The Taiwanese-American Occultation Survey (TAOS) project has collected more than a billion photometric measurements since 2005 January. These sky survey data-covering timescales from a fraction of a second to a few hundred days-are a useful source to study stellar variability. A total of 167 star fields, mostly along the ecliptic plane, have been selected for photometric monitoring with the TAOS telescopes. This paper presents our initial analysis of a search for periodic variable stars from the time-series TAOS data on one particular TAOS field, No. 151 (RA=17:30:6.7, DE=27:27:30, J2000), which had been observed over 47 epochs in 2005. A total of 81 candidate variables are identified in the 3deg^2^ field, with magnitudes in the range 8<R<16. On the basis of the periodicity and shape of the light curves, 29 variables, 15 of which were previously unknown, are classified as RR Lyrae, Cepheid, delta Scuti, SX Phonencis, semi-regular, and eclipsing binaries.
This draft standard describes a means to present usage examples for
TAP services in a way that is partially machine readable while
primarily being consumable by humans. This is now part of DALI;
identifiers created as fragments into this record are invalid and must
now point to fragments of http://www.ivoa.net/rdf/examples.
The 4XMM-DR14 catalogue contains source detections drawn from 13864 XMM-Newton EPIC observations,
covering an energy interval from 0.2 keV to 12 keV.
These observations were made between 2000 February 3 and 2023 December 31 and all datasets
were publicly available by 2023 December 31, but not all public observations are included i
n this catalogue.
The median flux in the total photon energy band (0.2 - 12 keV) of the catalogue detections
is ~ 2.2 × 10-14 erg cm-2 s-1; in the soft energy band (0.2 - 2 keV) the median flux
is ~ 5.2 × 10-15, and in the hard band (2 - 12 keV) it is ~ 1.2 × 10-14.
About 23% of the sources have total fluxes below 1 × 10-14 erg cm-2 s-1.
About a tenth of the observations have features that may cause spurious detections
(mainly the wings of bright sources and large extended emission), and it is strongly
recommended to use a filter (both per source, based on the summary flag column,
and per observation, based on the observation class column).
The TAP server for Konkoly's TAP end point. The Table Access
Protocol (TAP) lets you execute queries against our database tables,
inspect various metadata, and upload your own data. It is thus the
VO's premier way to access public data holdings.
Tables exposed through this endpoint include: columns, groups, key_columns, keys, schemas, tables from the tap_schema schema, epn_core from the sbnaf schema.
TAROT (Telescope a Action Rapide pour les Objets Transitoires) is a robotic observatory designed to observe very early optical transients of gamma-ray bursts (GRBs). As GRBs do not often occur, we use TAROT for various other celestial targets spread over the sky. For every field observed by TAROT, we computed the magnitudes of every star. From this work, we found 1175 new variable stars brighter than 17mag. We selected the best variable star candidates and compiled them in the TSVSC1 (TAROT Suspected Variable Star Catalog, ver. 1), which also contains Fourier-series coefficients that fit the light curves.
The Tartarus database contains the results of a detailed but systematic analysis of ASCA observations of active galactic nuclei (AGN). It contains source and background events files, spectra, ancillary response files and response matrices, images, and assorted light curves for a large number of ASCA AGN observations. Spectral fit results are done by automatic XSPEC fitting. This database table allows easy access to reduced AGN data for the whole community, allowing the maximum scientific return from the data. Availability of publishable light curves, images, and spectra (which can also be readily re-fitted) should be particularly valuable to astronomers with little direct experience in the reduction of X-ray data. Version 3.1 has been created by analyzing all ASCA observing sequences with targets designated as AGN, as indicated by a leading "7" in the ASCA observing sequence number. Version 3.1 contains products for all 611 observing sequences designated as AGN observations. This is a significant improvement over Versions 1 and 2. Moreover, the 611 sequences for which products are available are complete in the sense that either the target object was not detected (in which case an upper limit on GIS2 source counts is given) or the intended AGN target was detected and the data were fully analyzed. In order to obtain the most accurate background subtraction and minimize contamination from any nearby sources, version 3.1 makes more use of custom extraction regions than previous versions. It is expected that version 3.1 will be replaced when the final ASCA calibration is completed. This database table has been created by the Tartarus Team, and they, rather than Imperial College London or the HEASARC, are responsible for the contents. It was ingested by the HEASARC in August, 2005. This is a service provided by NASA HEASARC .
