TY - JOUR
T1 - The Big Sibling of AU Mic
T2 - A Cold Dust-rich Debris Disk around CP-72 2713 in the β Pic Moving Group
AU - Moór, Attila
AU - Moór, Attila
AU - Pawellek, Nicole
AU - Pawellek, Nicole
AU - Pawellek, Nicole
AU - Ábrahám, Péter
AU - Ábrahám, Péter
AU - Kóspál, Ágnes
AU - Kóspál, Ágnes
AU - Kóspál, Ágnes
AU - Vida, Krisztián
AU - Vida, Krisztián
AU - Pál, András
AU - Pál, András
AU - Dutrey, Anne
AU - Folco, Emmanuel Di
AU - Hughes, A. Meredith
AU - Kral, Quentin
AU - Pascucci, Ilaria
N1 - Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.
PY - 2020/6
Y1 - 2020/6
N2 - Analyzing Spitzer and Herschel archival measurements we identified a debris disk around the young K7/M0 star CP-72 2713. The system belongs to the 24 Myr old β Pic moving group. Our new 1.33 mm continuum observation, obtained with the Atacama Large Millimeter/submillimeter Array 7 m array, revealed an extended dust disk with a peak radius of 140 au, probably tracing the location of the planetesimal belt in the system. The disk is outstandingly large compared to known spatially resolved debris disks and protoplanetary disks around stars of comparable masses. The dynamical excitation of the belt at this radius is found to be reconcilable with planetary stirring, while self-stirring by large planetesimals embedded in the belt can work only if these bodies form very rapidly, e.g., via pebble concentration. By analyzing the spectral energy distribution, we derived a characteristic dust temperature of 43 K and a fractional luminosity of 1.1 × 10-3. The latter value is prominently high; we know of only four other similarly dust-rich Kuiper Belt analogs within 40 pc of the Sun.
AB - Analyzing Spitzer and Herschel archival measurements we identified a debris disk around the young K7/M0 star CP-72 2713. The system belongs to the 24 Myr old β Pic moving group. Our new 1.33 mm continuum observation, obtained with the Atacama Large Millimeter/submillimeter Array 7 m array, revealed an extended dust disk with a peak radius of 140 au, probably tracing the location of the planetesimal belt in the system. The disk is outstandingly large compared to known spatially resolved debris disks and protoplanetary disks around stars of comparable masses. The dynamical excitation of the belt at this radius is found to be reconcilable with planetary stirring, while self-stirring by large planetesimals embedded in the belt can work only if these bodies form very rapidly, e.g., via pebble concentration. By analyzing the spectral energy distribution, we derived a characteristic dust temperature of 43 K and a fractional luminosity of 1.1 × 10-3. The latter value is prominently high; we know of only four other similarly dust-rich Kuiper Belt analogs within 40 pc of the Sun.
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U2 - 10.3847/1538-3881/ab8f98
DO - 10.3847/1538-3881/ab8f98
M3 - Article
AN - SCOPUS:85086860782
VL - 159
JO - Astronomical Journal
JF - Astronomical Journal
SN - 0004-6256
IS - 6
M1 - 288
ER -