GENERAL NOTES: - To make the description simple we show the relevant parts of sample files and avoid byte-by-byte description if possible. Some formats are strict, some formats are free. - To handle different formats for the light curves, one needs to change the input routines in "tran_k2_v0.f" accordingly. - In the DESCRIPTION section we show either an arbitrary single line from the file or, if there is a header, then the header and the first data line. The same type of data lines are repeated for all stars entering in the given file. The excerpt from the file is bracketed by "----" - All input/output files are standard ASCII text files [except for the plot files]. - Not all output files listed below are generated/modified after each run. The output file list is controlled by the setting of the parameter file "tran_k2_v0.par". >>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>> INPUT FILES <<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<< ****************** * filename.lis * ****************** PURPOSE: IDs and paths of the stars to be analyzed DESCRIPTION: - for LCs originating from the the Kepler pipeline: ----------------------------------------------------------------- 211754117 LC/211754117-c05pdc.txt ----------------------------------------------------------------- - for LCs originating from the the k2phot/TERRA (by Petigura et al.) pipeline: ----------------------------------------------------------------- 211754117 LC/211754117-c05.txt ----------------------------------------------------------------- FORMAT: a9,9x,a20 [i.e., 9 digits for the star ID, followed by 9 spaces and up 20 characters for the path] File names in the subdirectory "LC" must have the 9-digit star ID and the 3-character K2 campaign ID in the format shown. It is recommended to have directory LC as a symbolic link to the main database. ************* * ref.pos * ************* PURPOSE: IDs, coordinates, and average magnitudes available in the database DESCRIPTION: The columns are: |star ID| |RA| |DE| |Kp| ----------------------------------------------------------------- 211340040 125.98004 10.63206 5.83500 ----------------------------------------------------------------- FORMAT: free ****************** * template.lis * ****************** PURPOSE: List of IDs and paths of the pre-selected stars constituting the TFA filter DESCRIPTION: - for LCs originating from the the Kepler pipeline: ----------------------------------------------------------------- 212138834 LC/212138834-c05pdc.txt 19 ----------------------------------------------------------------- - for LCs originating from the the k2phot/TERRA (by Petigura et al.) pipeline: ----------------------------------------------------------------- 212138834 LC/212138834-c05.txt 19 ----------------------------------------------------------------- FORMAT: The same as for "filename.lis", but followed by an integer after 5 (Kepler) or 3 (k2phot) spaces. These numbers originally show the tile number, but they could be arbitrary, because they are not used in the code. ****************** * LIGHT CURVES * ****************** - for LCs originating from the the Kepler pipeline: FORMAT: Strict in the header (5 lines exactly, starting with #). Free in all other data lines. These files are in a custom-made format from the original *.tbl files downloaded from the NASA/IPAC exoplanet site. ----------------------------------------------------------------- # # SAP/PDC photometry of EPIC-211609360 # SOURCE: EPIC/ExoFOP # # BJD FLUX_SAP e_FLUX_SAP FLUX_PDC e_FLUX_PDC X Y BG 2457139.631236 4816302.5000 57.3500 4816259.0000 56.6846 930.2307 446.0094 55062.8750 ----------------------------------------------------------------- - for LCs originating from the the k2phot/TERRA pipeline: FORMAT: Strict in the header (40 lines exactly, starting with #). Free in all other data lines. Please note that these are the ORIGINAL files downloaded from the NASA/IPAC/ExoFop site. ----------------------------------------------------------------- # Photometry of EPIC-211609360 # # Description # # This photometry was produced by Erik Petigura using the `k2phot` # code. We used a stationary 104.0 pixel aperture to # construct simple aperture