Astrophysics and cosmology
with KID cameras
J.F. Macías-Pérez – LPSC
on behalf of the Grenoble KID collaboration

The KID collaboration at Grenoble
Alessandro MONFARDINI – Director of research
Alain BENOIT – Director of research (Emeritus)
Sébastien TRIQUENAUX – Research engineer
Martino CALVO – Research engineer* Aurélien BIDEAUD – Research engineer (postdoc)* Johannes GOUPY – Research expert (postdoc)* Alessandro FASANO - PhD Started 10/2017
Juan MACIAS-PEREZ – Director of research
Andrea CATALANO – Researcher
Olivier BOURRION – Research engineer
Frédéric MAYET – LectureLaurence PEROTTO – Researcher* Florian RUPPIN – PhD Started 10/2015
Karl SCHUSTER – Director
Eduard DRIESSEN – Scientist
Samuel Leclerq - Scientist* Shibo SHU – PhD Started 10/2016
François-Xavier DESERT – Astronomer / Director
Nicolas PONTHIEU – Researcher* Aina ANDRIANASOLO – PhD Started 10/2016
J.F. Macías-Pérez

Evoluton of the Universe - TGSW2018

2Outline
I. From cosmology/astrophysics challenges to instrumental
requirements at mm wavelengths
II. Kinetic Inductance Detectors for the new generation of mmcameras
III. The NIKA2 camera for cluster cosmology
IV. Large wide-field mm spectroscopy with KIDs

J.F. Macías-Pérez

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Inflation

CMT& BPani

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Brief history of the Universe

J.F. Macías-Pérez

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Main science drivers at mm wavelenths● Detection of primordial CMB B-modes polarisation anisotropies (primordialgrativational waves) to measure the energy scale of inflation● Detailed measurement of the Sunyaev-Zeldovic effect in clusters of galaxies
to obtain independent and complementary cosmological constraints● Deep observations of distant galaxies in cosmological fields (COSMOS,GOODS, etc) to the confusion limit● Detailed understanding of the reionization processes (stellar mass function)
at high redshift via spectroscopic observations● Multi-color continuum observations of Galactic and extra-Galactic sources athigh resolution over a wide-field to measure the dust mass and infer starformation

J.F. Macías-Pérez

Evoluton of the Universe - TGSW20185From science to technological requirements
Requirements
B-ModesSpectral distortions

SZ Effect

Re-ionisationhigh sensitivity for low r values
multi-frequency for foreground removal
Wide-field high sensitivity spectroscopic camera

high resolution, high sensitivity mapping of distant clusters
spectroscopy measurements of nearby clusters mapping
thermodynamic properties
measurements of molecules lines
at high red-shifthigh sensitivity
mapping large sky areas

Large high sensitivity detector arrays are needed !!
J.F. Macías-Pérez

Evoluton of the Universe - TGSW20186Kineti nduitanie Deteitors (K D)

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Why K Ds?
✔ Direct multiplexing (300 detectors or more)✔ Can adapt to low and high background: from ground to satellite
experiments✔ Fast response (time constant << 1 ms)✔ Not too sensitive to comic-rays hits
✔ Large spectral coverage: frequency range from 70-1000 GHz✔ High sensitivity in intentsity and in polarisation✔ Cheap to fabricate and if possible to do it at home

J.F. Macías-Pérez

Evoluton of the Universe - TGSW2018

9Brief Grenoble K D+readout history
NIKA02000
KID Concept(Caltech-JPL)

2009
10 mm

30 pixels

x2
NIKA1

2010-201336 mm

2014-2017
3000 pixels

80mm

2008
We “join” the KID community
400 pixels
2009
30 pixels  NIKA0 (first ever KID camera)2014 - 2017
- Background-limited ( NEP < 10-17 W/Hz0.5 )- Readout line 2.5 m long !! Litho !!
- Al high-quality, uniform thickness film (10nm)

NIKA2

x 20
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K D speitral response

3000 pixels

x 20
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A bit more than just K D arrays
Cryogenics

KID arrayOptIcs6mm

Data analysis

Electronics

raw data
cleaned data

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Technical developments driven by instruments

