Publication: Incidence of debris discs around FGK stars in the solar neighbourhood
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2016-09
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Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their counterparts in the solar system are the asteroid and Edgeworth-Kuiper belts.
Aims. The aim of this paper is to provide robust numbers for the incidence of debris discs around FGK stars in the solar neighbourhood.
Methods. The full sample of 177 FGK stars with d ≤ 20 pc proposed for the DUst around NEarby Stars (DUNES) survey is presented. Herschel/PACS observations at 100 and 160 μm were obtained, and were complemented in some cases with data at 70 μm and at 250, 350, and 500 μm SPIRE photometry. The 123 objects observed by the DUNES collaboration were presented in a previous paper. The remaining 54 stars, shared with the Disc Emission via a Bias-free Reconnaissance in IR and Sub-mm (DEBRIS) consortium and observed by them, and the combined full sample are studied in this paper. The incidence of debris discs per spectral type is analysed and put into context together with other parameters of the sample, like metallicity, rotation and activity, and age.
Results. The subsample of 105 stars with d ≤ 15 pc containing 23 F, 33 G, and 49 K stars is complete for F stars, almost complete for G stars, and contains a substantial number of K stars from which we draw solid conclusions on objects of this spectral type. The incidence rates of debris discs per spectral type are 0.26^+0.21_-0.14 (6 objects with excesses out of 23 F stars), 0.21^+0.17_-0.11 (7 out of 33 G stars), and 0.20^+0.14_-0.09 (10 out of 49 K stars); the fraction for all three spectral types together is 0.22^+0.08_-0.07 (23 out of 105 stars). The uncertainties correspond to a 95% confidence level. The medians of the upper limits of L_dust/L_∗ for each spectral type are 7.8 × 10^-7 (F), 1.4 × 10^-6 (G), and 2.2 × 10^-6 (K); the lowest values are around 4.0 × 10^-7. The incidence of debris discs is similar for active (young) and inactive (old) stars. The fractional luminosity tends to drop with increasing age, as expected from collisional erosion of the debris belts.
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© ESO 2016. Artículo firmado por 19 autores. The authors are grateful to the referee for the careful revision of the original manuscript, and for the comments and suggestions. We also thank Francisco Galindo, Mauro López del Fresno, and Pablo Riviere for their valuable help. B. Montesinos and C. Eiroa are supported by Spanish grant AYA2013-45347-P; they and J.P. Marshall and J. Maldonado were supported by grant AYA2011-26202. A.V. Krivov acknowledges the DFG support under contracts KR 2164/13-1 and KR 2164/15-1. J.P. Marshall is supported by a UNSW Vice-Chancellor's postdoctoral fellowship. R. Liseau thanks the Swedish National Space Board for its continued support. A. Bayo acknowledges financial support from the Proyecto Fondecyt de Iniciación 11140572 and scientific support from the Millenium Science Initiative, Chilean Ministry of Economy, Nucleus RC130007. J.-C. Augereau acknowledges support from PNP and CNES. F. Kirchschlager thanks the DFG for finantial support under contract WO 857/151. C. del Burgo has been supported by Mexican CONACyT research grant CB-2012-183007.
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