Improving Precision in Exoplanet Transit Detection. Aimée Hall Institute of Astronomy, Cambridge Supervisor: Simon Hodgkin
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1 Improving Precision in Exoplanet Transit Detection Supervisor: Simon Hodgkin
2 SuperWASP Two observatories: SuperWASP-North (Roque de los Muchachos, La Palma) SuperWASP-South (South African Astronomical Observatory) Wide-Angle Search for Planets: 8 cameras per observatory Each camera has 7.8x7.8 degree field of view 20,000-30,000 stars per field 100 transiting exoplanets discovered
3 SuperWASP Successful planet hunter 21.5 millimagnitude depth
4 SuperWASP can it get even better? Systematics: A.M.S Smith et al MNRAS (2006) Noise ~10 mmag Binned: 4-5 mmag White noise limit: 1-2 mmag Post-SYSREM: Noise ~6-7 mmag Binned: 3-4 mmag White noise limit: <2 mmag
5 So many small exoplanets A. W. Howard et al., Ap. J. S (2012) 0.25 R Jupiter f R R R Jupiter R Jupiter Half the radius = 3.8 times more planets
6 The ground is the limit? SuperWASP Kepler All known
7 Brighter is better Pont (2010, Magnitude distribution of SuperWASP Planets Brighter stars better for atmospheric detection
8 SuperWASP New Analysis Co-located list driven photometry Soft-edged apertures Robust background estimator Seasonal Flatfields Up to late 2011 Survey Mode 6 minute Cadence After late 2011 Stare Mode 1 minute Cadence
9 SuperWASP Archival Data There is a huge volume of archived SuperWASP data 3.2x10 11 data points 30.8 million objects 10.6 million images (V=15) More than half of the observations span at least 4 years (up to 7) Mean of 15,000 epochs per star
10 Noise reduction: Survey mode New analysis Previous analysis Previous analysis + trend removal (SYSREM) 3mmag
11 The colour of noise I - Survey Mode
12 XO-5b Single Transit
13 SuperWASP Stare Mode 24 nights between Nov-Dec fields in this analysis raw frames per field 70% of frames have suitable: Average source ellipticity Frame astrometric fit error Seeing Sky level Zero point magnitude
14 The colour of noise II Stare Mode 2009 Survey Mode 2011 Stare Mode
15 Planet Candidates BLS search for potential transits Selected if: SNR > 6 More than 3 transits observed < 80% of transit data from 1 night 74 candidates have R < 2R J Smallest candidate radius ~0.6R J Bold symbols: Includes Nov-Dec 2012 (1 field)
16 Example Candidates Period: 0.31 days Depth ~3.5mmag Period: 1.68 days Depth ~6 mmag
17 SuperWASP: Current capabilities Period: 0.31 days Depth ~3.5mmag Period: 1.68 days Depth ~6 mmag
18 Future SuperWASP upgraded to stare-mode in late 2011: ~90% of stare mode data left to analyse. Reducing rms noise allows smaller transits (smaller planets) to be detectable Planets half the size are 3-4 times more common For every SuperWASP exoplanet, potential to find 3 new ones! SuperWASP has found more than 30 new planets since 2012
19 Summary We have developed and tested new processing strategies for SuperWASP: Reach 1mmag noise on stare-mode SuperWASP data on transit duration timescales Improved noise characteristics increase sensitivity to smaller planets and at longer periods Lightcurves can tell blends from true planet candidates, saving follow-up resources With just 44 nights we have 74 candidates with radii between 0.63 R J and 2R J Window of opportunity to extend this analysis to the rest of the SuperWASP data to find planets for planet characterisation
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