APEX-Sunyaev-Zel’dovich Observations - Astronomy · APEX-Sunyaev-Zel’dovich Observations - R...

APEX-Sunyaev-Zel’dovich Observations - R Kneissl - SnowCluster Utah - March 29 2010

APEX-Sunyaev-Zel’dovich Observations

Rüdiger Kneissl (ALMA / ESO)

• APEX: SZ-Camera, LABOCA

• Cluster Results with APEX

• SZ prospects with ALMA


The APEX-SZ CollaborationU.C. Berkeley / LBNLU.C. Berkeley / LBNLBrad BensonBrad BensonHsiao-Mei ChoHsiao-Mei ChoJohn ClarkeJohn ClarkeDaniel FerruscaDaniel FerruscaBill HolzapfelBill HolzapfelBrad JohnsonBrad JohnsonZigmund KermishZigmund KermishAdrian LeeAdrian LeeMartin LuekerMartin LuekerJared MehlJared MehlTom PlaggeTom PlaggeChristian ReichardtChristian ReichardtPaul RichardsPaul RichardsDan SchwanDan SchwanHelmuth SpielerHelmuth SpielerBen WestbrookBen WestbrookMartin WhiteMartin WhiteOliver ZahnOliver Zahn

C.U. BoulderC.U. BoulderAmy BenderAmy Bender

Nils HalversonNils HalversonMcGill UniversityMcGill University

Matt DobbsMatt DobbsJames KennedyJames KennedyTrevor LantingTrevor Lanting

Onsala SpaceOnsala SpaceObservatoryObservatory

Cathy HorellouCathy HorellouDaniel JohanssonDaniel Johansson

CardiffPeter Ade

Carole TuckerALMA/ESO(Santiago)

Rüdiger Kneissl

MPIfRKaustuv BasuRolf GuestenErnst KreysaKarl MentenDirk MudersMartin Nord

Bonn UniversityFrank BertoldiMatthias Klein

Felipe NavarretteFlorian Pacaud

Reinhold SchaafMartin Sommer

MPEHans BöhringerGayoung Chon

Rene FassbenderRobert Suhada


The Sunyaev-Zeldovich Effect

Single ClustersSingle Clusters–– Measures pressure along line of sightMeasures pressure along line of sight–– Peculiar velocities at high zPeculiar velocities at high z–– Distances, HDistances, Hoo, H(z), H(z)–– Cluster gas mass fractions, gas densityCluster gas mass fractions, gas density

and thermal and thermal structure, etc.structure, etc.Cluster SurveysCluster Surveys

–– integrated pressure = total thermalintegrated pressure = total thermalenergyenergy, SZ redshift independence, SZ redshift independence

–– Measure growth of structureMeasure growth of structure–– Cluster abundance and evolution areCluster abundance and evolution are

critically dependent on cosmology (darkcritically dependent on cosmology (darkenergy)energy)

!

"TSZ

TCMB

# neTe$ dl


Galaxy Cluster Science

Galaxy Clusters

ClusterCosmology

Cluster Physics

SZ Mass Calibration

Ωm, σ8, w(z),..Baryon, Dark Matter DensityTemperature Distribution

Amy Bender talk


APEX-SZ overview

•• APEX telescope: 12 meter ALMA prototype antenna APEX telescope: 12 meter ALMA prototype antenna•• 24 arc-min field of view24 arc-min field of view•• 280 element TES280 element TES Bolometer Array at 150 Bolometer Array at 150 GHzGHz•• 11 arc-min arc-min resolutionresolution•• 2D2D maps using circular scans up to 24 arc min diam. maps using circular scans up to 24 arc min diam.

•• Probe to outskirts of low-Probe to outskirts of low-zz clustersclusters•• Deep integrations with small footprints Deep integrations with small footprints

•• at ALMA location at ALMA location in Chile (Chajnantor in Atacama)in Chile (Chajnantor in Atacama)•• high site, dry conditions high site, dry conditions•• multi-wavelength observationsmulti-wavelength observations


The APEX-SZ Experiment

•• PIPI instrument on APEX instrument on APEX

•• First light: December 2005First light: December 2005•• 2007-09 2007-09 –– 2-4 weeks/year 2-4 weeks/year observobserv..

