2014ApJ...797..119M


Query : 2014ApJ...797..119M

2014ApJ...797..119M - Astrophys. J., 797, 119 (2014/December-3)

Constraining the exozodiacal luminosity function of main-sequence stars: complete results from the Keck nuller mid-infrared surveys.

MENNESSON B., MILLAN-GABET R., SERABYN E., COLAVITA M.M., ABSIL O., BRYDEN G., WYATT M., DANCHI W., DEFRERE D., DORE O., HINZ P., KUCHNER M., RAGLAND S., SCOTT N., STAPELFELDT K., TRAUB W. and WOILLEZ J.

Abstract (from CDS):

Forty-seven nearby main-sequence stars were surveyed with the Keck Interferometer mid-infrared Nulling instrument (KIN) between 2008 and 2011, searching for faint resolved emission from exozodiacal dust. Observations of a subset of the sample have already been reported, focusing essentially on stars with no previously known dust. Here we extend this previous analysis to the whole KIN sample, including 22 more stars with known near- and/or far-infrared excesses. In addition to an analysis similar to that of the first paper of this series, which was restricted to the 8-9 µm spectral region, we present measurements obtained in all 10 spectral channels covering the 8-13 µm instrumental bandwidth. Based on the 8-9 µm data alone, which provide the highest signal-to-noise measurements, only one star shows a large excess imputable to dust emission (η Crv), while four more show a significant (>3σ) excess: β Leo, β UMa, ζ Lep, and γ Oph. Overall, excesses detected by KIN are more frequent around A-type stars than later spectral types. A statistical analysis of the measurements further indicates that stars with known far-infrared (λ ≥ 70 µm) excesses have higher exozodiacal emission levels than stars with no previous indication of a cold outer disk. This statistical trend is observed regardless of spectral type and points to a dynamical connection between the inner (zodi-like) and outer (Kuiper-Belt-like) dust populations. The measured levels for such stars are clustering close to the KIN detection limit of a few hundred zodis and are indeed consistent with those expected from a population of dust that migrated in from the outer belt by Poynting-Robertson drag. Conversely, no significant mid-infrared excess is found around sources with previously reported near-infrared resolved excesses, which typically have levels of the order of 1% over the photospheric flux. If dust emission is really at play in these near-infrared detections, the absence of a strong mid-infrared counterpart points to populations of very hot and small (submicron) grains piling up very close to the sublimation radius. For solar-type stars with no known infrared excess, likely to be the most relevant targets for a future exo-Earth direct imaging mission, we find that their median zodi level is 12±24 zodis and lower than 60 (90) zodis with 95% (99%) confidence, if a lognormal zodi luminosity distribution is assumed.

Abstract Copyright:

Journal keyword(s): circumstellar matter - infrared: stars - instrumentation: interferometers

