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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)