High resolution SZ observations at the IRAM 30

High resolution SZ
observations at the IRAM 30-m
telescope with the NIKA
camera
Rémi Adam for the NIKA collaboration
Rencontres de Moriond - March 2014 - La Thuile
http://ipag.osug.fr/nika2
R. Adam, A. Adane, P. Ade, P. André, A. Beelen, B. Belier, A. Benoît, A. Bideaud,
N. Billot, N. Boudou, O. Bourrion, M. Calvo, A. Catalano, G. Coiffard, B. Comis,
A. D’Addabbo, F.-X. Désert, S. Doyle, J. Goupy, C. Kramer, S. Leclercq,
J. F. Macias-Perez, J. Martino, P. Mauskopf, F. Mayet, A. Monfardini, F. Pajot,
E. Pascale, L. Perotto, E. Pointecouteau, N. Ponthieu, V. Revéret, L. Rodriguez,
F. Ruppin, G. Savini, K. Schuster, A. Sievers, C. Tucker, R. Zylka
Outline
1. The Sunyaev-Zel’Dovich effect (SZ) as
a mass proxy
2. The Kinetic Inductance Detectors (KIDs)
3. The New IRAM KIDs Array (NIKA)
4. First SZ results with the NIKA prototype
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The Sunyaev-Zel’Dovich effect (SZ)
217 GHz
negative
SZ flux
positive
SZ flux
Inverse Compton scattering
of hot electrons in the ICM
[J. E. Carlstrom et al. (2002)]
[L. Van Speybroeck]
SZflux /
➡
Z
Pe dl
The SZ effect is a distortion of the CMB spectrum
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SZ flux - mass scaling relation
SZflux ! thermal pressure ! thermal energy ! hydrostatic mass
Planck versus the MUSIC simulation
required for cosmology
[Planck Collaboration XX (2013)]
• Bias due to non gravitational
processes (e.g. non virialized
structures)
Mhyd = (1
(SZflux )
• SZ flux - total mass calibration is
b)Mtot
• Need to look at clusters in detail:
Scatter + bias
projection effects, relativistic
corrections, ...
• SZ in complement to X-ray, lensing
and radio can break biases and
degeneracies
➡
[F. Sembolini et al. (2012)]
High resolution SZ observations are needed
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Towards the next generation of mm wavelength
instruments
How to improve high resolution SZ
observations ?
Reduce the noise
Increase statistics
Increase statistics
30 m
1. Space/ballon
experiments
Low resolution
2. Observe
longer
3. Use more
detectors
Telescope time is
expensive
Kinetic Inductance Detectors (KIDs) offer an
alternative to bolometers for large array instruments
The New IRAM KIDs Array (NIKA):
➡ Dual-band KID camera
➡ Developed in Grenoble (France)
➡ Observing at the IRAM 30m telescope (Granada, Spain)
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The Kinetic Inductance Detectors (KIDs)
• KIDs are high-Q superconducting RLC resonators
T ⇠ 100 mK ⌧ Tc ' 1.2 K
• Absorbed photons change the kinetic inductance
by breaking Cooper pairs (charge carriers)
Single KID:
Aluminum on silicon wafer
δ f0 ∝ δ Lk ∝ Popt
Feed-line
Transfer function of a single KID
Inductance
(absorber)
Capacitor
Dark
Illumination
Illumination
[A. Monfardini et al. (2010)]
➡ KIDs probe optical power via the shift of their resonance frequencies
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Frequency multiplexing with KIDs
• KID arrays are pixels connected to a
single transmission line
• Cheap and easy to make
• Not sensitive to temperature fluctuations
...
