Search for cold debris disks around M-dwarfs. II

¹ Observatoire de Paris - CNRS, 77 Av. Denfert Rochereau, 75014 Paris, France e-mail: jean-francois.lestrade@obspm.fr
² Institute of Astronomy, University of Cambridge, Cambridge, CB3 OHA, UK e-mail: wyatt@ast.cam.ac.uk
³ Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: bertoldi@astro.uni-bonn.de
⁴ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: kmenten@mpifr-bonn.mpg.de
⁵ École Normale Supérieure de Cachan, 61 avenue du Président Wilson, 94235 Cachan, France e-mail: glabaigt@rip.ens-cachan.fr

Received: 8 April 2009
Accepted: 6 July 2009

Abstract

Although 70% of the stars in the Galaxy are M-dwarfs, thermal emission searches for cold debris disks have been conducted mostly for A-type and solar-type stars. We report on new  mm continuum observations of thirty M-dwarfs, using the MAMBO-2 bolometer array camera at the IRAM 30 m telescope. For a statistical analysis, we combine these data with our prior SCUBA and MAMBO-2 observations of 20 other M-dwarfs. Our sample consists of M-dwarfs in moving groups, with relatively young ages, and of nearby M-dwarfs with unknown ages. Only one cold debris disk (GJ842.2) was detected significantly. We compare the implied disk abundance constraints with those found in two comparable submillimeter surveys of 10 to 190 Myr old A- and FGK-type stars. For the 19 youngest (ages less than 200 Myr) M-dwarfs in our sample, we derive a cold disk fraction of %, compared to % for FGK-stars and % for A-stars. Hence, for this age group, there is an apparent trend of fewer cold disks for later stellar types. Although its statistical significance is marginal, this trend is strengthened by the deeper observations of our M-dwarf sample. We derive a cold disk fraction of <10% for the older (likely a few Gyr) M-dwarfs in our sample. Finally, although inconclusively related to a debris disk, we present the complex millimeter structure found around the position of the M 1.5 dwarf GJ526 in our sample.