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1. Sunrise Chromospheric Infrared SpectroPolarimeter (SCIP) for sunrise III: system design and capability

Author

C. Quintero Noda, Andreas Lagg, Shin Nagata, Sami K. Solanki, J. C. del Toro Iniesta, Yusuke Kawabata, Yukio Katsukawa, Ryoko Ishikawa, Yoshinori Suematsu, A. C. López Jiménez, Achim Gandorfer, Kiyoshi Ichimoto, Ryohei Kano, M. Balaguer Jiménez, Tetsu Anan, Kazuya Shinoda, J. P. Cobos Carrascosa, Toshifumi Shimizu, Tomohiro Tamura, Hirohisa Hara, D. Orozco Suárez, M. Kubo, Fumihiro Uraguchi, Alex Feller, Yoshifumi Nodomi, T. Matsumoto, T. Oba, T. L. Riethmueller, and Toshihiro Tsuzuki

Subjects
Physics, Solar observatory, business.industry, Polarimetry, Waveplate, Optical telescope, law.invention, Wavelength, Optics, law, Sunrise, business, Spectrograph, Beam splitter
Abstract

The Sunrise balloon-borne solar observatory carries a 1 m aperture optical telescope and provides us a unique platform to conduct continuous seeing-free observations at UV-visible-IR wavelengths from an altitude of higher than 35 km. For the next flight planned for 2022, the post-focus instrumentation is upgraded with new spectro- polarimeters for the near UV (SUSI) and the near-IR (SCIP), whereas the imaging spectro-polarimeter Tunable Magnetograph (TuMag) is capable of observing multiple spectral lines within the visible wavelength. A new spectro-polarimeter called the Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) is under development for observing near-IR wavelength ranges of around 770 nm and 850 nm. These wavelength ranges contain many spectral lines sensitive to solar magnetic fields and SCIP will be able to obtain magnetic and velocity structures in the solar atmosphere with a sufficient height resolution by combining spectro-polarimetric data of these lines. Polarimetric measurements are conducted using a rotating waveplate as a modulator and polarizing beam splitters in front of the cameras. The spatial and spectral resolutions are 0.2" and 2 105, respectively, and a polarimetric sensitivity of 0.03 % (1σ) is achieved within a 10 s integration time. To detect minute polarization signals with good precision, we carefully designed the opto-mechanical system, polarization optics and modulation, and onboard data processing.

Published
2020
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2. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the sun

