Very Small Array

Very Small Array

Infobox Telescope
bgcolour =
name = Very Small Array


caption =
organization = Cavendish Astrophysics Group, University of Cambridge
Jodrell Bank Observatory, University of Manchester
Instituto de Astrofisica de Canariascite web | url=http://www.mrao.cam.ac.uk/telescopes/vsa/ | title=University of Cambridge webpage on the VSA | accessdate=2007-06-23]
location = Observatorio del Teide, Tenerife
coords =
altitude = 2,500mcite web | url=http://www.jb.man.ac.uk/tech/technology/vsa.html | title=Jodrell Bank Observatory - VSA Receivers | accessdate=2007-06-23]
weather =
wavelength = 26–36GHz
built = Installed December 1999cite web | url=http://www.jb.man.ac.uk/research/cmb/vsa/ | title=Jodrell Bank webpage on the VSA | accessdate=2007-06-23]
first_light =
website = [http://www.mrao.cam.ac.uk/telescopes/vsa/ www.mrao.cam.ac.uk/telescopes/vsa]
[http://www.jb.man.ac.uk/research/cmb/vsa/ www.jb.man.ac.uk/research/cmb/vsa]
style = Aperture synthesis interferometer
diameter =
angular_resolution = 0.2—3 degrees
area =
focal_length =
mounting = Tip-table
dome =
The Very Small Array is a 14-element interferometric radio telescope operating between 26 and 36 GHz that is used to study the cosmic microwave background radiation. It is a collaboration between the University of Cambridge, University of Manchester and the Instituto de Astrofisica de Canarias (Tenerife), and is located at the Observatorio del Teide on Tenerife. The array was built at the Mullard Radio Astronomy Observatory by the Cavendish Astrophysics Group and Jodrell Bank Observatory, and was funded by PPARC (now STFC). The design was strongly based on the Cosmic Anisotropy Telescope.

The telescope is comparable in terms of capabilities to several other CMB experiments, including the balloon-based BOOMERanG and MAXIMA, and the ground-based DASI and CBI.Watson et al. (2003)]

Design

The telescope consists of 14 elements (yielding 91 baselines), each of which have a horn reflector antenna focusing astrophysical signals into individual receivers (pseudomorphic HFET amplifiers, with a system temperature around 25 K and a physical temperature of 12 K, based on an NRAO design). The separate elements are combined using a correlator to form an aperture synthesis array. The elements are mounted on a tip-table, which is capable of tracking the sky and can tilt up to 35 degrees from the zenith.

The telescope has been used in three different configurations - 'compact', 'extended' and 'super-extended', each of which differ in the separation distance between the elements (the difference between compact and extended is a factor of 2.25), and the size of the antennas. While the compact array has antennas 143mm in diameter, the extended array uses 322mm diameter antennas.Grainge et al. (2003)] This means that the compact array has a primary beam of 4.5 degrees, and a resolution of 30 arcminutes (multipoles between 100 and 800), while the extended array has a primary beam of 2 degrees, a resolution of 12 arcminutes and can hence observe multipoles between 250 and 1500.cite web | url=http://www.jb.man.ac.uk/research/cmb/vsa/VSA_Technical_Specs.html | title=Technical specifications of the VSA | publisher=Jodrell Bank Observatory | accessdate=2007-06-23] The extended array is also a factor of 5 more sensitive than the compact array.Grainge et al. (2003)] The super-extended array will be able to measure multipoles up to 3000,Dickinson et al. (2004)] and has 550mm antenna mirrors. The front-end amplifiers were also upgraded.Cleary et al. (2004)]

The telescope can be tuned to frequencies between 26 and 36GHz, with 1.5GHz bandwidth, meaning that the telescope can carry out observations at different frequencies.Taylor et al. (2003)]

It also includes two 3.7m radio telescopes, also working at 30GHz,cite web | url=http://www.jb.man.ac.uk/research/cmb/vsa/VSA_source_Subtractors.html | title=VSA Source Subtractors | publisher=Jodrell Bank Observatory | accessdate=2007-06-23] which are dedicated to monitoring foreground sources.Watson et al. (2003)] These source subtraction dishes were upgraded to more accurate ones following the first series of observations, to allow the monitoring of much weaker sources than previously.Grainge et al. (2003)]

Both the source subtractor dishes, and the VSA itself, are surrounded by large metal ground shields.

