We identify a set of planetary systems observed by Kepler that merit transit-timing variation (TTV) analysis given the orbital periods of transiting planets, the uncertainties for their transit times, and the number of transits observed during the Kepler mission. We confirm the planetary nature of four Kepler Objects of Interest within multicandidate systems. We forward-model each of the planetary systems identified to determine which systems are likely to yield mass constraints that may be significantly improved upon with follow-up transit observations. We find projected TTVs diverge by more than 90 minutes after 6000 days in 27 systems, including 22 planets with orbital periods exceeding 25 days. Such targets would benefit the most from additional transit-timing data. TTV follow-up could push exoplanet characterization to lower masses, at greater orbital periods and at cooler equilibrium temperatures than is currently possible from the Kepler data set alone. Combining TTVs and recently revised stellar parameters, we characterize an ensemble of homogeneously selected planets and identify planets in the Kepler field with large-enough estimated transmission annuli for atmospheric characterization with James Webb Space Telescope.
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.
