The 492 GHz Atmospheric Opacity at the Geographic South Pole

Chamberlin, Richard; Lane, Alan M.; Stark, A. A.

doi:10.1086/303621

Cited by 67 publications

(67 citation statements)

References 7 publications

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“…Schneider et al 2009;Tremblin et al 2011;Matsushita et al 1999;Peterson et al 2003) have already shown that a few sites are well-suited to submm/mid-IR, and FIR-astronomy and their transmission properties are rather well determined (for example by Fourier transform spectrometer obervations in the 0.5-1.6 THz range at Mauna Kea/Hawaii; Pardo et al 2001). The high-altitude (>5000 m) Chilean sites are known for dry conditions (see Matsushita et al 1999;Peterson et al 2003), and site testing is now being carried out at the driest place on Earth, Antarctica (see Chamberlin et al 1997;Yang et al 2010;Tremblin et al 2011). Comparisons between Antarctic and Chilean sites are difficult and uncertain since they rely on ground-based instruments that use different methods and calibration techniques (see Peterson et al 2003, for example).…”

Section: Introductionmentioning

confidence: 99%

Worldwide site comparison for submillimetre astronomy

Tremblin¹,

Schneider²,

Minier³

et al. 2012

A&A

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Aims. The most important limitation for ground-based submillimetre (submm) astronomy is the broad-band absorption of the total water vapour in the atmosphere above an observation site, often expressed as the precipitable water vapour (PWV). A long-term statistic on the PWV is thus mandatory to characterize the quality of an existing or potential site for observational submm-astronomy. In this study we present a three-year statistic (2008)(2009)(2010) of the PWV for ground-based telescope sites all around the world and for stratospheric altitudes relevant for SOFIA (Stratospheric Observatory for Far-Infrared Astronomy). The submm-transmission is calculated for typical PWVs using an atmospheric model. Methods. We used data from IASI (Infrared Atmospheric Sounding Interferometer) on the Metop-A satellite to retrieve water vapour profiles for each site (11 in total, comprising Antarctica, Chile, Mauna Kea, Greenland, Tibet). The use of a single instrument to make the comparison provides unbiased data with a common calibration method. The profiles are integrated above the mountain/stratospheric altitude to get an estimation of the PWV. We then applied the atmospheric model MOLIERE (Microwave Observation and LIne Estimation and REtrieval) to compute the corresponding atmospheric absorption for wavelengths between 150 μm and 3 mm. Results. We present the absolute PWV values for each site sorted by year and time percentage. The PWV corresponding to the first decile (10%) and the quartiles (25%, 50%, 75%) are calculated and transmission curves between 150 μm and 3 mm for these values are shown. The Antarctic and South-American sites present very good conditions for submillimetre astronomy. The 350 μm and 450 μm atmospheric windows are open all year long, whereas the 200 μm atmospheric window opens reasonably for 25% of the time in Antarctica and the extremely high-altitude sites in Chile. Potential interesting new facilities are Macon in Argentina and Summit in Greenland, which show similar conditions to for example, Mauna Kea (Hawaii). For SOFIA, we present transmission curves for different altitudes (11 to 14 km), PWV values, and higher frequencies (up to 5 THz) in more detail. Though the atmosphere at these altitude is generally very transparent, the absorption at very high frequencies becomes more important, partly caused by minor species. The method presented in this paper could identify sites on Earth, with great potential for submillimetre astronomy, and guide future site testing campaigns in situ.

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Section: Introductionmentioning

confidence: 99%

Worldwide site comparison for submillimetre astronomy

Tremblin¹,

Schneider²,

Minier³

et al. 2012

A&A

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“…After the first summer measurements (Dragovan et al 1990;Pajot et al 1989) the Antarctic Submillimetre Telescope and Remote Observatory (AST/RO) was installed at the South Pole (Stark et al 2001). However, while the South Pole has indeed proven to be an exceptionally good site (Chamberlin 2001;Chamberlin, Lane, & Stark 1997), other sites on the Antarctic Plateau could provide still better transparencies and lower atmospheric emission and fluctuations at this and at other wavelength regions, as they feature an higher elevation and are located on the top of a dome where katabatic (gravity-driven) winds, and consequently atmospheric turbulence, are expected to be much lower. Among these sites are Dome C (75 • 05 S, 123 • 06 E, alt.…”

Section: Introductionmentioning

confidence: 99%

Submillimeter Site Testing at Dome C, Antarctica

Calisse

Ashley

Burton

et al. 2004

Publ. – Astron. Soc. Aust

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Abstract:We have developed a 350 µm radiometer to perform automated site testing in remote regions of Antarctica. In summer 2000-2001 the instrument operated at Concordia, a new station under construction at Dome C on the Antarctic Plateau. We present the results, and compare them with the atmospheric opacity measured at the South Pole in the same five-week period. During these five weeks, observing conditions at Dome C were, on average, substantially better than those at the South Pole.

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“…Figure 1 shows 5 months of Pre-HEAT submillimeter opacities, demonstrating the exceptional stability and extremely favorable conditions of the site. The seasonal opacity trends echo those seen at the South Pole (Chamberlin et al 1997): the best conditions are typically observed in late winter and early spring, and generally accompany conditions of low atmospheric pressure (550 mbar, a pressure altitude of 4700 m), calm surface winds (denoted by a strong radiative cooling gradient at the surface), and cold surface temperatures (À80°C).…”

Section: Observationsmentioning

confidence: 61%

Exceptional Terahertz Transparency and Stability above Dome A, Antarctica

Yang¹,

Kulesa²,

Walker³

et al. 2010

Publications of the Astronomical Society of the Pacific

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ABSTRACT. We present the first direct measurements of the terahertz atmospheric transmission above Dome A, the highest point on the Antarctic plateau at an elevation of 4.1 km. The best-quartile atmospheric transmission during the Austral winter is 80% at a frequency of 661 GHz (453 μm), corresponding to a precipitable water vapor column of 0.1 mm. Daily averages as low as 0.025 mm were observed. The Antarctic atmosphere is very stable, and excellent observing conditions generally persist for many days at a time. The exceptional conditions over the high Antarctic plateau open new far-infrared spectral windows to ground-based observation. These windows contain important spectral-line diagnostics of star formation and the interstellar medium which would otherwise only be accessible to airborne or space telescopes.

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The 492 GHz Atmospheric Opacity at the Geographic South Pole

Cited by 67 publications

References 7 publications

Worldwide site comparison for submillimetre astronomy

Worldwide site comparison for submillimetre astronomy

Submillimeter Site Testing at Dome C, Antarctica

Exceptional Terahertz Transparency and Stability above Dome A, Antarctica

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