2009A&A...497..409R


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.13CEST02:56:17

2009A&A...497..409R - Astronomy and Astrophysics, volume 497, 409-421 (2009/4-2)

Long-wavelength observations of debris discs around Sun-like stars.

ROCCATAGLIATA V., HENNING T., WOLF S., RODMANN J., CORDER S., CARPENTER J.M., MEYER M.R. and DOWELL D.

Abstract (from CDS):

Tracing the evolution of debris discs is essential for our understanding of the architecture of planetary system. Even though the evolution of their inner discs has been recently studied with the Spitzer Space Telescope at mid- to far-infrared wavelengths, the outer discs are best characterised by sensitive millimetre observations. The goal of our study is to understand the evolution timescale of circumstellar debris discs, and the physical mechanisms responsible for such evolution around solar-type stars. In addition, we make a detailed characterisation of the detected debris discs. Two deep surveys of circumstellar discs around solar-type stars at different ages were carried out at 350µm with the CSO and at 1.2mm with the IRAM 30-m telescope. The dust disc masses were computed from the millimetre emission, where the discs are optically thin. Theoretically, the mass of the disc is expected to decrease with time. To test this hypothesis, we performed the generalised Kendall's tau correlation and three different two-sample tests. A characterisation of the detected debris discs has been obtained by computing the collision and Poynting-Robertson timescales and by modelling the spectral energy distribution. The Kendall's tau correlation yields a probability of 76% that the mass of debris discs and their age are correlated. Similarly, the three two-sample tests give a probability between 70 and 83% that younger and older debris systems belong to different parent populations in terms of dust mass. We detected submillimetre/millimetre emission from six debris discs, enabling a detailed SED modelling. Our results on the correlation and evolution of dust mass as a function of age are conditioned by the sensitivity limit of our survey. Deeper millimetre observations are needed to confirm the evolution of debris material around solar-like stars. In the case of the detected discs, the comparison between collision and Poynting-Robertson timescales supports the hypothesis that these discs are dominated by collisions. All detected debris disc systems show the inner part evacuated from small micron-sized grains.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planetary systems: formation - stars: late-type - Kuiper Belt

