William Herschel Telescope

"Herschel Telescope" redirects here. For the far-infrared space telescope, see Herschel Space Observatory. For the telescope used by William Herschel, see 40-foot telescope.
William Herschel Telescope

View of large all white building with the biggest part being a spherical shaped section placed atop a rectangular prism. The building sits atop a mountain with clouds showing in the distance above and below the height of the building.

The William Herschel Telescope building
Organisation Isaac Newton Group of Telescopes
Location(s) Roque de los Muchachos Observatory, La Palma, Canary Islands, Spain
Coordinates 28°45′37.7″N 17°52′53.8″W / 28.760472°N 17.881611°W / 28.760472; -17.881611Coordinates: 28°45′37.7″N 17°52′53.8″W / 28.760472°N 17.881611°W / 28.760472; -17.881611
Altitude 2344m
Weather 75% clear nights
Median seeing 0.7"[1]
Wavelength Optical / near-infrared
Built 1983–1987
First light 1 June 1987
Telescope style Ritchey-Chrétien Cassegrain, Nasmyth or Prime focus reflector[2]
Diameter 4.2m
Secondary dia. 1.0m
Collecting area 13.8m2
Mounting Alt-azimuth
Enclosure Onion
Website WHT Homepage

The William Herschel Telescope (WHT) is a 4.20-metre (165 in) optical/near-infrared reflecting telescope located at the Observatorio del Roque de los Muchachos on the island of La Palma in the Canary Islands, Spain. The telescope, which is named after William Herschel, is part of the Isaac Newton Group of Telescopes. It is funded by research councils from the United Kingdom, the Netherlands and Spain.

At the time of construction in 1987, the WHT was the third largest single optical telescope in the world.[note 1][3][4] It is currently the second largest in Europe,[note 2] and was the final telescope constructed by Grubb Parsons in their 150-year history.

The WHT is equipped with a wide range of instruments operating over the optical and near-infrared regimes. These are used by professional astronomers to conduct a wide range of astronomical research. Astronomers using the telescope discovered the first evidence for a supermassive black hole (Sgr A*) at the centre of the Milky Way, and made the first optical observation of a gamma-ray burst.

History

The WHT was first conceived in the late 1960s, when the 3.9 m (150 in) Anglo-Australian Telescope (AAT) was being designed. The British astronomical community saw the need for telescopes of comparable power in the northern hemisphere. In particular, there was a need for optical follow-up of interesting sources in the radio surveys being conducted at the Jodrell Bank and Mullard observatories, both located in the UK.[5]

The AAT was completed in 1974, at which point the British Science and Engineering Research Council began planning for a group of three telescopes located in the northern hemisphere (now known as the Isaac Newton Group of Telescopes, ING). The telescopes were to be a 1.0 m (39 in) (which became the Jacobus Kapteyn Telescope), the 2.5 m (98 in) Isaac Newton Telescope which was to be moved from its existing site at Herstmonceux Castle, and a 4m class telescope, initially planned as a 4.5 m (180 in).[5] A new site was chosen at an altitude of 2,344 m (7,690 ft) on the island of La Palma in the Canary Islands, that is now the Observatorio del Roque de los Muchachos. The project was led by the Royal Greenwich Observatory (RGO), who also operated the telescopes until control passed to an independent ING when the RGO closed in 1998.[4][6][7]

By 1979 the 4 m was on the verge of being scrapped due to a ballooning budget,[5] whilst the aperture had been reduced to 4.2 m (170 in). A panel known as the Tiger Team[8] was convened to reduce the cost; a re-design cut the price-tag by 45%.[note 3] Savings were primarily made by reducing the focal length of the telescope – which allowed the use of a smaller dome – and relocating non-essential functions outside the dome to a simpler (and thus cheaper) rectangular annexe.[8] In the same year, the Isaac Newton Telescope was moved to Roque de los Muchachos Observatory, becoming the first of the Isaac Newton Group of Telescopes. In 1981 the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (Netherlands Organization for Scientific Research, NWO) bought a 20% stake in the project, allowing the WHT to be given the go-ahead. That year was the 200th anniversary of the discovery of Uranus by William Herschel, and it was decided to name the telescope in his honour.[5]

