Exceptional Terahertz Transparency and Stability above Dome A, Antarctica

Yang, Huigen; Kulesa, Craig; Walker, Christopher K.; Tothill, N.; Yang, Ji; Ashley, M. C. B.; Cui, Xiangqun; Li, Feng; Lawrence, Jon; Luong-Van, D.; McCaughrean, M. J.; Storey, J. W. V.; Wang, Lifan; Zhou, Xu; Zhu, Zhenxi

doi:10.1086/652276

Cited by 66 publications

(30 citation statements)

References 19 publications

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“…The Antarctic plateau offers a number of unique advantages for precision, ground-based, time-domain as-tronomy, such as the ability to observe continuously during winter, low scintillation noise, excellent seeing above a very low boundary layer, low airmass variations, low aerosols, low water vapor, more stable atmospheric transmission, wider wavelength windows, and a dark sky in the infrared (Lawrence et al 2004(Lawrence et al , 2006(Lawrence et al , 2008Moore et al 2008;Kulesa et al 2008;Aristidi et al 2009;Burton 2010;Zou et al 2010;Yang et al 2010;Sims et al 2010;Bonner et al 2010;Lascaux et al 2011;Tremblin et al 2011;Pei et al 2011Pei et al , 2012Sims et al 2012a,b;Giordano et al 2012;Storey 2013;Hu et al 2014;Ashley 2013;Yang et al 2016). There is thus considerable interest in overcoming the technical challenges of operating in Antarctica, so that the advantages for astronomy can be realized (Tothill et al 2008;Kulesa et al 2008;Crouzet et al 2010;Chapellier et al 2016;Mékarnia et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

Wang

et al. 2017

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AST3-1 is the second-generation wide-field optical photometric telescope dedicated to time domain astronomy at Dome A, Antarctica. Here we present the results of i band images survey from AST3-1 towards one Galactic disk field. Based on time-series photometry of 92,583 stars, 560 variable stars were detected with i magnitude ≤ 16.5 mag during eight days of observations; 339 of these are previously unknown variables. We tentatively classify the 560 variables as 285 eclipsing binaries (EW, EB, EA), 27 pulsating variable stars (δ Scuti, γ Doradus, δ Cephei variable and RR Lyrae stars) and 248 other types of variables (unclassified periodic, multi-periodic and aperiodic variable stars). Among the eclipsing binaries, 34 show O'Connell effects. One of the aperiodic variables shows a plateau light curve and another one shows a secondary maximum after peak brightness. We also detected a complex binary system with RS CVn-like light curve morphology; this object is being followed-up spectroscopically using the Gemini South telescope.

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Section: Introductionmentioning

confidence: 99%

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

Wang

et al. 2017

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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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“…However, these SN type Ia standard candles are more accurate when measured in the near-IR than in the optical (Barone-Nugent et al, 2012). Improved measurements of the distance scale All parameters quoted from the literature (Zhou et al, 2010b;Yang et al, 2010;Bonner et al, 2010). …”

Section: Supernovae and The Expansion Of The Universementioning

confidence: 99%

Astronomy From the High Antarctic Plateau

Burton¹,

Yang²,

Ichikawa³

2015

Publications of The Korean Astronomical Society

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The Antarctic high plateau offers exceptional conditions for infrared and terahertz astronomy, as well as for programs requiring long, uninterrupted periods for measurements made with high cadence and photometric precision (i.e. time domain astronomy). In this review we summarise the special conditions of the Antarctic plateau which facilitate these observing regimes. We also outline some high profile science programs in each that could be conducted most effectively from the Antarctic high plateau, involving the first light in the Universe, the life cycle of our Galaxy, and the equation of state for the Universe. Three high plateau sites are under particular consideration for furthering such scientific programs-Dome A, Dome F and Ridge A. We summarise the activity underway at each site, which includes the building of new stations and the construction of facilities for optical, infrared and terahertz astronomy, as well as the plans for their future development.

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Exceptional Terahertz Transparency and Stability above Dome A, Antarctica

Cited by 66 publications

References 19 publications

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

Worldwide site comparison for submillimetre astronomy

Astronomy From the High Antarctic Plateau

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