Extrasolar Planet Transit Finder
This page contains up-to-date elements of all known transiting extrasolar planets from exoplanets.org, and will calculate all observable transits for a specified location and time range. For each observable transit event, the program will return the planet name, V magnitude, the dates of ingrees, mid-transit, and egress, the air mass at each time, and the predicted eclipse depth* based on the system parameters, sorted by the field of your choosing. There is also an option to include secondary eclipses** for each system, which use the system's eccentricity and longitude of periastron to accurately calculate the secondary timing offset.
Select an observatory, (or select 'other' and input your own longitude and latitude), along with a range of JD to search, and the program will return all observable transit events for which the entirety of the transit fits within the JD range, the airmass is less than 3.0 for the whole transit, and the sun's altitude is less than -6 degrees (i.e. at least civil twilight) for the entirety of the transit.
To see the list of planets, and the input parmaters for each, click here. (Last updated 5/02/2013 - 283 planets. If it's been a while since an update, or a system you want isn't there, just e-mail me and I'll update ASAP :)
Bug Warning/Fix 5/2/2013 - I accidentally introduced a bug in my last update (2/20/2013) that caused me to pull the time of periastron, instead of the time of transit center, from exoplanets.org. As such, some systems were affected and had incorrect T0 values, causing their predicted times of transit to be wrong. The bug has now been fixed and the parameter list updated. If you used this page between 2/20 and 5/2/2013, I strongly suggest re-calculating your parameters. My apologies for the bug.
*Predicted primary eclipse depths are calculated via the simple square of the ratio of planet radius to the stellar radius.
**Secondary eclipse depths are calculated by first balancing the flux recieved by the planet from the star to that emmitted by the planet to obtain an equilibrium temperature of the dayside. Then, the secondary eclipse depth is the square of the ratio of the planet radius to the stellar radius times the ratio of the blackbody intensities of the planet and star at the specified wavelength.
This page uses routines from John Thorstensen's SKYCALC program (so thanks John!).
Please send any suggestions for improvements, observatories to add, or any other comments to firstname.lastname@example.org