United States Naval Observatory Flagstaff Station
Alternative namesNOFS
OrganizationUnited States Naval Observatory
Observatory code 689 Edit this on Wikidata
LocationCoconino County, near Flagstaff, Arizona
Coordinates35°11′03″N 111°44′26″W / 35.18417°N 111.74056°W / 35.18417; -111.74056
Altitude2,273 m (7,457 ft)
Established1955
WebsiteUnited States Naval Observatory's Flagstaff Station
Telescopes
Kaj Strand Telescope1.55 m (61 in) reflector
DFM/Kodak/Corning1.3 m reflector
Unnamed telescope1.0 m (40 in) Ritchey–Chrétien reflector
Flagstaff Astrometric Scanning Transit Telescope8-inch (20 cm) catadioptric
Navy Precision Optical Interferometerinterferometer (Located at Anderson Mesa)
United States Naval Observatory Flagstaff Station is located in the United States
United States Naval Observatory Flagstaff Station
Location of United States Naval Observatory Flagstaff Station
  Related media on Commons

The United States Naval Observatory Flagstaff Station (NOFS), is an astronomical observatory near Flagstaff, Arizona, US. It is the national dark-sky observing facility under the United States Naval Observatory (USNO).[1] NOFS and USNO combine as the Celestial Reference Frame[2] manager for the U.S. Secretary of Defense.[3][4]

General information

The Flagstaff Station is a command which was established by USNO (due to a century of eventually untenable light encroachment in Washington, D.C.) at a site five miles (8.0 km) west of Flagstaff, Arizona in 1955, and has positions for primarily operational scientists (astronomers and astrophysicists), optical and mechanical engineers, and support staff.

NOFS science supports every aspect of positional astronomy to some level, providing national support and beyond. Work at NOFS covers the gamut of astrometry and astrophysics in order to facilitate its production of accurate/precise astronomical catalogs. Also, owing to the celestial dynamics (and relativistic effects[5]) of the huge number of such moving objects across their own treks through space, the time expanse required to pin down each set of celestial locations and motions for a perhaps billion-star catalog, can be quite long. Multiple observations of each object may themselves take weeks, months or years, by themselves. This, multiplied by the large number of cataloged objects that must then be reduced for use, and which must be analyzed after observation for a very careful statistical understanding of all catalog errors, forces the rigorous production of most extremely precise and faint astrometric catalogs to take many years, sometimes decades, to complete.

The United States Naval Observatory, Flagstaff Station celebrated its 50th anniversary of the move there from Washington, D.C. in late 2005.[6] Dr. John Hall, Director of the Naval Observatory's Equatorial Division from 1947, founded NOFS. Dr. Art Hoag became its first director in 1955 (until 1965); both later were to also become directors of nearby Lowell Observatory.[7] NOFS has had 6 directors since 1955; its current and 7th acting director is Dr. Scott Dahm.[8]

NOFS remains active in supporting regional dark skies,[9][10] both to support its national protection mission,[11][12] and to promote and protect a national resource legacy for generations of humans to come.[13][14][15]

Night-time panoramic of operations at the United States Naval Observatory Flagstaff Station (NOFS)
Dark-sky operations at the United States Naval Observatory Flagstaff Station (NOFS)

Site description

NOFS is adjacent to Northern Arizona's San Francisco Peaks, on the alpine Colorado Plateau and geographically above the Mogollon Rim. Flagstaff and Coconino County minimize northern Arizona light pollution[16] through legislation of progressive code – which regulates local lighting.[17][18][19][20][21][22][23][24][25][26]

Indeed, despite a half-century-young history, NOFS has a rich heritage[27] which is derived from its parent organization, USNO, the oldest scientific institution in the U.S.[28] Notable events have included support to the Apollo Astronaut program hosted by USGS' nearby Astrogeology Research Center; and the discovery of Pluto's moon, Charon, in 1978 (discussed below). At an elevation of approximately 7,500 feet (2,300 m), NOFS is home to a number of astronomical instruments[29] (some also described in the worldwide list of optical telescopes); some additional instrumentation is on nearby Anderson Mesa. NOFS (with parent USNO) also do fundamental science on the UKIRT Infrared telescope in Hawaii.

The Navy provides stewardship of the facility, land and related dark sky protection efforts through its Navy Region Southwest, through Naval Air Facility El Centro.

