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Cross-correlation between the thermal Sunyaev-Zeldovich effect and the Integrated Sachs-Wolfe effect
Authors
Amare Abebe
Aroonkumar Beesham
+6Β more
Xuelei Chen
Wei-Ming Dai
Ayodeji Ibitoye
Yin-Zhe Ma
Denis Tramonte
Patricio Vielva
Publication date
15 January 2024
Publisher
View
on
arXiv
Abstract
We present a joint cosmological analysis of the power spectra measurement of the Planck Compton parameter and the integrated Sachs-Wolfe (ISW) maps. We detect the statistical correlation between the Planck Thermal Sunyaev-Zeldovich (tSZ) map and ISW data with a significance of a
3.6
Ο
3.6\sigma
3.6
Ο
confidence level~(CL), with the autocorrelation of the Planck tSZ data being measured at a
25
Ο
25 \sigma
25
Ο
CL. The joint auto- and cross-power spectra constrain the matter density to be
Ξ©
m
=
0.31
7
β
0.031
+
0.040
\Omega_{\rm m}= 0.317^{+0.040}_{-0.031}
Ξ©
m
β
=
0.31
7
β
0.031
+
0.040
β
, the Hubble constant
H
0
=
66.
5
β
1.9
+
2.0
β
k
m
β
s
β
1
β
M
p
c
β
1
H_{0}=66.5^{+2.0}_{-1.9}\,{\rm km}\,{\rm s}^{-1}\,{\rm Mpc}^{-1}
H
0
β
=
66.
5
β
1.9
+
2.0
β
km
s
β
1
Mpc
β
1
and the rms matter density fluctuations to be
Ο
8
=
0.73
0
β
0.037
+
0.040
\sigma_{8}=0.730^{+0.040}_{-0.037}
Ο
8
β
=
0.73
0
β
0.037
+
0.040
β
at the 68% CL. The derived large-scale structure
S
8
S_{8}
S
8
β
parameter is
S
8
β‘
Ο
8
(
Ξ©
m
/
0.3
)
0.5
=
0.755
Β±
0.060
S_8 \equiv \sigma_{8}(\Omega_{\rm m}/0.3)^{0.5} = 0.755\pm{0.060}
S
8
β
β‘
Ο
8
β
(
Ξ©
m
β
/0.3
)
0.5
=
0.755
Β±
0.060
. If using only the diagonal blocks of covariance matrices, the Hubble constant becomes
H
0
=
69.
7
β
1.5
+
2.0
β
k
m
β
s
β
1
β
M
p
c
β
1
H_{0}=69.7^{+2.0}_{-1.5}\,{\rm km}\,{\rm s}^{-1}\,{\rm Mpc}^{-1}
H
0
β
=
69.
7
β
1.5
+
2.0
β
km
s
β
1
Mpc
β
1
. In addition, we obtain the constraint of the product of the gas bias, gas temperature, and density as
b
g
a
s
(
T
e
/
(
0.1
β
k
e
V
)
)
(
n
Λ
e
/
1
β
m
β
3
)
=
3.0
9
β
0.380
+
0.320
b_{\rm gas} \left(T_{\rm e}/(0.1\,{\rm keV}) \right ) \left(\bar{n}_{\rm e}/1\,{\rm m}^{-3} \right) = 3.09^{+0.320}_{-0.380}
b
gas
β
(
T
e
β
/
(
0.1
keV
)
)
(
n
Λ
e
β
/1
m
β
3
)
=
3.0
9
β
0.380
+
0.320
β
. We find that this constraint leads to an estimate on the electron temperature today as
T
e
=
(
2.4
0
β
0.300
+
0.250
)
Γ
1
0
6
β
K
T_{\rm e}=(2.40^{+0.250}_{-0.300}) \times 10^{6} \,{\rm K}
T
e
β
=
(
2.4
0
β
0.300
+
0.250
β
)
Γ
1
0
6
K
, consistent with the expected temperature of the warm-hot intergalactic medium. Our studies show that the ISW-tSZ cross-correlation is capable of probing the properties of the large-scale diffuse gas.Comment: 25 pages, 15 figures, 2 table
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Last time updated on 20/08/2024