192 research outputs found
Photometric Variability in the CSTAR Field: Results From the 2008 Data Set
The Chinese Small Telescope ARray (CSTAR) is the first telescope facility
built at Dome A, Antarctica. During the 2008 observing season, the installation
provided long-baseline and high-cadence photometric observations in the i-band
for 18,145 targets within 20 deg2 CSTAR field around the South Celestial Pole
for the purpose of monitoring the astronomical observing quality of Dome A and
detecting various types of photometric variability. Using sensitive and robust
detection methods, we discover 274 potential variables from this data set, 83
of which are new discoveries. We characterize most of them, providing the
periods, amplitudes and classes of variability. The catalog of all these
variables is presented along with the discussion of their statistical
properties.Comment: 38 pages, 11 figures, 4 tables; Accepted for publication in ApJ
Do I-Pass for FAIR?:A self-assessment tool to measure the FAIR-ness of an organization
The 15 FAIR data principles are intended to be applied to a dataset, but the acronym FAIR is also used as an adjective for other (digital) matters, such as FAIR data stewardship, FAIR data infrastructure and FAIR data services. Moreover, in the context of Open Science and scientific integrity, more and more Dutch universities and research organizations discuss a FAIR organization as an important goal, thus implementing RDM practices and support with the FAIR principles as a main driver.
Triggered by this use of the acronym FAIR for organizations, an LCRDM (National Coordination Point Research Data Management) task group explored the definition, characteristics and principles of a so-called ‘FAIR enabling organization’. The task group delivered two products: (1) a definition for a FAIR enabling organization and (2) a self-assessment tool to evaluate the FAIR-ness of a research organization (research institute, university or university of applied sciences).
This self-assessment tool is a simple instrument, presented in an editable PDF form. By answering the questions and evaluating the level (beginner, intermediate, or advanced) at which you assess the performance of your organization, you will be able to define the actual FAIR-ness. In addition you can define a Road Map to become a FAIR Enabling Research Organization using the information in de more advances level(s)
Eclipsing Binaries From the CSTAR Project at Dome A, Antarctica
The Chinese Small Telescope ARray (CSTAR) has observed an area around the
Celestial South Pole at Dome A since 2008. About light curves in the i
band were obtained lasting from March to July, 2008. The photometric precision
achieves about 4 mmag at i = 7.5 and 20 mmag at i = 12 within a 30 s exposure
time. These light curves are analyzed using Lomb--Scargle, Phase Dispersion
Minimization, and Box Least Squares methods to search for periodic signals.
False positives may appear as a variable signature caused by contaminating
stars and the observation mode of CSTAR. Therefore the period and position of
each variable candidate are checked to eliminate false positives. Eclipsing
binaries are removed by visual inspection, frequency spectrum analysis and
locally linear embedding technique. We identify 53 eclipsing binaries in the
field of view of CSTAR, containing 24 detached binaries, 8 semi-detached
binaries, 18 contact binaries, and 3 ellipsoidal variables. To derive the
parameters of these binaries, we use the Eclipsing Binaries via Artificial
Intelligence (EBAI) method. The primary and the secondary eclipse timing
variations (ETVs) for semi-detached and contact systems are analyzed.
Correlated primary and secondary ETVs confirmed by false alarm tests may
indicate an unseen perturbing companion. Through ETV analysis, we identify two
triple systems (CSTAR J084612.64-883342.9 and CSTAR J220502.55-895206.7). The
orbital parameters of the third body in CSTAR J220502.55-895206.7 are derived
using a simple dynamical model.Comment: 41 pages, 12 figures; published online in ApJ
The First Release of the CSTAR Point Source Catalog from Dome A, Antarctica
In 2008 January the 24th Chinese expedition team successfully deployed the
Chinese Small Telescope ARray (CSTAR) to DomeA, the highest point on the
Antarctic plateau. CSTAR consists of four 14.5cm optical telescopes, each with
a different filter (g, r, i and open) and has a 4.5degree x 4.5degree field of
view (FOV). It operates robotically as part of the Plateau Observatory, PLATO,
with each telescope taking an image every 30 seconds throughout the year
whenever it is dark. During 2008, CSTAR #1 performed almost flawlessly,
acquiring more than 0.3 million i-band images for a total integration time of
1728 hours during 158 days of observations. For each image taken under good sky
conditions, more than 10,000 sources down to 16 mag could be detected. We
performed aperture photometry on all the sources in the field to create the
catalog described herein. Since CSTAR has a fixed pointing centered on the
South Celestial Pole (Dec =-90 degree), all the sources within the FOV of CSTAR
were monitored continuously for several months. The photometric catalog can be
used for studying any variability in these sources, and for the discovery of
transient sources such as supernovae, gamma-ray bursts and minor planets.Comment: 1 latex file and 9 figures The paper is accepted by PAS
The sky brightness and transparency in i-band at Dome A, Antarctica
The i-band observing conditions at Dome A on the Antarctic plateau have been
investigated using data acquired during 2008 with the Chinese Small Telescope
ARray. The sky brightness, variations in atmospheric transparency, cloud cover,
and the presence of aurorae are obtained from these images. The median sky
brightness of moonless clear nights is 20.5 mag arcsec^{-2} in the SDSS
band at the South Celestial Pole (which includes a contribution of about 0.06
mag from diffuse Galactic light). The median over all Moon phases in the
Antarctic winter is about 19.8 mag arcsec^{-2}. There were no thick clouds in
2008. We model contributions of the Sun and the Moon to the sky background to
obtain the relationship between the sky brightness and transparency. Aurorae
are identified by comparing the observed sky brightness to the sky brightness
expected from this model. About 2% of the images are affected by relatively
strong aurorae.Comment: There are 1 Latex file and 14 figures accepted by A
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