2009
Prototype

2016

2017

2018

2019

2020

2021

2025

NIKA 1NIKA 23000 KIDs
From 150-300 GHz

KISS

Spectroscopy prototype
Low frequency > 70 GHz
Spectrometer with 5000 KID
120 – 400 GHz
Low background70 – 1000 GHz

J.F. Macías-Pérez

CONCERTO

R&D for CMB BALLOON/SATELLITE

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N KA2a millimeter iamera
for iluster iosmology

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The “standard” iosmologiial model

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The N KA2 iamera
Duaa band mm KID camera operatng and 150 and 260 GHz
Specifc optcaa system toobtain the widest fead
Diauton cryostat:
180 mK nominaa
temperature
Arrays of 1140 (616) KIDs:
8 (4) independent feedaines
with up to 200 KID each

300 muatpaexing factor

20 boxes (one per feedaine)arranged in 3 crates (one perarray)
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The N KA2 iamera
September 2015 : instaaaaton at IRAM
➢ October 2015 : First aights➢ September 2016 : compaete
instrumentaa setup➢ Apria 2017 : commissioning succesfuaay
fnished ;e performance beter than
expected➢

Science with NIKA2

Frequency

150 GHz260 GHz# KIDs616 (553)

2 x 1140 (960)

FOV diameter

6.5 arcmin

6.5 arcmin

Sensitvity

8±1 mJy/s1/2

33±2 mJy/s1/2

Anguaar res.

17.7 arcsec

11.2 arcsec[N KA iollaboraton, Adam et al, 2018]

Muat-purpose camera open to the astrophysicaa community● Open tme observatons for at aeast one decade ( aaready 4 campaings)● The NIKA2 coaaaboraton has been awarded 1300 hours of GT shared
between 5 Large programs for astrophysics and cosmoaogy:● Gaaactc studies in intensity and poaarisaton● Nearby and distant gaaaxies● Causters of gaaaxies●J.F. Macías-Pérez

Evoluton of the Universe - TGSW201818

Sunyaev-Zeldoviih efeit
Galaxies
3%

Ionized gas
12 %Dark matter85 %No cosmoaogicaa diming
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SZ efeit with N KA2
NIKA2 is a perfect instrument for the tSZ effects in clusters of galaxies
Two frequency bands, negatve & zero tSZ signaa●Wide-fead: size of PLANCK beam

●High resoauton : 17 tmes beter than Paanck

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The N KA iamera
prototype of NIKA2● operated at the IRAM 30 m teaescope from 2009-2014● Duaa band camera with 336 KIDs
● Poaarisaton capabiaites in both bands● First KID based camera to provide scientfc graderesuats●NIKA

150 GHz260 GHz

NIKA2150 GHz

260 GHz# KIDs132

224# KIDs616

2 x 1140

FOVdiameter

1.8 arcmin

2.0 arcmin

FOVdiameter

6.5 arcmin

6.5 arcmin

Sensitvity

14 mJy/s1/2

40 mJy/s1/2

Sensitvity

6 mJy/s1/2

20 mJy/s1/2

Anguaar res.

18 arcsec

12 arcsec

Anguaar res.

17.7 arcsec

11.2 arcsec[Adam & N KA iollaboraton, 2014,
Catalano & N KA iollaboraton 2014]

J.F. Macías-Pérez[N KA2 iollaboraton, 2017]

Evoluton of the Universe - TGSW201821[Adam & N KA iollaboraton, 2014, 2015.2016,2017
Ruppin & N KA iollaboraton 2017, Romero & N KAiollaboraton 2017]

SZ pilot sample for iluster physiis

J.F. Macías-Pérez
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MACS J0717-3745 and kSZ●●High sensitvity NIKA data (12 hours on source)+ High quaaity X-ray, optcaa and IR data

MACS J0717-3745

However, mapping kSZ is very chaaaenging:
Compaex system (5 subcausters
Foreground emission
Degeneracy reaatvistc tSZ and kSZ●Use the two NIKA channea maps
+ temperature map from X-rays[Adam & N KA iollaboraton, 2016]

J.F. Macías-Pérez

Evoluton of the Universe - TGSW201823

MACS J0717-3745 and kSZ●●High sensitvity NIKA data (12 hours on source)+ High quaaity X-ray, optcaa and IR data

