2009A&A...508.1057N


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.04CET20:57:45

2009A&A...508.1057N - Astronomy and Astrophysics, volume 508, 1057-1065 (2009/12-3)

A submillimetre search for cold extended debris disks in the β Pictoris moving group.

NILSSON R., LISEAU R., BRANDEKER A., OLOFSSON G., RISACHER C., FRIDLUND M. and PILBRATT G.

Abstract (from CDS):

Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid- and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. The β Pictoris moving group is a nearby stellar association of young (∼12Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870µm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. From our sample, β Pic, HD181327, and HD172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. We find a mean fractional dust luminosity fdust=1.1x10–3 at t≃12Myr, which together with recent data at 100Myr suggests an fdust∝t–α decline of the emitting dust, with α>0.8.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planetary systems - planetary systems: formation

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 15115 PM* 02 26 16.2457708887 +06 17 33.187984874   7.15 6.80   6.33 F4IV 159 0
2 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1733 1
3 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3064 0
4 V* AF Lep RS* 05 27 04.7631691589 -11 54 03.466187467   6.832 6.295     F8V(n)k: 213 0
5 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1696 1
6 IRAS 13134-6242 mul 13 16 42.9 -62 58 45           ~ 29 0
7 [WBH98] 13134-6242 HII 13 16 46.3 -62 58 35           ~ 23 0
8 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 594 0
9 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1078 1
10 GAL 005.88-00.41 HII 18 00 30.388 -24 04 00.20           ~ 303 0
11 HD 164249 PM* 18 03 03.4097129717 -51 38 56.434160321   7.438 7.007 7.90   F6V 98 0
12 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 244 0
13 CD-64 1208 ** 18 45 36.903120 -64 51 47.31228   10.52 9.433 9.69   K5Ve 60 0
14 * eta Tel PM* 19 22 51.2064652963 -54 25 26.152538950   5.035 5.020   4.99 A0V+M7/8V 193 0
15 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 238 0
16 HD 191089 PM* 20 09 05.2158287736 -26 13 26.520539765   7.62 7.18     F5V 122 0
17 V* AT Mic Er* 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 331 0
18 HD 197489 * 20 43 19.9941779987 +25 49 29.133726438 7.59 7.38 7.04     A5II 26 0
19 V* AU Mic LM* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 931 0
20 HD 199143 PM* 20 55 47.6748980673 -17 06 51.062191525   7.84 7.32 8.29   F8V 110 0
21 HD 358623 BY* 20 56 02.738688 -17 10 53.80428   11.603 10.625 10.18 8.847 K7 81 0

    Equat.    Gal    SGal    Ecl

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