simulating 21cm sky - ska-jp.orgska-jp.org/skajpws2019/day2/2-16_nishizawa.pdf · • assume ska...
TRANSCRIPT
SIMULATING 21CM SKY
Atsushi J. Nishizawa (Nagoya) Kiyotomo Ichiki (Nagoya) Rika Ando (Nagoya)
HI AS A PROBE OF LARGE-SCALE STRUCTURE
Robertson+ ’13
dark
mat
ter h
alo
HI d
ensit
y
z=1
CMB-LENSING IS USEFUL FOR HI
redshift
CMB
Lens
ing
kern
el
EoR
post-EoR decoupling
⌃⇤�1cr (�) =
(�⇤ � �)�
�⇤
• Lensing efficiency for CMB lensing
• It has a maximum at the post-EoR
•Kernel Matches
h(aHIlm + aFGlm )almi = h(aHI
lmalmi = C�HIl
• CMB lens and Galactic foreground is NOT correlated each other
• We are free from the FG!!
•Foreground
-> 田中君のトーク (Tanaka, [AJN]+ 2019)
CMB /Z z⇤
0
dz
H(z)(1 + z)⌃⇤�1
cr �m<latexit sha1_base64="3I6HDE0OZXQWlVTjQJ1NaLiJVJo=">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</latexit>
IS FOREGROUND REALLY NOT THE PROBLEM?
Santos+’05
Gal. Synchrotron
Ext. Gal. PS
Gal. Free-Free
Ext. Gal. F-F
21cm signal
6 orders larger!!
• How much is the effect of foreground on the cross correlation?
• To what extent we need to consider the foreground removal?
SIMULATION - DARK MATTER -• Use Takahashi+ 2017 ray tracing simulation for CMB lensing and DM
★
…
… L=450Mpc/h
14L=6.5Gpc/h
z=7.1
z=1100
……..random Gaussian
• redshift shell 150Mpc/h • source redshifts are
equally spanned from 0.051 to 5.342 (w 150Mpc/h width) and additionally zs=1100
• outputs
�2Dcdm(n, zi)
(n, zi)
CMB(n)
halo(x, M)
SIMULATION - HI PASTING -• HI is pasted to the DM distribution (calibrated with Illustris TNG)
• linear bias • MHI-Mh relation (fitting, scatter, …) • more complex modeling…
�Tb =3
32⇡
hc3A10
kBmp⌫221
(1 + z)2
H(z)⇢̄HI�HI(n, z)
Ando, AJN+ 2019Villaescusa-Navaro+ 2018 (Illustris TNG)
MHI(Mh, z) = M0
✓Mh
Mmin
◆↵
exp
✓�Mmin
Mh
◆�HI = bHI ? �cdm
• linear bias approximation is only valid on large scales (k<0.2 h/Mpc)
SIMULATION - MAPS AND AUTO SPECTRA -
CMB lensing map
Brightness temperature map @ z=1
`(`+ 1)C`
1 10 102 103
`(`+ 1)CHI` [mK2]
ANTENNA NOISE• We approximate the noise as white spectrum • values quoted from Bull et al. 2015 • assume SKA interferometer covers 20,000 deg2 in 10,000 hours • SKA-MID (Wide: Band 1) specifications • Tsys = Tinst + Tsky ~ 20 + 60*(300MHz/nu)^2.5 [K] • generate noise map with random-Gaussian
CN=
T 2
sys
⌫21
ttot
�4Asky
A2
eFoV
1
Nbn(u)<latexit sha1_base64="HenzqlbQTHdQPbnEY6838eg0gEA=">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</latexit>
100 101 102 103
multipole `
10�5
10�4
10�3
10�2
10�1
100
`(`
+1)
C`
[mK
2 ]
simulated HI @ z=1.0
SKA-MID1 (Intef.) noise
`(`+ 1)CHI` [mK]2
<latexit sha1_base64="PYjoVIRYotV5toCFWGcZ/HJ4BBo=">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</latexit>
`(`+ 1)C�HI` [mK]
<latexit sha1_base64="k95WWkn6ruwnYHApn6eCSwc7Vb8=">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</latexit>
GALACTIC FOREGROUND• So far, Galactic synchrotron radiation (most dominant) only, but others are
straightforward to implement. • FG map is based on the Haslam template w/ finer structures from random
Gaussian under position dependent power spectrum. • publicly available code CRIME (Aronso+ 2014)
synchrotron map @ 700 MHz
CROSS CORRELATION• Cross correlation signal is highly contaminated. • it is expected consistent with “zero” but with a huge scatter. • despite the null signal, we anyway need to reduce the level of foreground
CL^HI-KAPPA W/O
FOREGROUND REMOVAL
anything within the error bar can be a statistical fluke!