Construction of the telescope was by Grubb Parsons, the last telescope that company produced in its 150-year history.[8][9] Work began at their workshop in Newcastle-upon-Tyne in 1983, and the telescope was shipped to La Palma in 1985[5] (the two other telescopes of the Isaac Newton Group began operating in 1984[4]). The WHT saw first light on 1 June 1987;[5] it was the third largest optical telescope in the world at the time.[note 1][3] The total cost of the telescope, including the dome and the full initial suite of instruments, was £15M (in 1984, equivalent to £43M in 2016[10]); within budget once inflation is taken into account.[note 4]

Design

White metal truss frame inside white dome atop a circular base and flanked by two rectangular boxes on either side.
The William Herschel Telescope inside its dome. The two black tubes are light baffles, the two large enclosures on the left and right are the Nasmyth platforms, instruments at the Cassegrain focus are visible at the base, and the three black boxes in the centre house the calibration lamps located at folded Cassegrain.

Optics

The telescope consists of a 4.20 m (165 in) f/2.5 primary mirror made by Owens-Illinois from Cervit, a zero-expansion glass-ceramic material, and ground by Grubb Parsons.[2][4][8] The mirror blank was produced in 1969 as one of a set of four, along with those for the AAT, CFHT and Blanco telescopes, and was purchased for the WHT in 1979, ten years after it was made.[9] The primary is solid and un-thinned, so no active optics system is required,[2] despite its weight of 16.5 tonnes (16.2 long tons).[8][11] The mirror support cell holds the main mirror on a set of 60 pneumatic cylinders.[8] Even under the most extreme loading (with the telescope pointing at the horizon, so the mirror is vertical) the shape of the mirror changes by only 50 nanometres (2.0×10−6 in);[4] during normal operation the deformation is much smaller.

In its most usual configuration, a 1.00 m (39 in) hyperbolic secondary mirror made of Zerodur is used to form a Ritchey Chretien f/11 Cassegrain system with a 15 arcmin field of view.[2][4][8] An additional flat fold mirror allows the use of any one of two Nasmyth platforms or two folded Cassegrain stations, each with 5 arcmin fields of view.[2][4][8] The telescope sometimes operates in a wide-field prime focus configuration, in which case the secondary is removed and a three element field-correcting lens inserted, which provides an effective f/2.8 focus with a 60 arcmin field of view (40 arcmin unvignetted).[2][8] Changing between the Cassegrain and Nasmyth foci takes a matter of seconds and may be done during the night; switching to and from prime focus requires replacing the secondary mirror with a prime focus assembly during daytime (the two are mounted back-to-back)[4] which takes around 30 minutes.[8]

A Coudé focus was planned as a later addition, to feed an optical interferometer with another telescope,[8] but this was never built. A chopping f/35 secondary mirror was planned for infrared observations, but was placed on hold by the cost-saving re-design and never implemented.[8]

Mount

The optical system weighs 79,513 kg (78.257 long tons) and is manoeuvred on an alt-azimuth mount, with a total moving mass of 186,250 kg (183.31 long tons) (plus instruments).[3] The BTA-6 and Multi Mirror Telescope had demonstrated during the 1970s the significant weight (and therefore cost) savings which could be achieved by the alt-azimuth design compared to the traditional equatorial mount for large telescopes. However, the alt-azimuth design requires continuous computer control, compensation for field rotation at each focus, and results in a 0.2 degree radius blind spot at zenith where the drive motors cannot keep up with sidereal motion (the drives have a maximum speed of one degree per second in each axis).[4][8][12] The mount is so smooth and finely balanced that before the drive motors were installed it was possible to move the then 160 long tons (160,000 kg) assembly by hand.[4] During closed loop guiding, the mount is capable of an absolute pointing accuracy of 0.03 arcseconds.[8][12]

Dome

Aerial view of white domed building on side of mountain with floor of white clouds extending to the horizon below and behind the mountain.
The WHT dome above a sea of clouds

