As the KELT followup up network has grown larger and demonstrates its potential, we have started adding new types of targets to the target list. They fall into several categories, and some of them involve different observing requirements than regular KELT transit targets. Here is a partial list of them:
Warm Jupiters - These are a set of transiting Jupiters from the K2 mission that have been selected by Avi Shporer as a class of "Warm Jupiters" that can be used to probe certain properties of giant planets including various theories for inflated planets. These Warm Jupiters generally fall well on the other side of the regime from the highly insolated Hot Jupiters that dominate the studies of inflated planets. Avi has selected 11 Warm Jupiters from K2, and we want to get followup photometry from KELT, mainly to confirm and refine the ephemerides of these systems, since the K2 campaigns did not last too long. These targets have V-mags of 10 to 15, periods ranging from 10-60 days, transit durations from 2.5 to 7.5 hours, and depths from 2-40 mmag. These will generally be hard to observe, although still tractable. And even partial transits will be useful for refining the ephemeris. These objects are listed with the name prefix "K2WJ".
Kepler EBs - These are particular EBs discovered by Kepler that are of interest for dynamical purposes. Either they have eclipse timing variations (ETVs) due to third bodies in the system, or they have circumbinary planets. On the transit finder, they are listed with the prefix "Kepler-EB" or "KOI". These targets normally have deep eclipses (much larger than 1%) but are also very long, in many cases much longer than a typical observing night. For these cases, follow the following guidelines:
Observing just an ingress or egress is fine, but make sure to get at least 30 minutes baseline data.
You can observe just the bottom of the eclipse. The important thing to to capture an inflection point so that we can get good timing of the event.
Less worry about photometric precision. RMS of 1-2% should be fine.
Some objects are faint. Make sure your observing cadence is better than 10 minutes.
KELT M-dwarf EBs - These targets are eclipsing binaries with M dwarf companions wherein the primary star is more luminous -- i.e. B/A/F/G dwarfs -- and more massive. The target names are denoted by the prefixes "KEBC" (northern EBs), "KEBS" (southern EBs), "KEBJ" (north-south joint field EBs), and "HTR-" (EBs provided by the HAT survey). For these targets, we recommend following these guidelines:
If no previous observations have pinned down the ingress/egress, then partial transits are useful, so long as there's sufficient data outside the predicted transit (~30 minutes or so). This is particularly true for the very long duration events. Some of the ephemerides are quite old -- particularly for the HAT EBs -- so reconnaissance observations are particularly useful for those. Partials will likely not be included in the final analyses.
If the timing has been confirmed, then high-precision, full transits are the most helpful in the final analyses. Precision is key, so filters that provide the highest signal-to-noise (likely i' or I) are preferred; however, bluer filters (V/g') can be useful for improving the precision on the effective temperature via the limb darkening, while redder (z') filters can improve the precision on the primary stellar density inferred from the ingress/egress duration.
Otherwise, standard transit reporting procedures apply.
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