2013A&A...555A.104A


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.25CET09:37:46

2013A&A...555A.104A - Astronomy and Astrophysics, volume 555A, 104-104 (2013/7-1)

A near-infrared interferometric survey of debris-disc stars. III. First statistics based on 42 stars observed with CHARA/FLUOR.

ABSIL O., DEFRERE D., COUDE DU FORESTO V., DI FOLCO E., MERAND A., AUGEREAU J.-C., ERTEL S., HANOT C., KERVELLA P., MOLLIER B., SCOTT N., CHE X., MONNIER J.D., THUREAU N., TUTHILL P.G., TEN BRUMMELAAR T.A., McALISTER H.A., STURMANN J., STURMANN L. and TURNER N.

Abstract (from CDS):

Dust is expected to be ubiquitous in extrasolar planetary systems owing to the dynamical activity of minor bodies. Inner dust populations are, however, still poorly known because of the high contrast and small angular separation with respect to their host star, and yet, a proper characterisation of exozodiacal dust is mandatory for the design of future Earth-like planet imaging missions. We aim to determine the level of near-infrared exozodiacal dust emission around a sample of 42 nearby main sequence stars with spectral types ranging from A to K and to investigate its correlation with various stellar parameters and with the presence of cold dust belts. We use high-precision K-band visibilities obtained with the FLUOR interferometer on the shortest baseline of the CHARA array. The calibrated visibilities are compared with the expected visibility of the stellar photosphere to assess whether there is an additional, fully resolved circumstellar emission source. Near-infrared circumstellar emission amounting to about 1% of the stellar flux is detected around 13 of our 42 target stars. Follow-up observations showed that one of them (eps Cep) is associated with a stellar companion, while another one was detected around what turned out to be a giant star (kap CrB). The remaining 11 excesses found around single main sequence stars are most probably associated with hot circumstellar dust, yielding an overall occurrence rate of 28+8–6% for our (biased) sample. We show that the occurrence rate of bright exozodiacal discs correlates with spectral type, K-band excesses being more frequent around A-type stars. It also correlates with the presence of detectable far-infrared excess emission in the case of solar-type stars. This study provides new insight into the phenomenon of bright exozodiacal discs, showing that hot dust populations are probably linked to outer dust reservoirs in the case of solar-type stars. For A-type stars, no clear conclusion can be made regarding the origin of the detected near-infrared excesses.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planetary systems - binaries: close - stars: fundamental parameters - techniques: interferometric