photometry from the K2 target pixel # file. We then modeled time- and position-dependent photometric # variability. The size and shape of the aperture was chosen to # minimize noise on three-hour timescales. # # Attribution # # If you use this photometry, please cite # # 1. Petigura et al. 2015, ApJ, 811, 102 # 2. Aigrain et al. 2016, MNRAS, 459, 2408 # # Code Availability # # Public URL: https://github.com/petigura/k2phot # Version: v1.0 # Git SHA: 0e63443fee2083618488daec2635a9d1af284731 # # Column Description # # t (float): Time [BJD_TDB] # cad (int): Unique cadence number # fbg (float): Background flux [e-/s/pixel] # fsap (float): Simple aperture photometry [e-/s] # fdt_t_rollmed (float): Flux after removing variability associated with # pixel position [e-/s] # fdt_t_roll_2D (float): Flux after removing variability associated with # pixel position and time [e-/s] # bgmask (bool): Outlier in background flux # thrustermask (bool): Thruster fire # fdtmask (bool): Observation excluded from Gaussian process model # fmask (bool): Observation ignored in transit search # # t,cad,fsap,fbg,fdt_t_rollmed,fdt_t_roll_2D,bgmask,thrustermask,fdtmask,fmask 2457139.610803,107552,4808099.732990,27.304028,4807929.998388,4810635.698561,False,False,False,False ----------------------------------------------------------------- >>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>> OUTPUT FILES <<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<< filename.lis : Updated target list four_ord.dat : Statistical parameters obtained in the optimization of the Fourier order ts_4.dat : Non-reconstructed time series pre_bls.dat : Time series used in the BLS analysis ts_ar.dat : Time series for testing the AR model at the edges sp.dat : BLS compressed spectrum of the input data outlier.dat : List of single outliers at various steps of analysis (see "NOTE on *outlier.dat*") rec_tfa.dat : Reconstructed time series (using the main component only) sp00.dat - sp05.dat : BLS spectra from that of the input data (00) to the last prewhitening (05) pa00.dat - pa05.dat : Folding parameters of the transit components found from the input data (00) to the last prewhitening (05) lc00.dat - lc05.dat : Time series derived at the various stages of the prewhitening process multi_bls.dat : Peak signal properties at the various stages of the prewhitening process tr1.lc - tr5.lc : Reconstructed time series derived for the individual transit components tr1_fit.lc - tr5_fit.lc : Transit model fits to tr1.lc - tr5.lc tr_all.lc : Reconstructed time series by using all significant transit components simultaneously test_par.dat : Test signal parameters ("nearly" the copy of the test section of the input parameter file) multi_par.dat : Component-by-component reconstructed transit signal properties snr.dat : Transit signal parameters of the main component of the signal analyzed spec/*.sp : Saved BLS spectra from the analysis of the input time series (*=star ID) flc/*.lc : Filtered, but non-reconstructed time series before the BLS analysis cand_4_plot.png : 4-panel diagnostic plot on the main transit component mult_plot.png : Significant individual signal components (BLS spectra and folded LCs) plots/*.png : Saved plots of the above type NOTE on *outlier.dat* : This file is generated FIRST by "outlier_1g". Then, if "jsm=1" in "tran_k2_v0.par", it is overwritten by "outlier_1m". AUXILIARY files [i.e., temporal files generated during the run], listed for completeness: temp.dat a_rec.dat c5.dat lc.dat fold.par fold.dat c7.dat qtran.txt nr.dat a.dat sname.txt ************************ * COLUMN description * ************************ NOTES: - If the description below is not clear, please check the corresponding part of the code - t0=2400000.0 - t1=first (smallest) BJD in the time series - Column names (if any) in the individual files may differ from those shown in the table below. ====================================================================================================== file/col# 1 2 3 4 5 6 7 8 9 ------------------------------------------------------------------------------------------------------ filename.lis ID path four_ord.dat mf sig_mf sig_lin rat1 r2 ts_4.dat BJD-t0 