Kaj Strand Telescope

The 1.55-meter (61-inch) Kaj Strand Telescope (or Kaj Strand Astrometric Reflector, KSAR) remains the largest telescope operated by the U.S. Navy. Congress appropriated funding in 1961 and it saw first light in 1964.[30] This status will change when the NPOI four 1.8-meter telescopes see their own first light in the near future. KSAR rides in the arms of an equatorial fork mount. The telescope is used in both the visible spectrum, and in the near infrared (NIR),[31] the latter using a sub-30-kelvin, helium-refrigerated, InSb (Indium antimonide) camera, "Astrocam".[32] In 1978, the 1.55-m telescope was used to "discover the moon of dwarf planet Pluto, named 'Charon'". (Pluto itself was discovered in 1930, across town at Lowell Observatory). The Charon discovery led to mass calculations which ultimately revealed how tiny Pluto was, and eventually caused the IAU to reclassify Pluto as a dwarf (not a principal) planet.[33][34][35] The 1.55-meter telescope was also used to observe and track NASA's Deep Impact Spacecraft, as it navigated to a successful inter-planetary impact with the celebrated Comet 9p/Tempel, in 2005. This telescope is particularly well-suited to perform stellar parallax studies, narrow-field astrometry supporting space navigation, and has also played a key role in discovering one of the coolest-ever known brown dwarf objects, in 2002.[36] The KSAR dome is centrally located on NOFS grounds, with support and office buildings attached to the dome structures. The large vacuum coating chamber facility is also located in this complex. The chamber can provide very accurate coatings and overcoatings of 100±2 Angstrom thickness (approximately 56 aluminium atoms thick), for small-to-multi-ton optics up to 1.8-meter (72-inch) in diameter, in a vacuum exceeding 7×106 Torr, using a vertical-optic, 1500-ampere discharge system. A dielectric coating capability has also been demonstrated. Large optics and telescope components can be moved about NOFS using its suite of cranes, lifts, cargo elevators and specialized carts. The main complex also contains a controlled-environment, optical and electronics lab for laser, adaptive optics, optics development, collimation, mechanical, and micro-electronic control systems needed for NOFS and NPOI.

The KSAR Telescope's 18-meter (60-foot) diameter steel dome is quite large for the telescope's aperture, owing to its telescope's long f/9.8 focal ratio (favorable for very accurate optical collimation, or alignment, needed for astrometric observation). It uses a very wide 2-shutter, vertical slit. Development studies have taken place to successfully show that planned life-cycle replacement of this venerable instrument can be efficiently done within the original dome, for a future telescope with an aperture of up to 3.6-meter (140-inch), by using fast, modern-day optics.[37] However, the 61-inch telescope remains unique in its ability to operationally conduct both very high-accuracy relative astrometry to the milliarcsecond level, and close-separation, PSF photometry. Several key programs take advantage of this capability to this day.

1.3-m telescope

The 1.3-meter (51-inch) large-field Ritchey–Chrétien telescope was produced by DFM Engineering and then corrected and automated by NOFS staff.[38] Corning Glass Works and Kodak made the primary mirror. The hyperbolic secondary has an advanced, computer-controlled collimation (alignment) system in order to permit very precise positions of stars and satellites (milliarcsecond astrometry) across its wide field of view. This system analyzes optical aberrations of the optical path, modeled by taking slope fits of the wavefront deviations revealed using a Hartmann mask. The telescope also now sports a state-of-the art, cryogenic wide-field mosaic CCD[39] camera.[40][41] It will also permit employment of the new "Microcam", an orthogonal transfer array (OTA), with Pan-STARRS heritage.[42][43][44][45] Other advanced camera systems are also deployed for use on this telescope, such as the LANL-produced RULLI single photon counter, nCam.[46][47][48][49][50] Using the telescope's special software controls, the telescope can track both stars and artificial satellites orbiting the Earth, while the camera images both. The 1.3 m dome itself is compact, owing to the fast overall optics at f/4. It is located near by and southwest of, the very large 61-inch dome. In addition to astrometric studies (such as for Space Situational Awareness, SDSS[51] and SST), research on this telescope includes the study of blue and K-Giant stars, celestial mechanics and dynamics of multiple star systems, characterizations of artificial satellites, and the astrometry and transit photometry of exoplanets.

1.0-m telescope

The 1.0-meter (40-inch) "Ritchey–Chrétien Telescope" is also an equatorially driven, fork-mounted telescope.[52] The Ritchey is the original Station telescope which was moved from USNO in Washington in 1955. It is also the first R-C telescope ever made from that famous optical prescription, and was coincidentally the last telescope built by George Ritchey himself. The telescope is still in operation after a half century of astronomy at NOFS. It performs key quasar-based reference frame operations (International Celestial Reference Frame), transit detections of exoplanets, Vilnius photometry, M-Dwarf star analysis, dynamical system analysis, reference support to orbiting space object information, horizontal parallax guide support to NPOI, and it performs photometric operations support to astrometric studies (along with its newer siblings). The 40-inch telescope can carry a number of liquid nitrogen-cooled cameras, a coronagraph, and a nine-stellar magnitude neutral density spot focal plane array camera, through which star positions are cross-checked before use in fundamental NPOI reference frame astrometry.

