J/A+A/617/A64 3D density & temp. profiles of 5 clusters (Bartalucci+, 2018)
Resolving the hydrostatic mass profiles of galaxy clusters at z ∼ 1
with XMM-Newton and Chandra.
Bartalucci I., Arnaud M., Pratt G.W., Le Brun A.M.C.
<Astron. Astrophys. 617, A64 (2018)>
=2018A&A...617A..64B 2018A&A...617A..64B (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Morphology
Keywords: X-rays: galaxies: clusters - dark matter
Abstract:
We present a detailed study of the integrated total hydrostatic mass
profiles of the five most massive (M500SZ>5x1014M☉)
galaxy 500 clusters selected at z∼1 via the Sunyaev-Zel'dovich
effect. These objects represent an ideal laboratory to test structure
formation models where the primary driver is gravity. Optimally
exploiting spatially-resolved spectroscopic information from
XMM-Newton and Chandra observations, we used both parametric (forward,
backward) and non-parametric methods to recover the mass profiles,
finding that the results are extremely robust when density and
temperature measurements are both available. Our X-ray masses at
R500 are higher than the weak lensing masses obtained from the
Hubble Space Telescope (HST), with a mean ratio of 1.39+0.47-0.35.
This offset goes in the opposite direction to that expected in a
scenario where the hydrostatic method yields a biased, underestimated,
mass. We investigated halo shape parameters such as sparsity and
concentration, and compared to local X-ray selected clusters, finding
hints for evolution in the central regions (or for selection effects).
The total baryonic content is in agreement with the cosmic value at
R500. Comparison with numerical simulations shows that the mass
distribution and concentration are in line with expectations. These
results illustrate the power of X-ray observations to probe the
statistical properties of the gas and total mass profiles in this
high-mass, high-redshift regime.
Description:
We report the deprojected density and 3D temperature radial profiles
of the 5 clusters of the sample presented in the paper. For each
cluster we report the effective radius at which the quantity is
computed, as defined in equation (2) of the paper, the boundaries of
the annuli in which the data have been measured, the deprojected
density and 3D temperature profiles and the respective 1-sigma
uncertainties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 62 5 List of clusters
profiles.dat 208 433 3D density and temperature profiles of the
five clusters
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Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Cluster Cluster name (SPT-CLJHHMM+DDMM)
18- 19 I2 h RAh Right ascension (J2000)
21- 22 I2 min RAm Right ascension (J2000)
24- 28 F5.2 s RAs Right ascension (J2000)
30 A1 --- DE- Declination sign (J2000)
31- 32 I2 deg DEd Declination (J2000)
34- 35 I2 arcmin DEm Declination (J2000)
37- 40 F4.1 arcsec DEs Declination (J2000)
42- 46 F5.3 --- z Redshift
48- 62 A15 --- OName PLANCK name of the cluster
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Byte-by-byte Description of file: profiles.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Cluster SPT name of the cluster
20- 32 F13.10 arcmin Rneeff Density effective radius
36- 48 F13.10 arcmin Rnein Density minimum anuli radius
52- 64 F13.10 arcmin Rneout Density maximum anuli radius
68- 80 F13.10 cm-3 ne Deprojected density
84- 96 F13.10 cm-3 e_ne 1-sigma lower density error
100-112 F13.10 cm-3 E_ne 1-sigma higher density error
116-128 F13.10 arcmin RkTeff Temperature effective radius
132-144 F13.10 arcmin RkTin Temperature minimum anuli radius
148-160 F13.10 arcmin RkTout Temperature maximum anuli radius
164-176 F13.10 keV kT Deprojected temperature
180-192 F13.10 keV e_kT 1-sigma lower temperature error
196-208 F13.10 keV E_kT 1-sigma higher temperature error
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Acknowledgements:
Iacopo Bartalucci, iacopo.bartalucci(at)cea.fr
(End) Iacopo Bartalucci [CEA, Saclay], Patricia Vannier [CDS] 28-Aug-2018