Author

F. Lucarelli, Roberto Sordini, Stavro Ivanovski, Vito Mennella, Hans Rickman, M. Ferrari, Michael F. A'Hearn, Mark Leese, Vincenzo Della Corte, Bo Å. S. Gustafson, E. Bussoletti, Luisa Lara, Jean-Loup Bertaux, M. Antonietta Barucci, Laurent Jorda, Rafael Rodrigo, Ernesto Palomba, Dennis Bodewits, Philippe Lamy, Detlef Koschny, Stefano Debei, Paul R. Weissman, J. Knollenberg, Francesco Marzari, Jean-François Crifo, Nilda Oklay, Nicolas Thomas, Stephen C. Lowry, Marco Fulle, Carsten Güttler, H. U. Keller, L. Sabau, K. P. Wenzel, J. E. Rodriguez, Michael Küppers, Vladimir Zakharov, A. Molina, Pedro J. Gutiérrez, Gabriele Cremonese, F. Giovane, Cesare Barbieri, Mario Accolla, Antonio C. López-Jiménez, Sonia Fornasier, Francesco Angrilli, Ekkehard Kührt, Francesca Esposito, Harald Michalik, José Juan López-Moreno, Elena Mazzotta Epifani, Vania Da Deppo, Jessica Agarwal, José M. Jerónimo, Fernando Moreno, Eberhard Grün, M. Cosi, Ivano Bertini, Olivier Groussin, R. Morales, Pasquale Palumbo, Simon F. Green, Stubbe F. Hviid, Jose Luis Ortiz, R. Kramm, Alessandra Rotundi, John C. Zarnecki, Giampiero Naletto, J. Anthony M. McDonnell, Wing Ip, Mariolino De Cecco, Colin Snodgrass, Stefano Mottola, Jean-Marie Perrin, Luigi Colangeli, Nicolas Altobelli, Monica Lazzarin, Jean-Baptiste Vincent, Björn Davidsson, Cecilia Tubiana, M. Herranz, Holger Sierks, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Dipartimento di Scienze e Tecnologie [Napoli] (DIST), Universita degli studi di Napoli 'Parthenope' [Napoli], Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), International Space Science Institute [Bern] (ISSI), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk (PAN), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig [Braunschweig], Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Akademie der Wissenschaften zu Göttingen, European Space Astronomy Centre (ESAC), European Space Agency (ESA), Department of Industrial Engineering [Padova], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), INAF - Osservatorio Astronomico di Padova (OAPD), HEPPI - LATMOS, CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), University of Trento [Trento], INAF - Osservatorio Astronomico di Capodimonte (OAC), Virginia Polytechnic Institute and State University [Blacksburg], University of Florida [Gainesville], School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], DLR Institute of Planetary Research, German Aerospace Center (DLR), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Institute of Astronomy [Taiwan] (IANCU), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], School of Physical Sciences [Canterbury], Institut für Datentechnik und Kommunikationsnetze, Departamento de Fisica Aplicada [Granada], Universidad de Granada (UGR), Department of Information Engineering [Padova] (DEI), Faculté d'Informatique [Namur], Facultés Universitaires Notre Dame de la Paix (FUNDP) - Namur, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Instituto Nacional de Técnica Aeroespacial (INTA), Center for Space and Habitability (CSH), University of Bern, Physikalisches Institut [Bern], Universität Bern [Bern], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), NASA-California Institute of Technology (CALTECH), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, HELIOS - LATMOS, University of Florida [Gainesville] (UF), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Facultés Universitaires Notre Dame de la Paix (FUNDP), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Università degli Studi di Padova = University of Padua (Unipd), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Agence Spatiale Européenne = European Space Agency (ESA), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Universidad de Granada = University of Granada (UGR), Universität Bern [Bern] (UNIBE), ITA, USA, GBR, FRA, and DEU

Subjects
67P/Churyumov-Gerasimenko, genetic structures, Comet dust, Astronomical unit, comet 67P, coma, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, law.invention, Orbiter, comet, Planet, law, Rosetta, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Multidisciplinary, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Medicine (all), Astronomy, Mass ratio, Billion years, Accretion (astrophysics), 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, dust, Formation and evolution of the Solar System
Abstract

Critical measurements for understanding accretion and the dust/gas ratio in the solar nebula, where planets were forming 4.5 billion years ago, are being obtained by the GIADA (Grain Impact Analyser and Dust Accumulator) experiment on the European Space Agency’s Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko. Between 3.6 and 3.4 astronomical units inbound, GIADA and OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) detected 35 outflowing grains of mass 10 −10 to 10 −7 kilograms, and 48 grains of mass 10 −5 to 10 −2 kilograms, respectively. Combined with gas data from the MIRO (Microwave Instrument for the Rosetta Orbiter) and ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instruments, we find a dust/gas mass ratio of 4 ± 2 averaged over the sunlit nucleus surface. A cloud of larger grains also encircles the nucleus in bound orbits from the previous perihelion. The largest orbiting clumps are meter-sized, confirming the dust/gas ratio of 3 inferred at perihelion from models of dust comae and trails.