The telescope is housed in an onion-shaped steel dome with an internal diameter of 21 m (69 ft),[4][8][13] manufactured by Brittain Steel. The telescope mount is located on a cylindrical concrete pier so that the centre of rotation is 13.4 m (44 ft) above ground level, which lifts the telescope above ground-layer air turbulence for better seeing.[4][8][13] A conventional up-down 6m-wide[8] shutter with wind-blind, several large vents with extractor fans for thermal control, and a 35-tonne (34-long-ton) capacity crane (used for moving the primary mirror e.g. for aluminising) are all incorporated.[13] The size and shape of the shutter allow observations down to 12° above the horizon,[4] which corresponds to an airmass of 4.8. The total moving mass of the dome is 320 tonnes (310 long tons), which is mounted on top of a three-storey cylindrical building.[13] The dome was designed to minimise wind stresses and can support up to its own weight again in ice during inclement weather.[4] The dome and telescope rest on separate sets of foundations (driven 20 metres (66 ft) down into the volcanic basalt),[4] to prevent vibrations caused by dome rotation or wind stresses on the building affecting the telescope pointing.[8]

Attached to the dome is a three-storey rectangular building which houses the telescope control room, computer room, kitchen etc.[4] Almost no human presence is required inside the dome, which means the environmental conditions can be kept very stable.[4][13] As a result, the WHT obtains perfect dome seeing.[14] This building also houses a detector laboratory and a realuminising plant. Because the WHT has the largest single mirror at the Observatorio del Roque de los Muchachos, its realuminising plant has a vacuum vessel large enough to accommodate the mirrors from any other telescope on the mountain. As a result, all of the other telescopes at the observatory contract to use the WHT plant for their realuminising[15] (with the exception of the Gran Telescopio Canarias, which has its own plant).

Operations

Series of white structures along the side of a mountain with a sea of clouds below and behind the mountain extending to the horizon which is red, orange, and yellow.
Part of Roque de los Muchachos Observatory, including the Isaac Newton Group of Telescopes. The William Herschel Telescope is the large dome on the left, the Isaac Newton Telescope is located second from the right, and the Jacobus Kapteyn Telescope is located on the far right.

The WHT is operated by the Isaac Newton Group of Telescopes (ING), together with the 2.5m Isaac Newton Telescope and 1.0m Jacobus Kapteyn Telescope. Offices and administration are located an hour's drive away in Santa Cruz de La Palma, the island's capital. Funding is provided by the UK's Science and Technology Facilities Council (STFC, 65%), the Netherlands' Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO, 25%) and Spain's Instituto de Astrofísica de Canarias (IAC, 10%) (2008 values). Telescope time is distributed in proportion to this funding, although Spain receives an additional 20% allocation in return for use of the observatory site. Five percent of observing time is further reserved for astronomers of other nationalities. As a competitive research telescope, the WHT is heavily oversubscribed, typically receiving applications for three to four times as much observing time as is actually available.[16]

The vast majority of observations are carried out in visitor mode i.e. with the investigating astronomer physically present at the telescope. A shift to service mode operations (those carried out by observatory staff on behalf of astronomers who do not travel to the telescope) has been considered and rejected on scientific and operational grounds.[17]

Instruments

The WHT is equipped with a wide range of scientific instruments, providing astronomers with the capabilities to conduct a large variety of scientific investigations. As of 2010, the current common-user instrumentation is:[18]

ACAM
Auxiliary-port CAMera – optical imager/spectrograph, with broad- and narrow-band imaging over an 8' field and low-resolution (R < 900) spectroscopy. Permanently mounted at one of the broken-Cassegrain foci.
AF2
Autofib2 – robot fibre positioner, 150 science fibres and 10 fiducial bundles over a 1° field. Mounted at prime focus.
WYFFOS
Wide field Fibre Fed Optical Spectrograph – bench-mounted optical spectrograph fed from AF2, R = 200-11,000. Located in one of the Nasmyth enclosures, though it does not use the Nasmyth focus.
ISIS
Intermediate dispersion Spectrograph and Imaging System – medium resolution (R = 1,800-20,000) long-slit dual-beam optical spectrograph. Mounted at Cassegrain focus. ISIS was one of the original first generation of WHT instruments.[8]
LIRIS
Long-slit Intermediate Resolution Infrared Spectrograph – near-infrared imager/spectrograph, with imaging over a 4' field, spectral resolutions R = 700-2500, spectropolarimetry, and long slit and multi-object slit-masks. Mounted at Cassegrain focus.
NAOMI
Natural-guide-star Adaptive Optics for Multi-purpose Instrumentation – an adaptive optics feed, operating over the entire optical and near-infrared wavelength regions. Permanently mounted at one of the Nasmyth foci.
GLAS
Ground-layer Laser Adaptive optics System – laser guide star for optional use with NAOMI
INGRID
Isaac Newton Group Red Imaging Device – high spatial resolution near-infrared camera for use with NAOMI
OSCA
Optimised Stellar Coronograph for Adaptive Optics – high-contrast coronograph for optional use with INGRID
OASIS
Optically Adaptive System for Imaging Spectroscopy – optical integral field unit for use with NAOMI
PFIP
Prime Focus Imaging Platform – wide field optical camera, with broad- and narrow-band imaging over a 16' field. Mounted at prime focus.

