This tool displays selected spectra or light curves
from missions archived within MAST.
It uses the HTML5 Canvas API for drawing graphics.
Canvas is supported by the latest versions of all popular
browsers including IE 9, but it is NOT directly supported by IE 6,7 or 8.
can be run locally on the users
computer and therefore can be executed fairly quickly.
Reloading the page or clicking the "Start again" button
will retrieve the data from the MAST web server, which takes a little longer,
but allows you to return to the original display.
Note: to reset parameters to their initial values, click the shift key
which clicking the reload button. Clicking "Start again" will re-display
Zoom - To zoom in on a particular region, click
the mouse button and drag it across the desired region. You can
drag the mouse right to left or vice versa. As you drag the mouse,
a box will be drawn showing the region to be displayed.
Releasing the mouse button will display the selected region and
the min and max values shown above the plot will be updated.
The zoomed-in region will be displayed in histogram mode to
more accurately described the digitized data whereas the inital plot
is drawn by just connecting points with straight lines.
Note zooming with the cursor may not work properly
if any part of the plotted data is on the edge or outside the plot window.
Slightly increasing the min/max y values will help alleviate the problem.
Also, if no points appear, click "Start again" to redraw the
Changing plot limits - Besides zooming, the min and max
X and Y axes limits can be specified manually by entering new values
in the boxes provided. Unlike zooming with the mouse, one can
zoom in or OUT by specifying new limits.
To make a change, type in a new value and click return.
The new plot range will appear without the page refreshing.
Reading Cursor Positions - Moving the mouse
across the plot window will display the X any Y positions
of the cursor (in data units) just below the plot window.
Scaling one plot to another - If more than one
observation is plotted, a set of scale factors will appear just
above the plot window.
Changing the default value of 1.00 to another value
and clicking return will scale the flux (y-axis)
values for one plot with respect to the other(s). Typically
small scale factors should be used so the modified values
do not go beyond the plotted flux limits.
Setting a scale value to 0.0 will remove that entry from the plot
(it can be re-displayed by entering a value > 0).
Multiple Plots - Up to 30 observations can be coplotted
however the more data points requested, the more memory
is required and the
longer it takes to download data from the server to your browser.
Tests have shown plotting up to 900,000 data points is possible,
but over 1,000,000 points may cause problems.
Label Display - By default, the dataset name(s) are displayed
in the upper right corner of the plot in the same color as the
corresponding spectrum or light curve. The labels can be removed or re-added
by clicking the On/Off buttons displayed on the plot page.
Note that for Kepler/K2 plots when 2 light curves
are displayed for each observation, the dataset name will appear
in two different colors, one for the raw data and one for corrected.
Labels have not been added to the Kepler
preview page though.
Select Light Curve for plotting - For the k2hlsp_plot program,
there is an option to display (separately) the project light curve (designated as "KTWO")
and any available HLSP light curves (currently K2VARCAT, K2SC, EVEREST, K2GAP, KEGS,
POLAR, and K2SFF). Note some targets may have HLSP light curves but not project-produced
Select Data for plotting - For Kepler, K2, K2VARCAT, EVEREST, KEGS, K2SC,
and K2SFF plots,
you can plot raw flux (i.e., Sap or Extracted), corrected flux (i.e., PDCsap or Detrended),
or in some cases, both fluxes. For Kepler, KEGS, and K2SFF
the initial plot is displayed and scaled for both fluxes.
Note K2GAP and POLAR did not include a raw flux vector so the corrected flux
will be displayed for both options.
For K2 and K2VARCAT, although either flux can be selected,
the initial plot is scaled for the corrected (detrended)
fluxes only. Because of the difference in
flux values for some missions/ High level science products,
plotting both fluxes together may not be an option.
Changing Selected Files - If you know the file names
of observations from the same mission, and the plotted names
appear on the plot page, it's possible to add or
remove them from the plot without returning to the search form.
Just change the name or names displayed in the "Selected File(s)" box and click
"start again". More than one file can be specified using commas as
delimiters. Files not found will be listed under "Plotted Data Sets".
(Note this option may not be available for all plots.)
Label Color/Font -
The color and font for the X and Y axes
can be changed using the various options in the displayed pulldown menu.
Plot Color -
The color of individual spectra/light curves can be
changed using the listed pulldown menus. First select the file name
of the spectrum or light curve you want to change, then select a color.
The change will appear if either the the data set name or the color is changed and will
remain changed until another color is selected or the web page is reloaded.
Clicking "start again" does not change the colors, click the shift key & reload instead.
Note the color of the displayed data set names will change to match the data.
See the Line library
page for a list of the available line lists, their sources,
wavelength range, and number of line IDs. Most are in the UV region,
but hopefully we can add more in the future.
Clicking "Start again" will replot the data and
reset all parameters to their default values except for
Kepler light curves for which the data type remains unchanged.
Write down scale factors if you want to save them.
For Kepler previews, clicking "Back to previous quarter" will display
the previous page displayed in the same browser window.
For spectra dominated by a few bright emission lines, it may be hard
to zoom in on the continuum if it lies close to the minimum flux value.
To make it easier to zoom in, first decrease the "Min Flux" value.
When plotting multiple spectra, you can use the scale factor to
individual spectra. For example, changing a particular scale factor from
the default 1.0 to 1.1 will cause that particular spectrum to stand out.
Changing individual plot colors also works.
To quickly remove a spectrum from a multi-spectrum plot,
set its scale factor to 0.0. Resetting it to 1.0
or clicking "start again" will restore it. For more permanent removal,
delete the file name from the "Selected File(s)" window. This
will remove it until a new plot is drawn from the search results page.
To save a plot, either click the "Create png image" button,
or do a screen capture of the original page. Note the png image appears to have
a black background but it will appear gray when you save it to disk.
When printing, the background color will not appear.
When plotting multiple spectra/light curves, widening the browser window
slightly may help organize the scale factor list.
Source of Data
The data available for plotting comes from various sources.
The files used for the various MAST missions
are as follows:
Kepler - Data is extracted from the online (public)
FITS light curve files produced by the Kepler project. Bothe the
PDCsap and the Sap Flux vectors are plotted by default.
K2SFF - Fluxes and times are extracted from the
FITS files produced as a K2 High Level Science Product
by Andrew Vanderburg at
Both raw and corrected fluxes are displayed, with "bad" points removed.
K2VARCAT - Fluxes and times are extracted from the
FITS files produced as a K2 High Level Science Product
by D. J. Armstrong et al. at the University of Warwick, UK.
HST - FITS preview files created at CADC
IUE - ASCII preview files created by NSSDC
Note that small aperture observations will only be displayed
when there is no corresponding large aperture observation.
If both double aperture exposures are submitted for plottng, the large
aperture spectrum is displayed twice.
FUSE - ASCII preview files created by MAST(?)
TUES - merged ASCII preview files created by MAST
BEFS - merged ASCII preview files created by MAST
EUVE - FITS "spectral container" files created by MAST
WUPPE - FITS "spectral container" files created by MAST
HPOL - FITS "spectral container" files created by MAST
HUT - FITS "spectral container" files created by MAST
Note: only the first HUT spectrum is plotted for those
cases where two are stored in the same file.