Published
2015
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3. The Second Flight of the Sunrise Balloon-borne Solar Observatory: Overview of Instrument Updates, the Flight, the Data, and First Results

Author

L. Sabau-Graziati, G. Card, Peter Barthol, H.-P. Doerr, V. Martínez Pillet, A. C. López Jiménez, J. C. del Toro Iniesta, Andreas Lagg, C. Halbgewachs, M. Balaguer Jiménez, Thomas Berkefeld, M. Kolleck, G. Tomasch, W. Deutsch, Alberto Álvarez-Herrero, Sami K. Solanki, Laurent Gizon, Johann Hirzberger, Tino L. Riethmüller, Alex Feller, M. van Noort, M. Knölker, D. Germerott, K. Heerlein, Sanja Danilovic, D. Orozco Suárez, Rebecca Centeno, A. Lecinski, J. L. Gasent Blesa, J. Blanco Rodríguez, Wolfgang Schmidt, I. Pérez Grande, Achim Gandorfer, R. Meller, B. Grauf, Max Planck Society, Ministerio de Economía y Competitividad (España), National Science Foundation (US), National Aeronautics and Space Administration (US), and National Research Foundation of Korea

Subjects
Brightness, 010504 meteorology & atmospheric sciences, photosphere [Sun], Polarimetry, FOS: Physical sciences, chromosphere [Sun], Sun: faculae, plages, Astrophysics, polarimetric [Techniques], 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sunrise, faculae, plages [Sun], Sun: magnetic fields, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Photosphere, Solar observatory, Sunspots, Sun: chromosphere, Techniques: polarimetric, Sun: photosphere, Astronomy and Astrophysics, Polarimeter, Astrophysics - Solar and Stellar Astrophysics, magnetic fields [Sun], Space and Planetary Science, Data reduction
Abstract

S. K. Solanki et. al., ©2017 The American Astronomical Society. All rights reserved.The Sunrise balloon-borne solar observatory, consisting of a 1 m aperture telescope that provides a stabilized image to a UV filter imager and an imaging vector polarimeter, carried out its second science flight in 2013 June. It provided observations of parts of active regions at high spatial resolution, including the first high-resolution images in the Mg ii k line. The obtained data are of very high quality, with the best UV images reaching the diffraction limit of the telescope at 3000 Å after Multi-Frame Blind Deconvolution reconstruction accounting for phase-diversity information. Here a brief update is given of the instruments and the data reduction techniques, which includes an inversion of the polarimetric data. Mainly those aspects that evolved compared with the first flight are described. A tabular overview of the observations is given. In addition, an example time series of a part of the emerging active region NOAA AR 11768 observed relatively close to disk center is described and discussed in some detail. The observations cover the pores in the trailing polarity of the active region, as well as the polarity inversion line where flux emergence was ongoing and a small flare-like brightening occurred in the course of the time series. The pores are found to contain magnetic field strengths ranging up to 2500 G, and while large pores are clearly darker and cooler than the quiet Sun in all layers of the photosphere, the temperature and brightness of small pores approach or even exceed those of the quiet Sun in the upper photosphere., The German contribution to Sunrise and its reflight was funded by the Max Planck Foundation, the Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR, and private donations by supporting members of the Max Planck Society, which is gratefully acknowledged. The Spanish contribution was funded by the Ministerio de Economía y Competitividad under Projects ESP2013-47349-C6 and ESP2014-56169-C6, partially using European FEDER funds. The National Center for Atmospheric Research is sponsored by the National Science Foundation. The HAO contribution was partly funded through NASA grant number NNX13AE95G. This work was partly supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea. L.G. acknowledges research funding from the State of Lower Saxony, Germany. SDO is a mission of NASA's Living With a Star (LWS) program. The SDO/HMI data were provided by the Joint Science Operation Center (JSOC). The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy (AURA) Inc. under a cooperative agreement with the National Science Foundation.

