Strumentazione sub-mm/mm
pre-ALMA
APEX
SCUBA & SCUBA-2
IRAM
SMA
CSO
OVRO, BIMA  CARMA
NMA
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
APEX:
Atacama Pathfinder EXperiment
Location:
Llano de Chajnantor
(Chile, 5000 m)
Antenna modified
copy of US ALMA
prototype
MPIfR=50%
Onsala Sp. Obs=23%
ESO=27%
12 m diameter
Bologna, 6 giugno 2005
PI: Karl Menten
PS: Peter Schilke
300-1500 μm=
230-1200 GHz
Riunione ALMA extragalattica
Instruments
Heterodyne receivers:
Bolometers arrays:
1.
1.
2.
3.
4.
5.
230 GHz (1.3 mm)+340 GHz (0.9 mm)
receivers (from SEST)
460 GHz (650 micron) 16-pixel
CHAMP array (from CSO)
810 GHz (370 micron) receiver
(from JCMT)
Upgrade of CHAMP/dual receiver:
650 and 810 GHz (next)
Experimental receivers above 1 THz
(next)
Bologna, 6 giugno 2005
LABOCA (LArge BOlometer
CAmera):
870 micron (345 GHz)
295 channels
beam size=18 arcsec
FOV=11.4 arcmin
scanning and jiggling required
for fully sampled maps
2. 350 micron (850 GHz) array:
37-channel bolometer (next)
3. 2 mm (150 GHz) array:
3oo channel bol. for SZ (next)
Riunione ALMA extragalattica
Summary of the first generation
facility instruments
Receiver
Frequency
(GHz/mm)
APEX-1a
210-275
Q1 2004
APEX-1b
210-275
Q3 2004
APEX-2b
275-370
Q3 2004
APEX-3b
375-500
Q3 2004
APEX-T2
1240-1400
TBD
LABOCA
0.8
300
Q2 2004
350 μm
0.37
37
Q2 2004
Bologna, 6 giugno 2005
Elements
Riunione ALMA extragalattica
Notes
Observing Time
Consortium:
The Astronomical Institute at the University of Bochum (AIRUB),
the European Southern Observatory (ESO) and
the Onsala Space Observatory (OSO) and the
Max-Planck-Institut für Radioastronomie (MPIfR)
 10% observing time for Chilean astronomers
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
SCUBA: the Sub-mm Common-User
Bolometer Array
15-m diameter telescope (Mauna Kea, Hawaii, 4092 m)
INSTRUMENTS
Sub-mm bolometers:
 Simultaneous observations at 850 μm (353 GHz, 37 bolometers) and
450 μm (670 GHz, 91 bolometers)
 Diameter f.o.v.=2.3 arcmin, beam=15-7 arcsec; cooled at 100 mK
 UK, Canada, and The Netherlands collaboration, ~5-10% observing
time to international programs.
Spectral line receivers:
 3 receivers: A3: 230 GHz – B3: 345 GHz – W: 460 and 690 GHz
Heterodyne polarimeter:
 all frequencies. Next: ROVER (2-3 mm window)
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
The SCUBA-2 project
SCUBA-2:
 Transition Edge Sensor arrays: two dc-coupled, monolithic, filled
arrays with a total of 10240 bolometers
 Two focal-plane units  each unit has 4 sub-arrays with 40x32
elements
 Observing bands: 850 μm and 450 μm
 F.O.V.=50 arcmin sq.=12xSCUBA
 Sensitivity: a factor ~2-3 better than SCUBA
 1000 times faster than SCUBA to reach the same S/N
for maps (fully sampled image in just one pointing)
 Cooled at 120 mK  limited by the sky background photon noise
Delivered to the JCMT in Feb. 2006 (2 sub-arrays) and completed in
Nov. 2006 (all sub-arrays)
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
SCUBA-2 focal plane
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
IRAM: Institut de Radio
Astronomie Millimetrique
French-German-Spanish collaboration
Two observatories
1. 30-m single-dish telescope on Pico Veleta (2850 m, Spain)
2. 6-antenna (15 m each) interferometer on the Plateau de Bure
(2550 m, France)
1. 30-m Telescope
Bolometer systems:
 MAMBO I: 1.2mm, beam=11 arcsec, 37 pixels
 MAMBO II: 1.2mm, beam=11 arcsec, 117 pixels
plus receivers in the range 80-272 GHz
2. PdBI


Receiver at 1.3 mm (205-250 GHz), resolution~0.5 arcsec, f.o.v.=20”
Receiver at 3 mm (81-115 GHz)
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
SMA: Sub-Millimeter Array
Smithsonian Astrophysical Observatory + Academia Sinica of
Astronomy and Astrophysics collaboration
8 x 6-m antenna interferometer on Mauna Kea (~4000m, Hawaii),
baseline as long as 500 m, ≈180-900 GHz band
2 simultaneous receivers/element
Receiver bands: 230, 345, 460, 690, and 850 GHz
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
CSO: Caltech Submillimeter
Observatory
10.4-m diameter telescope (Mauna Kea, Hawaii)
INSTRUMENTS
Bolometer systems:
 BOLOCAM: 115 working pixels, f.o.v.=8 arcmin (circular),
beam size=30 arcsec (1.1 mm) and 60 arcsec (2.1 mm)
 SHARC II: 12x32 array of bolometers at 350-450 μm
f.o.v.=1.0x2.5 arcmin sq., beam~8.5 arcsec (350 μm)
COMPLEMENTARY TO SCUBA
Heterodyne receivers:
230, 345,490, and 665 GHz
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
OVRO: Owens Valley Radio
Observatory
Caltech / National Science Foundation
6 x 10.4-m antenna interferometer (California, ~1200 m)
Beam-width=65” at 100 GHz
Receiver bands: 86-116 GHz (3 mm) and 210-270 GHz (1 mm)
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
BIMA: Berkeley Illinois Maryland
Association
10 x 6.1-m antenna interferometer
OVRO and BIMA have now ceased operations
 CARMA
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
CARMA: Combined Array for
Research in Millimeter-wave
Astronomy
CARMA=OVRO+BIMA on a site in Eastern California (~3000 m a.s.l.)
NSF + Universities
SPECIFICATIONS
ARRAY: 15 antennas (6 x 10.4 m + 9 x 6.1 m), 772 m2 , 0.5 arcsec res.
at 230 GHz
RECEIVERS: 115, 230, and 345 GHz
Fully operational: end of 2005?
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
NMA: Nobeyama Millimeter Array
ARRAY: 6 x 10m antennas
BANDS: 3 mm (85-116 GHz), 2 mm (126-152 GHz), and 1 mm
(213-237 GHz)
10 m sub-mm
resolution down to 1 arcsec
NMA plus the 45 m single-dish telescope  RAINBOW
(f.o.v.=20 arcsec at 3 mm)
Bologna, 6 giugno 2005
Riunione ALMA extragalattica
ASTE
if you have questions…
I’m not sure I can answer …
Bologna, 6 giugno 2005
Riunione ALMA extragalattica