2010A&A...518A..40N


Query : 2010A&A...518A..40N

2010A&A...518A..40N - Astronomy and Astrophysics, volume 518, A40-40 (2010/7-2)

Kuiper belts around nearby stars.

NILSSON R., LISEAU R., BRANDEKER A., OLOFSSON G., PILBRATT G.L., RISACHER C., RODMANN J., AUGEREAU J.-C., BERGMAN P., EIROA C., FRIDLUND M., THEBAULT P. and WHITE G.J.

Abstract (from CDS):

The existence of dusty debris disks around a large fraction of solar type main-sequence stars, inferred from excess far-IR and submillimetre emission compared to that expected from stellar photospheres, suggests that leftover planetesimal belts analogous to the asteroid- and comet reservoirs of the solar system are common. Sensitive submillimetre observations are essential to detect and characterise cold extended dust originating from collisions of small bodies in disks, belts, or rings at Kuiper-belt distances (30-50AU or beyond). Measurements of the flux densities at these wavelengths will extend existing IR photometry and permit more detailed modelling of the Rayleigh-Jeans tail of the disks spectral energy distribution (SED), effectively constraining dust properties and disk extensions. By observing stars spanning from a few up to several hundred Myr, the evolution of debris disks during crucial phases of planet formation can be studied. We observed 22 exo-Kuiper-belt candidates at 870µm, as part of a large programme with the LABOCA bolometer at the APEX telescope. Dust masses (or upper limits) were calculated from integrated 870µm fluxes, and fits to the SED of detected sources revealed the fractional dust luminosities fdust, dust temperatures Tdust, and power-law exponents β of the opacity law. A total of 10 detections with at least 3σ significance were made, out of which five (HD95086, HD131835, HD161868, HD170773, and HD207129) have previously never been detected at submillimetre wavelengths. Three additional sources are marginally detected with >2.5σ significance. The best-fit β parameters all lie between 0.1 and 0.8, in agreement with previous results indicating the presence of significantly larger grains than those in the ISM. From our relatively small sample we estimate fdust∝t–α, with α∼0.8-2.0, and identify an evolution of the characteristic radial dust distance Rdust that is consistent with the t1/3 increase predicted from models of self-stirred collisions in debris disks.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planetary systems - planets and satellites: formation - Kuiper belt: general - submillimeter: planetary systems