Published
2017
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4. Giada: its Status after the Rosetta Cruise Phase and On-Ground Activity in Support of the Encounter with Comet 67P/CHURYUMOV-GERASIMENKO

Author

Philippe Lamy, J. E. Rodriguez, F. Lucarelli, Simon F. Green, M. Ferrari, Jean-François Crifo, Roberto Sordini, Paul R. Weissman, R. Rodrigo, V. Mennella, A. C. López Jiménez, Stavro Ivanovski, A. Aronica, M. Herranz, J. M. Jeronimo, F. Moreno, Ernesto Palomba, Mario Accolla, Francesca Esposito, John C. Zarnecki, Luigi Colangeli, Pasquale Palumbo, J. A. M. McDonnell, F. J. M. Rietmeijer, Marco Fulle, E. Bussoletti, Eberhard Gruen, M. Cosi, J. M. Perrin, Alessandra Rotundi, J. J. Lopez-Moreno, R. Morales, V. Della Corte, V. Zakharov, E. Mazzotta Epifani, Antonio Molina, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Earth and Planetary Sciences [Albuquerque] (EPS), The University of New Mexico [Albuquerque], INAF - Osservatorio Astronomico di Capodimonte (OAC), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universita degli studi di Napoli 'Parthenope' [Napoli], European Space Agency (ESA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), HEPPI - LATMOS, The Open University [Milton Keynes] (OU), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Physics, ESA Rosetta, 010504 meteorology & atmospheric sciences, Spacecraft, business.industry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Cruise, Dust particles, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy and Astrophysics, GIADA, calibration, 01 natural sciences, dust instrument, Astrobiology, Outgassing, 13. Climate action, in flight data, 0103 physical sciences, business, 010303 astronomy & astrophysics, Instrumentation, 0105 earth and related environmental sciences
Abstract

GIADA (Grain Impact Analyser and Dust Accumulator) on-board the Rosetta mission to comet 67P/Churyumov-Gerasimenko was designed to study the physical and dynamical properties of dust particles ejected by the comet during the encounter. In this paper we report the results of the analysis of data collected by GIADA during the past seven years of the cruise phase. During this period the GIADA detection subsystems were switched on for periodic in-flight payload checkouts to monitor their state-of-health including potential changes in its performance that could affect its data collection. Only slight variations in sensitivity and dynamical range were identified that will not affect the GIADA measurement capability during the Rosetta comet encounter and rendezvous phase. The GIADA microbalance system detected the presence of low-volatility material over a period of about 169 days when the GIADA cover remained partially opened. It is highly probable that this material originated from the spacecraft itself, as a spacecraft's outgassing was observed by the ROSINA mass spectrometer (on-board Rosetta) during the cruise phase. The identification of the low-volatility mass deposited on the microbalances as self-contamination will allow us to evaluate the mass rate background to be subtracted from the GIADA science data. These results obtained from GIADA cruise data analysis coupled with laboratory calibration data obtained from measurements using the GIADA spare model for selected cometary dust analogs will be the basis for the interpretation of the GIADA scientific data.

Published
2014
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5. The Imaging Magnetograph eXperiment (IMaX) for the Sunrise balloon-borne solar observatory

Author

P. Mellado, M. Menendez, D. Orozco Suárez, J. M. Jeronimo, Ph. Rodriguez, Juan L. Ramos, B. Aparicio, W. Schmidt, J. C. del Toro Iniesta, V. Domingo, C. Pastor, A. C. López Jiménez, Sami K. Solanki, R. Morales, Alberto Álvarez-Herrero, Javier Piqueras, R. L. Heredero, V. Martínez Pillet, W. Deutsch, M. Knoelker, Peter Barthol, Achim Gandorfer, R. Meller, Alex Feller, Thomas Berkefeld, L. R. Bellot Rubio, J. L. Gasent Blesa, F. Girela, M. Reina, J. A. Bonet, Tomás Belenguer, E. Ballesteros, S. Vargas Domínguez, A. Sánchez, M. Balaguer, M. Herranz, H. Laguna, Manuel Collados, B. Grauf, L. González Fernández, Néstor Uribe-Patarroyo, Gonzalo Ramos, López Heredero, R. [0000-0002-2197-8388], López Jiménez, A. [0000-0002-6297-0681], Balaguer, M. [0000-0003-4738-7727], Del Toro Iniesta, J. C. [0000-0002-3387-026X], Reina Aranda, M. [0000-0003-0248-2771], Álvarez Herrero, A. [0000-0001-9228-3412], Herranz de la Revilla, M. L. [0000-0003-4343-6632], Morales Muñoz, R. [0000-0003-1661-0594], Pastor, C. [0000-0001-9631-9558], Gasent Blesa, J. L. [0000-0002-1225-4177], Collados, M. [0000-0002-6210-9648], Jerónimo, J. M. [0000-0002-4944-5823], Bellot Rubio, L. R. [0000-0001-8669-8857], Martínez Pillet, V. [0000-0001-7764-6895], Ministerio de Ciencia e Innovación (MICINN), Deutsches Zentrum für Luft- und Raumfahrt (DLR), and National Aeronautics and Space Administration (NASA)

