- ID:
- ivo://nasa.heasarc/corotexlog
- Title:
- CoRoT Stellar Targets for Exoplanet Detection Observation Log
- Short Name:
- COROTEXLOG
- Date:
- 09 May 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- CoRoT was a space astronomy mission devoted to the study of the variability with time of stars' brightness, with an extremely high accuracy (100 times better than from the ground), for very long durations (up to 150 days) and with a very high duty cycle (more than 90%). The mission was led by CNES in association with four French laboratories, and 7 participating countries and agencies (Austria, Belgium, Brazil, Germany, Spain, and the ESA Science Programme). The satellite is composed of a PROTEUS platform (the 3rd in the series), and a unique instrument: a stellar photometer. It was launched on December 27th, 2006 on a Soyuz Rocket, from Baikonour. The mission has lasted almost 6 years (the nominal 3 years duration and a 3 years extension) and has observed more than 160,000 stars. It suddenly stopped sending data on November 2nd, 2012. CoRoT performed Ultra High Precision Photometry of Stars to detect and characterize the variability of their luminosity with two main objectives: (i) the variability of the object itself: oscillations, rotation, magnetic activity, etc.; (ii) variability due to external causes such as bodies in orbit around the star: planets and companion stars. The original scientific objectives were focused on the study of stellar pulsations (asteroseismology) to probe the internal structure of stars, and the detection of small exoplanets through their transit in front of their host star, and the measurement of their sizes. This lead to the introduction of two modes of observations, working simultaneously: - The bright star mode dedicated to very precise seismology of a small sample (171) of bright and nearby stars (presented in the file named "Bright_star.dat" in the CDS version at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/corot/">https://cdsarc.cds.unistra.fr/ftp/cats/B/corot/</a>): these data are not included in this HEASARC table, notice; - The faint star mode, observing a very large number of stars at the same time, to detect transits, which are rare events, as they imply the alignment of the star, the planet and the observer (these data are presented in the file named "Faint_star.dat" in the CDS version at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/corot/">https://cdsarc.cds.unistra.fr/ftp/cats/B/corot/</a>): this HEASARC table is based on this sample. The large amount of data gathered in this mode mode turned out to be extremely fruitful for many topics of stellar physics. Due to project constraints, two regions of the sky were accessible (circles of 10 degrees centered on the equator around Right Ascensions of 06<sup>h</sup> 50<sup>m</sup> and 18<sup>h</sup> 50<sup>m</sup>). They are called the CoRoT 'eyes': the first one is called the "anticenter" eye, whereas the second one is called the "center eye". Each pointing covers 1.4 x 2.8 square degrees. The CoRoT project is still processing the data, aiming at removing instrumental artifacts and defects. Therefore the format and content of the catalog is still somewhat evolving. More details on the data can be found in the file <a href="http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/CoRoT_N2_versions_30sept2014.pdf">http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/CoRoT_N2_versions_30sept2014.pdf</a>. More details on the CoRoT N2 data may be found in the documentation file <a href="http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/DescriptionN2v1.5.pdf">http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/DescriptionN2v1.5.pdf</a>. This HEASARC table contains information on stars observed by CoRoT in its exoplanet detection program. A few percent of these stars have 2 entries since they were observed in different windows (as specified by the corot_window_id parameter) in a subsequent observing run to the initial run in which they were observed. Each entry in this table corresponds to the unique specification of target and corot_window_id, each with a link to its associated N2 data products. The original names of the parameters in this table, as given in the CoRoT mission documentation, are given in square brackets at the end of the parameter descriptions listed below. This table was created by the HEASARC in May 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/corot">CDS Catalog B/corot</a> file Faint_star.dat. The HEASARC routinely updates this table after updates are made to the CDS version of this catalog. This is a service provided by NASA HEASARC .
