This document defines the catalog entries describing
the K2 Data Archive.
Clicking on entries in this column will mark the entry for retrieval.
To mark all entries, click one of the buttons labelled
'Mark All','Mark public', or 'Mark Proprietary'.
(Unmarking all entries can be done the same way
using the appropriate button.)
For missions with proprietary data, the mark button element
will have a yellow background and a '@' symbol to indicate
data sets not yet public.
Click the button labelled 'Submit marked data for retrieval from
STDADS'. This will send all the marked data set names to the
data retrieval page. Follow the directions on the displayed pages.
After selecting up to 15 observations to be plotted, click on
the "Plot marked spectra" button to coplot the selected observations.
The spectra that you selected will be automatically scaled
to the full range of wavelengths and nearly the full range of
fluxes (i.e., y axis plot scale runs from 0 (or .25 * the minimum flux
for spectra with negative fluxes) to the 10th highest flux). Each
spectrum is automatically assigned a color, up to a maximum of 15.
For plotting Kepler light curves, y-axis scaling is slightly different.
Plots scale simply from the minimum to the
maximum flux. It is also recommended that only Kepler light curves
from the same target be co-plotted due to the differences in flux values.
The spectra are labelled by their dataset names, with a
summary of the datasets plotted given below the plot. After inspecting
the plot, you may wish to change the selection of datasets which are
displayed. Use your browser "Back" button to do this.
Plot range Adjust the minimum and maximum wavelengths (in Angstroms)
and minimum and maximum fluxes (in erg /cm2/sec/A) to select the
spectral region of interest and to exclude noisy data.
Note Kepler light curves are in units of time and uncalibrated fluxes.
Plot dimensions Adjust the X size and Y size in pixels to create the size of plot
desired. The maximum dimensions are 850 by 640 pixels.
Redraw plot Use this button to replot the spectra when you have changed the plot range or plot dimensions.
Non-unique K2 ID identifying corresponding entry in EPIC or the custom aperture file. Note multiple observations can be made with the same Kepler ID. Also used in naming data files. 200000811 to 251809654
An integer number indicating the campaign in which the exposure was made. Campaigns 9a and 9b are designated as numbers 91 and 92. Campaigns 10a and 10b will be 101 and 102. Campaigns 11a and 11b are 111 and 112. Entering numbers 9, 10 or 11 will return both subsets. Campaigns 12 and 13 are also included. 0 to 112
Type of object based on EPIC values ("star" or "extended") and target names assigned to Custom Aperture observations. examples: star, extended, ASTEROID, COMET, CLUSTER.M80, and TNO.2002 GV31. Many are null.
archive class in science table used to distinguish long and short cadence light curves and target pixel files only KTL and KTS (i.e., long and short cadence target pixel files) for now. Starting with Campaign 3, we will also have KLC,KSC for long and short cadence light curves. Note if both a light curve and a target pixel file exist, or just a light curve file exists, the archive class will refer to the light curve.
Investigation ID assigned by the Kepler project describing a particular GO or project observing program. GO0001, GO0001_GO0032, etc. (Note wild cards are added automatically before and after the user-entered ID(s).)
The fraction of target flux obtained in the optimal aperture averaged for the specified data. The flux fraction in any given cadence will differ from this mean value. This value is not to be confused with the Flux Fraction value given on the Target Search page which gives a predictive values. 0 to 1
The RMS Combined Differential Photometric Precision (CDPP) time series calculated by the Kepler pipeline for a transit duration of length 3-hrs over a single quarter, in units of parts per million. 12.3590 to 93163495424