Subjects
Physics, Solar observatory, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Polarimeter, Astronomy and Astrophysics, Astrophysics, Spectral line, Integrated Sun Observations Polarization, symbols.namesake, Wavelength, Magnetic Fields, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Velocity Fields, symbols, Stokes parameters, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Data Management, Spectral resolution, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Imaging Magnetograph eXperiment (IMaX) is a spectropolarimeter built by four institutions in Spain that flew on board the Sunrise balloon-borne telesocope in June 2009 for almost six days over the Arctic Circle. As a polarimeter IMaX uses fast polarization modulation (based on the use of two liquid crystal retarders), real-time image accumulation, and dual beam polarimetry to reach polarization sensitivities of 0.1%. As a spectrograph, the instrument uses a LiNbO3 etalon in double pass and a narrow band pre-filter to achieve a spectral resolution of 85 mAA. IMaX uses the high Zeeman sensitive line of Fe I at 5250.2 AA and observes all four Stokes parameters at various points inside the spectral line. This allows vector magnetograms, Dopplergrams, and intensity frames to be produced that, after reconstruction, reach spatial resolutions in the 0.15-0.18 arcsec range over a 50x50 arcsec FOV. Time cadences vary between ten and 33 seconds, although the shortest one only includes longitudinal polarimetry. The spectral line is sampled in various ways depending on the applied observing mode, from just two points inside the line to 11 of them. All observing modes include one extra wavelength point in the nearby continuum. Gauss equivalent sensitivities are four Gauss for longitudinal fields and 80 Gauss for transverse fields per wavelength sample. The LOS velocities are estimated with statistical errors of the order of 5-40 m/s. The design, calibration and integration phases of the instrument, together with the implemented data reduction scheme are described in some detail., Comment: 17 figures

Published
2010
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6. IMaX: a polarimeter based on Liquid Crystal Variable Retarders for an aerospace mission

Author

N. Uribe‐Patarroyo, A. Alvarez‐Herrero, R. L. Heredero, J. C. del Toro Iniesta, A. C. López Jiménez, V. Domingo, J. L. Gasent, L. Jochum, V. Martínez Pillet, null The IMaX Team, Del Toro Iniesta, J. C. [0000-0002-3387-026X], López Jiménez, A. [0000-0002-6297-0681], López Heredero, R. [0000-0002-2197-8388], Álvarez Herrero, A. [0000-0001-9228-3412], Gasenta Blesa, J. L. [0000-0002-1225-4177], and Martínez Pillet, V. [0000-0001-7764-6895]

Subjects
Physics, Zeeman effect, business.industry, Polarimetry, Polarimeter, Radiation, Condensed Matter Physics, law.invention, Telescope, Orbiter, symbols.namesake, Optics, law, symbols, Figure of merit, Demodulation, business, Remote sensing
Abstract

