James Clerk Maxwell Telescope

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Scale model of JCMT

The James Clerk Maxwell Telescope (JCMT) is a submillimetre-wavelength telescope at Mauna Kea Observatory in Hawaii. The telescope is near the summit of Mauna Kea at 13,425 feet (4,092 m). Its primary mirror is 15 metres (16.4 yards) across: it is the largest astronomical telescope that operates in submillimetre wavelengths of the electromagnetic spectrum (far-infrared to microwave).[1] Scientists use it to study our Solar System, interstellar dust and gas, and distant galaxies. JCMT will be shut down at the end of 2014, if a new operator is not found.[2]

The JCMT is funded by a partnership between the United Kingdom and Canada. It is operated by the Joint Astronomy Centre and was named in honour of mathematical physicist James Clerk Maxwell.

The JCMT has the second-largest telescope mirror on Mauna Kea. (The largest is the VLBA antenna.)

The telescope was combined with the Caltech Submillimeter Observatory next to it to form the first submillimetre interferometer. This success was important in pushing ahead the construction of the Submillimeter Array and the Atacama Large Millimeter Array interferometers.

History[edit]

The JCMT sub-mm telescope in the centre

In the late 1960s, the Astronomy Committee of the UK's Science Research Council (SRC, the forerunner of STFC) considered the importance of astronomical observations at submillimetre and millimetre wavelengths. After a series of proposals and debates, in 1975, the SRC millimetre steering committee concluded that it would be possible to construct a 15-metre diameter telescope capable of observing at wavelengths down to 750 µm. The project, then called the National New Technology Telescope (NNTT), was to be an 80/20 per cent collaboration with the Netherlands Organisation for the Advancement of Science. Site tests were made at Mauna Kea in Hawaii, the Pinaleno Mountains in Arizona, and a site in Chile; and Mauna Kea was chosen. The NNTT is a unique facility, larger and with a more instruments than competing telescopes such as the CSO and SMT.

The final specifications called for the "world's largest telescope optimised for submillimetre wavelengths". It was to be a parabolic 15-metre antenna composed of 276 individually adjustable panels with a surface accuracy of better than 50 µm. It would be an altitude-azimuth mounted Cassegrain telescope with a tertiary mirror to direct the incoming radiation onto a number of different receivers. The antenna and mountings were to be protected from the elements by a co-rotating carousel with a transparent membrane stretched across the carousel aperture. Building work started in 1983 and went well apart from a small delay caused by the hijacking of the ship carrying the telescope across the Pacific by modern-day pirates. The telescope saw first light in 1987. The name for the final facility was changed to the James Clerk Maxwell Telescope.

The JCMT is currently funded under an agreement between the United Kingdom (75 percent) and Canada (25 percent) (until March 31, 2013 this was United Kingdom (55 percent), Canada (25 percent), the Netherlands (20 percent)). The telescope itself is operated by the Joint Astronomy Centre (JAC), from Hilo, Hawaii. The telescope site agreement with the University of Hawaii provides observer accommodation and infrastructure in exchange for open access to international proposals and 10 per cent of the observing time for the University's own projects. Proposals for telescope usage are submitted to one of the national Telescope Allocation Groups (TAGs) and if successful are awarded time in the next six-monthly semester.

Instrumentation[edit]

The primary mirror seen from behind, showing the construction from many panels

The JCMT has two kinds of instrumentsbroadband continuum detectors and heterodyne detection spectral line receivers.

Continuum emission is a tracer of star formation in other galaxies and gives astronomers clues to the presence, distance, and evolution history of galaxies other than our own. Within our own galaxy dust emission is associated with stellar nurseries and planet forming solar systems.

Spectral-line observations can be used to identify particular molecules in molecular clouds, study their distribution and chemistry and determine gas velocity gradients across astronomical objects (because of the doppler effect).

SCUBA[edit]

The Submillimetre Common-User Bolometer Array

The older continuum single pixel UKT14 bolometer receiver was replaced in the 1990s by the Submillimetre Common-User Bolometer Array (SCUBA). This instrument operated simultaneously at wavelengths of 450 and 850 micron (with 91 and 37 pixels, respectively), and was sensitive to the thermal emission from interstellar dust. It was retired from service in 2005. It was succeeded by SCUBA-2, another continuum instrument that was commissioned in 2011. This ground-breaking camera consists of large arrays of superconducting transition edge sensors with a mapping speed hundreds of times larger than SCUBA. It has 5120 array elements at both 450 and 850 micron wavelength (10,240 total pixels). It has been conducting the JCMT legacy surveys since November, 2011, including the SCUBA-2 All Sky Survey, and was made available for general astronomical observations in February, 2012. [3] Two ancillary instruments, FTS-2 and POL-2, add spectroscopic and polarimetric capabilities to SCUBA-2.

Spectral line detectors[edit]

The JCMT is also equipped with three heterodyne receivers, which allow submillimetre spectral line observations to be made. The spectral-line mapping capabilities of the JCMT have been greatly enhanced by the commissioning of HARP-B, a 350 GHz, 16 element heterodyne array receiver. HARP-B, and the other heterodyne instruments, can be used in conjunction with the JCMT's new digital autocorrelation spectrometer, ACSIS.

See also[edit]

External links[edit]

References[edit]

  1. ^ W.S. Holland et al., SCUBA: a common-user submillimetre camera operating on the James Clerk Maxwell Telescope, Monthly Notices of the Royal Astronomical Society: Letters Volume 303 Issue 4, Pages 659–672, 2002 doi:10.1046/j.1365-8711.1999.02111.x
  2. ^ Farewell UKIRT
  3. ^ http://scuba2.wordpress.com/

Coordinates: 19°49′22″N 155°28′38″W / 19.822842°N 155.477346°W / 19.822842; -155.477346