ERRATUM: “THE SKY BRIGHTNESS AND TRANSPARENCY IN<i>i</i>-BAND AT DOME A, ANTARCTICA” (2010, AJ, 140, 602)

Zou, Hu; Zhou, Xu; Jiang, Zhaoji; Ashley, M. C. B.; Cui, Xiangqun; Feng, Longlong; Gong, Xiaoli; Hu, Jingyao; Kulesa, C. A.; Lawrence, Jon; Liu, Genrong; Luong-Van, D.; Ma, Jun; Moore, Anna; Pennypacker, C. R.; Qin, W.; Shang, Zhaohui; Storey, J. W. V.; Sun, Bo; Travouillon, Tony; Walker, C. K.; Wang, Jiali; Wang, Lifan; Wu, Jianghua; Wu, Zhaoyang; Xia, Lirong; Yan, Jun; Yang, Ji; Yang, Huigen; Yao, Yongqiang; Yuan, Xiangyan; York, Donald G.; Zhang, Zhanhai; Zhu, Zhenxi

doi:10.1088/0004-6256/140/6/2146

Cited by 23 publications

(47 citation statements)

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“…For instance, the median seeing measured at the ground surface at Dome C is about 2 (Aristidi et al 2009). On the other hand, the sky background in these examples is about 19.5 mag arcsec −2 and would be one mag darker in a moonless polar night (Zou et al 2010), which AST3-1 observations did not sample as a result of the power supply problem in early May 2012. Consequently, we infer that AST3 is able to approach a depth of i ∼ 20 in a 60 s exposure during dark nights under seeing-limited conditions within the turbulent boundary layer.…”

Section: Photometric Accuracymentioning

confidence: 85%

The first release of the AST3-1 Point Source Catalogue from Dome A, Antarctica

Shang

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The three Antarctic Survey Telescopes (AST3) aim to carry out time domain imaging survey at Dome A, Antarctica. The first of the three telescopes (AST3-1) was successfully deployed on January 2012. AST3-1 is a 500 mm aperture modified Schmidt telescope with a 680 mm diameter primary mirror. AST3-1 is equipped with a SDSS i filter and a 10k × 10k frame transfer CCD camera, reduced to 5k × 10k by electronic shuttering, resulting in a 4.3 deg 2 field-of-view. To verify the capability of AST3-1 for a variety of science goals, extensive commissioning was carried out between March and May 2012. The commissioning included a survey covering 2000 deg 2 as well as the entire Large and Small Magellanic Clouds. Frequent repeated images were made of the center of the Large Magellanic Cloud, a selected exoplanet transit field, and fields including some Wolf-Rayet stars. Here we present the data reduction and photometric measurements of the point sources observed by AST3-1. We have achieved

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Section: Photometric Accuracymentioning

confidence: 85%

The first release of the AST3-1 Point Source Catalogue from Dome A, Antarctica

Shang

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…It is a great opportunity and yet a tremendous challenge in technology and implementation. So far many endeavors have been undertaken and it is worth mentioning some works like the first catalog released by Zhou et al (2010a) and sky brightness and transparency analysis by Zou et al (2010). Recently, the photometric precision has been twice improved by Wang et al (2012Wang et al ( , 2013 after considering the inhomogeneous effect of cloud cover and diurnal effect.…”

Section: Introductionmentioning

confidence: 99%

Ghost Image Correction in CSTAR Photometry

Meng

Zhang

et al. 2013

Publications of the Astronomical Society of the Pacific

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During the Polar Night of 2008 at Dome A site (Antarctica), the Chinese Small Telescope ARray (CSTAR) gathered i-band photometric information (a total of over 300,000 images) of the 20 deg 2 sky vicinity around the South Pole automatically and continuously. Within all the acquired images, we carry out an elaborate series of analyses and study the origin and influence of the ghost images in each frame. The point source catalog has also been amended by removing the ghost image effects from the real overlapped stars. This work provides a generalized ghost reduction pipeline and improves the photometric precision of the stars in the CSTAR FOV for the future search for transiting exoplanets.

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“…The CSTAR data have already been successfully used to test the site characteristics of Dome A (Zou et al 2010), for detection of the variable stars (Wang et al 2011), and to study the stability of the snow surface of Dome A.…”

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confidence: 99%

“…4). Dome A has a darker sky background than the other Antarctic astronomical sites, even allowing for calibration and other uncertainties of up to several tenths of a magnitude (Zou et al 2010).…”

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Progress and Results from the Chinese Small Telescope ARray (CSTAR)

Ashley

Cui

et al. 2012

Proc. IAU

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In 2008 January the 24th Chinese expedition team successfully deployed the Chinese Small Telescope ARray (CSTAR) to Dome A, the highest point on the Antarctic plateau. CSTAR consists of four 14.5 cm optical telescopes, each with a different filter (g, r, i and open) and has a 4.5 • × 4.5 • field of view (FOV). Based on the CSTAR data, initial statistics of astronomical observational site quality and light curves of variable objects were obtained. To reach higher photometric quality, we are continuing to work to overcome the effects of uneven cirrus cloud cirrus, optical "ghosts" and intra-pixel sensitivity. The snow surface stability is also tested for further astronomical observational instrument and for glaciology studies.Due to the extremely cold, dry, calm, thin atmosphere and the absence of light and air pollution, we can obtain a low infrared background, new observation windows, and high quality photometric images from the Antarctic Plateau (Burton 2010). Over the long polar night, the observation of high quality, long-baseline uninterrupted time-series 231

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ERRATUM: “THE SKY BRIGHTNESS AND TRANSPARENCY INi-BAND AT DOME A, ANTARCTICA” (2010, AJ, 140, 602)

Cited by 23 publications

References 0 publications

The first release of the AST3-1 Point Source Catalogue from Dome A, Antarctica

The first release of the AST3-1 Point Source Catalogue from Dome A, Antarctica

Ghost Image Correction in CSTAR Photometry

Progress and Results from the Chinese Small Telescope ARray (CSTAR)

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