Cubes polarization model Nulling maps at image plane Simple

2. Focal plane. P'. 1. X”. (P'). Crossed- cubes nuller. Monolithic telescope ... Institut de Planétologie et d'Astrophysique de Grenoble, Université Joseph Fourier, CNRS, B.P. 53, 38041 Grenoble – France ... parallel to both cubes SR layers.
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Cheapest nuller in the World: Crossed beamsplitter cubes François Hénault Institut de Planétologie et d’Astrophysique de Grenoble, Université Joseph Fourier, CNRS, B.P. 53, 38041 Grenoble – France Alain Spang Laboratoire Lagrange, Université de Nice-Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, B.P. 4229, 06304 Nice – France Cube 2

Principle

Cube 1 Beam 1

Beam 3

Y’ SubPupil 2

X’

0

SubPupil 1

Z SubPupil 3

Y’ Polarization Y’

0

X’

π

π

• 

0

π X’

SubPupil 4

• 

X’

• 

0

π

• 

Cubes polarization model

U

1 arcsec

1 arcsec

have their semi-reflective (SR) perpendicular one to the other The input beams propagates parallel to both cubes SR layers It is spitted into four parallel beams, being recombined axially A “null” is created at the focal plane centre It is independent of polarization orientation and of wavelength (at least theoretically) This is actually an Achromatic phase shifter

U

1 arcsec

1 arcsec V

Unpolarized

1 arcsec

Beam 4

X’ Polarization Y’

Y’ Polarization V

•  Two “crossed” beamsplitter cubes

Beam 2

Y’

X’ Polarization V

U

1 arcsec

Nulling maps at image plane

Secondary Mirror

Advantages

Monolithic telescope

(P)

Converging optics Diverging optics Fold mirror Beamsplitter or dichroïcs

Primary Mirror

Relay optics

Wavefront sensor

Crossedcubes nuller

Multi-axial combiner (exit pupil plane)

P’1

O’

(P’)

P’2 F’

B’ Focal plane

O” Z

X”

Simple, compact, low mass and volume Reasonable manufacturing tolerances Potentially not expensive High throughput, close to maximum Can be implemented into a nulling coronagraph telescope or a sparseaperture nulling interferometer •  Very small Inner working angle (IWA) when used as a coronagraph •  Capacity for fringes rotation and baseline modulation •  Good candidate for future space missions characterizing extra-solar planets atmospheres •  •  •  •  • 

B

P1

O

P2

Telescope 1

Telescope 2

Relay optics 1

Crossedcubes nuller

(P)

Relay optics 2

Fringe tracker 2-3 Tip-tilt sensors

Fringe tracker 1-4 Tip-tilt sensors

Fringe tracker 14-23

(P’) O’

O”

F’

Focal plane Z

Contacts [email protected] [email protected]