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Entry ID: CN_NADC_2015_Antarctic_2015_AST3-2_Antarctic_Survey_Telescope
Publish Date: 2016-10-12
Author:
Keywords: Antarctic astronomy, variable detection, Antarctic wide field surveys, AST-2, Antarctic
Dataset: Files(0) Filesize(0 字节)
Summary: Antarctic Schmidt Telescopes (AST3) is a trio of 50-cm optical telescopes. A platform to supply power and connectivity is being installed at Dome A, and the telescopes will be transported and set up starting in the next Antarctic summer; Kunlun station, the base of operations at Dome A, is not yet habitable year-round. The three independent, remotely controlled telescopes will be used to study variable objects, such as supernova explosions and the afterglow of gamma-ray bursts, and to search for extrasolar planets.
Entry ID: CN_NADC_2015_Dome-A_Dome-A_Young_41342_Thermometer_Description
Publish Date: 2016-06-07
Author: Hu Yi
Keywords: Automatic Weather Station, Astronomical seeing, Site Condition, site testing, Atmospheric Properties
Location: Dome-A
Dataset: Files(2) Filesize(130.1 MB)
Summary: The second generation Kunlun Automated Weather Station (KLAWS-2G) for monitoring astronomical site at Dome A has a mast of 15m high. At different heights, there are 10 temperature sensors (-1m, 0m, 1m, 2m, 4m, 6m, 8m, 10m, 12m and 14m), 7 wind speed and direction measurements (2m, 4m, 6m, 8m, 10m, 12m, and 14m), one pressure measurement (2m), and one relative humidity measurement (2m). Temperature is measured with Young 4-wire RTD (Model 41342). Wind speed and direction are measured with propeller anemometers (Young Wind Monitor-AQ model 05305V). Air pressure is measured with barometric pressure sensor (Young Model 61302V). Relative humidity is measured with a relative-humidity/temperature probe (Young Model 41382VC). The customized electronic box of KLAWS-2G sits at the foot of the mast with an active thermal control system to keep it at working temperature. The KLAWS-2G is connected to PLATO-A for power and real-time data transfer via Iridium satellites. According to the manuals from Young company, uncertainty on all temperature measurements is 0.32 Degrees Celsius (but should be more accurate, see Hu et al. 2014, PASP, 126, 686), wind speed error is 0.2m/s, direction error is 0.5 degree (plus installation offset), and pressure error is 15hPa.
Entry ID: CN_NADC_NADC_2015_Dome-A_AST3-2_Description
Publish Date: 2016-06-07
Author: Hu Yi
Keywords: Antarctic astronomy, AST-2, Supernova, Outer planet
Location: Dome-A
Dataset: Files(3) Filesize(162.9 MB)
Summary: AST3-2 Data Sets obtained at Chinese Antarctic Kunlun Station from 24,Mar to 26,April of 2015 ,including the 815GB fits format files and 0.038MB log files.
Entry ID: CN_NADC_2011_Dome-A_Dome-A_Young_Temperature_Young_Wind_Monitor__Young_Barometric_Pressure_Sensor_Description
Publish Date: 2015-09-08
Author: Hu Yi, Shang Zhaohui
Keywords: Dome A, site testing, Automatic Weather Station
Location: Dome A
Dataset: Files(2) Filesize(108.7 MB)
Summary: PRIC-CCAA Kunlun Automatic Weather Station (KL-AWS) has a tower of 15m high. At different heights, there are 9 temperature sensors (-1m, 0m 1m, 2m, 4m, 6m, 9.5m, 12m and14.5m), 4 wind speed and direction measurements (2m, 4m, 9.5m and 14.5m) and one pressure measurement (1m). Temperature is measured with Young 4-wire RTD (Model 41342). Wind speed and direction is measured with 2D sonic anemometers (Young Model 85000), and propeller anemometers (Young Wind Monitor-AQ model 05305V).
Entry ID: CN_NADC_NADC_2009_Dome-A_Antarctica_Nigel
Publish Date: 2011-04-21
Author:
Keywords: spectrometer, sky brightness, aurora, Nigel
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: As part of the 2009 servicing mission of PLATO, Nigel was deployed to Dome A by the Polar Research Institute of China (PRIC). The Nigel instrument is both a site-testing and scientific instrument designed to measure the optical sky brightness and the aurora contributions of the Dome A sky.
Entry ID: CN_NADC_2010-2011_Dome-A_Antarctica_FTS_Description
Publish Date: 2011-04-21
Author:
Keywords: water vapor continuum models, atmospheric transmission, FTS(Dome A Fourier Transform Spectrometer), THz
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: The Dome A FTS was first installed in PLATO at Dome A during January 2010. It is a site survey instrument to evaluate the atmospheric transmission from 0.75 THz to 15 THz. This broad spectral coverage is particularly important at Dome A, where the extremely cold temperatures lie well outside the tested range of water vapor continuum models. The FTS is a polarizing Martin-Puplett interferometer operated in rapid-scan mode. The two output ports of the interferometer are equipped with different detector/filter combinations, providing a high throughput, low frequency band covering 0.75 THz to 3.5 THz, and a lower throughput, high frequency band covering 0.75 THz to 15 THz. The resolution for both bands is 10 GHz. At Dome A, cryogenic cooling of the detectors and calibration loads is not practical due to the large power requirements. Instead, the FTS is equipped with ambient-temperature DLATGS pyroelectric detectors. For calibration, one input port of the interferometer always views a passive reference load on the optics bench, while the second input port alternates between the sky and a second movable passive reference load at outdoor ambient temperature. A complete measurement cycle on load and sky takes 10 minutes. The interferometer subsystem and detectors were built to specification by Blue Sky Spectroscopy of Lethbridge, Canada, and QMC Instruments in the UK. The data acquisition system and outdoor calibration load assembly were produced at Purple Mountain Observatory in Nanjing. The first of two identical instruments was installed at Dome A in January 2010.