The IMaX Team IMaX is the Imaging Magnetograph eXperiment, an instrument part of the payload of SUNRISE, a stratospheric balloon mission in Antarctica. It is also the precursor of the Visible Imaging Magnetograph of the future ESA Solar Orbiter mission. It is essentially a diffraction-limited imager that carries out spectropolarimetric measurements of high resolution (bandwidth of < 100 mÅ at 525.02 nm), and relates the polarimetric properties of the incoming light through a telescope with magnetic fields in the Sun, via the Zeeman effect. At the core of the instrument there are the polarization modulation components, two Liquid Crystal Variable Retarders (LCVRs). A demodulation efficiency is defined and used as the figure of merit, and it serves to find the theoretical optimum states for the LCVRs as well as to judge the quality of the pre-flight calibration of the system. This calibration and the method used to optimize the actual efficiency is explained. Also, the space qualification of the LCVRs is presented, where ellipsometry played a major role in studying the effects of radiation, vacuum and temperature in the operation of the LCVRs. (© 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) Peerreview

Published
2008
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7. Detailed design of the imaging magnetograph experiment (IMaX): a visible imager magnetograph for the Sunrise mission

Author

L. Jochum, E. Ballesteros, J. C. del Toro Iniesta, J. González, Johel Rodríguez, M. Herranz, J. Castillo Lorenzo, C. Pastor, R. Morales, A. C. López Jiménez, V. Martínez Pillet, J. A. Bonet, G. Ramos, J. Villanueva, P. Mellado, P. Rodríquez, R. L. Heredero, M. Reina, L. González, Manuel Collados, J. L. Medina Trujillo, Tomás Belenguer, A. Sánchez, Cobo B. Ruiz, J. L. Gasent, J. M. Jeronimo, Alberto Álvarez-Herrero, V. Domingo, and L. Sabau

Subjects
Physics, Spectrometer, business.industry, Optical engineering, Detector, Sun, Polarimetry, Polarimeter, Balloon Borne Telescopes, law.invention, Telescope, Optics, law, Liquid Crystal Retarders, Spectral resolution, business, Image resolution, Remote sensing
Abstract

COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only. In this work, it is described the Imaging Magnetograph eXperiment, IMaX, one of the three postfocal instruments of the Sunrise mission. The Sunrise project consists on a stratospheric balloon with a 1 m aperture telescope, which will fly from the Antarctica within the NASA Long Duration Balloon Program. IMaX will provide vector magnetograms of the solar surface with a spatial resolution of 70 m. This data is relevant for understanding how the magnetic fields emerge in the solar surface, how they couple the photospheric base with the million degrees of temperature of the solar corona and which are the processes that are responsible of the generation of such an immense temperatures. To meet this goal IMaX should work as a high sensitivity polarimeter, high resolution spectrometer and a near diffraction limited imager. Liquid Crystal Variable Retarders will be used as polarization modulators taking advantage of the optical retardation induced by application of low electric fields and avoiding mechanical mechanisms. Therefore, the interest of these devices for aerospace applications is envisaged. The spectral resolution required will be achieved by using a LiNbO3 Fabry-Perot etalon in double pass configuration as spectral filter before the two CCDs detectors. As well phase-diversity techniques will be implemented in order to improve the image quality. Nowadays, IMaX project is in the detailed design phase before fabrication, integration, assembly and verification. This paper briefly describes the current status of the instrument and the technical solutions developed to fulfil the scientific requirements. Peerreview

Published
2006
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8. The imaging magnetograph eXperiment for the SUNRISE balloon Antarctica project

