Volume 595, November 2016
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||28 October 2016|
The microlensing rate and distribution of free-floating planets towards the Galactic bulge
1 Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester, UK
2 Institut Utinam, CNRS UMR 6213, Université de Franche-Comté, Observatoire de Besançon, 41bis avenue de l’Observatoire, 25000 Besançon, France
Received: 22 June 2016
Accepted: 30 July 2016
Context. Ground-based optical microlensing surveys have provided tantalising, if inconclusive, evidence for a significant population of free-floating planets (FFPs). Both ground- and space-based facilities are being used and developed which will be able to probe the distrubution of FFPs with much better sensitivity. It is also vital to develop a high-precision microlensing simulation framework to evaluate the completeness of such surveys.
Aims. We present the first signal-to-noise limited calculations of the FFP microlensing rate using the Besançon Galactic model. The microlensing distribution towards the Galactic centre is simulated for wide-area ground-based optical surveys (I-band) such as OGLE or MOA, a wide-area ground-based near-infrared survey (K-band), and a targeted space-based near-infrared survey (H-band) which could be undertaken with Euclid or WFIRST.
Methods. We present a calculation framework for the computation of the optical and near-infrared microlensing rate and optical depth for simulated stellar catalogues which are signal-to-noise limited, and take account of extinction, unresolved stellar background light, and finite source size effects, which can be significant for FFPs.
Results. We find that the global ground-based I-band yield over a central 200 deg2 region covering the Galactic centre ranges from 20 Earth-mass FFPs yr-1 up to 3500 yr-1 for Jupiter FFPs in the limit of 100% detection efficiency, and almost an order of magnitude larger for a K-band survey. For ground-based surveys we find that the inclusion of finite source and the unresolved background reveals a mass-dependent variation in the spatial distribution of FFPs. For a targeted space-based H-band covering 2 deg2, the yield depends on the target field but maximises close to the Galactic centre with around 76 Earth to 1700 Jupiter FFPs per year. For near-IR space-based surveys like Euclid or WFIRST the spatial distribution of FFPs is found to be largely insensitive to the FFP mass scale.
Key words: infrared: ISM / planets and satellites: detection / gravitational lensing: micro / X-rays: bursts
© ESO, 2016
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