Number of results to display per page
Search Results
4402. CoRoT transit catalogue
- ID:
- ivo://CDS.VizieR/J/A+A/619/A97
- Title:
- CoRoT transit catalogue
- Short Name:
- J/A+A/619/A97
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CoRoT space mission observed 163665 stars over 26 stellar fields in the faint star channel. The exoplanet teams detected a total of 4123 transit-like features in the 177454 light curves. We present the complete re-analysis of all these detections carried out with the same softwares so that to ensure their homogeneous analysis. Although the vetting process involves some human evaluation, it also involves a simple binary flag system over basic tests: detection significance, presence of a secondary, difference between odd and even depths, colour dependence, V-shape transit, and duration of the transit. We also gathered the information from the large accompanying ground-based programme carried out on the planet candidates and checked how useful the flag system could have been at the vetting stage of the candidates. From the initial list of transit-like features, we identified and separated 824 false alarms of various kind, 2269 eclipsing binaries among which 616 are contact binaries and 1653 are detached ones, 37 planets and brown dwarfs, and 557 planet candidates. We provide the catalogue of all these transit-like features, including false alarms. For the planet candidates, the catalogue gives not only their transit parameters but also the products of their light curve modelling: reduced radius, reduced semi-major axis, and impact parameter, together with a summary of the outcome of follow-up observations when carried out and their current status. For the detached eclipsing binaries, the catalogue provides, in addition to their transit parameters, a simple visual classification. Among the planet candidates whose nature remains unresolved, we estimate that eight (within an error of three) planets are still to be identified. After correcting for geometric and sensitivity biases, we derived planet and brown dwarf occurrences and confirm disagreements with Kepler estimates, as previously reported by other authors from the analysis of the first runs: small-size planets with orbital period less than ten days are underabundant by a factor of three in the CoRoT fields whereas giant planets are overabundant by a factor of two. These preliminary results would however deserve further investigations using the recently released CoRoT light curves that are corrected of the various instrumental effects and a homogeneous analysis of the stellar populations observed by the two missions.
- ID:
- ivo://CDS.VizieR/J/ApJ/813/96
- Title:
- CO ro-vibrational transitions
- Short Name:
- J/ApJ/813/96
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present calculated rate coefficients for ro-vibrational transitions of CO in collisions with H atoms for a gas temperature range of 10K<=T<=3000K, based on the recent three-dimensional ab initio H-CO interaction potential of Song et al. (2013JPCA..117.7571S). Rate coefficients for ro-vibrational v=1,j=0-30->v'=0,j' transitions were obtained from scattering cross sections previously computed with the close-coupling (CC) method by Song et al. (2015JChPh.142t4303S). Combining these with the rate coefficients for vibrational v=1-5->v'<v quenching obtained with the infinite-order sudden approximation, we propose a new extrapolation scheme that yields the rate coefficients for ro-vibrational v=2-5,j=0-30->v',j' de-excitation. Cross sections and rate coefficients for ro-vibrational v=2,j=0-30->v'=1,j' transitions calculated with the CC method confirm the effectiveness of this extrapolation scheme. Our calculated and extrapolated rates are very different from those that have been adopted in the modeling of many astrophysical environments. The current work provides the most comprehensive and accurate set of ro-vibrational de-excitation rate coefficients for the astrophysical modeling of the H-CO collision system. The application of the previously available and new data sets in astrophysical slab models shows that the line fluxes typically change by 20%-70% in high temperature environments (800K) with an H/H_2_ ratio of 1; larger changes occur for lower temperatures.
- ID:
- ivo://CDS.VizieR/J/AJ/154/142
- Title:
- Corrected photometry for GJ 1132 for all eclipses
- Short Name:
- J/AJ/154/142
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of a search for additional bodies in the GJ 1132 system through two methods: photometric transits and transit timing variations of GJ 1132b. We collected 21 transit observations of GJ 1132b with the MEarth-South array. We obtained 100 near-continuous hours of observations with the Spitzer Space Telescope, including two transits of GJ 1132b and spanning 60% of the orbital phase of the maximum (6.9-day) period at which bodies coplanar with GJ 1132b would transit. We exclude transits of additional Mars-sized bodies, such as a second planet or a moon, with a confidence of 99.7%. We find that the planet-to-star radius ratio inferred from the MEarth and Spitzer light curves are discrepant at the 3.7{sigma} level, which we ascribe to the effects of starspots and faculae. When we combine the mass estimate of the star (obtained from its parallax and apparent K_s_ band magnitude) with the stellar density inferred from our high-cadence Spitzer light curve (assuming zero eccentricity), we measure the stellar radius of GJ 1132 to be 0.2105_-0.0085_^+0.0102^ R_{sun}_, and we refine the radius measurement of GJ 1132b to 1.130+/-0.056 R_{Earth}_. Combined with HARPS RV measurements, we determine the density of GJ 1132b to be 6.2+/-2.0 g/cm^3^. We refine the ephemeris of the system (improving the period determination by an order of magnitude) and find no evidence for transit timing variations, which would be expected if there was a second planet near an orbital resonance with GJ 1132b.