RAW RAW-TFA RAW-FOUR FLC SYNT pre_bls.dat BJD-t0 FLCA XFA WE ts_ar.dat BJD-t1 RAW X_fit X_pred X_Four X_W sp.dat Freq BLS outlier.dat BJD-t0 X FX [jsm = 0] outlier.dat BJD-t0 X FX [jsm > 0] rec_tfa.dat BJD-t0 X_REC XFT SYNT SYN_TRAN FOUR_REC TFA_REC sp0#.dat Freq BLS pa0#.dat ID nper Freq Tc [this is row-wise in the file] lc0#.dat BJD-t0 X_W X_fit multi_bls.dat iw f[1/d] depth qtran Tc N_intr SNR N_event tr#.lc PH XTR XFT tr#_fit.lc PH XFT tr_all.lc BJD-t0 XTR XFT test_par.dat sname tfreq0 dep0 t14_0 pht0 frin0 tfreq1 dep1 t14_1 pht1 frin1 amootv phootv frootv iflare igen std 1.0d0+rfac*fdep iseed0 multi_par.dat EPIC f [c/d] depth t14/P t12/t14 T_c-t0 DSP spec/*.sp Freq BLS flc/*.lc BJD-t0 FLCA XFA TFATS snr.dat SNAME N TOT AVMAG SIG_FINAL F0 DEPTH SNR SPD DSP QTRAN TCEN NEV NDIT SIG_FOUR SIG_TFA SNRT FRET RING ITOC F03 SNR03 F35 SNR35 M_FOUR ************************ * SYMBOL description * ************************ %.......................................................................... filename.lis ID = Star ID (i.e, EPIC number) path = Path to the data file % %.......................................................................... four_ord.dat mf = Fourier order sig_mf = Standard deviation of the Fourier fit of order "mf" sig_lin = Linear fit to the high-mf part of the "sig_mf" function rat1 = Normalized difference between "sig_lin" and "sig_mf" r2 = The ratio of the observed variance (sig_mf**2) and the theoretical standard deviation of this variance. % %.......................................................................... ts_4.dat BJD-t0 = BJD, t0 subtracted RAW = Raw (measured) flux RAW-TFA = TFA-filtered flux [no Fourier correction] RAW-FOUR = FOUR-filtered flux [no TFA correction] FLC = [TFA+FOUR]-filtered, non-reconstructed flux (FLC=RAW-TFA-FOUR) SYNT = Synthetic test signal % %.......................................................................... pre_bls.dat BJD-t0 = BJD, t0 subtracted FLCA = TFA+FOUR-filtered, non-reconstructed flux with AR approximation at the edges XFA = Fourier fit with AR approximation at the edges WE = Point-by-point weight used in the robust fit % %.......................................................................... ts_ar.dat BJD-t1 = BJD, t1 subtracted X_fit = 1.0 at the edges, where the AR model is used, Fourier fit elsewhere X_pred = AR model at the edges, Fourier fit elsewhere X_Four = Fourier fit X_W = RAW-X_pred-TFA, i.e, X_W is free from systematics and stellar variability % %.......................................................................... sp.dat Freq = Frequency [c/d] BLS = BLS power % %.......................................................................... outlier.dat [from outlier_1g] BJD-t0 = BJD, t0 subtracted XX = RAW-TFA-FOUR (non-reconstructed, [FOUR+TFA]-filtered) X = Corrected outlier value (= average of the neighbours) % %.......................................................................... outlier.dat [from outlier_1m] BJD-t0 = BJD, t0 subtracted X = RAW-TFA-FOUR (reconstructed, [FOUR+TFA]-filtered data) FX = Corrected outlier value (= best model value) % %.......................................................................... rec_tfa.dat BJD-t0 = BJD, t0 subtracted X_REC = RAW-FOUR-TFA (reconstructed with the dominant transit) XFT = Best-fitting transit model to X_REC SYNT = Test signal (transit+other variations) SYN_TRAN = Test transit signal (only) FOUR_REC = FOUR in the full (reconstructed) model TFA_REC = TFA in the full (reconstructed) model % %.......................................................................... sp0#.dat Freq = Frequency [c/d] BLS = BLS power % %.......................................................................... pa0#.dat ID = Star ID (i.e, EPIC number) nper = Number of folding periods Freq = Frequency [c/d] Tc = Epoch of the center of the transit % %.......................................................................... lc0#.dat BJD-t0 = BJD, t0 subtracted X_W = Non-reconstructed, [TFA+FOUR]-filtered LC TR_fit = Best-fitting transit signal to X_W % %.......................................................................... multi_bls.dat iw = Prewhitening cycle (iw=1 for the analysis of the RAW