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 - 2023
#notes
1 HD 105 PM* 00 05 52.5447817152 -41 45 11.044988352   8.13 7.53     G0V 171 0
2 HD 377 PM* 00 08 25.7454555168 +06 37 00.489407808   8.22 7.59   6.90 G2V 136 0
3 HD 8907 PM* 01 28 34.3596466296 +42 16 03.688114260   7.15 6.66     F8 84 0
4 * gam Tri PM* 02 17 18.8670335 +33 50 49.895049   4.03 4.00   4.05 A1Vnn 191 0
5 HD 15115 PM* 02 26 16.2457848552 +06 17 33.186453252   7.15 6.80   6.33 F4IV 185 0
6 * tau01 Eri PM* 02 45 06.1988006895 -18 34 21.442179919 4.94 4.94 4.46 4.03 3.76 F7V 219 0
7 HD 17390 PM* 02 46 45.1042039656 -21 38 22.278982308   6.850 6.469     F3IV/V 54 0
8 HD 21997 PM* 03 31 53.6470102728 -25 36 50.940001116   6.501 6.372   6.25 A3IV/V 145 0
9 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1837 1
10 Cl Melotte 22 OpC 03 46 24 +24 06.8           ~ 3279 0
11 HD 25457 TT* 04 02 36.7442719512 -00 16 08.119921152   5.88 5.38     F7V 257 0
12 HD 30447 * 04 46 49.5286580976 -26 18 08.851615452   8.25 7.86   7.39 F3V 73 0
13 HD 31392 PM* 04 54 04.2085021752 -35 24 16.263520632   8.40 7.61     G9V 80 0
14 V* V1005 Ori BY* 04 59 34.8342878424 +01 47 00.669818328   11.48 10.107 9.603 8.239 M0Ve 327 0
15 HD 32297 * 05 02 27.4358754192 +07 27 39.678553260   8.32 8.14     A0V 179 0
16 * gam Lep PM* 05 44 27.7906169580 -22 26 54.187756254 4.08 4.07 3.60 3.15 2.89 F6V 417 0
17 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1814 1
18 HD 39944 PM* 05 54 43.1950949280 -25 34 40.295379036   10.10 9.56     G1V 12 0
19 * psi05 Aur PM* 06 46 44.3369350032 +43 34 38.728429752       4.9   F9V 247 0
20 HD 61005 PM* 07 35 47.4623556456 -32 12 14.045086368   8.96 8.22     G8Vk 210 0
21 HD 78702 PM* 09 09 04.2106655736 -18 19 42.785652648   5.724 5.722     A0/1V 41 0
22 HD 95086 * 10 57 03.0215719872 -68 40 02.449216128   7.60 7.36     A8III 158 1
23 HD 98800B SB* 11 22 05.288454 -24 46 39.04974   11.18 9.92     ~ 123 1
24 HD 98800 TT* 11 22 05.28975 -24 46 39.7571   10.20 9.28 9.26 7.386 K5V(e) 359 0
25 HD 104860 PM* 12 04 33.7308619800 +66 20 11.712857172   8.50 7.91     G0/F9V 86 0
26 HD 107146 PM* 12 19 06.5018840304 +16 32 53.867731128   7.61   6.7   G2V 258 0
27 * eta Crv PM* 12 32 04.2264018482 -16 11 45.618615379   4.658 4.294     F2V 306 0
28 HD 109573 PM* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774 7.25 5.81 A0V 603 1
29 HD 123160 * 14 06 12.8537830392 -11 49 57.866749680   10.19 8.65     K5III 25 0
30 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 710 0
31 * sig Boo PM* 14 34 40.8173867232 +29 44 42.457673940 4.76 4.84 4.47 4.13 3.94 F4VkF2mF1 592 0
32 HD 131835 * 14 56 54.4677661992 -35 41 43.658813184   8.05 7.86     A2IV 111 0
33 * g Lup PM* 15 41 11.3768069149 -44 39 40.341696305   5.036 4.633     F3/5V 194 0
34 V* GQ Lup Or* 15 49 12.1053805848 -35 39 05.058139788 12.19 12.76 11.66 11.15   K7Ve 268 1
35 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 510 0
36 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 259 1
37 * gam Oph PM* 17 47 53.5597327 +02 42 26.199985 3.83 3.80 3.75 3.71 3.71 A1VnkA0mA0 381 0
38 HD 164249 PM* 18 03 03.4097283792 -51 38 56.432149872   7.438 7.007 7.90   F6V 112 0
39 HD 170773 PM* 18 33 00.9167301456 -39 53 31.275122964   6.630 6.217     F5V 70 0
40 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2623 0
41 HD 181327 PM* 19 22 58.9437222504 -54 32 16.975668624   7.50 7.04   6.49 F6V 268 0
42 HD 191089 SB? 20 09 05.2156358688 -26 13 26.520165768   7.62 7.18     F5V 137 0
43 HD 193307 PM* 20 21 41.0365243245 -49 59 57.900101995   6.82 6.28     F9V 123 0
44 * phi01 Pav PM* 20 35 34.8500676912 -60 34 54.296843484   5.036 4.745     F0V 79 0
45 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1056 0
46 HD 207129 PM* 21 48 15.7511634187 -47 18 13.017893348   6.18 5.58     G2V 315 0
47 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1195 3
48 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1058 0
49 NAME Local Bubble ISM ~ ~           ~ 821 0

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2023.01.30-22:27:28

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