Bolometer Camera Plans

1
Bolometer Camera Plans at 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

2
SABOCAAPEX facility instrument with 37
bolometers at ? 350µm
3
SABOCA layout
Multiplexer chip (10x)
TES detector chip
37 TES detectors 4 multiplexers ? 350 µm 200
µm option
Scale 2 mm
4
SABOCA focal plane
heater
TES
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
5
APEX-SZ
LABOCA

AC
AC

E.Kreysa MPIfR
N.Halverson UCB

6
SABOCA in Cass. cabin
7
Atmospheric transmission at the APEX site pwv
during SABOCA run in Oct 2008 often lt 0.3 mm !
1mm
350µm
200µm
Chajnantor best
Chajnantor avg
good site
8
Extinction plot with Uranus

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

9
Beamsize 7.5, close to nominal Sidelobes at 5
level Sensitivity 170 250 mJy?s equivalent to
750 mJy on sky
_at_ 0.5 mm water
SABOCA performance
10
Quick map of Orion

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

11
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

12
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 ?
• gt1200 bolometers in APEXSZ field (0.4) !
• New optical design required !
• 200 ?m camera ?

13
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)
14
Resolution Sensitivity
Resolution 345 GHz 18 150 GHz 1'
More collecting area will give higher angular
resolution and more Sensitivity for compact
structures! Excellent sky stability at 150 GHz
will allow deep integrations Large field of
view of a 1000 element array will enable imaging
of extended signals (like SZ effect)
Resolution 150 GHz 18
15
Science Highlights High-resolution SZE Imaging

• 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
APEX-SZ _at_150 GHz LABOCA _at_ 345 GHz
Temperature
profiles
With 15 resolution we can resolve the entropy
structure near the cluster center! This is
predicted to be a major indicator of the
cluster's dynamical state and hence its mass.
16
Science Highlights High-resolution SZE Imaging
GasDM simulation of cluster merger
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)
Perseus cluster seen by Chandra
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 to unravel gas physics in
galaxy clusters!
17
Science Highlights Cold Dust Near and Far
Measurement at 2 mm will help to model the SEDs
of cold dust (lt 15K) accurately. Sensitivity and
high resolution is the key for separating it from
the hot dust component (which dominates the
total emission)!
NGC 1068 Papadopoulos Seaquist (1999)
At high redshifts (z3) the cold dust emission
peaks near 1 mm. With a new highly sensitive
bolometer array at 2 mm, we can do the same
modeling of dust and star formation activity at
high-z, that so far has been done only for the
local universe!
SLUGS sample Dunne Eales (2001)