Simbad objects: 53

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Number of rows : 53
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * bet Cas dS* 00 09 10.68518 +59 08 59.2120 2.73 2.61 2.27 1.97 1.77 F2III 509 0
2 * eta Cas PM* 00 49 06.2945942922 +57 48 54.638239716 4.04 4.02 3.44 2.94 2.58 F9V 619 0
3 * ups And PM* 01 36 47.8415443907 +41 24 19.651368029 4.70 4.64 4.10 3.64 3.35 F9V 922 1
4 * 107 Psc PM* 01 42 29.7625251280 +20 16 06.645657710 6.57 6.08 5.24 4.55 4.12 K1V 528 0
5 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1176 1
6 BD+20 307 SB* 01 54 50.3440413288 +21 18 22.461011784   9.57 9.01     G0 101 0
7 * bet Tri SB* 02 09 32.62712 +34 59 14.2694 3.26 3.14 3.00 2.86 2.78 A5III 212 0
8 * del Tri SB* 02 17 03.2303387763 +34 13 27.235383770 5.50 5.48   4.5   G0.5VFe-0.5 383 0
9 HD 15407 PM* 02 30 50.6559832920 +55 32 54.256925724   7.43 6.95     F5V 74 0
10 * tet Per PM* 02 44 11.9866154103 +49 13 42.414669174 4.62 4.62 4.11 3.67 3.37 F8V 396 0
11 * bet Per EB* 03 08 10.1324535 +40 57 20.328013 1.70 2.07 2.12 2.08 2.11 B8V 1183 1
12 * iot Per PM* 03 09 04.0193012009 +49 36 47.802053343 4.76 4.64   3.7   G0V 526 0
13 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 850 0
14 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1808 1
15 * 10 Tau PM* 03 36 52.3837044168 +00 24 05.992097829 5.23 5.15 4.30 4.09 3.77 F9IV-V 543 0
16 * pi.03 Ori PM* 04 49 50.4109057 +06 57 40.588294 3.620 3.630 3.190 2.77 2.51 F6V 553 0
17 * lam Aur PM* 05 19 08.4754499121 +40 05 56.585080940 5.46 5.33 4.71 4.18 3.86 G1.5IV-VFe-1 510 0
18 * gam Lep PM* 05 44 27.7906169580 -22 26 54.187756254 4.08 4.07 3.60 3.15 2.89 F6V 412 0
19 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 291 0
20 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1789 1
21 * chi01 Ori RS* 05 54 22.9829893 +20 16 34.222038 5.08 5.00 4.40 3.90 3.59 G0V 824 0
22 * eta Lep PM* 05 56 24.2934904501 -14 10 03.718335613 4.05 4.05 3.72 3.39 3.23 F2V 329 0
23 * lam Gem PM* 07 18 05.5789195368 +16 32 25.389581244   3.674 3.559     A4IV 244 0
24 HD 69830 PM* 08 18 23.9469682407 -12 37 55.817187530   6.74 5.95     G8:V 496 1
25 * omi Leo SB* 09 41 09.0330479 +09 53 32.310183 4.22 4.01 3.52 3.11 2.88 F8-G0III+A7m 149 0
26 HD 88230 Er* 10 11 22.1399492383 +49 27 15.251007087 9.23 7.94 6.61 5.36 4.56 K6VeFe-1 446 0
27 * 47 UMa PM* 10 59 27.9727514012 +40 25 48.920572724   5.66   4.7   G1-VFe-0.5 748 1
28 * bet UMa PM* 11 01 50.4765370 +56 22 56.733912 2.35 2.35 2.37 2.31 2.35 A1IVps 426 1
29 HD 95735 Er* 11 03 20.1948195942 +35 58 11.576182057 10.030 8.960 7.520 5.99 4.79 M2+V 673 0
30 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 562 0
31 * bet Vir PM* 11 50 41.7185158616 +01 45 53.001539131 4.26 4.15 3.60 3.13 2.85 F9V 895 0
32 * del UMa PM* 12 15 25.5606327 +57 01 57.415606 3.460 3.410 3.320 3.25 3.25 A2Vn 288 0
33 * eta Crv PM* 12 32 04.2264018482 -16 11 45.618615379   4.658 4.294     F2V 304 0
34 * bet Com PM* 13 11 52.3938268062 +27 52 41.462309460 4.92 4.84 4.25 3.77 3.47 F9.5V 872 0
35 * 61 Vir PM* 13 18 24.3139864471 -18 18 40.297748582 5.710 5.440 4.740     G6.5V 632 1
36 * 70 Vir PM* 13 28 25.8085908881 +13 46 43.638308807 5.930 5.680 4.970 4.37 3.98 G4Va 696 1
37 * tau Boo Ro* 13 47 15.7381720026 +17 27 24.809555600 5.02 4.98 4.49 4.09 3.85 F7IV-V 943 1
38 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 466 0
39 * alf CrB EB* 15 34 41.26800 +26 42 52.8940 2.19 2.22 2.24 2.21 2.25 A1IV 467 0
40 * kap CrB PM* 15 51 13.9312943632 +35 39 26.573691158 6.69 5.82 4.82 4.06 3.57 K1IVa 249 1
41 * gam Ser PM* 15 56 27.1826948 +15 39 41.820500 4.31 4.34 3.84 3.37 3.13 F6V 546 0
42 * gam Oph PM* 17 47 53.5597327 +02 42 26.199985 3.83 3.80 3.75 3.71 3.71 A1VnkA0mA0 378 0
43 * 70 Oph A SB* 18 05 27.2484131991 +02 30 00.526614953       3.6   K0V 213 0
44 * 70 Oph ** 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 629 0
45 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2600 0
46 * zet Aql PM* 19 05 24.6080155 +13 51 48.518212 2.99 3.00 2.99 2.98 2.98 A0IV-Vnn 335 0
47 * mu. Aql PM* 19 34 05.3529921054 +07 22 44.184329526 6.87 5.63 4.45 3.55 2.94 K3-IIIbFe0.5 258 1
48 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 848 0
49 * 61 Cyg A BY* 21 06 53.9395895022 +38 44 57.902349973 7.50 6.39 5.21 4.19 3.54 K5V 998 0
50 * alf Cep PM* 21 18 34.77233 +62 35 08.0681 2.770 2.680 2.460 2.22 2.11 A8Vn 347 0
51 * iot Peg SB* 22 07 00.6655101792 +25 20 42.356386464 4.190 4.200 3.770 3.36 3.11 F5V 434 1
52 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1185 3
53 * iot Psc PM* 23 39 57.0413764 +05 37 34.647529 4.640 4.620 4.120 3.68 3.37 F7V 599 0

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2022.08.10-06:13:01

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