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Title:
An anomaly detector with immediate feedback to hunt for planets of Earth mass and below by microlensing
Authors:
Dominik, M.; Rattenbury, N. J.; Allan, A.; Mao, S.; Bramich, D. M.; Burgdorf, M. J.; Kerins, E.; Tsapras, Y.; Wyrzykowski, Ł.
Affiliation:
AA(SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews KY16 9SS), AB(Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL), AC(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AD(Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL), AE(Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700 Santa Cruz de La Palma, Canary Islands, Spain), AF(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD), AG(Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL), AH(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD), AI(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA; Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 380, Issue 2, pp. 792-804. (MNRAS Homepage)
Publication Date:
09/2007
Origin:
MNRAS
MNRAS Keywords:
gravitational lensing , methods: observational , planetary systems
Abstract Copyright:
(c) 2007 The Authors. Journal compilation © 2007 RAS
DOI:
10.1111/j.1365-2966.2007.12124.x
Bibliographic Code:
2007MNRAS.380..792D

Abstract

The discovery of OGLE 2005-BLG-390Lb, the first cool rocky/icy exoplanet, impressively demonstrated the sensitivity of the microlensing technique to extrasolar planets below 10M⊕. A planet of 1M⊕ instead of the expected 5M⊕ for OGLE 2005-BLG-390Lb (with an uncertainty factor of 2) in the same spot would have provided a detectable deviation with an amplitude of ~3 per cent and a duration of ~12h. While a standard sampling interval of 1.5-2.5 h for microlensing follow-up observations appears to be insufficient for characterizing such light curve anomalies and thereby claiming the discovery of the planets that caused these, an early detection of a deviation could trigger higher-cadence sampling which would have allowed the discovery of an Earth-mass planet in this case. Here, we describe the implementation of an automated anomaly detector, embedded into the eSTAR system, that profits from immediate feedback provided by the robotic telescopes that form the RoboNet-1.0 network. It went into operation for the 2007 microlensing observing season. As part of our discussion about an optimal strategy for planet detection, we shed some new light on whether concentrating on highly magnified events is promising and planets in the `resonant' angular separation equal to the angular Einstein radius are revealed most easily. Given that sub-Neptune mass planets can be considered being common around the host stars probed by microlensing (preferentially M and K dwarfs), the higher number of events that can be monitored with a network of 2-m telescopes and the increased detection efficiency for planets below 5M⊕ arising from an optimized strategy gives a common effort of current microlensing campaigns a fair chance to detect an Earth-mass planet (from the ground) ahead of the COROT or Kepler missions. The detection limit of gravitational microlensing extends even below 0.1M⊕, but such planets are not very likely to be detected from current campaigns. However, these will be within the reach of high-cadence monitoring with a network of wide-field telescopes or a space-based telescope.
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