2015A&A...581A..80R


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.14CEST08:55:08

2015A&A...581A..80R - Astronomy and Astrophysics, volume 581A, 80-80 (2015/9-1)

Detection limits with spectral differential imaging data.

RAMEAU J., CHAUVIN G., LAGRANGE A.-M., MAIRE A.-L., BOCCALETTI A. and BONNEFOY M.

Abstract (from CDS):

Direct imaging of exoplanets is polluted by speckle noise that severely limits the achievable contrast. Angular and spectral differential imaging have been proposed to make use of the temporal and chromatic properties of the speckles. Both modes, associated with extreme adaptive-optics and coronagraphy, are at the core of the new generation of planet imagers SPHERE and GPI. We aim to illustrate and characterize the impact of the SDI and SDI+ADI (ASDI) data reduction on the detection of giant planets. We also propose an unbiased method to derive the detection limits from SDI/ASDI data. Observations of AB Dor B and β Pictoris made with VLT/NaCo were used to simulate and quantify the effects of SDI and ASDI. The novel method is compared to the traditional injection of artificial point sources. The SDI reduction process creates a typical radial positive-negative pattern of any point-source. Its characteristics and its self-subtraction depend on the separation, but also on the spectral properties of the object. This work demonstrates that the self-subtraction cannot be reduced to a simple geometric effect. As a consequence, the detection performances of SDI observations cannot be expressed as a contrast in magnitude with the central star without the knowledge of the spectral properties of detectable companions. In addition, the residual noise cannot be converted into contrast and physical characteristics (mass, temperature) by standard calibration of flux losses. The proposed method takes the SDI bias into account to derive detection limits without the cost of massively injecting artificial sources into the data. Finally, the sensitivity of ASDI observations can be measured only with a control parameter on the algorithms that controls the minimum rotation that is necessary to build the reference image.

Abstract Copyright:

Journal keyword(s): instrumentation: adaptive optics - techniques: high angular resolution - planets and satellites: detection - methods: data analysis

Simbad objects: 19

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Number of rows : 19

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME GU Psc b BD* 01 12 35.0519481316 +17 03 55.571226067           T3.5 43 0
2 NAME 2MASS 0122-2439 b Pl 01 22 50.9353253987 -24 39 50.693320318           ~ 20 1
3 HD 36705B ** 05 28 44.4833327579 -65 26 46.034324029     13.0     M5+M5-6 83 0
4 HD 36705 TT* 05 28 44.8916324761 -65 26 55.289846904 8.259 7.856 6.999 6.496 5.993 K0V 907 0
5 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1596 1
6 HD 44627 BY* 06 19 12.9129838711 -58 03 15.524890610   10.01 9.205   8.185 K1V(e) 131 2
7 HD 44627B BD* 06 19 12.94 -58 03 20.9           L1 105 1
8 2MASS J11101001+0116130 BD* 11 10 10.011 +01 16 13.09           T5.5 58 0
9 TWA 27 BD* 12 07 33.467 -39 32 54.00     19.95 17.99 15.88 M8Ve 303 1
10 * e Vir b Pl 13 16 46.51596 +09 25 26.9590           ~ 72 1
11 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 425 1
12 NAME 1RXS1609 b Pl 16 09 30.3076191853 -21 04 58.945280778           ~ 88 1
13 2MASS J17410280-4642218 BD* 17 41 02.807 -46 42 21.85           L5:gamma 13 0
14 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2470 0
15 2MASS J21140802-2251358 BD* 21 14 08.026 -22 51 35.84           L7+1 66 0
16 HD 206860B BD* 21 44 28.47168 +14 46 07.7988           T2.5 77 0
17 NAME CFBDSIR J214947.2-040308.9 BD* 21 49 47.20 -04 03 08.9           T7 26 0
18 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 853 1
19 HD 218396b Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 184 1

    Equat.    Gal    SGal    Ecl

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2019.10.14-08:55:08

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