This document defines the catalog entries describing the SWIFTUVOT 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.
After selecting the desired observations, and file format, click the button labelled 'Download selected datasets'. Current choices for file format include a zipped file, a gzipped tar file, or a shell script of WGET commands (the user can then run the shell script from his own computer to download files). The WGET option will list all the associated data sets as they are stored online within MAST. Several files may be included for each observation and may be gzipped or uncompressed.
If you select the WGET option on the search form under "Output Format", you will get a shell script of WGET commands to download only the Sky coordinate images (i.e., the *_sk.img.gz files). Using the WGET option from the search results the returned file will list all the online files associated with the selected observation.
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.
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.
Adjust the X size and Y size in pixels to create the size of plot desired. The maximum dimensions are 850 by 640 pixels.
Use this button to replot the spectra when you have changed the plot range or plot dimensions.