data) f[1/d] = Peak frequency [c/d] depth = Transit depth [relativ flux change, non-reconstructed] qtran = Transit duration divided by the period Tc = Center of the transit minus t0 N_intr = Total number of intransit data points SNR = Signal-to-Noise-Ratio N_event = Number of transit events % %.......................................................................... tr#.lc PH = Phase XTR = Reconstructed time series for the #-th component XFT = Best transit fit to XTR % %.......................................................................... tr#_fit.lc PH = Phase XFT = Best transit fit to XTR (close to the transit center) % %.......................................................................... tr_all.lc BJD-t0 = BJD, t0 subtracted XTR = Reconstructed time series including all components XFT = Best fit transit model including all components % %.......................................................................... test_par.dat sname = Star ID (i.e, EPIC number) tfreq0 = Frequency of the 1st transit dep0 = Depth of the 1st transit t14_0 = Transit length [d] of the 1st transit pht0 = Phase of the 1st transit [0,1] frin0 = Relative ingress duration of the 1st transit tfreq1 = Frequency of the 2nd transit dep1 = Depth of the 2nd transit t14_1 = Transit length [d] of the 2nd transit pht1 = Phase of the 2nd transit [0,1] frin1 = Relative ingress duration of the 2nd transit amootv = OOT frequency phootv = OOT sinusoidal amplitude frootv = OOT sinusoidal phase iflare = Include/not include (1/0) flares in the test data igen = 1=Add Gausian noise to the synthetic signal; 0=Add input time series std = Standard deviation of the Gaussian noise, if igen=1 dep_fac = Transit depth modification factor: dep# --> dep_fac*dep#; # = 0,1 iseed0 = Seed of the random number generator % %.......................................................................... multi_par.dat EPIC = Star ID (i.e, EPIC number) f [c/d] = Peak frequency at the given prewhitening step depth = Transit depth (in the units of the relative flux) t14/P = Transit duration (in the units of the orbital period) t12/t14 = Ingress duration over the total transit duration T_c - t0 = BJD of the moment of the transit center, with t0 subtracted DSP = Dip significance parameter % %.......................................................................... spec/*.sp Freq = Frequency [c/d] BLS = BLS power % %.......................................................................... flc/*.lc BJD-t0 = BJD, t0 subtracted FLCA = [TFA+FOUR]-filtered, non-reconstructed flux with AR approximation at the edges XFA = Fourier fit with AR approximation at the edges TFATS = TFA time series used in the derivation of FLCA % %.......................................................................... snr.dat SNAME = Star ID (i.e, EPIC number) N = Total number of data points TOT = Total time span [d] AVMAG = Average Kp magnitude SIG_FINAL = Unbiased standard deviation of the residuals of RAW_LC - MODEL_LC F0 = Peak frequency [c/d] DEPTH = Transit depth (relative flux units) SNR = Signal-to-Noise Ratio of the peak in the BLS spectrum SPD = Spectral Peak Density DSP = Dip Significance Parameter QTRAN = Relative transit duration (t14/P) TCEN = BJD-t0 of the transit center NEV = Number of the transit events NDIT = Number of in-transit data points including all events SIG_FOUR = Standard deviation of the non-reconstructed Fourier component (with a possible AR component at the edges) SIG_TFA = Standard deviation of the non-reconstructed TFA component SNRT = SNR of the Fourier spectrum of the OOT section of the folded LC by the period of the transit (1/F0) FRET = Peak frequency of the above OOT spectrum RING = Ingress duration over full transit duration (t12/t14) ITOC = Transit Occupation Code F03 = Fourier peak frequency in [0,3] c/d for the [FOUR+TFA]-filtered, non-reconstructed time series SNR03 = SNR of the peak in the above spectrum F35 = Fourier peak frequency in [3,5] c/d for the [FOUR+TFA]-filtered, non-reconstructed time series SNR35 = SNR of the peak in the above spectrum M_FOUR = Order of the FOUR component of the signal % %..........................................................................