Bolometer Camera Plansat MPIfR, Bonn

E. Kreysa, Kaustuv moni Basu, H.-P. Gemünd, G. Siringo, A. Kovacs, F. Schuller, A. Weiß, K. Menten

Max-Planck-Institute for Radioastronomy, Bonn, Germany

S. Anders, R. Boucher, L. Fritzsch, T. May, M. Starkloff,V. Zakosarenko, H.-G. Meyer

Institute for Photonic Technology, Jena, Germany

SABOCAAPEX facility instrument with 37

bolometers at = 350µm

SABOCA layout

TES detectorchip

Multiplexer chip(10x)

37 TES detectors

4 multiplexers

λ = 350 μm

200 μm option

Scale2 mm

SABOCA focal plane

16 bolometer arrays with 6 different thermal and absorber designs are on each SABOCA wafer.

For test purposes the wafer has also 4 test chips with with 6 single bolometers of each variety..single bolometer

TESheater

LABOCA

E.KreysaMPIfR

APEX-SZ

N.HalversonUCB

AC AC

SABOCA in Cass. cabin

Atmospheric transmission at the APEX sitepwv during SABOCA run in Oct 2008 often < 0.3 mm !

1mm 350μm 200μm

Chajnantor bestChajnantor best

Chajnantor avg

“good” site

Extinction plot with Uranus

•Stable conditions•pwv 0.2 – 0.3•Low sky noise•Opacity consistent with that derived from taumeter

Beamsize: 7.5“, close to nominalSidelobes at 5% levelSensitivity: 170 – 250 mJysequivalent to 750 mJy on sky @ 0.5 mm water

SABOCAperformance

Quick mapof Orion

• 1.5 h int.time• contours at 0.5 Jy 3.0 Jy 10 Jy 30 Jy 100 Jy 300 Jy

Work in progress at APEX

• Finish commissioning of SABOCA

2008

• Polarization option for LABOCA

Jan/Feb 2009

• LABOCA-2, 300 TES, MUX readout

pulse tube

2009

Options for future large arrays at APEX

• 350 m version of LABOCA ?

1800 bolometers fit into field of LABOCA (0.2°) !

LABOCA optical design is good for 350 m ! • Full field version version of LABOCA ?

>1200 bolometers in APEXSZ field (0.4°) !

New optical design required !• 200 m camera ?

Configuration Field-Ø [º]

F/D A[mm² sterad]

APEX

12 m

ALMA secondary

APEX-SZ

LABOCA

0.448

0.4

0.2

8.0

8.0 (12)

8.0

5430

4329 (1923)

1028

MRT

30 m

Nasmyth 0.084 9.73 1193

JCMT

15 m

Cassegrain

SCUBA (Nasmyth)

SCUBA-2

0.092

0.019

50 (‘)2

12

16

1421

62

748

CCAT

25 m

Cassegrain (bent)

Nasmyth

0.1667

(0.333)

3262

(13049)

Resolution & SensitivityResolution & Sensitivity

Resolution345 GHz ~ 18”150 GHz ~ 1'

Resolution150 GHz ~ 18”

More collecting area will give higherangular resolution and moreSensitivity for compact structures!

Excellent sky stability at 150 GHz will allow deep integrations

Large field of view of a ~1000 elementarray will enable imaging of extended signals (like SZ effect)

Science Highlights: High-resolution SZE High-resolution SZE ImagingImaging

• The Sunyaev-Zel'dovich Effect (SZE) provides integrated pressure maps for the hot gas in galaxy clusters

• Joint SZE and X-ray analysis can reveal the gas density and temperature structure — important for cluster physics & cosmology

What high-resolution SZ imaging can do: Galaxy cluster Abell 2163

With 15” resolution we can resolve the entropy structure With 15” resolution we can resolve the entropy structure near the cluster center! This is predicted to be a major indicator near the cluster center! This is predicted to be a major indicator of the cluster's dynamical state – and hence its mass.of the cluster's dynamical state – and hence its mass.

APEX-SZ @150 GHz LABOCA @ 345 GHz Temperature profiles

Science Highlights: High-resolution SZE High-resolution SZE ImagingImaging

resolving bubbles and filaments in clusters (pressure equilibrium?)

resolving the bow shocks and sub-

structures in cluster mergers

also, high sensitivity and resolution at 150 GHz is ideal for detecting clusters from high redshifts with SZE (sensitivity to SZE power is maximum near 100 GHz, and no confusion from IR-bright sources)

Scope for X-ray observation is saturating – no major new instruments for the next 15 years!

High-resolution SZE imaging is currently the most promising way High-resolution SZE imaging is currently the most promising way to unravel gas physics in galaxy clusters!to unravel gas physics in galaxy clusters!

Perseus cluster seen by Chandra

Gas+DM simulation of cluster merger

Science Highlights: Cold Dust Near Cold Dust Near and Farand Far

Measurement at 2 mm will help tomodel the SEDs of cold dust (< 15K)accurately. Sensitivity and high resolutionis the key for separating it from the hotdust component (which dominates the total emission)!

At high redshifts (z~3) the cold dustemission peaks near 1 mm. With a newhighly sensitive bolometer array at 2 mm,we can do the same modeling of dust and star formation activity at high-z, that so farhas been done only for the local universe!

NGC 1068: Papadopoulos & Seaquist (1999)

SLUGS sample: Dunne & Eales (2001)