During the last 4 years, the first steps have been taken towards investigating the Universe using direct submm-wave surveys. The technologies of the class of detectors that made these initial surveys possible are still developing rapidly. Many instrumentation projects are underway, which will allow us to increase the sizes of samples of distant submm galaxies, and to study known examples in more detail; some of their key features are outlined in Tables 1-3.
Name | NEFD | FOV | Confusion | |
(µm) | (mJy / (Hz)1/2) | (arcmin2) | (mJy) | |
SCUBA | 850 | 80 | 1.7 | 0.12 (9 × 10-4) |
450 | 160 | 1.7 | 0.053 (3 × 10-3) | |
MAMBO1,2 | 1250 | 95 | 1.0 | 0.05 (7× 10-5) |
SCUBA-II | 850 | 28 | 64 | 0.12 (9 × 10-4) |
450 | 90 | 64 | 0.053 (3 × 10-3) | |
HAWC-SOFIA | 200 | 408 | 9.0 | 1.2 (0.30) |
BOLOCAM-CSO | 1100 | 42 | 44 | 0.32 (2 × 10-3) |
BOLOCAM-LMT | 1100 | 2.8 | 2.5 | 6 × 10-3 (4 × 10-5) |
BLAST | 750 | 115 | 10 | 3.9 (0.25) |
450 | 130 | 10 | 6.8 (0.7) | |
300 | 150 | 10 | 7.8 (1.1) | |
SMA | 850 | 170 | 0.2 | < 10-7 ( < 10-6) |
450 | 1700 | 0.05 | < 10-8 ( < 10-4) | |
ALMA | 870 | 1.9 | 0.050 | < 10-7 ( < 10-6) |
450 | 11 | 0.013 | < 10-8 ( < 10-4) | |
Extended VLA | 20.5 cm | 0.40 | 700 | ~ 0 (~ 0) |
SKA | 20.5 cm | ~ 10-2 | TBD | ~ 0 (~ 0) |
An estimate of the speed of a survey down
to a chosen depth can be obtained by multiplying the FOV by the
the square of the NEFD value. The approximate extragalactic confusion
noise values are the flux density at which there is one brighter
source per beam
(Blain et al., 1998;
Fig. 13).
This corresponds approximately to the width of peak in the non-Gaussian
confusion noise distribution (see
Fig. 12).
The expected ISM confusion noise
(in brackets) is calculated for a 100-µm surface
brightness B0=1 MJy sr-1
(Helou and Beichman,
1990),
and scales as B01.5. Other instruments
under development, which have not published detailed performance
estimates include the 350-µm SHARC-II camera for the CSO.
The FOV and NEFD values
are chosen to provide the correct results for making a fully-sampled
image of the sky, not measuring the flux from a single galaxy. Updated
from Table 1 in
Blain (1999b).
Relevant references are listed in
Table 3. TBD: to be decided.
|
Name | NEFD | FOV | Confusion | |
(µm) | (mJy / [(Hz)1/2]) | (arcmin2) | (mJy) | |
Herschel-SPIRE | 500 | 114 | 40 | 2.9 (0.16) |
350 | 90 | 40 | 2.6 (0.12) | |
250 | 84 | 40 | 1.6 (0.24) | |
Herschel-PACS | 170 | 24 | 6.1 | 0.80 (0.16) |
90 | 24 | 6.1 | 0.03 (0.01) | |
SIRTF-MIPS | 160 | 18 | 2.5 | 6.6 (3.1) |
70 | 4.5 | 25 | 0.28 (0.07) | |
24 | 1.8 | 25 | 6 × 10-4 (2 × 10-4) | |
SIRTF-IRAC | 8.0 | 0.15 | 26 | 8 × 10-2 (~ 10-6) |
Planck Surveyor | 350 | 26 | All-sky | 50 (70) |
550 | 19 | All-sky | 22 (12) | |
850 | 16 | All-sky | 8.1 (1.6) | |
SPECS testbed | 250 | 0.17 | 4 | ~ 10-5 (~ 10-3) |
SPIRIT | ||||
Note that the values listed for Planck Surveyor apply to an all-sky survey. Another instrument under development, which has not published detailed performance estimates is the 50-200-µm sky survey from the Japanese ASTRO-F/IRIS satellite sky survey. |
Name | Information |
SCUBA | Holland et al. (1999) |
MAMBO | Kreysa et al. (1998) |
SCUBA-II | www.jach.hawaii.edu/JACpublic/JCMT/Continuum_ observing/SCUBA-2/home.html |
SOFIA | Davidson et al. (1999); sofia.arc.nasa.gov |
BOLOCAM | Glenn et al. (1998); www-lmt.phast.umass.edu/ins/continuum/bolocam.html |
BLAST | Devlin (2001); http://chile1.physics.upenn.edu/blastpublic/ |
SMA | Ho (2000); http://sma-www.harvard.edu/ |
ALMA | Wootten (2001); www.alma.nrao.edu |
SKA | www.astron.nl/p/skaframe.htm |
Herschel-SPIRE | www.ssd.rl.ac.uk/spire |
Herschel-PACS | pacs.ster.kuleuven.ac.be |
SIRTF-MIPS & IRAC | sirtf.caltech.edu |
Planck Surveyor | astro.estec.esa.nl/Planck |
SPECS / SPIRIT | Mather et al. (1998); space.gsfc.nasa.gov/astro/specs |