Author

J.M. Jeronimo, G. Ramos, R. Morales, C. Pastor, R. L. Heredero, M. Reina, J. A. Bonet, J. Castillo Lorenzo, V. Domingo, Jose Carlos del Toro Iniesta, J. L. Medina Trujillo, Valentin Martinez Pillet, S. Mathew, P. Mellado, Manuel Collados, P. Rodriguez, M. Menendez, B. Ruiz Cobo, Alberto Álvarez-Herrero, M. Herranz, J. Villanueva, A. C. López Jiménez, Johel Rodríguez, J. L. Gasent, Tomás Belenguer, A. Sánchez, L. Jochum, López Heredero, R. [0000-0002-2197-8388], López Jiménez, A. [0000-0002-6297-0681], Reina, M. [0000-0003-0248-2771], Del Toro Iniesta, J. C. [0000-0002-3387-026X], Álvarez Herrero, A. [0000-0001-9228-3412], De la Revilla, M. L. [0000-0003-4343-6632], Callados, M. [0000-0002-6210-9648], Morales Muñoz, R. [0000-0003-1661-0594], Rodríguez Gómez, J. [0000-0002-6757-5912], Ruiz Cobo, B. [0000-0001-9550-6749], Gasent Blesa, J. L. [0000-0002-1225-4177], Jerónimo, J. M. [0000-0002-4944-5823], and Pastor, C. [0000-0001-9631-9558]

Subjects
Physics, Diffraction, Photon, Balloon-borne telescopes, business.industry, Polarimetry, Sun, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Magnetic field, law.invention, Fabry-Perot etalons, Telescope, Optics, law, Sunrise, Astrophysics::Solar and Stellar Astrophysics, business, Magnetographs, Fabry–Pérot interferometer, Remote sensing
Abstract

13 pages, 8 figures.-- Published in: "Optical, Infrared, and Millimeter Space Telescopes" [Section: Solar], edited by John C. Mather.-- Contributed to the conference with same title, Glasgow, Jun 21, 2004., Final full-text version available Open Access at: http://www.iaa.es/~jti/publications/SPIE2Valentin.pdf, The SUNRISE balloon project is a high-resolution mission to study solar magnetic fields able to resolve the critical scale of 100 km in the solar photosphere, or about one photon mean free path. The Imaging Magnetograph eXperiment (IMaX) is one of the three instruments that will fly in the balloon and will receive light from the 1m aperture telescope of the mission. IMaX should take advantage of the 15 days of uninterrupted solar observations and the exceptional resolution to help clarifying our understanding of thesmall-scale magnetic concentrations that pervade the solar surface. For this, IMaX should act as a diffraction limited imager able to carry out spectroscopic analysis with resolutions in the 50.000-100.000 range and capable to perform polarization measurements. The solutions adopted by the project to achieve all these three demanding goals are explained in this article. They include the use of Liquid Crystal Variable Retarders for the polarization modulation, oneLiNbO3 etalon in double pass and two modern CCD detectors that allow for the application of phase diversity techniques by slightly changing the focus of one of the CCDs., This project is funded by the Spanish Programa Nacional del Espacio under project ESP2003-07735.

