2001A&A...367..371B

Query : 2001A&A...367..371B

2001A&A...367..371B - Astronomy and Astrophysics, volume 367371-380 (2001/2-3)

Dark-speckle coronagraphic detection of binary stars in the near-IR.

BOCCALETTI A., MOUTOU C., MOUILLET D., LAGRANGE A.-M. and AUGEREAU J.-C.

Abstract (from CDS):

In this paper, we present the first attempt to obtain images of binary stars in the near IR using the dark-speckle method on the 3.6 m telescope at La Silla. Promising results are presented, despite the effect of the detector high read-out noise affecting the efficiency of speckle observations. We give some comparisons with the long exposure method. We derive in these data a reliable limit of detection for binary star companions, around mK<4 stars, which is about ΔmK≃6-7 for angular separations ranging from 0.5'' to 0.9''.

Abstract Copyright: ∼

Journal keyword(s): methods: data analysis - techniques: interferometric - instrumentation: adaptives optics - binaries: close - planetary systems

Simbad objects: 24

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Number of rows : 24
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * eta Psc ** 01 31 29.0081880156 +15 20 44.994632991 5.320 4.600 3.620 2.90 2.40 G7IIIa 255 0
2 * omi Psc PM* 01 45 23.6252151720 +09 09 27.902640312 5.90 5.22 4.26 3.53 3.04 G8III 174 0
3 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1586 0
4 V* AB Dor TT* 05 28 44.8712165880 -65 26 55.199147208 8.259 7.856 6.999 6.496 5.993 K0V 1080 0
5 * eps Car ** 08 22 30.83526 -59 30 34.1431 3.32 3.13 1.86     K3:III+B2:V 98 0
6 HD 91416 ** 10 32 51.2619322752 -26 36 34.015704408   9.14 7.52     M0/1III 15 0
7 * pi. Hya PM* 14 06 22.2980035207 -26 40 56.501676257 5.45 4.41 3.28 2.40 1.85 K2-IIIFe-0.5 150 0
8 * tet Cen PM* 14 06 40.94752 -36 22 11.8371 3.94 3.04 2.05 1.29 0.76 K0-IIIb 262 1
9 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 525 0
10 * bet01 Sco bC* 16 05 26.2319826 -19 48 19.630018 1.68 2.55 2.62 2.60 2.69 B1V 577 0
11 * ups Oph SB* 16 27 48.1733121458 -08 22 18.415622756   4.80 4.63     kA2hA5VmA5 144 0
12 V* V2215 Oph RS* 17 16 13.3624141798 -26 32 46.136563394   7.50 6.34   4.8 K5V 334 0
13 * alf Oph ** 17 34 56.06945 +12 33 36.1346 2.32 2.22 2.07 1.93 1.85 A5IVnn 495 0
14 * gam Oph PM* 17 47 53.5605898827 +02 42 26.204838837 3.83 3.80 3.75 3.71 3.71 A1VnkA0mA0 411 0
15 * nu. Oph PM* 17 59 01.5922136612 -09 46 25.080976810 5.20 4.33 3.34 2.64 2.16 G9IIIa 226 1
16 HD 170657 PM* 18 31 18.9610074312 -18 54 31.729814604 8.217 7.678 6.810 6.324 5.897 K2V 146 0
17 * 29 Sgr V* 18 49 40.1079977424 -20 19 28.756704684   6.615 5.210     K2III 42 0
18 * tau Sgr PM* 19 06 56.4031131168 -27 40 13.496293992 5.65 4.51 3.31 2.44 1.85 K1.5IIIb 164 0
19 HD 184713 ** 19 38 10.9542139488 -50 27 33.537154248   10.03 8.91     K0III 12 0
20 * alf01 Cap ** 20 17 38.8691281056 -12 30 29.563869708 6.14 5.34 4.27 3.49 2.94 G3Ib 142 0
21 * alf02 Cap PM* 20 18 03.2555957142 -12 32 41.467632703 5.20 4.51 3.58 2.91 2.42 G9III 181 0
22 * rho Cap ** 20 28 51.61448 -17 48 49.2693           F2V 142 0
23 HD 222493 PM* 23 41 08.9122868619 -11 40 50.345125880   6.92 5.92     K0III 50 0
24 HD 223170 HB* 23 47 15.9119280096 -11 54 40.061255796   6.805 5.731     K0III 43 0

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