Entry ID: CN_NADC_2008_2009_Dome-A_Antarctica_Pre-HEAT_Description
Publish Date: 2011-02-27
Author:
Keywords: site testing, Antarctic astronomy, submillimeter instrumentation, terahertz spectroscopy, heterodyne receiver, interstellar medium, star formation
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: The submillimeter-wave instrument on PLATO is called Pre-HEAT. Its name reflects that it is a prototype for the HEAT (High Elevation Antarctic Terahertz) telescope, a larger, more sophisticated telescope which is targeted for deployment on the 2012 timeframe. Pre-HEAT performed astronomical observations and measured the transparency of the sky above Dome A during 2008 at submillimeter wavelengths using a high frequency heterodyne receiver. The principles behind the operation of Pre-HEAT’s heterodyne receiver are very similar to an ordinary FM radio. However, the Pre-HEAT receiver is many orders of magnitude more sensitive and is operating at frequencies that are 6600 times higher -- 660 GHz, or equivalently 0.66 THz. Pre-HEAT completed its measurements in 2008, during the first year of operation of PLATO. The data showed extraordinarily low values of precipitable water vapour in the atmosphere. See the section on Refereed Publications below. Of the many varied "colors" in the electromagnetic spectrum of light, submillimeter-waves are perhaps the last unexplored frontier. Nestled between traditional radio astronomy and optical/infrared astronomy, the submillimeter part of the spectrum is one of the richest treasure-troves for understanding the cold gas in galaxies that gives rise to the formation of stars and planets. On a larger scale, distant galaxies give off prodigious amounts of thermal energy at submillimeter wavelengths. It is possible that the oldest and most distant galaxies in the Universe will be detected at submillimeter wavelengths. The submillimeter-wave Universe has gone mostly unexplored because of the difficulty of instrumentation, and the fact that even minute traces of water vapor in the air absorb submillimeter light from space before reaching the ground. Thus, submillimeter-wave telescopes must be placed on the highest, driest sites on the planet. Large telescopes have already been placed on sites like Mauna Kea, Hawaii and (increasingly) on the high plains of the Atacama desert in northern Chile. However, because cold air holds less water vapor than warm air, expectations are that the high plateau of Antarctica will be even better, due to the extreme conditions which prevail there. This was the motivation for building the prototype Pre-HEAT telescope for PLATO.
Entry ID: CN_NADC_NADC_2010_Dome-A_Dome-A_Snodar
Publish Date: 2011-02-27
Author:
Keywords: Antarctic, Atmospheric boundary layer, site testing, Antarctic astronomy, SODAR
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: A new site-testing instrument, Snodar (Surface layer NOn-Doppler Acoustic Radar), is designed to measure the height and intensity of the atmospheric boundary layer on the Antarctic plateau. The nature of the atmospheric boundary layer above the Antarctic plateau is of interest both to atmospheric scientists and to astronomers wishing to plan future optical telescopes. Snodar works by sending an intense acoustic pulse into the atmosphere and listening for backscatter off inhomogeneities resulting from temperature gradients and wind shear. The theory of operation is very similar to that of the well known underwater sounding techniques of SONAR. We obtained a week of data in 2008. In 2009 we deployed a new Snodar and obtained excellent data until August 2009, when snow on the dish reduced the sensitivity. Snodar is again operational and taking data during 2010. Snodar is a monostatic acoustic radar with a minimum sampling height of 5m, a range of at least 200m, a vertical resolution of 1m. Snodar operates at frequencies between 4kHz and 15kHz. Such high frequencies propagate relatively well in the low temperature of the Antarctic atmosphere. Snodar uses a single horn-loaded compression driver as both transmitter and receiver, and an off-axis parabolic dish to collimate the acoustic beam. The signal is acquired using a USB sound card. A PC/104 computer performs the signal processing in real time. Snodar runs autonomously, storing raw data on USB flash disks for retrieval the following summer, while uploading processed data via the Iridium satellite network. The Iridium communication also allows Snodar to be remotely controlled.
Entry ID: CN_NADC_2012_Dome-A_Antarctic_AST3_Description
Publish Date: 2014-05-16
Author:
Keywords: site testing, Antarctic astronomy, astrometry, astrophysics, Antarctic
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: Antarctic Schmidt Telescopes (AST3) is a trio of 50-cm optical telescopes. A platform to supply power and connectivity is being installed at Dome A, and the telescopes will be transported and set up starting in the next Antarctic summer; Kunlun station, the base of operations at Dome A, is not yet habitable year-round. The three independent, remotely controlled telescopes will be used to study variable objects, such as supernova explosions and the afterglow of gamma-ray bursts, and to search for extrasolar planets.
Entry ID: CN_NADC_NADC_NADC_2008-2011_Dome-A_Antarctica
Publish Date: 2011-04-21
Author:
Keywords: Chinese small telescope array (CSTAR), variable detection, continuous observation, Dome A
Location: Dome A
Dataset: Files(0) Filesize(0 字节)
Summary: CSTAR (Chinese Small Telescope ARray) is composed of four identical telescopes with an entrance aperture 145 mm and a 4.5° × 4.5° field of view. Each telescope observes through a different filter: either g, r, i or open. The main science goals of CSTAR are observations of variable stars, and to do measurements of atmosphere extinction and sky brightness. Data is available by offline.