In
f0
~50 mm
(1)
f0
(2)
f0
(N )
Out
A
Te
xt
e
132 KID array (140 GHz)
[A. Monfardini et al. (2010)]
➡ KIDs are intrinsically frequency-multiplexed
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The NIKA and NIKA2 projects
The IRAM 30m telescope:
The dilution cryostat:
The dedicated optics:
• 6.5’ (1.8’) field of view
• Beam splitting in two bands
• Filters + mirrors + lenses
~100 mK
[O. Bourrion et al. (2012)]
• 12” resolution at 260 GHz
• 17” resolution at 150 GHz
The two KID arrays:
• 2x2000 (224) KIDs at 260 GHz
• 1000 (132) KIDs at 150 GHz
• State-of-the-art sensitivity
➡
➡
The dedicated NIKEL
readout electronics
NIKA2
(NIKA prototype)
The NIKA prototype is currently operating
NIKA2 will be commissioned by 2015
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SZ scientific goal
• Calibrating the SZ flux as a mass proxy and its evolution with redshift
• Planck/ACT (unresolved) clusters are a working basis to define a representative sample
• Characterize the structural properties and clusters’ dynamical state
150 GHz
260 GHz
➡
SZ observations are at the core of the NIKA2 project
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First results with the NIKA prototype:
RX J1347.5-1145 (z=0.45)
Texte
• Observation performed in
November 2012
• Dual-band common-mode
decorrelation form the 240
GHz band
• Large scales are recovered
140 GHz
• Integration time: 5h47min
Texte
➡
The first SZ observation with KIDs, using the NIKA prototype
[R. Adam, B. Comis, J. F. Macías-Pérez et al. (2013) - accepted]
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SZ results: RX J1347.5-1145
complementarity with X-ray data
Texte
• The X-ray emission is due to
bremsstrahlung from hot electrons
Center
X ray /
2
ne
p
Te
SZ / Pe / ne Te
• SZ is well adapted for the
Shock
measurement of shocks
• RX J1347.5-1145 is an ongoing
merger (strong SE extension)
➡ Detection and SZ mapping achieved
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SZ results: RX J1347.5-1145
pressure distribution
• We fit the relaxed North region of RX J1347.5-1145 using a
gNFW pressure profile parametrization [D. Nagai et al. (2007)]
data
best fit model
Texte
Texte
P(r) =
P0
⎛ r⎞ ⎛ ⎛ r⎞ ⎞
⎜⎝ r ⎟⎠ ⎜ 1+ ⎜⎝ r ⎟⎠ ⎟
s
s
⎝
⎠
γ
α
β −γ
α
Slopes fixed to:
[M. Arnaud et al. (2010)]
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↵ = 1.2223
= 5.4905
= 0.7736
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SZ results: RX J1347.5-1145
pressure distribution
• We fit the relaxed North region of RX J1347.5-1145 using a
gNFW pressure profile parametrization [D. Nagai et al. (2007)]
data
best fit model
residual
Texte
Texte
Overpressure
➡
RX J1347.5-1145 is well described by a relaxed cool-core
subject to a merging on its South-East part
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CL J1226.9+3332 - z=0.89
Very preliminary results of the campaign of February 2014
• 150 GHz signal to
noise map shown
• 7.4 h on source
shown here
Texte
➡ SZ mapping of high redshift cluster
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MACS J0717.5+3745 - z=0.55
Very preliminary results of the campaign of February 2014
• Signal to noise
maps
• 5.3 h on source
shown here
• Foreground galaxy
detected
150 GHz
Te
xt
260 GHz
Texte
• X-ray/optics simulation
• Includes tSZ+kSZ
+relativistic corrections
Texte
➡ SZ mapping of a very disturbed cluster at 150 and 260 GHz
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Conclusions
• KIDs are a promising alternative to
bolometers for large array instruments
• We demonstrate the capability of KIDs for SZ
observation with the NIKA prototype
• NIKA2 will be a well-suited for in-depth
studies of the ICM from local to distant clusters
(e.g. follow up of PLANCK’s clusters at high
redshift)
• NIKA2 project accepted by IRAM and funded
• Commissioning on mid 2015, first scientific
run end 2015 - beginning 2016
1000 pixels KIDs array
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