F5.2 10+14Msun e_M500PSZ2 [0.05/0.5] Uncertainty in M500PSZ2
82- 86 F5.2 Mpc2 YX-Mpc2 [0.3/43.8] Yx value in Mpc squared
88- 91 F4.2 Mpc2 e_YX-Mpc2 [0.06/8.5] Lower uncertainty in YX-Mpc2
93- 96 F4.2 Mpc2 E_YX-Mpc2 [0.07/9.2] Upper uncertainty in YX-Mpc2
98- 104 F7.2 arcmin2 YX-Arc2 [96/3657] Yx value in arcmin squared
106- 112 F7.2 arcmin2 e_YX-Arc2 [15/1038] Lower uncertainty in YX-Arc2
114- 120 F7.2 arcmin2 E_YX-Arc2 [17/1183] Upper uncertainty in YX-Arc2
122- 126 F5.2 Mpc2 YSZ-Mpc2 [0.34/41.4] Ysz value in Mpc squared
128- 131 F4.2 Mpc2 e_YSZ-Mpc2 [0.07/1.2] Lower uncertainty in YSZ-Mpc2
133- 136 F4.2 Mpc2 E_YSZ-Mpc2 [0.07/1.2] Upper uncertainty in YSZ-Mpc2
138- 144 F7.2 arcmin2 YSZ-Arc2 [95/2174] Ysz value in arcmin squared
146- 151 F6.2 arcmin2 e_YSZ-Arc2 [19/127] Lower uncertainty in YSZ-Arc2
153- 158 F6.2 arcmin2 E_YSZ-Arc2 [19/127] Upper uncertainty in YSZ-Arc2
160- 163 F4.2 --- rmax [0.76/2.66] Maximum radius, R500 (1)
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Note (1): Where the emission integral is computed, in units of R500.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Dec-2022