Simbad objects: 51

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Number of rows : 51

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 * bet Cas dS* 00 09 10.68518 +59 08 59.2120 2.73 2.61 2.27 1.97 1.77 F2III 498 0
2 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 532 1
3 * eta Cas PM* 00 49 06.2907161 +57 48 54.675740 4.04 4.02 3.44 2.94 2.58 F9V+M0-V 601 0
4 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 895 1
5 * 107 Psc PM* 01 42 29.7634932653 +20 16 06.660242064 6.57 6.08 5.24 4.55 4.12 K1V 510 0
6 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1105 1
7 * tet Per PM* 02 44 11.9870420 +49 13 42.411120 4.62 4.62 4.11 3.67 3.37 F8V 383 0
8 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1720 1
9 * 10 Tau PM* 03 36 52.1448022536 +00 23 58.536917738 5.23 5.15 4.30 4.09 3.77 F9IV-V 526 0
10 * pi.03 Ori PM* 04 49 50.4109057 +06 57 40.588294 3.620 3.630 3.190 2.77 2.51 F6V 528 0
11 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 282 0
12 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1676 1
13 * eta Lep PM* 05 56 24.2930042 -14 10 03.718884 4.05 4.05 3.72 3.39 3.23 F2V 318 0
14 * ksi Gem PM* 06 45 17.3643205 +12 53 44.131127 3.85 3.79 3.36 2.97 2.74 F5IV-V 202 0
15 * lam Gem PM* 07 18 05.5801227701 +16 32 25.396438474   3.674 3.559     A4IV 232 0
16 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 471 1
17 * 30 Mon PM* 08 25 39.6320108 -03 54 23.117820 3.85 3.88 3.90 3.87 3.92 A0Va 259 0
18 * bet UMa PM* 11 01 50.4765370 +56 22 56.733912 2.35 2.35 2.37 2.31 2.35 A1IVps 411 1
19 * del Leo PM* 11 14 06.50142 +20 31 25.3853 2.79 2.68 2.53 2.44 2.41 A5IV(n) 265 0
20 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 544 0
21 * bet Vir PM* 11 50 41.7182390 +01 45 52.991019 4.26 4.15 3.60 3.13 2.85 F9V 859 0
22 * del UMa PM* 12 15 25.5606327 +57 01 57.415606 3.460 3.410 3.320 3.25 3.25 A2Vn 282 0
23 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.658 4.294     F2V 281 0
24 HD 113766 ** 13 06 35.83622 -46 02 02.0178   7.91 7.56     F3/5V 95 1
25 * 70 Vir PM* 13 28 25.8081883620 +13 46 43.642951116 5.930 5.680 4.970 4.37 3.98 G4Va 675 1
26 * iot Vir PM* 14 16 00.8695049 -06 00 01.963348 4.64 4.60 4.08     F7III 335 0
27 * sig Boo PM* 14 34 40.8171808483 +29 44 42.463685978 4.76 4.84 4.47 4.13 3.94 F4VkF2mF1 573 0
28 * ksi Boo BY* 14 51 23.37993 +19 06 01.6994 5.618 5.370 4.593 3.91 3.48 G7Ve+K5Ve 436 0
29 * alf CrB Al* 15 34 41.26800 +26 42 52.8940 2.19 2.22 2.24 2.21 2.25 A1IV 457 0
30 * lam Ser PM* 15 46 26.6144291449 +07 21 11.041647444 5.13 5.03 4.42 3.92 3.60 G0-V 536 0
31 * kap CrB PM* 15 51 13.9314685012 +35 39 26.564729663 6.69 5.82 4.82 4.06 3.57 K1IVa 237 1
32 * chi Her PM* 15 52 40.5411372117 +42 27 05.451105113 5.19 5.19 4.62 4.14 3.82 F8VFe-2Hdel-1 479 0
33 * gam Ser PM* 15 56 27.1826948 +15 39 41.820500 4.31 4.34 3.84 3.37 3.13 F6V 533 0
34 * mu.01 Her ** 17 46 27.5266778 +27 43 14.437984 4.56 4.17 3.42 2.89 2.51 G5IV 654 0
35 * gam Oph PM* 17 47 53.5597327 +02 42 26.199985 3.83 3.80 3.75 3.71 3.71 A1VnkA0mA0 361 0
36 * 70 Oph A SB* 18 05 27.370543 +02 29 59.31669       3.6   K0V 207 0
37 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2524 0
38 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 239 0
39 * 110 Her PM* 18 45 39.7257041 +20 32 46.717099 4.66 4.65 4.19 3.80 3.54 F5.5IV-V 382 0
40 * gam Lyr * 18 58 56.6224137 +32 41 22.400295 3.140 3.200 3.250 3.27 3.28 B9III 267 0
41 * eps Aql SB* 18 59 37.3616087625 +15 04 05.880705609 6.14 5.10 4.02 3.26 2.74 K1-IIICN0.5 179 0
42 * zet Aql PM* 19 05 24.6080155 +13 51 48.518212 2.99 3.00 2.99 2.98 2.98 A0IV-Vnn 324 0
43 * sig Dra PM* 19 32 21.5902990 +69 39 40.234737 5.860 5.460 4.680 4.04 3.63 K0V 586 0
44 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 825 0
45 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 952 0
46 * 61 Cyg ** 21 06 53.95 +38 44 57.9           ~ 158 0
47 * 61 Cyg B Er* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 672 1
48 * sig Cyg sg* 21 17 24.9524404 +39 23 40.852798 3.98 4.37 4.24 4.06 3.92 A0Ia 251 0
49 * alf Cep PM* 21 18 34.77233 +62 35 08.0681 2.770 2.680 2.460 2.22 2.11 A8Vn 341 0
50 * eps Cep dS* 22 15 02.2114686271 +57 02 36.835994498   4.47   4.0   F0V(Sr) 218 0
51 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1129 3

    Equat.    Gal    SGal    Ecl

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2020.11.25-09:37:46

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