Simbad objects: 49

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Number of rows : 49

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 377 PM* 00 08 25.7456097412 +06 37 00.488182642   8.22 7.59   6.90 G2V 117 0
2 V* V443 And BY* 01 10 41.9048197146 +42 55 54.593813267       7.2   G7V 54 0
3 HD 8907 PM* 01 28 34.3602968986 +42 16 03.688888803   7.15 6.66     F8 76 0
4 V* DK Cet Ro* 01 57 48.9776543901 -21 54 05.343324011   8.73 8.057   7.343 G4V 117 1
5 Cl Melotte 20 750 * 03 27 37.8038556228 +48 59 28.792232769   11.18 10.59     F9V 28 0
6 BD+47 837 SB* 03 29 26.2412946881 +48 12 11.692542362   10.60 10.00     F9V 32 0
7 HD 22179 TT* 03 35 29.9009895335 +31 13 37.443803080   9.536 8.932 8.59   G5IV 35 0
8 V* V963 Tau BY* 03 43 37.7296428161 +23 32 09.562231360 11.82 11.4 10.6     G5V 53 0
9 Cl Melotte 22 250 SB* 03 44 04.2464661452 +24 59 23.415056429   11.4 10.7     G2 52 0
10 Cl Melotte 22 514 * 03 45 04.0131709191 +25 15 28.254425214   11.4 10.7   9.97 ~ 46 0
11 HD 282954 PM* 03 46 38.7740775017 +24 57 34.725395027   10.9 10.27   9.55 ~ 66 1
12 BD+22 553 * 03 46 50.5365789599 +23 14 21.046191243   10.48 9.97   9.27 ~ 64 0
13 HD 25457 TT* 04 02 36.7451443573 -00 16 08.118566607   5.88 5.38     F7V 237 0
14 V* AF Lep RS* 05 27 04.7631691589 -11 54 03.466187467   6.832 6.295     F8V(n)k: 208 0
15 HD 38207 * 05 43 20.9562637826 -20 11 21.439223613   8.83 8.47     F2V 31 0
16 HD 38529 PM* 05 46 34.9129896843 +01 10 05.512540812       5.4   G8III/IV 309 2
17 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 173 0
18 HD 60737 PM* 07 38 16.4409933710 +47 44 55.221629265       7.3   G0 42 0
19 HD 61994 SB* 07 47 30.5384617494 +70 12 24.198261184       6.7   G6V 80 0
20 HD 69076 PM* 08 15 07.7249321962 -06 55 08.087343830   9.01 8.26     K0V 45 0
21 V* V478 Hya BY* 08 22 49.9528448767 +01 51 33.554224835   9.30 8.711   7.999 G1/2V 85 2
22 HD 72687 * 08 33 15.3791970197 -29 57 23.718925835   8.92 8.26     G5V 47 0
23 HD 77407 ** 09 03 27.0836286593 +37 50 27.500788701       6.7   G0V+M3V-M6V 88 0
24 HD 82943 PM* 09 34 50.7352288445 -12 07 46.363303103   7.17 6.53     F9VFe+0.5 403 2
25 HD 85301 PM* 09 52 16.7699312976 +49 11 26.853810105       7.3   G5 63 0
26 HD 90905 PM* 10 29 42.2300405874 +01 29 28.039591756       6.5   G1V 71 0
27 HD 104860 PM* 12 04 33.7309194735 +66 20 11.714041465   8.50 7.91     G0/F9V 71 0
28 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 224 0
29 * 70 Vir PM* 13 28 25.8081883620 +13 46 43.642951116 5.930 5.680 4.970 4.37 3.98 G4Va 670 1
30 HD 122652 PM* 14 02 31.6386077760 +31 39 39.088737566   7.69 7.15     F8 68 0
31 HD 134319 BY* 15 05 49.9042264447 +64 02 49.941455806   9.05 8.41 8.0   G5V: 111 0
32 HD 135363 ** 15 07 56.2503196449 +76 12 02.714809400       8.1   G5V+M2V-M4V 62 0
33 HD 136923 PM* 15 22 46.8339041095 +18 55 08.259017204 8.315 7.932 7.123 6.697 6.302 G9V 70 0
34 HD 143006 Or* 15 58 36.9127773803 -22 57 15.221492622   10.92 10.14   8.70 G5IVe 168 0
35 HD 145229 PM* 16 09 26.6276341871 +11 34 28.047846746   8.03 7.44     G0 63 0
36 [T64] 6 Em* 16 12 39.1668724365 -18 59 28.460261730   15.5   13.99 11.84 K2.5IV 21 1
37 CD-22 11432 TT* 16 14 11.0697507472 -23 05 36.071480044   11.90 10.70   9.255 K2IV 66 0
38 BD-21 4369 BY* 16 29 48.6929181158 -21 52 11.930870950   12.54 11.315   9.740 K2IVe 41 0
39 HD 150706 PM* 16 31 17.5833539505 +79 47 23.199471923   7.622 7.016     G0 179 1
40 WRAY 15-1880 TT* 18 42 57.9812315659 -35 32 42.824626801   12.91 11.77     K2 44 0
41 2MASS J18521730-3700119 TT* 18 52 17.3009516263 -37 00 11.951133600   12.7 12.194   10.842 K7V 43 0
42 HD 187897 PM* 19 52 09.3864855855 +07 27 36.160166614   7.75 7.13     G5 76 0
43 HD 191089 PM* 20 09 05.2158287736 -26 13 26.520539765   7.62 7.18     F5V 115 0
44 HD 201219 PM* 21 07 56.5198482794 +07 25 58.594323368       7.6   G5 55 0
45 HD 204277 PM* 21 27 06.6144955041 +16 07 26.945052672   7.226 6.725     F8V 53 0
46 HD 205905 PM* 21 39 10.1510425032 -27 18 23.666026265   7.36 6.74     G1.5IV-V 79 0
47 HD 206374 PM* 21 41 06.1971622745 +26 45 02.395916138   8.16   7.0   G6.5V 77 0
48 V* KZ And BY* 23 09 57.3641653876 +47 57 30.042914842   8.841 7.912     K2-Ve 118 0
49 HD 219498 PM* 23 16 05.0252464828 +22 10 34.824758804   9.77 9.05     G5 21 0

    Equat.    Gal    SGal    Ecl

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2020.08.13-02:56:17

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