- ID:
- ivo://CDS.VizieR/J/other/Ser/182.35
- Title:
- Corrected proper motion for HIP stars
- Short Name:
- J/other/Ser/182.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- During the last century, there were many so-called independent latitude (IL) stations with the observations which were included into data of a few international organizations (like Bureau International de l'Heure - BIH, International Polar Motion Service - IPMS) and the Earth rotation programmes for determining the Earth Orientation Parameters - EOP. Because of this, nowadays, there are numerous astrometric ground-based observations (made over many decades) of some stars included in the Hipparcos Catalogue (ESA 1997, Cat. <A HREF="http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/239">I/239</A>). We used these latitude data for the inverse investigations - to improve the proper motions in declination µ<SUB>δ</SUB> of the mentioned Hipparcos stars. We determined the corrections Δµ<SUB>δ</SUB> and investigated agreement of our µ<SUB>δ</SUB> and those from the catalogues Hipparcos and new Hipparcos (van Leeuwen 2007, Cat. <A HREF="http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/311">I/311</A>). To do this we used the latitude variations of 7 stations (Belgrade, Blagoveschtschensk, Irkutsk, Poltava, Pulkovo, Warsaw and Mizusawa), covering different intervals in the period 1904.7-1992.0, obtained with 6 visual and 1 floating zenith telescopes (Mizusawa). On the other hand, with regard that about two decades have elapsed since the Hipparcos ESA mission observations (the epoch of Hipparcos catalogue is 1991.25), the error of apparent places of Hipparcos stars has increased by nearly 20mas because of proper motion errors. Also, the mission lasted less than four years which was not enough for a sufficient accuracy of proper motions of some stars (such as double or multiple ones). Our method of calculation, and the calculated µ<SUB>δ</SUB> for the common IL/Hipparcos stars are presented here. We constructed an IL catalogue of 1200 stars: there are 707 stars in the first part (with at least 20 years of IL observations) and 493 stars in the second one (less than 20 years). In the case of µ<SUB>δ</SUB> of IL stars observed at some stations (Blagoveschtschensk, Irkutsk, Mizusawa, Poltava and Pulkovo) we find the formal errors less than the corresponding Hipparcos ones and for some of them (stations Blagoveschtschensk and Irkutsk) even less than the new Hipparcos ones.
- ID:
- ivo://CDS.VizieR/J/AN/341/770
- Title:
- Corrected proper motion for HIP stars
- Short Name:
- J/AN/341/770
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Independent Latitude Stations (INDLS) catalog of proper motion in declination {mu}_{delta}_ for 682 bright Hipparcos (HIP) stars is presented. It is obtained in the Hipparcos reference frame, and only the Hipparcos mean position at epoch 1991.25 is used for INDLS data to calculate independent {mu}_{delta}$ (the HIP {mu}_{delta}_ values are not entering the INDLS data). Catalog comparisons were made in pairs for the four catalogs (HIP, new Hipparcos -- NHIP, Gaia DR2, INDLS) to look for possible systematic differences as a function of brightness, color, position coordinates ({alpha}, {delta}). All catalogs were found in agreement, except: 0.21mas/yr for differences INDLS-DR2 in line with the brightness, -0.13mas/yr and 0.24mas/yr for differences HIP-DR2 in line with the free term and brightness respectively, -0.16mas/yr, 0.23mas/yr and 0.13mas/yr for differences NHIP$-$DR2 in line with the free term, brightness and color respectively. A slightly better consistency is in the cases INDLS-NHIP and INDLS-DR2 than HIP-DR2 and NHIP-DR2. The systematic error is in line with brightness on the level 0.1mas/yr in DR2, and near 0.1mas/yr in line with color. An indication that the bright reference frame of DR2 rotates by about 0.1mas/yr relative to the faint quasar frame is in line with a presented sinusoidal curve of differences {mu}_{delta}_ as a function of {alpha}. Its amplitude is A=0.53+/-0.11mas/yr for INDLS-DR2 (0.26+/-0.07 for INDLS-NHIP); about 0.2 belongs to DR2. The level of formal errors is near 1.9mas/yr for the case INDLS-DR2, and near 1.5 for: INDLS-NHIP, HIP-DR2, NHIP-DR2. The values {mu}_{delta}_ of bright DR2 stars could be underestimated; the astrometry is unreliable for G<=6mag due to detector saturation.
- ID:
- ivo://CDS.VizieR/J/AN/350/789
- Title:
- Corrected proper motion for HIP stars (Damljanovic, 2020)
- Short Name:
- J/AN/350/789
- Date:
- 21 Jul 2020 05:54:18
- Publisher:
- CDS
- Description:
- The INDLS catalog of for 682 bright stars is presented.