•• 280 TES Bolometer channels @280 TES Bolometer channels @150 GHz150 GHz

•• Demonstrates new technologiesDemonstrates new technologies

•• TES TES bolometersbolometers

•• Frequency domain multiplexedFrequency domain multiplexedreadoutreadout

•• Pulse-tube cooler to eliminatePulse-tube cooler to eliminateliquid cryogensliquid cryogens

•• NET (870 NET (870 →→ 500) 500) µµKKCMB CMB ss1/21/2

through better optical couplingthrough better optical coupling

~1m


LABOCA on APEX

•• FacilityFacility instrument instrument since Maysince May2007 provided by2007 provided by MPIfRMPIfR

•• 295 semiconducting composite 295 semiconducting compositebolometerbolometer @ @ 345345 GHzGHz

•• higher resolution SZ: 18.6 arc- higher resolution SZ: 18.6 arc-sec beam with 11.4 arc-min FoVsec beam with 11.4 arc-min FoV

•• sensitivity per channel 75 mJy sensitivity per channel 75 mJyss1/21/2

•• observing modes: OTF, rasterobserving modes: OTF, rasterspiral, and now also fastspiral, and now also fast‘‘photometryphotometry’’ mode mode

•• polarimeter planned polarimeter planned


APEX-SZ Scan Strategy

•• APEX => single clusterAPEX => single clusterscansscans

•• Circular drift scan patternCircular drift scan pattern–– 20 circles, 5 second20 circles, 5 second

periodperiod•• 10-20 10-20 arcmin/s arcmin/s scanscan

speedspeed–– No No deadtimedeadtime–– Constant ground Constant ground pickuppickup


Data Filtering and Transfer Function

•• 0.2 Hz high pass 0.2 Hz high pass filterfilter

–– removesremoves low-frequency readout noise. low-frequency readout noise.

•• Subtract cosecant(elev) + polynomial(t) (1 d.o.f. perSubtract cosecant(elev) + polynomial(t) (1 d.o.f. percircle)circle)

–– removesremoves air mass signal and drift air mass signal and drift

•• Remove spatial polynomial at each time step (Sayers etRemove spatial polynomial at each time step (Sayers etalal.).)

–– Largely array average + Largely array average + tilttilt

•• Data filtering is done to cluster simulated models (e.g.Data filtering is done to cluster simulated models (e.g.Beta)Beta)

–– Accounts for Accounts for ““transfer functiontransfer function””

•• Maps and radial profiles => transfer function corrected orMaps and radial profiles => transfer function corrected orsource source ““flaggedflagged””


The APEX-SZ Bullet cluster (1E 0657-56) imageHalverson et al. 2009

X-ray image with APEX-SZ (white contour and weak-lensing (green contours)

23 sigma detection

Jackknife noise map

no evidence for significant 150 GHz emission from 13.5 mJy @ 270 GHz point source reported by Aztec.

Mass-weighted SZ temperature = 10.8± 0.9 KeV


Bullet cluster model fitBeta model fit residual map

•• Gas profile fit well by an isothermal elliptical beta model (adequate for sensitivityGas profile fit well by an isothermal elliptical beta model (adequate for sensitivityand resolution of these maps and resolution of these maps –– despite the complex nature of this system) despite the complex nature of this system)

•• Model parameters and gas-mass fraction consistent with those from X-ray dataModel parameters and gas-mass fraction consistent with those from X-ray data

Zhang et al (2006): fgas= 0.161± 0.018 (1.42 Mpc), Bradac et al (2006): fgas= 0.14±0.03 (4.9’x3.2’)


APEX-SZ and LABOCA imaging of A2163Nord et al. 2009APEX-SZ

LABOCA (345 GHz)

+ APEX-SZ + LABOCA


De-projected density and temperature profiles

Consistent with XMM (Markevitch, Vikhlinin 2001)

r500

Shaded region: xray (Squires et al.,1997)

WMAP5Isothermal

De-projectedprofile

No parametric model such as Beta or Nagai, but inverse Abel transformation assuming spherical symmetry

