Extrasolar Planet Transit Finder


While this page should still work, it is no longer maintained or updated. I reccommend using the NExScI transit prediction service at http://exoplanetarchive.ipac.caltech.edu/cgi-bin/TransitView/nph-visibletbls?dataset=transits


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 Aug. 5, 2014 - 1,012 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 :)



Select an Observatory
        If Other,
        Latitdue in Decimal Degrees North
        Longtidue in Decimal Hours West

Enter start JD
Enter end JD  

Sort By Name   Mid-Transit Time   Vmag   Depth

Include UT Dates and Times in Output?

Include Secondary Eclipses?
        Secondary Eclipse calculation parameters
        Wavelength (μm) =
        Planet Albedo A =
        Heat Redistribution Factor F =



*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 jlcough@nmsu.edu