2008A&A...485..897S


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.09CET21:59:37

2008A&A...485..897S - Astronomy and Astrophysics, volume 485, 897-915 (2008/7-3)

The nature of mid-infrared excesses from hot dust around Sun-like stars.

SMITH R., WYATT M.C. and DENT W.R.F.

Abstract (from CDS):

Studies of the debris disk phenomenon have shown that most systems are analogous to the Edgeworth-Kuiper Belt (EKB). However a rare subset of sun-like stars possess dust which lies, in contrast, in the terrestrial planet region. In this study we aim to determine how many sources with apparent mid-infrared excess are truly hosts of warm dust, and investigate where the dust in these systems must lie. We observed using ground-based mid-infrared imaging with TIMMI2, VISIR and MICHELLE a sample of FGK main sequence stars previously reported to have hot dust. A new modelling approach was developed to determine the constraints that can be set on the radial extent of excess emission in such observations by demonstrating how the detectability of a disk of a given flux as a fraction of the total flux from the system (Fdisk/Ftotal) depends primarily on the ratio of disk radius to PSF width and on the uncertainty on that PSF width. We confirm the presence of warm dust around three of the candidates; η Corvi, HD145263 and HD202406. For η Corvi modelling constrains the dust to lie in regions smaller than ∼3.5AU. The modelling constrains the dust to regions smaller than 80-100AU for HD145263 and HD202406, with SED fitting suggesting the dust lies at a few tens of AU. Of two alternative models for the η Corvi excess emission, we find that a model with one hot dust component at less than 0.164" (<3AU) (combined with the known submm dust population at ∼150AU) fits all the data better at the 2.6σ level than an alternative model with two populations of dust emitting in the mid-infrared: hot dust at less than 0.19" (<3.5AU) and a mid-temperature component at ∼0.66" (12AU). We identify several systems which have a companion (HD65277 and HD79873) or background object (HD53246, HD123356 and HD128400) responsible for their mid-infrared excess, and for three other systems we were able to rule out a point-like mid-infrared source near the star at the level of excess observed in lower resolution observations (HD12039, HD69830 and HD191089). Hot dust sources are either young and possibly primordial or transitional in their emission, or have relatively small radius steady-state planetesimal belts, or they are old and luminous with transient emission. High resolution imaging can be used to constrain the location of the disk and help to discriminate between different models of disk emission. For some small disks, interferometry is needed to resolve the disk location.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planets and satellites: formation

CDS comments: Paragraph 7. HD 69380 is a probable misprint for HD 69830.

Simbad objects: 27

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Number of rows : 27

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 10800 SB* 01 37 55.5539674750 -82 58 29.967316861 6.58 6.48 5.87     G1V 80 1
2 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1069 1
3 V* DK Cet BY* 01 57 48.9776543901 -21 54 05.343324011   8.73 8.057   7.343 G4V 111 1
4 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1662 1
5 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1606 1
6 HD 53246 * 07 03 23.9583053036 -22 34 10.566127614   8.82 8.11     G6V 6 0
7 MSX5C G234.4643-07.5741 IR 07 03 30.2 -22 34 32           ~ 1 0
8 HD 65277 PM* 07 57 57.7842802784 -00 48 51.874649687   9.105 8.077     K4V 72 0
9 HD 65277B PM* 07 57 58.0722547212 -00 48 49.098554049           ~ 6 1
10 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 456 2
11 HD 79873 PM* 09 16 39.9780593316 +00 43 44.540224860   7.18 6.76     F3V 33 1
12 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 371 2
13 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.69 4.31     F2V 270 0
14 HD 123356 ** 14 07 33.882 -21 04 35.97   10.9 9.7     G1V 10 0
15 HD 123356B * 14 07 34.017 -21 04 37.51       11.61   ~ 3 1
16 HD 128400 PM* 14 41 52.4595434093 -75 08 22.124448333 7.725 7.482 6.765 6.381 6.015 G6V 61 2
17 2MASS J14421386-7508356 * 14 42 13.8582277203 -75 08 35.649717120           ~ 1 1
18 HD 145263 * 16 10 55.1055882785 -25 31 21.668325032   9.39 8.98     F2V 56 0
19 NAME Upper Sco Association As* 16 12 -23.4           ~ 964 1
20 HD 155826 ** 17 15 35.9021317723 -38 35 38.168900773   6.54 5.96     G0V 78 0
21 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2475 0
22 HD 191089 PM* 20 09 05.2158287736 -26 13 26.520539765   7.62 7.18     F5V 108 0
23 [DB2002b] G40.54-35.47 MoC 21 11.5 -09 43           ~ 14 0
24 [DB2002b] G41.00-35.85 MoC 21 13.6 -09 33           ~ 9 0
25 [DB2002b] G40.57-36.61 MoC 21 15.7 -10 11           ~ 9 0
26 HD 202406 * 21 15 55.0359748862 -09 23 28.118932382   8.18 7.82     F2IV/V 21 0
27 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1101 3

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2019.12.09-21:59:37

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