In addition the WHT is a popular telescope for single-purpose visitor instruments, which in recent years have included GHαFaS, INTEGRAL, PLANETPOL, PNS, SAURON, FASTCAM and ULTRACAM.[19] Visitor instruments can use either the Cassegrain focus or one of the Nasmyth foci.

A common set of calibration lamps (Helium and Neon arc lamps, and a Tungsten flat-field lamp) are permanently mounted at one of the broken-Cassegrain foci, and can be used for any of the other instruments.

The ISIS and LIRIS are the workhorses of the WHT, and approximately two-thirds of all time awarded is for these two instruments.[20]

Scientific research

Low angle picture from ground showing sand and a large rock with a man looming a few feet back against a blue sky.
Peter Jenniskens with a fragment of 2008 TC3, an asteroid observed by the WHT just days earlier

Astronomers use the WHT to conduct scientific research across most branches of observational astronomy, including solar system science, galactic astronomy, extragalactic astronomy and cosmology. Most of the instruments are designed to be useful for a range of different research.

The WHT has been used to make many significant new discoveries. Some of the more notable include the first evidence of a supermassive black hole (Sgr A*) at the centre of the Milky Way (in 1995)[21] and the first optical observation of a gamma-ray burst (GRB 970228) (in 1997).[22]

Since the mid-1990s the WHT has faced increasing competition from newer 8-to-10 m (310-to-390 in) telescopes. Nevertheless, a wide range of research continues to be done with the telescope. In recent years (as of 2010) this has included:

Future developments

The upcoming generation of extremely large telescopes (ELTs) will require sophisticated adaptive optics in order to be used to their full capability. Because the WHT has an advanced adaptive optics system already operating, it is receiving attention from the various ELT programs. The European Southern Observatory's European-ELT (E-ELT) project has begun a programme to utilise the WHT as a test-bed for its adaptive optics system, and will receive several nights per year for on-sky testing.[17][34] The project involves construction of new optical experiments at one of the Nasmyth foci, and is called CANARY. CANARY will demonstrate the multi-object adaptive optics (MOAO) required for the EAGLE instrument on the E-ELT.[35]

The UK's STFC (originally the major financial contributor) has gradually reduced its funding for the ING telescopes over a number of years. Some of this funding shortfall has been made up by other partners increasing their contributions, and some by efficiency savings and cutbacks. As a result, the shares of observing time will become UK 33%, Netherlands 28%, Spain 34% and 5% for any nationality.[36] A new development, started in 2010, is the development of a new wide-field multi-object spectroscopy facility (WEAVE), being developed by a UK-led consortium involving major contributions from the Netherlands, Spain, France, and Italy, which is expected to be in place by the end of 2017. WEAVE will provide medium-high resolution spectroscopy in the visible (360-950 nm) range for up to 1000 simultaneous targets over a 2 degree field of view, and is currently expected to operate through to at least 2023.[37]

Notes

  1. 1 2 The BTA-6 (6.0 m) and Hale telescope (5.1 m) were both larger; the Multiple Mirror Telescope also had a larger collecting area but did not have a single primary mirror
  2. ↑ The neighbouring Gran Telescopio Canarias (10.4 m) overtook the WHT in 2009 to become the largest in Europe
  3. ↑ From £18M to £10M, at 1979 values[5]
  4. ↑ The budget of £10M set in 1979 was equivalent to £15.7M in 1984 due to inflation.[10]

