The TP3-WFS: a new guy in town. (arXiv:1811.05607v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Colodro_Conde_C/0/1/0/all/0/1">Carlos Colodro-Conde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Velasco_S/0/1/0/all/0/1">Sergio Velasco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_R/0/1/0/all/0/1">Roberto L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oscoz_A/0/1/0/all/0/1">Alejandro Oscoz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_Hernando_Y/0/1/0/all/0/1">Yolanda Mart&#xed;n-Hernando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rebolo_R/0/1/0/all/0/1">Rafael Rebolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Garrido_A/0/1/0/all/0/1">Antonio P&#xe9;rez-Garrido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Valdivia_J/0/1/0/all/0/1">Juan Jos&#xe9; Fern&#xe1;ndez-Valdivia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labadie_L/0/1/0/all/0/1">Lucas Labadie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackay_C/0/1/0/all/0/1">Craig Mackay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puga_M/0/1/0/all/0/1">Marta Puga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Coira_G/0/1/0/all/0/1">Gustavo Rodr&#xed;guez-Coira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Ramos_L/0/1/0/all/0/1">Luis Fernando Rodr&#xed;guez-Ramos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Ramos_J/0/1/0/all/0/1">Jos&#xe9; Manuel Rodr&#xed;guez-Ramos</a>

The TP3-WFS (Two Pupil Plane Positions Wavefront Sensor) is, to the best of
the authors’ knowledge, the first physical implementation of the geometrical
wavefront reconstruction algorithm that has been tested in a telescope as part
of an actual AO-enabled instrument. The main advantage of this algorithm is
that it theoretically provides a fairly good reconstruction accuracy even under
very low levels of light, in the order of a few hundreds of photons. This paper
presents the first control-related results obtained at the William Herschel
Telescope (WHT). Such results demonstrate the feasibility of this novel WFS as
part of a real-time AO control loop.

The TP3-WFS (Two Pupil Plane Positions Wavefront Sensor) is, to the best of
the authors’ knowledge, the first physical implementation of the geometrical
wavefront reconstruction algorithm that has been tested in a telescope as part
of an actual AO-enabled instrument. The main advantage of this algorithm is
that it theoretically provides a fairly good reconstruction accuracy even under
very low levels of light, in the order of a few hundreds of photons. This paper
presents the first control-related results obtained at the William Herschel
Telescope (WHT). Such results demonstrate the feasibility of this novel WFS as
part of a real-time AO control loop.

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