Published
2004

9. The polarimetric and helioseismic imager on solar orbiter

Author

Reiner Volkmer, B. Dávila, J. Bosch, J. Villanueva, V. Hervier, D. Roma, C. Campuzano, E. Nakai, Kinga Albert, N. Szwec, I. Vera, Andreas Lagg, T. Scheiffelen, Stephan Werner, P. Rodríguez Martínez, D. Osorno Caudel, J. Barandiarán, Javier Piqueras, T. Appourchaux, R. Le Cocguen, P. García Parejo, A. Sánchez, A. Núñez Peral, Joachim Woch, R. Muller, Dirk Soltau, L. R. Bellot Rubio, J. L. Gasent Blesa, Achim Gandorfer, Johann Hirzberger, J. Blanco Rodríguez, J. C. del Toro Iniesta, A. Fernández-Medina, M. Herranz, H. Laguna, R. Enge, M. Carmona, M. Kolleck, R. Meller, D. Hernández Expósito, Sami K. Solanki, M. Balaguer Jiménez, J.-J. Fourmond, T. Maue, J. P. Cobos Carracosa, K. Heerlein, Dan Yang, B. Fiethe, S. Frahm, V. Martínez Pillet, Udo Schühle, Uwe Beckmann, M. Monecke, M. Royo, D. Orozco Suárez, B. Aparicio, Wolfgang Schmidt, D. Germerott, Björn Löptien, D. Oberdorfer, J. Bochmann, I. Zouganelis, F. Heidecke, R. Navarro, Manuel Silva-López, D. Busse, S. Ramanath, Michael Sigwarth, A. Casas, Ioanna Papagiannaki, Jesper Schou, Marc Chaigneau, A. Philippon, Juan L. Ramos, Isabel Pérez-Grande, S. Meyer, P. Boumier, E. Sanchis Kilders, Gustavo Alonso, J. C. Le Clec’h, G. Baranjuk, Ignacio Torralbo, Harald Michalik, Daniel Müller, M.-F. Müller, Carlos Dominguez-Tagle, Laurent Gizon, J.M. Gomez Cama, P. Labrousse, D. Garranzo-García, D. Álvarez García, L. Guerrero, Y. Guan, M. Bergmann, J. Baumgartner, Jan Staub, Th. Berkefeld, J. A. Martín, A. Herms, M. Alvarez Copano, Alberto Álvarez-Herrero, M. Bouzit, V. Domingo, A. Ferreres Sabater, S. Fahmy, Germán Fernández-Rico, María Cebollero, M. Sperling, W. Deutsch, F. Girela, V. Buttice, J. A. Bonet, J. Heinrichs, Alexander Bell, T. Lange, L. Bastide, H. Michel, Alejandro M. Gomez-San-Juan, J. Bischoff, C. Ruiz de Galarreta, Andreas Zerr, Thimo Meierdierks, B. Grauf, A. C. López Jiménez, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Centre National D'Etudes Spatiales (CNES), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Ministerio de Ciencia, Innovación y Universidades

Subjects
Solar Telescope, 010504 meteorology & atmospheric sciences, photosphere [Sun], Filtegrams, Highly elliptical orbit, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Telescope, Orbiter, Photosphere, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Helioseismology, Solar dynamo, 010303 astronomy & astrophysics, Sun: magnetic fields, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Sun: helioseismology, Physics, [PHYS]Physics [physics], Ellipsometry, polarimeters [Instrumentation], Spacecraft, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, instrumentation: polarimeters, Sun: photosphere, Heliosismologia, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, techniques: polarimetric, magnetic fields [Sun], Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics of Galaxies (astro-ph.GA), Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere, El·lipsometria
Abstract

This paper describes the Polarimetric and Helioseismic Imager on the Solar Orbiter mission (SO/PHI), the first magnetograph and helioseismology instrument to observe the Sun from outside the Sun-Earth line. It is the key instrument meant to address the top-level science question: How does the solar dynamo work and drive connections between the Sun and the heliosphere? SO/PHI will also play an important role in answering the other top-level science questions of Solar Orbiter, as well as hosting the potential of a rich return in further science. SO/PHI measures the Zeeman effect and the Doppler shift in the FeI 617.3nm spectral line. To this end, the instrument carries out narrow-band imaging spectro-polarimetry using a tunable LiNbO_3 Fabry-Perot etalon, while the polarisation modulation is done with liquid crystal variable retarders (LCVRs). The line and the nearby continuum are sampled at six wavelength points and the data are recorded by a 2kx2k CMOS detector. To save valuable telemetry, the raw data are reduced on board, including being inverted under the assumption of a Milne-Eddington atmosphere, although simpler reduction methods are also available on board. SO/PHI is composed of two telescopes; one, the Full Disc Telescope (FDT), covers the full solar disc at all phases of the orbit, while the other, the High Resolution Telescope (HRT), can resolve structures as small as 200km on the Sun at closest perihelion. The high heat load generated through proximity to the Sun is greatly reduced by the multilayer-coated entrance windows to the two telescopes that allow less than 4% of the total sunlight to enter the instrument, most of it in a narrow wavelength band around the chosen spectral line., Comment: 36 pages, 41 figures

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