The solar survey at Pic du Midi: calibrated data and improved images. (arXiv:1902.06980v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Koechlin_L/0/1/0/all/0/1">Laurent Koechlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dettwiller_L/0/1/0/all/0/1">Luc Dettwiller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Audejean_M/0/1/0/all/0/1">Maurice Audejean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valais_M/0/1/0/all/0/1">Maël Valais</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ariste_A/0/1/0/all/0/1">Arturo Lopez Ariste</a>
At Pic du Midi observatory we carry a solar survey with images of the
photosphere, prominences and corona. This survey, CLIMSO, is in the following
spectral lines: Fe~XIII corona (1.075~$mu$m), H-$alpha$ (656.3~nm) and He~I
(1.083~$mu$m) prominences, H-$alpha$ and Ca~II (393.4~nm) photosphere. All
frames cover 1.3 times the diameter of the Sun with an angular resolution
approaching one arc second. The frame rate is one per minute per channel
(weather permitting) for the prominences and chromosphere, and one per hour for
the Fe XIII corona. This survey started in 2007 for the disk and prominences,
in 2015 for the corona. We have almost completed one solar cycle, and hope to
cover several more, keeping the same wavelengths or adding others. We make the
solar CLIMSO images easier to use and more profitable to the scientific
community, by providing “Science ready” data. We have improved the contrast
capabilities of our coronagraphs, which now provide images of the Fe~XIII
corona, in addition to the previous spectral channels. We have also implemented
an autoguiding system based on a diffractive Fresnel array for precise
positioning of the Sun behind the coronagraphic masks. The images and films,
are publicly available and downloadable through virtual observatories and
dedicated sites: {it e.g.} this http URL For the H-$alpha$ and
and Ca II channels we calibrate the data in physical units, independent of
atmospheric or instrumental conditions: we provide solar maps of spectral
radiances in $rm {W m^{-2} sr^{-1} nm^{-1} }$. The instrumental improvements
and the calibration process are presented in this paper.
At Pic du Midi observatory we carry a solar survey with images of the
photosphere, prominences and corona. This survey, CLIMSO, is in the following
spectral lines: Fe~XIII corona (1.075~$mu$m), H-$alpha$ (656.3~nm) and He~I
(1.083~$mu$m) prominences, H-$alpha$ and Ca~II (393.4~nm) photosphere. All
frames cover 1.3 times the diameter of the Sun with an angular resolution
approaching one arc second. The frame rate is one per minute per channel
(weather permitting) for the prominences and chromosphere, and one per hour for
the Fe XIII corona. This survey started in 2007 for the disk and prominences,
in 2015 for the corona. We have almost completed one solar cycle, and hope to
cover several more, keeping the same wavelengths or adding others. We make the
solar CLIMSO images easier to use and more profitable to the scientific
community, by providing “Science ready” data. We have improved the contrast
capabilities of our coronagraphs, which now provide images of the Fe~XIII
corona, in addition to the previous spectral channels. We have also implemented
an autoguiding system based on a diffractive Fresnel array for precise
positioning of the Sun behind the coronagraphic masks. The images and films,
are publicly available and downloadable through virtual observatories and
dedicated sites: {it e.g.} this http URL For the H-$alpha$ and
and Ca II channels we calibrate the data in physical units, independent of
atmospheric or instrumental conditions: we provide solar maps of spectral
radiances in $rm {W m^{-2} sr^{-1} nm^{-1} }$. The instrumental improvements
and the calibration process are presented in this paper.
http://arxiv.org/icons/sfx.gif