A2163: A merging cluster


A2204: A relaxed cluster

APEX-SZ

r500 r200

SZ image with X-ray contours

Temperature profile

SZ profile

Basu et al. 2010

arXiv:0911.3905


Entropie

Slope of the entropy profile near the cluster center determines the extent of non-gravitational heating

Abell 2163

Chandra 80 ks

Abell 2204

A2204Entropy is a fundamental property of the ICM, describing its history of heating and cooling


APEX 150 GHz Power SpectrumReichardt et al 2009

• 0.8 sq degrees at 150 GHz,12 µKRMS per 1’ pixel

• Total Anisotropy < 105 µK2 at 95%.• σ8 < 1.18 at 95%

– Accounting for non-Gaussianstatistics, Gaussian: σ8 < 0.94

• ClPS ≈ 1 x 10-5 µK2

– Agrees with Negrello prediction• With BLAST 600 GHz data →spectral

index α=2.64 +0.4-0.2.

– Agrees with MAMBO/SCUBAindex, 2.65 Greve et al. (2004)

– Knox et al. 2004.• Dusty galaxies account for most

power in APEX-SZ maps.


ALMAAtacama Large Millimeter/Submillimeter Array•• Three antennas at 5000m and six acceptedThree antennas at 5000m and six accepted•• Phase closure was the start of commissioning Jan 2010Phase closure was the start of commissioning Jan 2010•• Current bands are 3, 6, 7 & 9Current bands are 3, 6, 7 & 9

•• Start of early science with 16 antennas in 2011Start of early science with 16 antennas in 2011•• Completion of 66 antenna array in 2013Completion of 66 antenna array in 2013•• A world-wide Collaboration: +ChileA world-wide Collaboration: +Chile


ALMA technical specifications


The population of sub-mm sources

Knudsen et al. 2006ALMA simulation: Cluster SZ (red)

and lensed submm sources (blue)5σ - 2h ALMA


ALMA (Compact) Configurations


Simulated observation of a high-z cluster

ALMA @ 90 GHZ

ALMA ACA only

ALMA sensitivity allows to get good images

of high-z clusters in hours to day observations,

also can probe non-thermal effects in cavities

Hydro-simulation of a merging cluster

at z=1.5, each component with M =

1 x 1014 M. (courtesy of G. Tormen)


Non-thermal electrons

e.g Pfrommer et al 2005, Colafrancesco 2005, Scaife & Grainge 2010


The case for ALMA Band 1 (31-45 GHz)

• ‘ALMA’s excellent imaging quality should allow the mm-wave Sunyaev-Zeldovich (SZ) effect to be mapped in exquisite detail.’

• ‘Band 1 enables SZ imaging and together with band 2 enables detection ofwell-understood CO emission lines from the end of reionization.’

• Estimated $7-10 M, technology straightforward, observing in higher PWV


Summary•• APEX-SZ is a 280 element 150 GHz bolometer arrayAPEX-SZ is a 280 element 150 GHz bolometer array

operating on the operating on the 12m12m APEX telescope APEX telescope–– Technology pathfinder role: TES bolometer array,Technology pathfinder role: TES bolometer array,

multiplexed readout, no expendable cryogens.multiplexed readout, no expendable cryogens.•• New SZ observations of the New SZ observations of the Bullet, A2163 and A2204Bullet, A2163 and A2204

–– General consistency with expectations from x-ray.General consistency with expectations from x-ray.•• FutureFuture APEX-SZ WorkAPEX-SZ Work

–– Scaling relations -> cosmology calibrationScaling relations -> cosmology calibration–– Detailed input to cluster Detailed input to cluster modelingmodeling

•• ALMA will offer unprecedented sensitivity and frequencyALMA will offer unprecedented sensitivity and frequencyrange below 20 arc-sec scales for SZ imagingrange below 20 arc-sec scales for SZ imaging–– high-z clusters, pressure sub-structurehigh-z clusters, pressure sub-structure–– sub-mm source environment, lensingsub-mm source environment, lensing

APEX-Sunyaev-Zel’dovich Observations - Astronomy · APEX-Sunyaev-Zel’dovich Observations - R...

Documents

Transcript of APEX-Sunyaev-Zel’dovich Observations - Astronomy · APEX-Sunyaev-Zel’dovich Observations - R...