2020A&A...634A..69H


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.17CET15:00:56

2020A&A...634A..69H - Astronomy and Astrophysics, volume 634A, 69-69 (2020/2-1)

RefPlanets: Search for reflected light from extrasolar planets with SPHERE/ZIMPOL.

HUNZIKER S., SCHMID H.M., MOUILLET D., MILLI J., ZURLO A., DELORME P., ABE L., AVENHAUS H., BARUFFOLO A., BAZZON A., BOCCALETTI A., BAUDOZ P., BEUZIT J.L., CARBILLET M., CHAUVIN G., CLAUDI R., COSTILLE A., DABAN J.-B., DESIDERA S., DOHLEN K., DOMINIK C., DOWNING M., ENGLER N., FELDT M., FUSCO T., GINSKI C., GISLER D., GIRARD J.H., GRATTON R., HENNING T., HUBIN N., KASPER M., KELLER C.U., LANGLOIS M., LAGADEC E., MARTINEZ P., MAIRE A.L., MENARD F., MEYER M.R., PAVLOV A., PRAGT J., PUGET P., QUANZ S.P., RICKMAN E., ROELFSEMA R., SALASNICH B., SAUVAGE J.-F., SIEBENMORGEN R., SISSA E., SNIK F., SUAREZ M., SZULAGYI J., THALMANN C., TURATTO M., UDRY S., VAN HOLSTEIN R.G., VIGAN A. and WILDI F.

Abstract (from CDS):

Aims. RefPlanets is a guaranteed time observation programme that uses the Zurich IMaging POLarimeter (ZIMPOL) of Spectro-Polarimetric High-contrast Exoplanet REsearch instrument at the Very Large Telescope to perform a blind search for exoplanets in wavelengths from 600 to 900 nm. The goals of this study are the characterisation of the unprecedented high polarimetic contrast and polarimetric precision capabilities of ZIMPOL for bright targets, the search for polarised reflected light around some of the closest bright stars to the Sun, and potentially the direct detection of an evolved cold exoplanet for the first time. Methods. For our observations of α Cen A and B, Sirius A, Altair, e Eri and τ Ceti we used the polarimetricdifferential imaging (PDI) mode of ZIMPOL which removes the speckle noise down to the photon noise limit for angular separations ≳ 0.6''. We describe some of the instrumental effects that dominate the noise for smaller separations and explain how to remove these additional noise effects in post-processing. We then combine PDI with angular differential imaging as a final layer of post-processing to further improve the contrast limits of our data at these separations. Results. For good observing conditions we achieve polarimetric contrast limits of 15.0-16.3mag at the effective inner working angle of ∼0.13'', 16.3-18.3mag at 0.5'', and 18.8-20.4mag at 1.5''. The contrast limits closer in (≲0.6'') display a significant dependence on observing conditions, while in the photon-noise-dominated regime (≳0.6'') the limits mainly depend on the brightness of the star and the total integration time. We compare our results with contrast limits from other surveys and review the exoplanet detection limits obtained with different detection methods. For all our targets we achieve unprecedented contrast limits. Despite the high polarimetric contrasts we are not able to find any additional companions or extended polarised light sources in the data obtained so far.

Abstract Copyright: © S. Hunziker et al. 2020

Journal keyword(s): instrumentation: high angular resolution - methods: data analysis - methods: observational - techniques: polarimetric - techniques: image processing - planets and satellites: detection

Simbad objects: 16

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Number of rows : 16

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 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1110 1
2 HD 13445 PM* 02 10 25.9190575041 -50 49 25.467227759   6.945 6.117     K1.5V 421 1
3 * eps Eri b Pl 03 32 55.8449634 -09 27 29.731165           ~ 104 1
4 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1726 1
5 HD 41004A PM* 05 59 49.6473573887 -48 14 22.805780232           ~ 29 1
6 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A1V+DA 1410 0
7 * alf Leo PM* 10 08 22.31099 +11 58 01.9516 0.88 1.24 1.40 1.37 1.47 B8IVn 814 1
8 NAME Proxima Centauri b Pl 14 29 42.9451234609 -62 40 46.170818907           ~ 235 0
9 NAME Proxima Centauri Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1004 0
10 * alf Cen ** 14 39 29.71993 -60 49 55.9990   0.4 -0.1     G2V+K1V 837 0
11 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 908 1
12 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1150 0
13 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 827 0
14 HD 196885 PM* 20 39 51.8753142885 +11 14 58.702911143   6.92 6.385 6.32   F8V 164 1
15 BD-15 6290b Pl 22 53 16.7323107416 -14 15 49.303409936           ~ 220 1
16 * gam Cep SB* 23 39 20.9015326708 +77 37 56.505477975 5.190 4.250   2.6   K1III-IVCN1 555 1

    Equat.    Gal    SGal    Ecl

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