AKARI/IRC 18 μm survey of warm debris disks
Subaru Telescope, National Astronomical Observatory of Japan,
650 North A’ohoku Place,
2 Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, 464-8602 Aichi, Japan
3 Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, 113-0033 Tokyo, Japan
4 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, 252-5210 Kanagawa, Japan
5 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, 181-0015 Tokyo, Japan
6 Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, 560-0043 Osaka, Japan
7 Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba-ku, Sendai, 980-8578 Miyagi, Japan
8 Research Institute of Science and Technology for Society, Japan Science and Technology Agency, K’s Gobancho Bldg 7, Gobancho, Chiyoda-ku, 102-0076 Tokyo, Japan
9 Departmento Física Teórica, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
10 Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
11 Space Science & Technology Department, The Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK
Received: 19 June 2012
Accepted: 21 November 2012
Context. Little is known about the properties of the warm (Tdust ≳ 150 K) debris disk material located close to the central star, which has a more direct link to the formation of terrestrial planets than does the low-temperature debris dust that has been detected to date.
Aims. To discover new warm debris disk candidates that show large 18 μm excess and estimate the fraction of stars with excess based on the AKARI/IRC Mid-Infrared All-Sky Survey data.
Methods. We searched for point sources detected in the AKARI/IRC All-Sky Survey, which show a positional match with A-M dwarf stars in the Tycho-2 Spectral Type Catalogue and exhibit excess emission at 18 μm compared to what is expected from the KS magnitude in the 2MASS catalogue.
Results. We find 24 warm debris candidates including 8 new candidates among A-K stars. The apparent debris disk frequency is estimated to be 2.8 ± 0.6%. We also find that A stars and solar-type FGK stars have different characteristics of the inner component of the identified debris disk candidates. While debris disks around A stars are cooler and consistent with steady-state evolutionary model of debris disks, those around FGK stars tend to be warmer and cannot be explained by the steady-state model.
Key words: circumstellar matter / zodiacal dust / infrared: stars
© ESO, 2013