References

  1. ↑ Chris Benn (28 May 2009). "Site Quality". ING website. Isaac Newton Group. Retrieved 28 Nov 2009.
  2. 1 2 3 4 5 6 Javier Méndez (25 Feb 2008). "WHT Telescope Optics". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  3. 1 2 3 Javier Méndez (3 Mar 2004). "General information on the William Herschel Telescope". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  4. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 Murdin, Paul; Boksenberg, Alec (July 1987). "The William Herschel telescope" (PDF). Astronomy Now. 1 (2): 17–25. Retrieved 12 July 2010.
  5. 1 2 3 4 5 6 7 Chris Benn (31 Oct 2005). "History of William Herschel Telescope". ING website. Isaac Newton Group. Retrieved 10 Jan 2010.
  6. ↑ Parker, Chas (February 1999). "CASTLE IN THE SKY – THE STORY OF THE ROYAL GREENWICH OBSERVATORY AT HERSTMONCEUX". In Moore, Patrick. The Yearbook of Astronomy 2000. London: Macmillan Publishers. Retrieved 8 October 2010
  7. ↑ Méndez, Javier (8 September 2009). "Chronology of the Isaac Newton Group of Telescopes". ING Website. Isaac Newton Group. Retrieved 8 October 2010.
  8. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 Boksenberg, Alec (1985). "The William Herschel telescope" (PDF). Vistas in Astronomy. Elsevier. 28 (3): 531–553. Bibcode:1985VA.....28..531B. doi:10.1016/0083-6656(85)90074-1. ISSN 0083-6656. Retrieved 18 May 2010.
  9. 1 2 Ridpath, Ian (August 1990). "The William Herschel telescope" (PDF). Sky & Telescope. 80: 136. Bibcode:1990S&T....80..136R. Retrieved 12 July 2010.
  10. 1 2 UK CPI inflation numbers based on data available from Gregory Clark (2016), "The Annual RPI and Average Earnings for Britain, 1209 to Present (New Series)" MeasuringWorth.
  11. ↑ Javier Méndez (16 Oct 2003). "WHT – Mirror Support Systems". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  12. 1 2 Javier Méndez (16 Oct 2003). "WHT – The Mounting". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  13. 1 2 3 4 5 Javier Méndez (3 Mar 2004). "The Dome and the Building of the William Herschel Telescope". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  14. ↑ "WHT Dome Seeing Investigation". ING website. Isaac Newton Group. 13 September 2010. Retrieved 13 September 2010.
  15. ↑ "An Overview of ING". ING website. Isaac Newton Group. 10 November 2009. Retrieved 25 September 2010.
  16. ↑ Chris Benn (19 May 2010). "WHT publication and oversubscription statistics". ING website. Isaac Newton Group. Retrieved 12 July 2010.
  17. 1 2 Balcells, Marc; Benn, Chris; Abrams, Don Carlos (26 Jan 2010). "ING Decadal Strategy 2010–2020". ING website. Isaac Newton Group. Retrieved 12 July 2010.
  18. ↑ Ian Skillen (10 Feb 2010). "ING Instrumentation Options". ING website. Isaac Newton Group. Retrieved 6 Apr 2010.
  19. ↑ S. A. Rix; C. R. Benn & M. Santander-García (4 March 2010). "Visiting Instruments at the 4.2m WHT" (PDF). Science with the William Herschel Telescope 2010–2020. Isaac Newton Group. Retrieved 14 September 2010.
  20. ↑ Benn, Chris (14 April 2010). "WHT OPERATIONS DURING 2009B". ING website. Isaac Newton Group. Retrieved 7 October 2010.
  21. ↑ Krabbe, A.; Genzel; Eckart; Najarro; Lutz; Cameron; Kroker; Tacconi-Garman; et al. (July 1995). "The Nuclear Cluster of the Milky Way: Star Formation and Velocity Dispersion in the Central 0.5 Parsec". Astrophysical Journal Letters. Institute of Physics Publishing. 447 (2): L95. Bibcode:1995ApJ...447L..95K. doi:10.1086/309579.
  22. ↑ van Paradijs, J.; Groot; Galama; Kouveliotou; Strom; Telting; Rutten; Fishman; et al. (April 1997). "Transient optical emission from the error box of the γ-ray burst of 28 February 1997". Nature. Nature Publishing Group. 386 (6626): 686–689. Bibcode:1997Natur.386..686V. doi:10.1038/386686a0.