�2CHI` =
[CHI` ]2 + [C
` +N` ][C
HI` +NHI
` +NFG` ]
(2`+ 1)fsky<latexit sha1_base64="bTUPF9bb3Uif5nkt8nfvJjbfPGU=">AAADH3ichVHLbtNAFL02rzI8msIGiY1FVFQUKRqnaXhISBWVStlA2pK2Uuxa4+kkWBk/ZDuRguUf4AdYsCoSQog/YMsCVogNi3wCYlkkNiy4flQNi8C17Dn33HOu78zYgXSimNKJop46febsubnz5MLFS5fnKwtXdiJ/GHLR4b70wz2bRUI6nujETizFXhAK5tpS7NqDtay+OxJh5Pje03gcCNNlfc/pOZzFSFmVD0bk9F2239DWrMQQUqb7iTFgQcASI3S1jUdpSu4ToxcynpDuTI2JDWraSb0o1x5bWVpm5rS98B0LpvJpxfrD1CRpQpYaGVnTb/WsnI8G45SkVqVK63dbenOlpeWgtVyCpq5rep3mUYUy2n7lLRhwAD5wGIILAjyIEUtgEOHTBR0oBMiZkCAXInLyuoAUCHqHqBKoYMgO8NvHrFuyHuZZzyh3c/yLxDdEpwaL9Bt9R4/oZ/qefqe/Z/ZK8h7ZLGNc7cIrAmv+xbXtX/91ubjG8OzE9c+ZY+jBnXxWB2cPcibbBS/8o+cvj7bvbS0mN+lr+gPnP6QT+hF34I1+8jebYusVELyA41PWZoOdRl1frtPNZnX1QXkVc3AdbsASnvdtWIUNaEMHuKIp68oTpa0eqp/UL+rXQqoqpecq/BXq5A/4hs97</latexit>
huge!!
IDEAL FOREGROUND REMOVAL• assume that the FG can be removed at %
�T obs
b = �T 21cm
b + (1� ↵)�TFG
b<latexit sha1_base64="UqXrRZ/RfJHJCjpFRjlLb75w/WE=">AAACsnichVHLahRBFD3p+EjGR0bdBNwUDgkRcbidjBMTCIQI6kbIa5JgJhmqK5WkSfWD7pqBZJgf8AdcuIogIi79BDf+gIvZ6kpcRsjGhXd6WkQleouqOnXqnlunqrzY+Kkl6g44g+fOX7g4NFy4dPnK1ZHitetradRMlK6pyETJhidTbfxQ16xvjd6IEy0Dz+h17+BBb3+9pZPUj8JVexjrrUDuhf6ur6RlqlF8Ut/Rxkqx2vC22/UkEJGXdsSc+JOedFXQEXfEhHu3Lk28L2//lfLwUadRLFF5pupW7lVFBqpTOai4rnDLlEUJeSxGxdeoYwcRFJoIoBHCMjaQSLltwgUhZm4LbeYSRn62r9FBgbVNztKcIZk94HGPV5s5G/K6VzPN1IpPMdwTVgqM0Ud6Qyf0gd7SF/p+Zq12VqPn5ZBnr6/VcWPk2ejK6X9VAc8W+79U//RssYv7mVefvccZ07uF6utbR89PVmaXx9rj9JK+sv9j6tJ7vkHY+qZeLenlFyjwB/x8ZXE2WJssu1NlWqqU5hfyrxjCTdzCBL/3NObxGIuo8bnv0MUnfHYqzlNHOqqf6gzkmhv4LRzzAzGppgE=</latexit>
↵<latexit sha1_base64="PyqU368ZIjjtW7iJPPjlolxocI0=">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</latexit>
• FG should be removed at 99.9%
CL^HI-KAPPA W/O
FOREGROUND REMOVAL
MASKING?• Half of the sky where the FG is significant is masked (>~100K) • Even after masking, the FG should be removed up to 99.5%
CL^HI-KAPPA W/O
FOREGROUND REMOVAL
SUMMARY• we consider the x-correlation of HI with CMB-lensing
• HI-CMBLens may be the most efficient way to extract cosmological information.
• HI-CMBLens has been expected to be free from FG
• Signal, Noise and FG are all simulated
• To find the signal, FG should be removed at 99.9% (99.5% if half masked)
— Future plan —
• Apply real FG removal method
• Include CMB Lens noise
• use more complex (realistic) HI-pasting model