This telescope is also used to test internally developed optical adaptive optics (AO) systems, using tip-tilt and deformable mirror optics. The Shack–Hartmann AO system allows for corrections of the wavefront's aberrations caused by scintillation (degraded seeing), to higher Zernike polynomials. AO systems at NOFS will migrate to the 1.55-m and 1.8-m telescopes for future incorporation there.

The 40-inch dome is located at the summit and highest point of the modest mountain upon which NOFS is located. It is adjacent to a comprehensive instrumentation shop, which includes sophisticated, CAD-driven CNC fabrication machinery, and a broad array of design and support tooling.

0.2-m FASTT

A modern-day example of a fully robotic transit telescope is the small 0.20-meter (8-inch) Flagstaff Astrometric Scanning Transit Telescope (FASTT) completed in 1981 and located at the observatory.[53][54] FASTT provides extremely precise positions of solar system objects for incorporation into the USNO Astronomical Almanac and Nautical Almanac. These ephemerides are also used by NASA in the deep space navigation of its planetary and extra-orbital spacecraft.[55] Instrumental to the navigation of many NASA deep space probes, data from this telescope is responsible for NASA JPL's successful 2005 navigation-to-landing of the Huygens Lander on Titan, a major moon orbiting Saturn, and provided navigational reference for NASA's New Horizons deep space mission to Pluto, which arrived in July 2015. FASTT was also used to help NASA's SOFIA Airborne Observatory correctly locate, track and image a rare Pluto occultation.[56] FASTT is located 150 yards (140 meters) southwest of the primary complex. Attached to its large "hut" is the building housing NOFS' electronics and electrical engineering laboratories and clean rooms, where most of the advanced camera electronics, cryogenics and telescope control drives are developed and made.

NOFS operates the Navy Precision Optical Interferometer (NPOI)[57][58][59] in collaboration with Lowell Observatory and the Naval Research Laboratory at Anderson Mesa, 15 miles (24 km) south-east of Flagstaff. NOFS (the operational astrometric arm of USNO) funds all principle operations, and from this contracts Lowell Observatory to maintain the Anderson Mesa facility and make the observations necessary for NOFS to conduct the primary astrometric science. The Naval Research Laboratory (NRL) also provides additional funds to contract Lowell Observatory's and NRL's implementation of additional, long-baseline siderostat stations, facilitating NRL's primary scientific work, synthetic imaging (both celestial and of orbital satellites). The three institutions – USNO, NRL, and Lowell – each provide an executive to sit on an Operational Advisory Panel (OAP), which collectively guides the science and operations of the interferometer. The OAP commissioned the chief scientist and director of the NPOI to effect the science and operations for the Panel; this manager is a senior member of the NOFS staff and reports to the NOFS Director.

NPOI is a successful astronomical interferometer[60] of the venerable and proven Michelson interferometer design. As noted, the majority of interferometric science and operations are funded and managed by NOFS; however, Lowell Observatory and NRL join in the scientific efforts through their fractions of time to use the interferometer; 85% Navy (NOFS and NRL); and 15% Lowell. NPOI is one of the few major instruments globally which can conduct optical interferometry.[60][61] See an illustration of its layout, at bottom. NOFS has used NPOI to conduct a wide and diverse series of scientific studies, beyond just the study of absolute astrometric positions of stars.[62] Additional NOFS science at NPOI includes the study of binary stars, Be stars, oblate stars, rapidly rotating stars, those with starspots, and the imaging of stellar disks (the first in history) and flare stars.[63] In 2007–2008, NRL with NOFS used NPOI to obtain first-ever closure phase image precursors of satellites orbiting in geostationary orbit.[64][65]

