Using Kepler as a Calibrator X. Huang, G. Á. Bakos and J. A. Hartman
[email protected] PROBLEM OBSERVATION The HATNet project is a wide-field ground-based search for transiting plan- ets around moderately bright stars. Like other wide-field ground-based transit sur- veys, HATNet is primarily sensitive to gas giant planets with orbital periods less than 10 days. The detection of smaller and longer pe- riod planets are difficult because of the fol- lowing aspects. 1. Large gap in time series, either due to rotation of earth, or inclement weather conditions. 2. Data quality is highly variable due The Kepler field was observed by HAT- period smaller than 20 days and size bigger to changing extinction, clouds, back- Net prior to the launch of the mission. The than Neptune in the center field G154. We ground, seeing, etc. whole Kepler field is overlapped with five use this sample to calibrate a new transit de- 3. The per-point photometry precision is HATNet fields in total. We select Kepler tection pipeline. worse compare to space based obser- planet candidates (Batalha et al.(2013)) with vations. The high quality light curves from Kepler mission provide a valuable opportunity for EXAMPLE HAT LIGHT CURVES RESULT us to improve our yield of smaller and longer We yield robust detections for Kepler period planets. -0.01 HAT1998264, unbinned candidates that were previously not selected HAT1998264, binned average -0.005 KOI12.01, binned average by HATNet (for instance, see the exam- 0 mag ple light curves of KOI12.01,KOI18.01 and METHOD 6 0.005 0.01 KOI98.01).