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Table: gaia_dr1.cepheid
(The bold columns are indexed columns)
| Column Name | Description | Datatype |
|---|---|---|
| epoch_g | The epoch of maximum light for the Gaia integrated G band. It corresponds to the Baricentric Julian day (BJD) of the maximum value of the light curve model which is closest to the BJD of the first observations -3\timesp1. The mentioned BJD is offset by JD 2455197.5 (= J2010.0). | DOUBLE |
| epoch_g_error | The uncertainty value of the epochG parameter. Its value is three times the error on the p1. | DOUBLE |
| int_average_g | The intensity-averaged magnitude in the G-band. The intensity-averaged magnitude is obtained by computing the average flux and then converting the average flux to magnitude. | DOUBLE |
| int_average_g_error | This parameter is filled with the uncertainty value of the intAverageG parameter. The uncertainty is computed as the error(zp), where zp is the zero point obtained by the non linear Fourier modeling of the light curve. | DOUBLE |
| mode_best_classification | Best mode classification estimate: - FUNDAMENTAL: fundamental mode for typeBestClassification=DCEP or ACEP - FIRST_OVERTONE: first overtone for typeBestClassification=DCEP or ACEP - SECOND_OVERTONE: second overtone for typeBestClassification=DCEP or ACEP - UNDEFINED: if mode could not be clearly determined for typeBestClassification=DCEP or ACEP - NOT_APPLICABLE: when typeBestClassification=T2CEP Cepheid pulsation mode is assigned using the period-luminosity relations, which are different for the various pulsation modes, and the plot of the Fourier parameter R21 vs Period. | CHAR |
| num_harmonics_for_p1 | This parameter is filled with the number of harmonics used to model P1 of the light curve. The light curve of the target star is modeled with a truncated Fourier series (mag(t_j)=zp+\sum[A_i sin(i \times 2 \pi \nu_{max}t_j +\phi_i)]). Zero-point (zp), period (1/\nu_{max}), number of harmonics (i), amplitudes (A_i), and phases (\phi_i) of the harmonics are determined using the Levenberg-Marquardt non linear fitting algorithm. | INTEGER |
| p1 | This parameter is filled with the period of the maximum power peak in the frequencygram obtained from the modeling of the time series. The light curve of the target star is modeled with a truncated Fourier series (mag(t_j)=zp+\sum[A_i sin(i \times 2 \pi \nu_{max}t_j +\phi_i)]). Zero-point (zp), period (1/\nu_{max}), number of harmonics (i), amplitudes (A_i), and phases (\phi_i) of the harmonics, for the G-band light curve are determined using the Levenberg-Marquardt non linear fitting algorithm. | DOUBLE |
| p1_error | This parameter is filled with the uncertainty value of the p1 parameter. Its value is derived with Monte Carlo simulations that generate several (100) time series with the same time path as the data points but with magnitudes generated randomly around the corresponding data value. For each of these time series the period is derived from the non linear modeling with a truncated Fourier series of the light curve. The mean of all the periods found and its standard deviation are then computed, and the latter value is kept as value to fill the p1Error parameter. | DOUBLE |
| peak_to_peak_g | This parameter is filled with the peak-to-peak amplitude value of the G band light curve. The peak-to-peak amplitude is calculated as the (maximum) - (minimum) of the folded modeled light curve in the G band. The light curve of the target star is modeled with a truncated Fourier series (mag(t_j)=zp+\sum[A_i sin(i \times 2 \pi \nu_{max}t_j +\phi_i)]). Zero-point (zp), period (1/\nu_{max}), number of harmonics (i), amplitudes (A_i), and phases (\phi_i) of the harmonics, for the G-band light curve are determined using the Levenberg-Marquardt non linear fitting algorithm. | DOUBLE |
| peak_to_peak_g_error | This parameter is filled with the uncertainty value of the peakToPeakG parameter. The uncertainty is computed as the \sqrt{2}\times error(zp), where zp is the zero point obtained by the non linear Fourier modeling of the light curve. | DOUBLE |
| phi21_g | This parameter is filled with the Fourier decomposition parameter \phi_{21}: \phi_2 - 2\phi_1 value. The light curve of the target star is modeled with a truncated Fourier series (mag(t_j)=zp+\sum[A_i sin(i \times 2 \pi \nu_{max} t_j +\phi_i)]). Zero-point (zp), period (1/\nu_{max}), number of harmonics (i), amplitudes (A_i), and phases (\phi_i) of the harmonics, for the G-band light curve are determined using the Levenberg-Marquardt non linear fitting algorithm. | DOUBLE |
| phi21_g_error | This parameter is filled with the uncertainty of the phi21G parameter. Its value is derived by propagation of the errors in the phi1 and phi2 parameters. Errors in phi1,phi2 are computed from Monte Carlo simulations that generate several (100) time series with the same time path as the data points but with magnitudes generated randomly around the corresponding data value. For each of these time series the phi1, phi2 values are computed. The mean for each of these values and their standard deviation are then computed, and the latter values are kept as value to fill the uncertainty of the phi1 and phi2 parameters. | DOUBLE |
| r21_g | This parameter is filled with the Fourier decomposition parameter R_{21} = A_2/A_1, where A_2 is the amplitude of the 2nd harmonic and A_{1} is the amplitude of the fundamental harmonic of the truncated Fourier series defined hereafter. The light curve of the target star is modeled with a truncated Fourier series (mag(t_j)=zp+\sum[A_i sin(i \times 2 \pi \nu_{max}t_j +\phi_i)]). Zero-point (zp), period (1/\nu_{max}), number of harmonics (i), amplitudes (A_i), and phases (\phi_i) of the harmonics, are determined using the Levenberg-Marquardt non linear fitting algorithm. | DOUBLE |
| r21_g_error | This parameter is filled with the uncertainty value on the r21G parameter. Its value isderived by propagation of the errors in the A2 and A1 parameters. Errors in A1,A2 are computed from Monte Carlo simulations that generate several (100) time series with the same time path as the data points but with magnitudes generated randomly around the corresponding data value. The mean for each of these values and their standard deviations are then computed, and the latter values are kept as value to fill the uncertainty of the A1, A2 parameters. | DOUBLE |
| solution_id | All Gaia data processed by the Data Processing and Analysis Consortium comes tagged with a solution identifier. This is a numeric field attached to each table row that can be used to unequivocally identify the version of all the subsystems that where used in the generation of the data as well as the input data used. It is mainly for internal DPAC use but is included in the published data releases to enable end users to examine the provenance of processed data products. To decode a given solution ID visit | BIGINT |
| source_id | A unique single numerical identifier o f the source obtained from GaiaSource (for a detailed description see GaiaSource.sourceId) | BIGINT |
| type2_best_sub_classification | Sub-classification of a T2CEP Cepheids into BL Herculis (BL_HER), W Virginis (W_VIR) or RV Tauris (RV_TAU) sub-types depending on the source periodicity. | CHAR |
| type_best_classification | Classification of a Cepheid into CEP, 2CEP or CEP using the period-luminosity relations, which are different for the three different types of Cepheids. | CHAR |