NPOI Layout
Navy Precision Optical Interferometer (NPOI) Layout

See also

References

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  2. ↑ George H. Kaplan (2000). A Random Walk Through Astrometry (PDF). Sixth DoD Astrometry Forum – 5–6 December 2000 Washington, DC. Archived (PDF) from the original on 19 March 2012. Retrieved 18 February 2016.
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  6. ↑ "Naval Observatory Flagstaff Station Celebrates First Half Century". SpaceRef (Press release). 30 September 2005. Retrieved 18 October 2011.
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  51. ↑ Ivezić, Ž.; Bond, N.; Jurić, M.; Munn, J.A.; Lupton, R.H.; Pier, J.R. (2005). "Science Results Enabled by SDSS Astrometric Observations". In Seidelmann, P.K.; Monet, A.K.B. (eds.). Astrometry in the Age of the Next Generation of Large Telescopes, ASP Conference Series, Vol. 338, Proceedings of a meeting held 18-20 October 2004 at Lowell Observatory, Flagstaff, Arizona, USA. San Francisco: Astronomical Society of the Pacific. p. 201. arXiv:astro-ph/0701502. Bibcode:2005ASPC..338..201I. Archived from the original on 16 January 2016. Retrieved 11 May 2011.
  52. ↑ "The 1.0-m Ritchey-Chretien Reflector". United States Naval Observatory's Flagstaff Station. Archived from the original on 28 July 2011. Retrieved 18 October 2011.
  53. ↑ "The 0.2-m (8-inch) FASTT". United States Naval Observatory's Flagstaff Station. Archived from the original on 1 November 2008. Retrieved 18 October 2011.
  54. ↑ R.C. Stone; D.G. Monet; A.K.B. Monet; F.H. Harris; H.D. Ables; C.C. Dahn; B. Canzian; H.H. Guetter; H.C. Harris; A.A. Henden (2003). "Upgrades to the Flagstaff Astrometric Scanning Transit Telescope: A Fully Automated Telescope for Astrometry". The Astronomical Journal. The American Astronomical Society. 126 (4): 2060–80. Bibcode:2003AJ....126.2060S. doi:10.1086/377622. S2CID 36903369.
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  58. ↑ P.D. Shankland; D.J. Hutter; M.E. DiVittorio; J.A. Benson; R.T. Zavala1; K.J. Johnston (Winter 2010). "The Science with four 1.8-m Telescopes at the Navy Prototype Optical Interferometer" (PDF). BAAS. 215: 441.12. Bibcode:2010AAS...21544112S. Archived from the original (PDF) on 22 February 2012. Retrieved 18 February 2016.{{cite journal}}: CS1 maint: numeric names: authors list (link)
  59. ↑ Michael DiVittorio; Donald J. Hutter; Michael Kelley (28 July 2008). "Plans for utilizing the Keck Outrigger Telescopes at NPOI". In Markus Schöller; William C. Danchi; Françoise Delplancke (eds.). Proceedings SPIE 7013, Optical and Infrared Interferometry. SPIE Astronomical Telescopes and Instrumentation, 23–28 June 2008, Marseille, France. doi:10.1117/12.787635. Archived from the original on 30 December 2017. Retrieved 18 October 2011.
  60. 1 2 Armstrong, J. T.; Mozurkewich, D.; Creech-Eakman, M. C.; Akeson, R. L.; Buscher, D. F.; Ragland, S.; Ridgeway, S. T.; Ten Brummelaar, T.; Townes, C. H.; Wishnow, E.; Aufdenberg, J. P.; Baines, E. K.; Bakker, E. J.; Hinz, P.; Hummel, C. A.; Jorgensen, A. M.; Leisawitz, D. T.; Muterspaugh, M. W.; Schmitt, H. R.; Restaino, S. R.; Tycner, C.; Yoon, J. (2009). "Ground-based Optical/Infrared Interferometry: High Resolution, High Precision Imaging". Astro2010: The Astronomy and Astrophysics Decadal Survey. Vol. 2010. p. 27. Bibcode:2009astro2010T..27A.
  61. ↑ Andreas Quirrenbach (2001). "Optical Interferometry" (PDF). Annu. Rev. Astron. Astrophys. Annual Reviews. 39: 353–401. Bibcode:2001ARA&A..39..353Q. doi:10.1146/annurev.astro.39.1.353. Archived from the original (PDF) on 23 March 2012. Retrieved 14 November 2013.
  62. ↑ Hutter, D.J.; Benson, J.A.; DiVittorio, M.; Shankland, P.D.; Zavala, R.T.; Johnston, K.J. (May 2009). "Large-Angle Astrometry at the Navy Prototype Optical Interferometer (NPOI)". Bulletin of the American Astronomical Society. American Astronomical Society. 41: 675. Bibcode:2009AAS...21441102H.
  63. ↑ "Staff Publications". Archived from the original on 8 August 2014. Retrieved 18 February 2016.
  64. ↑ F.J. Vrba; M.E. DiVittorio; R.B. Hindsley; H.R. Schmitt; J.T. Armstrong; P.D. Shankland; D.J. Hutter; J.A. Benson. "A Survey of Geosynchronous Satellite Glints" (PDF). Advanced Maui Optical and Space Surveillance Technologies (AMOS) Conference. Archived (PDF) from the original on 3 September 2011. Retrieved 14 November 2013.
  65. ↑ A.M. Jorgensen; E.J. Bakker; G.C. Loos; D. Westpfahl; J.T. Armstrong; R.L. Hindsley; H.R. Schmitt; S.R. Restaino. "Satellite Imaging and Characterization with Optical Interferometry" (PDF). Advanced Maui Optical and Space Surveillance Technologies (AMOS) Conference. Archived (PDF) from the original on 3 September 2011. Retrieved 14 November 2013.
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