As the VSA is an interferometer, it directly measures the angular power spectrum of the CMB, rather than having to construct a map of the sky first.Scott et al. (2003)]

Results

The fields observed with the VSA were chosen to minimize the amount of bright radio sources and large clusters in the field (the latter to avoid the Sunyaev-Zel'dovich effect), as well as to avoid contamination by emission from our galaxy.Dickinson et al. (2004)] The radio point sources present in the VSA fields were observed with the Ryle Telescope at 15GHz, then monitored by the VSA source subtracters during the VSA observations.Watson et al. (2003)]

In the compact array configuration, the telescope observed three 7x7 degree areas of the sky to high precision in an observing session between August 2000 and August 2001.Maisinger et al. (2003)] These observations were taken at the highest frequency of the telescope, centered at 34GHz, to reduce foreground contamination.Taylor et al. (2003)] Another, larger area of the sky was also observed, but less precisely.Taylor et al. (2003)] The data from these observations were reduced independently at all three involved institutions. The results from these observations were published in a series of four papers in 2003; those by Watson et al., Taylor et al., Scott et al. and Rubino-Martin et al. (see References below). The key results were the power spectra of the Cosmic Microwave Background between multipoles of 150 and 900,Scott et al. (2003)] and the resulting limits on cosmological parameters when combined with data from observations from other experiments.Rubino-Martin et al. (2003)]

The second observing session ran between September 2001Maisinger et al. (2003)] and July 2003, and was using the extended array.cite web | url=http://www.jb.man.ac.uk/research/cmb/vsa/vsa_results.html | title=VSA Extended Array Power Spectrum Data | accessdate=2007-06-23] The first results from the extended array were published as a Letter in 2003, simultaneously with the first four publications, using data taken up until April 2002. The sections of the sky observed were located within the previously-observed fields, with the measurements being both more accurate and in greater detail. The result was an improved power spectrum of the CMB, going out to a multipole of 1400,Grainge et al. (2003)] and refined cosmological parameters.Slosar et al. (2003)] The second set of results were published in 2004, and consisted of the original observations plus more observations taken in the same regions of the sky, as well as observations in three new regions. This yielded measurements of the CMB power spectra out to l of 1500 much more accurately than previously,Dickinson et al. (2004)] and more accurate cosmological parameter estimates.Rebolo et al. (2004)]

Observations with the VSA continued until the end of August 2008, using the Super-Extended configuration. Also, the Ryle Telescope has been upgraded to detect lower flux point sources sources, and the OCRA receiver on a telescope in Poland will be used to more accurately subtract the point sources.Cleary et al. (2004)]

References and further reading

Journal articles


* | url=http://adsabs.harvard.edu/abs/2003MNRAS.341.1057W | doi=10.1046/j.1365-8711.2003.06338.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2003MNRAS.341.1066T | doi=10.1046/j.1365-8711.2003.06493.x | format=abstract
* | doi=10.1046/j.1365-8711.2003.06354.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2003MNRAS.341.1084R | doi=10.1046/j.1365-8711.2003.06494.x | format=abstract
* | doi=10.1046/j.1365-8711.2003.06563.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2004MNRAS.353..747R | doi=10.1046/j.1365-8711.2003.06564.x | format=abstract
* | doi=10.1046/j.1365-8711.2003.06995.x | format=abstract
* | doi=10.1111/j.1365-2966.2004.07578.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2005MNRAS.360..340C | doi=10.1111/j.1365-2966.2004.08206.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2004MNRAS.352..887S | doi=10.1111/j.1365-2966.2004.07885.x | format=abstract
* | journal=MNRAS | volume=353 | pages=747–759 | url=http://adsabs.harvard.edu/abs/2004MNRAS.353..747R | doi=10.1111/j.1365-2966.2004.08102.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2005MNRAS.359...16L | doi=10.1111/j.1365-2966.2005.08696.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2005MNRAS.360..340C | journal=MNRAS | volume=360 | pages=340–353 | doi=10.1111/j.1365-2966.2005.09037.x | format=abstract
* | year=2005 | doi=10.1111/j.1365-2966.2005.09405.x | format=abstract
* | doi=10.1111/j.1365-2966.2005.09519.x | format=abstract
* | url=http://adsabs.harvard.edu/abs/2006MNRAS.369..909R | doi=10.1111/j.1365-2966.2006.10341.x | format=abstract

See also

*Very Large Array

External links

* [http://webcam.vsa.iac.es/view/view.shtml Very Small Array Webcam]


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