COROTEXLOG - CoRoT Stellar Targets for Exoplanet Detection Observation Log
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 (these data are presented in the file currently named "astero.dat" in the CDS version at ftp://cdsarc.u-strasbg.fr/pub/cats/B/corot/astero.dat, but which should change in the near future to "bright star.dat"): 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 currently named "exo.dat" in the CDS version at ftp://cdsarc.u-strasbg.fr/pub/cats/B/corot/exo.dat, but which should change in the near future to "faint star.dat"): 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 06h 50m and 18h 50m). 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 http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/CoRoT_N2_versions_30sept2014.pdf. More details on the CoRoT N2 data may be found in the documentation file http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/DescriptionN2v1.5.pdf.
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.
Archive of the CoRoT Data Center, Release N2-4.4 (2016-03-23) CoRoT team <CoRoT Data Center (2016)>
The CoRoT data products generation date and time [crea_dat].
The directory structure and file name of the light curve file containing the time series data and available as a remote data product for this entry.
The version of the pipeline processing that generated the data products [pipe_ver].
The version number of the N2 primary scientific data products [n2_ver].
The CoRoT channel code flag, where a value of 0 means monochromatic results are presented, and of 1 means 3-channel results.
The size of the associated file, in bytes.
The UT date and time of the start time for the use of a given window for the target specified by the corot_id parameter [t_start_win].
The UT date and time of the end time for the use of a given window for the target specified by the corot_id parameter [t_end_win].
A 9-digit unique identifier for the CoRoT target [corotid].
The CoRoT target designation using the 'CoRoT' prefix and the corot_id parameter value, as recommended by the CDS Dictionary of Nomenclature of Celestial Objects.
The CoRoT run code for the target and observation, coded as 'tRpnn', where t = 'L' (long), 'S' (short), or 'I' (initial), 'R' stands for run, p = 'c' (Galactic center pointing) or 'a' (anticenter pointing), and nn = the run number; for example, 'LRa01', 'SRc01', etc [run_code].
The reference for the half CCD from which the product originates, where, for example, 'E1R' refers to the right ('R') CCD number 1 of the Exo-planet ('E') channel [hlfccdid].
The CoRoT target window identification. For the Exo channel, this can be from 0 to 8191 [win_id].
The magnitude of the target. The HEASARC does not know for certain in which band this is measured, but it is probably the V band [magnit_v?].
The Right Ascension of the target in the selected equinox. This was given in J2000 decimal degrees to a precision of 10-5 degrees in the original table.
The Declination of the target in the selected equinox. This was given in J2000 decimal degrees to a precision of 10-5 degrees in the original table.
The Galactic Longitude of the target.
The Galactic Latitude of the target.
The contamination factor for the target [contfact].
The exposure time in seconds for the individual samples, either 32 or 512, indicating if the series is oversampled or not. A value of -1 indicates that during the run a change occurred in the sampling, i.e., it either shifted from 512 to 32 s or the converse) [exptime].
The star magnitude in the B band from the EXODAT/COROTSKY database [magnit_B].
The star magnitude in the V band from the EXODAT/COROTSKY database [magnit_V].
The star magnitude in the R band from the EXODAT/COROTSKY database [magnit_R].
The star magnitude in the I band from the EXODAT/COROTSKY database [magnit_I].
The color temperature of the star from the EXODAT/COROTSKY database [coltemp].
The light curve mean, in electrons per second [lc_mean].
The light curve RMS, in electrons per second [lc_rms]
The number of hot pixels detected in the template [nbhotpix].
The mean of the light curve in the blue channel, in electrons per second [lc_mean_b].
The mean of the light curve in the green channel, in electrons per second [lc_mean_g].
The mean of the light curve in the red channel, in electrons per second [lc_mean_r].
The mean of the light curve in integrated white light in units of electrons s-1.
The RMS of the light curve in the blue channel, in electrons per second [lc_rms_b].
The RMS of the light curve in the green channel, in electrons per second [lc_rms_g].
The RMS of the light curve in the red channel, in electrons per second [lc_rms_r].
The RMS of the light curve in integrated white light, in electrons per second.
The spectral type of the star from the EXODAT/COROTSKY database, where if no spectral type is available, 'K5III' is used [spectype].
The directory structure and file name of the associated WINDESCRIPTOR file which describes the characteristics and history of the observation. This is available as a remote data product for this entry.
The HEASARC Browse object classification, based on the value of the spect_type parameter.