ALMA in a nutshell
Site
ALMA is constructed on the
Chajnantor plateau, at 5000 m altitude, near San Pedro de Atacama, in
northern Chile. The Array Operations
Site (AOS) is the location of the ALMA array and of the
correlator
building on the Plateau. All operations control and antenna maintenance
is performed from the Operations
Support Facility
(OSF), at ~2800 m altitude. The antennas are currently being
assembled at the OSF, in the contractors' areas. The antennas will be
transported by Otto and Lotte,
at the OSF (integration, tests,
maintenance), between the OSF and the AOS (30 km road), and at the AOS
(change of configuration).
ArrayWebcam at the OSF: camera1, camera2.
Receivers All ALMA and ACA
antennas will be equipped 6 receiver bands. At a later stage of the
ALMA developments, up to 10 bands may be installed in the cryostats.
Band 3, 4, 6, 7, 8, 9 are in
the
baseline project. Development of band 5 (for 6 antennas only) and
band 10 are also taking place. Bands 1 and 2 are not being built. The
receiver temperatures are the specs (max. Trec over 80% of the RF
band); see the ESO
front-end pages for more details.
CorrelatorThe table below gives the
correspondance between the Plateau de Bure and the ALMA bands, in the
atmospheric windows that can be observed with the PdBI.
The exact frequency coverage may be slightly different at the edges of the bands. Note that, PdBI band 4 (to be installed in winter 2008/09) are copies of the ALMA band 7 mixers. The ALMA correlator is
installed in a building at the high-altitude site (AOS). It is composed
of
four quadrants, each of which can process data coming from 16
different antennas (the complete correlator can thus process 64
antennas). The ACA array has its own correlator.
The ALMA
memo 556
gives more detailed information on the (many) correlator modes
available. Only a subset of these modes are planned to be available
during the Early Science.
Sensitivity The ESO web site
provides an on-line
ALMA sensitivity estimator.
Caution: point-source sensitivity
only depends on the collecting area.
Brightness sensitivity - which is the number to check for extended
sources - depends on the angular resolution. Doubling the angular
resolution (e.g. from 0.5 to 0.25 arcsec) implies a brightness
sensitivity reduced by a factor four (e.g. from 0.1 to 0.4 K
rms). This is because the angular resolution is improved while
the collecting area remains the same. Please consider this effect when
planning observations: the
brightness
sensitivity
depends on the angular resolution.
ALMA data reduction The ALMA data
reduction package will be CASA, developed by NRAO. The beta
version has
been released in October 2007, a patch 1 is available since April 2008.
The native data format for ALMA will be the ALMA Science Data Model (ASDM). The current version is 5.0. There is no
guaranteed time
on ALMA. For the time being, there are no plans to have specific large
or key programs. There should be one Time Allocation Committee (TAC)
per partner, i.e. one for the European community. ESO has ~35% of the
ALMA observing time (~35% for the North American
partners, ~20% for the Eastern-Asia partners, and 10% for Chile).
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