MACS J0717-3745

However, mapping kSZ is very chaaaenging:
Compaex system (5 subcausters
Foreground emission
Degeneracy reaatvistc tSZ and kSZ●Use the two NIKA channea maps
+ temperature map from X-rays

First direct mapping of kSZ emission[Adam & N KA iollaboraton, 2016]

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tSZ iluster iosmology
Cataaogue of 1653 tSZ detected causters
Redshif : optcaa foaaow-up● Hydrostatc mass by combining tSZ fux andX-ray data : Y500 – MYX (MHS)● Charaterisaton of the hydrostatc-totaa mass
bias via simuaatons: MHS = (1-b) Mtot●
●Number of clusters as function of redshift andmass is very sensitive to comology[Planik 2015 results XX , XX V, XXV ][Bolliet, Comis, Komatsu & JFMP 2018]

2-σ tension between CMB and tSZ (causter observabae) derived cosmoaogicaa parameters
Need to understand causter physics: hydrostatc bias, conditon for hydrostatc equiaibrium,
shocks in the ICM, non thermaa pressure, ...
J.F. Macías-Pérez

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N KA2 SZ Large program
One of the 5 NIKA2 LP (1300h in totaa)➢ 300 hours of tSZ observaton➢ 50 high redshif clusters 0.5 < z < 1.0➢ tSZ seaected causters from Paanck andACT cataaogues[Comis, 2016]

Anciaaary data
➢ X-ray foaaow-up with XMM➢ Optcaa data using GranTeCan➢ MUSIC hydrodynamic simuaatons
Main goaas➢ In-depth study of ICM➢ Thermodynamic propertes: pressure,density, temperature and entropy profaes➢ Mass – tSZ fux reaatonship

Redshif evoauton of:➢ Thermodynamic quanttes profaes➢ Scaaing aaws and hydrostatc bias

Variaton of causter propertes with:➢ Dynamicaa state (mergers)➢ Morphoaogy (eaaiptcity)[JFMP & NIKA2 collaboration 2017, arXiv:171107088 ]J.F. Macías-Pérez

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First N KA2 SZ iluster
PSZ2 G144[Ruppin et al, AA, 2018]

Paanck tSZ detected causter at redshif, z = 0.58, high mass M500 = 7.8 x 1014 Mʘ● 11h observatons with NIKA2 in poor weather conditons (atmospheric opacity 0.3@225 GHz)
● Aaready observed: SZ – MUSTANG & Boaocam, X-rays - XMM●

Detaiaed characterizaton of the causter pressure profae – overpressure foundHints of dependence of the hydrostatc mass bias with causter physics
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PRELIMINARYObserved N KA2 LP ilusters

Two more causters aaready observed
Very promising resuats, detaiaed anaaysis on going
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Coming soon
KISSCONCERTO

Measure physical properties of nearby cluster
via the SZ effectIntensity mapping of CII lines at high redshift tomeasure SFR + detection of clusters with SZ

Low resolution MP spectrometer from70 to 260 GHz

Low resolution MP spectrometer from
120 to 350 GHz

600 KIDs @ QUIJOTE telescope in Teide
Observatory

5000 KIDs @ APEX telescope in Atacama
Installation expected in 2021

Installation expected in November 2018
J.F. Macías-Pérez

Evoluton of the Universe - TGSW201829

Summary and ionilusions➢ Current science drivers in mm astronomy and cosmology needs high sensitivity andwide-field multi-color observations with large arrays of detectors➢ KIDs have achieved sufficient technical maturity to be a credible option to build thoselarge arrays (tens of thousands pixels) of photon noise limited detectors➢ NIKA first and now NIKA2, have demonstrated that KID based mm cameras canachieve state-of-art performance for astrophysics and cosmology➢ Cluster physics and cosmology via the SZ effect are a target of choice for KIDcameras➢ We are developping a new generation of KID based mm spectrometers that should
be on the sky very soon
➢ KID based mm instruments are emerging: AMKID, Olympo, DESHIMA, MUSCA,
GroundBird, KISS, Concerto, MKIDs for Nobeyama (Nitta-san talk)

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