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- ID:
- ivo://tohoku.univ.jp/__system__/services/registry
- Title:
- Tohoku University VO Server Registry
- Short Name:
- Tohoku Reg
- Date:
- 22 Jan 2023 00:00:06
- Publisher:
- The staff at the Tohoku University VO Server
- Description:
- The publishing registry for the Tohoku University VO Server.
- ID:
- ivo://tohoku.univ.jp/tap
- Title:
- Tohoku University VO Server TAP service
- Short Name:
- Tohoku TAP
- Date:
- 23 May 2017 13:26:14
- Publisher:
- Tohoku University
- Description:
- The Tohoku University VO Server'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: epn_core from the iitatehf schema, columns, groups, key_columns, keys, schemas, tables from the tap_schema schema, epn_core from the iprt schema, epn_core from the irtf_cshell schema, epn_core from the hisaki schema, epn_core from the sw_model schema, emptyobscore, obscore from the ivoa schema.
- ID:
- ivo://CDS.VizieR/J/AJ/153/258
- Title:
- 2007.5 to 2010.4 HST astrometry of HD 202206
- Short Name:
- J/AJ/153/258
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using Hubble Space Telescope Fine Guidance Sensor astrometry and previously published radial velocity measures, we explore the exoplanetary system HD202206. Our modeling results in a parallax, {pi}_abs_=21.96+/-0.12 milliseconds of arc, a mass for HD202206B of M_B_=0.089_-0.006_^+0.007M_{Sun}_, and a mass for HD202206c of M_c_=17.9_-1.8_^+2.9^M_Jup_. HD202206 is a nearly face-on G + M binary orbited by a brown dwarf. The system architecture that we determine supports past assertions that stability requires a 5:1 mean motion resonance (we find a period ratio, P_c_/P_B_=4.92+/-0.04) and coplanarity (we find a mutual inclination, {Phi}=6{deg}+/-2{deg}).
22305. TOI-269 b light curves
- ID:
- ivo://CDS.VizieR/J/A+A/650/A145
- Title:
- TOI-269 b light curves
- Short Name:
- J/A+A/650/A145
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We present the confirmation of a new sub-Neptune close to the transition between Super-Earths and sub-Neptunes transiting the M2 dwarf TOI-269. The exoplanet candidate is identified in multiple TESS sectors and is validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determine mass, radius and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P=3.7 days, a radius of 2.77+/-0.12R_{Earth}_, and a mass of 8.8+/-1.4M_{Earth}_. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e=0.425^+0.082^_-0.086_, TOI-269 b has one of the highest eccentricity among exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired a high eccentricity as it migrated inward through planet-planet interactions.
- ID:
- ivo://CDS.VizieR/J/AJ/160/22
- Title:
- TOI-1235 Radial velocities & optical spectroscopy
- Short Name:
- J/AJ/160/22
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period-radius space. Here we present the confirmation of TOI-1235b (P=3.44days, r_p_=1.738_-0.076_^+0.087^R_{Earth}_), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (R_s_=0.630{+/-}0.015R_{sun}_, M_s_=0.640{+/-}0.016M_{sun}_). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high- resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of 6.91_-0.85_^+0.75^M_{Earth}_, which implies an iron core mass fraction of 20_-12_^+15^% in the absence of a gaseous envelope. The bulk composition of TOI-1235b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be <0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin (P=21.8_-0.8_^+0.9^days, m_p_sini=13.0_-5.3_^+3.8^M_{Earth}_) that cannot be firmly ruled out by our data.
- ID:
- ivo://CDS.VizieR/J/A+A/656/A124
- Title:
- TOI-1201 RV and activity index
- Short Name:
- J/A+A/656/A124
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf (J~9.5mag, ~600-800Myr) in an equal-mass ~8arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite (TESS), along with follow-up transit observations. With an orbital period of 2.49d, TOI-1201~b is a warm mini-Neptune with a radius of R_b_=2.415+/-0.090R_{Earth}_. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of M_b_=6.28+/-0.88M_{Earth}_ and, thus, an estimated bulk density of 2.45^+0.48^_-0.42_g/cm^3^. The spectroscopic observations additionally show evidence of a signal with a period of 19d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19d signal to the stellar rotation period (P_rot_=19-23d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is an excellent target for atmosphere characterization (the transmission spectroscopy metric is 97^+21^_-16_) with the upcoming James Webb Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision.
- ID:
- ivo://CDS.VizieR/J/A+A/649/A26
- Title:
- TOI-178 six transiting planets
- Short Name:
- J/A+A/649/A26
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152_-0.070_^+0.073^ to 2.87_-0.13_^+0.14^ Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71-days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02^+0.28^_-0.23_ to 0.177^+0.055^_-0.061_ times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H=8.76mag, J=9.37mag, V=11.95mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.
- ID:
- ivo://CDS.VizieR/I/249
- Title:
- Tokyo meridian circle catalog of O-B stars
- Short Name:
- I/249
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A catalog of the O-B stars, selected from "Blaauw-Parenago" list (1955, First IAU Symposium, "Co-ordination of galactic research") and Rubin's catalog (1962AJ.....67..491R, Cat. <V/31>), has been compiled on the FK4 system by the observations made with Gautier 8-inch Meridian Circle at the Tokyo Astronomical Observatory during the period, 1971 to 1979. It contains 1059 stars and was compiled for the future establishment of high precision proper motions of O-B stars.
- ID:
- ivo://CDS.VizieR/I/198
- Title:
- Tokyo Photoelectric Meridian Circle Catalog 1989
- Short Name:
- I/198
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The fifth annual catalog of the Tokyo PMC is presented for 3466 stars (Part I and Part II) which were observed at least two times in the 1989 period, that is, from January 1, 1989, to December 31, 1989. The positions of the stars given in the catalog are those at the mean epoch of observations. The coordinates of the catalog are based on the FK5 system, and refer to the equinox and equator of J2000.0. The values of (O-C)s in the catalog are calculated by using the positions given in the source catalog, and by evaluating those at the mean epoch of observations of each star, with the equinox and equator at the mean epoch. The magnitudes of the stars given in the catalog can be transformed into the V-magnitude of the standard UBV system by the equation: V = V(TPMC) + 0.063 ( B-V ) - 0.045. The mean trends of the observed positions-FK5 positions for the basic FK5 stars are constructed and compared with those of the Tokyo PMC Catalogs 86, 87, and 88. The Part I of the catalog contains the positions of 1080 basic FK5 stars, 210 FK4 Suppl. stars, 1700 AGK3R stars, 131 OB stars, 36 NPZT stars, and 96 SAO stars, observed with the Tokyo PMC in the 1989 period based on FK5 system. The Part II of the catalog contains the positions of 210 zodiacal stars observed with the Tokyo PMC in the 1989 period based on the FK5 system. The stars of the Part II are usable for the reduction of lunar occultation. The Parts I and II are concatenated to form a single machine-readable catalog.