- ID:
- ivo://CDS.VizieR/J/MNRAS/465/2120
- Title:
- Correcting CIV-based virial black hole masses
- Short Name:
- J/MNRAS/465/2120
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CIV{lambda}{lambda}1498,1501 broad emission line is visible in optical spectra to redshifts exceeding z~5. CIV has long been known to exhibit significant displacements to the blue and these 'blueshifts' almost certainly signal the presence of strong outflows. As a consequence, single-epoch virial black hole (BH) mass estimates derived from CIV velocity widths are known to be systematically biased compared to masses from the hydrogen Balmer lines. Using a large sample of 230 high-luminosity (L_Bol_=10^45.5^-10^48^erg/s), redshift 1.5<z<4.0 quasars with both CIV and Balmer line spectra, we have quantified the bias in CIV BH masses as a function of the CIV blueshift. CIV BH masses are shown to be a factor of 5 larger than the corresponding Balmer-line masses at C IV blueshifts of 3000km/s and are overestimated by almost an order of magnitude at the most extreme blueshifts, ?=5000km/s. Using the monotonically increasing relationship between the CIV blueshift and the mass ratio BH(CIV)/BH(H{alpha}), we derive an empirical correction to all CIV BH masses. The scatter between the corrected CIV masses and the Balmer masses is 0.24dex at low CIV blueshifts (~0km/s) and just 0.10dex at high blueshifts (~3000km/s), compared to 0.40dex before the correction. The correction depends only on the CIV line properties - i.e. full width at half-maximum and blueshift - and can therefore be applied to all quasars where CIV emission line properties have been measured, enabling the derivation of unbiased virial BH-mass estimates for the majority of high-luminosity, high-redshift, spectroscopically confirmed quasars in the literature.
- ID:
- ivo://CDS.VizieR/J/MNRAS/484/L8
- Title:
- Correcting HIRES/Keck RVs for systematic errors
- Short Name:
- J/MNRAS/484/L8
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The HIRES spectrograph, mounted on the 10-m Keck-I telescope, belongs to a small group of radial-velocity (RV) instruments that produce stellar RVs with long-term precision down to ~1m/s. In 2017, the HIRES team published 64480 RVs of 1699 stars, collected between 1996 and 2014. In this bank of RVs, we identify a sample of RV-quiet stars, whose RV scatter is <10m/s, and use them to reveal two small but significant nightly zero-point effects: a discontinuous jump, caused by major modifications of the instrument in August 2004, and a long-term drift. The size of the 2004 jump is 1.5+/-0.1m/s, and the slow zero-point variations have a typical magnitude of <1m/s. In addition, we find a small but significant correlation between stellar RVs and the time relative to local midnight, indicative of an average intranight drift of 0.051+/-0.004m/s/h. We correct the 64480 HIRES RVs for the systematic effects we find, and make the corrected RVs publicly available. Our findings demonstrate the importance of observing RV-quiet stars, even in the era of simultaneously-calibrated RV spectrographs. We hope that the corrected HIRES RVs will facilitate the search for new planet candidates around the observed stars.
- ID:
- ivo://CDS.VizieR/J/other/Ser/177.109
- Title:
- Corrections to HIP proper motions
- Short Name:
- J/other/Ser/177.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We used the data on latitude variations obtained from observations with 10 classical photographic zenith tubes (PZT) in order to improve the Hipparcos proper motions in declinations µ<SUB>δ</SUB> for 807 stars. Part of observing programmes, carried out during the last century for the purpose of studying the Earth's rotation, were realized by using PZT instruments. These observations were performed within in the intervals (tens of years) much longer than that of the Hipparcos mission (less than 4 years). In addition, the annual number of observations for every PZT- programme star is several hundreds on the average. Though the accuracy of the star coordinates in the Hipparcos Catalogue is by two orders of magnitude better than that of the star coordinates from the PZT observations, the large number of observations performed a much longer time interval makes it possible to correct the Hipparcos proper motions and to improve their accuracy with respect to the accuracy given in the Hipparcos Catalogue. Long term examinations of latitude and time variations were used to form the Earth Orientation Catalogue (EOC-2), aimed at a more accurate determination of positions and proper motions for the stars included. Our method of calculating the corrections of the proper motions in declination from the latitude variations is different from the method used in obtaining the EOC-2 Catalogue. Comparing the results we have established a good agreement between our µ<SUB>δ</SUB> and the EOC-2 ones for the star sample used in the present paper.
