2010A&A...515A..95S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.14CEST04:18:23

2010A&A...515A..95S - Astronomy and Astrophysics, volume 515, A95-95 (2010/6-1)

Warm dusty discs: exploring the A star 24 µm debris population.

SMITH R. and WYATT M.C.

Abstract (from CDS):

Studies of the debris disc phenomenon have shown that most systems are analogous to the Edgeworth-Kuiper belt (EKB). In this study we aim to determine how many of the IRAS 25µm excesses towards A stars, which may be indicative of asteroid belt analogues, are real, and investigate where the dust must lie and so build up a picture of what these systems are like. We observe using ground-based mid-infrared imaging with TIMMI2, VISIR, Michelle and TReCS a sample of A and B-type main sequence stars previously reported as having mid-infrared excess. We combine modelling of the emission spectrum from multi-wavelength photometry with a modelling technique designed to constrain the radial extent of emission in mid-infrared imaging to constrain the possible location of the debris. We independently confirm the presence of warm dust around three of the candidates: HD 3003, HD 80950 and η Tel. For the binary HD3003 a stability analysis indicates the dust is either circumstellar and lying at ∼4AU with the binary orbiting at >14AU, or the dust lies in an unstable location; there is tentative evidence for temporal evolution of its excess emission on a ∼20 year timescale. For 7 of the targets we present quantitative limits on the location of dust around the star based on the unresolved imaging. We demonstrate that the disc around HD71155 must have multiple spatially distinct components at 2 and 60AU. We model the limits of current instrumentation to resolve debris disc emission and show that most of the known A star debris discs which could be readily resolved at 18 µm on 8m instruments have been resolved, but identify several that could be resolved with deep (>8h total) integrations (such as HD19356, HD139006 and HD102647). Limits from unresolved imaging can help distinguish between competing models of the disc emission, but resolved imaging is key to an unambiguous determination of the disc location. Modelling of the detection limits for extended emission can be useful for targeting future observational campaigns towards sources most likely to be resolved. MIRI on the JWST will be able to resolve the majority of the known A star debris disc population. METIS on the E-ELT will provide the opportunity to explore the hot disc population more thoroughly by detecting extended emission down to where calibration accuracy limits disc detection through photometry alone, reaching levels below 1 zodi for stars within 10pc.

Abstract Copyright:

Journal keyword(s): circumstellar matter - techniques: high angular resolution - infrared: stars

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 * bet03 Tuc ** 00 32 43.9055907013 -63 01 53.397968811 5.15 5.13 5.09     A0V 107 0
2 * 49 Cet PM* 01 34 37.7788265080 -15 40 34.898112472   5.667 5.607   5.54 A1V 229 0
3 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1062 1
4 * bet Per Al* 03 08 10.1324535 +40 57 20.328013 1.70 2.07 2.12 2.08 2.11 B8V 1134 2
5 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1657 1
6 HD 23281 * 03 43 33.8334560788 -10 29 08.360757051 5.88 5.80 5.61 5.40 5.30 A5III-IV 78 0
7 * 21 Tau PM* 03 45 54.4767610858 +24 33 16.241816694 5.49 5.72 5.76 5.71 5.74 B8V 192 0
8 Ced 19h ISM 03 46.0 +24 34           ~ 2 0
9 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2904 0
10 * pi.01 Ori PM* 04 54 53.7287660 +10 09 02.995200   4.723 4.648     A0Va_lB 236 0
11 HD 32297 * 05 02 27.4357771761 +07 27 39.682335894   8.32 8.14     A0V 137 0
12 HD 38206 * 05 43 21.6709387268 -18 33 26.906533478   5.711 5.727   5.72 A0V 89 0
13 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 277 0
14 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1596 1
15 * lam Gem PM* 07 18 05.57977 +16 32 25.3905   3.674 3.559     A4IV 229 0
16 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 450 2
17 * 30 Mon PM* 08 25 39.6320108 -03 54 23.117820 3.85 3.88 3.90 3.87 3.92 A0Va 256 0
18 * eta Cha * 08 41 19.5144242735 -78 57 48.102318990 5.02 5.351 5.453     B8V 208 0
19 HD 80950 * 09 17 27.5700510873 -74 44 04.522381833   5.844 5.857     A0V 43 0
20 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 533 0
21 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.69 4.31     F2V 269 0
22 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 533 1
23 * alf CrB Al* 15 34 41.26800 +26 42 52.8940 2.19 2.22 2.24 2.21 2.25 A1IV 451 0
24 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 454 0
25 * eps Ser PM* 15 50 48.9662218 +04 28 39.831153   3.844 3.693     kA2hA5mA7V 180 0
26 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2470 0
27 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 221 0
28 * eta Tel ** 19 22 51.20620 -54 25 26.1473   5.035 5.020   4.99 A0V+M7/8V 179 0
29 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 214 0
30 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1097 3

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2019.10.14-04:18:23

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