http://wikisend.com/download/931164/exo.zip

The CoRoT and KEPLER parts of this are updates.

Recent new data and new access points have occured for these. In the above file are corot.tdf, corot_exo.dat and kepler.tdf. These can be extracted to the Guide directory. Objects in the relavent fields appear as blue circles next to the star they are associated with.

Data can at times be returned in fits format, in which case

http://www.star.bris.ac.uk/~mbt/topcat/

is the most general alround conversion and scatter plotting too. (Try downloading the full version, it has VO data access capabilities). You need to have some level of JAVA on your system, most people have, even if they don't know it. If not search for and install SUN JRE, runtime, Java.

The data are primarily epoch photometry. Fluxes can be placed on a differential magnitude scaling via

-2.5 x log10(flux/median_flux)

or mean flux might be better than median (you figure that out yourself) for data with heavy numbers of outliers.

Various information are presented for each, and exoplanet identifiers and variable stars have been published from each, although not always accurately/correctly.

CoRoT outlinking goes here :-

http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/corot/exo

(press submit query button for a general example output, Guide outlinks to specific objects)

and the plot link at end of each row of vizier data launches graph plots of the photometry. Data can be downloaded from there too.


Kepler data access has changed a bit. Now outlinking goes to a summary of the files publicly available for the that object. These can be "marked" and on the fly graphs of the _raw_, not _corrected_, flux over time are then plotted in the browser.

An extra link in Guide now leads to the ftp subdirectory from where the fits files can be downloaded for local use and examined and/or analysed. However, there seems to be a bit of a bug here, as Guide seems to launch that page in internet explorer for me, rather than in the default browser as happens with http links. So some users may be surprised to find that although they've "uninstalled" internet explorer, it's still often there at core in most Windows OSes. If it really isn't there, the data link will probably not work or do something weird. Outinking from TDF is usually to http addresses, not ftp, so Guide likely isn't looking for ftp, likely.

Extract the tdf (which has the data built in for several thousand of the public released objects) and save it to the Guide directory. First look at colour - colour plots suggests that of the latest quarterly public release of 'dropped' and suchlike objects that the vast majority have probably been dropped because they are in fact galaxies, but I haven't checked this rigorously in any way.


And then we have the newly and recently released SuperWASP epoch photometry :-

http://www.wasp.le.ac.uk/public/

There's rather a lot of this, the three master list fits files add up to nearly a quarter of a gigabyte on their own. That's just the 'index' so to speak, not the full dataset.

So, what has been included here is the mere sixth of a million, just short of, brightest objects up to magnitude 10.00. The data for the fainter objects generally appears to be a bit noisy, and somewhat problematic for use, so this sampler will give a hint of how it works.

Still, to keep size down only the sexagesimal part of the Object ID has been kept (position and name can readily be regenerated from these), the number of datapoints in the dataset for a star, and the mean magnitude.

This magnitude is not meant to be a photometric reference value that I can see.

The stars are plotted as white stars to magnitude scale.

In More Info clicking on the red link will lead _directly_ to downloading the FITS table file of epoch data for that object, which can be viewed or converted to another file format in TopCat. Flux can be converted to representative magnitude via the formula mag = 15 - 2.5 x log10(Flux2) , and scatter plots made of TMID in seconds as x axis and FLUX2 as Y axis. FLUX2 is in "microVegas". Different, eh?

You can actually type that on the fly into the x axis input box in topcat scatter plots to get the scale needed.

Just extract the TDF and datafile to the Guide directory.

These lot are a bit esoteric, and not much use to observers, but will show how it all works, and show how to go about looking up known or news press objects and look at the data the article is on about directly, yourself.

For instance, Kepler 8b is KEPLER 006922244

http://archive.stsci.edu/prepds/kepler_hlsp/

Launch Guide, GOTO TDF, KEPLER OBJECTs, enter 006922244 (I'm afraid the preceding zeroes are important here), click on the blue circle, click on More Info, click on the red Kepler MAST link, and you get this :-

http://archive.stsci.edu/kepler/data_search/search.php?action=Search&ktc_kepler_id=006922244

the yellow flagged stuff is "proprietary", ie not public.

Click the two tick boxes that are public, at top, and you can press the "Plot Marked Light Curves" button and you can see a plot of the raw flux.

There are those exoplanet transits.

Click on the Kepler Data red link and you go to

ftp://archive.stsci.edu/pub/kepler/lightcurves/0069/006922244/

you can download these fits files and put them into topcat or whatever app you have that will read fits tables (that's fits _tables_, not _images_), and plot barytime (barycentric Julian Date, kind of) against app_corr_flux, the corrected aperture flux, which'll show the plot detrended (the graph will likely need some tweaking for best display results). In topcat you can zoom in on individual transits via rubberbanding.

And if you had the full superwasp master catalogue, which is way too big to upload anywhere, you could link out to

http://www.wasp.le.ac.uk/public/lc/get_lc.php?obj_id=1SWASP+J184509.15%2B422704.3

and see how superwasp ground based data looks for the self same star, ie how ground based experiments fair for faint stars, rather than the often brighter examples ground based often (but not always) finds. That link will lead you directly to the fits file.


Also, all these datasets contain unknown variables, or known variables that they can help correct the details for where necessary, if you're interested in that sort of thing.

Cheers

John