  23. ↑ Javier Méndez (8 Dec 2008). "The SAURON Project". ING website. Isaac Newton Group. Retrieved 17 May 2010.
  24. ↑ "SAURON Website". Leiden Observatory. Retrieved 18 May 2010.
  25. ↑ Jenniskens, P.; Shaddad, M. H.; Numan, D.; Elsir, S.; Kudoda, A. M.; Zolensky, M. E.; Le, L.; Robinson, G. A.; et al. (March 2009). "The impact and recovery of asteroid 2008 TC3". Nature. Nature Publishing Group. 458 (7237): 485–488. Bibcode:2009Natur.458..485J. doi:10.1038/nature07920. PMID 19325630.
  26. ↑ Javier Méndez (25 Feb 2009). "The Galaxy Zoo and Hanny's Voorwerp". ING website. Isaac Newton Group. Retrieved 17 May 2010.
  27. ↑ Lintott, Chris J.; Schawinski, Kevin; Keel, William; Van Arkel, Hanny; Bennert, Nicola; Edmondson, Edward; Thomas, Daniel; Smith, Daniel J. B.; et al. (October 2009). "Galaxy Zoo: 'Hanny's Voorwerp', a quasar light echo?". Monthly Notices of the Royal Astronomical Society. Royal Astronomical Society. 399 (1): 129–140. arXiv:0906.5304Freely accessible. Bibcode:2009MNRAS.399..129L. doi:10.1111/j.1365-2966.2009.15299.x. ISSN 0035-8711.
  28. ↑ Javier Méndez (4 Feb 2009). "Diffuse Bands Don't Originate in Circumstellar Envelopes". ING website. Isaac Newton Group. Retrieved 17 May 2010.
  29. ↑ R. Luna; N. L. J. Cox; M. A. Satorre; D. A. García Hernández; O. Suárez & P. García Lario (March 2008). "A search for diffuse bands in the circumstellar envelopes of post-AGB stars". Astronomy & Astrophysics. European Southern Observatory. 480 (1): 133–148. arXiv:0711.1843Freely accessible. Bibcode:2008A&A...480..133L. doi:10.1051/0004-6361:20065282. ISSN 0004-6361.
  30. ↑ Javier Méndez (3 Jan 2009). "SuperWASP Finds a Strongly-Irradiated Transiting Gas-Giant Exoplanet". ING website. Isaac Newton Group. Retrieved 17 May 2010.
  31. ↑ Pollacco, D.; Skillen; Collier Cameron; Loeillet; Stempels; Bouchy; Gibson; Hebb; et al. (April 2008). "WASP-3b: a strongly irradiated transiting gas-giant planet". Monthly Notices of the Royal Astronomical Society. Royal Astronomical Society. 385 (3): 1576–1584. arXiv:0711.0126Freely accessible. Bibcode:2008MNRAS.385.1576P. doi:10.1111/j.1365-2966.2008.12939.x. ISSN 0035-8711.
  32. ↑ Javier Méndez (23 Nov 2008). "Two Stellar Explosions at Exactly the Same Position". ING website. Isaac Newton Group. Retrieved 17 May 2010.
  33. ↑ Pastorello, J.; Smartt; Mattila; Eldridge; Young; Itagaki; Yamaoka; Navasardyan; et al. (June 2007). "A giant outburst two years before the core-collapse of a massive star". Nature. Nature Publishing Group. 447 (7146): 829–832. arXiv:astro-ph/0703663Freely accessible. Bibcode:2007Natur.447..829P. doi:10.1038/nature05825. PMID 17568740.
  34. ↑ Myers, Richard M.; Calia, D. Bonaccini; Devaney, N.; (23 authors); et al. (2007). "The European E-ELT WHT LGS Test Facility Consortium". Adaptive Optics: Analysis and Methods. Adaptive Optics: Methods, Analysis and Applications. Optical Society of America. Retrieved 10 Jan 2010.
  35. ↑ Evans, Chris J. (August 2008). "The European Extremely Large Telescope". Astronomy & Geophysics. Royal Astronomical Society. 49 (4): 4.22–4.25. Bibcode:2008A&G....49d..22E. doi:10.1111/j.1468-4004.2008.49422.x. ISSN 1366-8781.
  36. ↑ Benn, Chris; Abrams, Don; Skillen, Ian (2009). "ING La Palma – 2020 vision". Opticon. Retrieved 7 October 2010.
  37. ↑ Dalton, Gavin; Trager, Scott; Abrams, Don Carlos; (53 authors) (2014). "Project overview and update on WEAVE: the next generation wide-field spectroscopy facility for the William Herschel Telescope". Proc. SPIE. 9147: 0L–11. arXiv:1412.0843Freely accessible. doi:10.1117/12.2055132.

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