Dr. Klaus Gerhard Puschmann
Dr. Klaus Gerhard Puschmann

Welcome to my personal homepage

 

Introduction

This webpage replaces my former personal homepage at the Leibniz-Institut für Astrophysik Potsdam (AIP) which has been deleted by the AIP. Apart from already published material, this current webpage provides further details on technical innovations and achievements related to the GREGOR Fabry-Perot Interferometer and the BLue Imaging Solar Spectrometer, which I implemented or achieved as the Instrument Scientist. Some latest scientific results presented here have been achieved after the private purchase of the required computing hardware by the end of 2014. iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server is perfectly suited to perform all required computational tasks for data reduction, image reconstruction, spectral deconvolution and data analysis within a reasonable computational time, which is based on my proper GFPI Data Pipeline iSPOR-DP, the Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline.

 

Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline iSPOR-DP

The GREGOR Fabry-Perot Interferometer @VTT - Sensational Observational Discovery - Spicules, the main driver of solar chromospheric heating - 27 February 2016 - Klaus Gerhard Puschmann - Darmstadt, Germany - @copyright

 

Klaus Gerhard Puschmann - Interests and Skills:

Member of the SSA Preparatory Programme Office - OPS-L - ESA/ESOC - Space Weather Segment and NEO Segment [2014 - 2016]

Primary Focus: Development of the ESA L1 and L5 Lagrange Space Weather Missions which will consist of (1) a spectropolarimetric Fabry-Perot Imaging-Magnetograph and (2) an EUV Imager for Flare and CME now- and forecast, (3) a Coronagraph for the tracking of Coronal Mass Ejections (CMEs) and (4) a Heliospheric Imager for CME arrival time prediction and insitu-measurement payload. (5) A NEO imager for the observation and orbit characterization of inner earth-orbit objects is currently considered as optional remote sensing payload. Most of the suggested instruments will take their heritage from pervious missions like SOHO, STEREO or upcoming missions such as Solar Orbiter, but are expected to be optimised for enhanced operational space weather monitoring and forecast purposes with very high reliability and robustness demands, due to the need to operate particularly during severe space weather events. For details see S.Kraft, K.G. Puschmann, J.P. Luntama, ICSO, 2016



Secondary Focus on the 1m Near Earth Object flye-eye TELescope (NEOSTEL) development.The goal of the NEOSTEL project is to create a ground based network of telescopes for Near Earth Objects observation in the frame of the ESA Space Situational Awareness Programme.

 

Additional Contributions to the Development of ground-based Optical Telescopes (4-12m aperture class) for optical Space Link Communication.

 

See the Employment Reference Letter of the Director of Human Resources & Recruitment, RHEA Group/RHEA Systems for European Space Agency as well as the  personal reference letters of the Head of the Multidisciplinary Projects Unit and the Space Weather Space Segment Engineer of the Space Situational Awareness Office in the ESA Directorate of Operations, provided in Section "Employment Reference Letters".

 

 

Member - 1.5m Solar Telescope Project GREGOR [2003-2014] 

 

The 1.5m GREGOR solar telescope is Europe’s largest solar telescope and on third position worldwide.  GREGOR is designed as a Gregory system with three imaging mirrors. It posses an alt-azimuthal mounting and is protected by retractable dome. The telescope is built and operated at the Spanish Observatorium del Teide (OT) on Tenerife by a consortium of several German scientific institutions and their international partners. Its first light instrumentation includes the GREGOR Fabry-Perot Interferometer (GFPI), the GRating Infrared Spectro-polarimeter (GRIS) and the Broad-Band Imager (BBI). Its high-order adaptive optics system (GAOS) allows for diffraction-limited observations of the highly dynamic solar fine-structure and its related magnetic field at spatial scales down to 60 km on the solar surface. The impressive spatial resolution of the acquired images, spectra and magnetogramms will allow for the first time a direct comparison of the results with numerical simulations at smallest scales. As the Instrument Scientist of the GREGOR Fabry-Perot Interferometer and the BLue Imaging Solar Spectrometer my focus in the frame of the 1.5m GREGOR Solar Telescope Project was the development, deployment, verification and operation of the latter two instruments. 

Image under @copyright of Klaus Gerhard Puschmann - Click to enlarge the image
Image under @copyright of Klaus Gerhard Puschmann - Click to enlarge the image

Instrumental Development GREGOR Fabry-Perot Interferometer & Blue Imaging Solar Spectrometer [2004-2014] - Instrument Scientist

The GREGOR Fabry-Perot Interferometer (GFPI), an imaging spectropolarimeter,  is one of three first-light instruments of the German 1.5-meter GREGOR solar telescope at the Observatorio del Teide, Tenerife, Spain. The instrument has been developed at the Institut für Astrophysik Göttingen between 2004 and 2007, in collaboration between the respective solar physics group leader and myself, and further developed, commissioned, scientifically verified and finalized by myself in Potsdam. With two tunable etalons in its Narrow-Band Channel (NBC) in a collimated mount and large-format, high-cadence CCD detectors with sophisticated computer hard- and software, the instrument is capable of spectral line scanning in less than a minute.  The field-of-view (FOV) of 50’’ × 38’’ (25’’ x 38’’ in vector spectropolarimetric mode) in both NBC and Broad-Band Channel (BBC) is well suited for sunspot observations. The spectral coverage in the spectroscopic mode extends from 530-860 nm (580-660 nm in vector spectropolarimetric mode) with a theoretical spectral resolution of R ≈ 250,000. The combination of fast spectropolarimetric narrow-band imaging  and post-factum image restoration has the potential for discovery science concerning the dynamic solar photospheric and chromospheric fine structure and its magnetic field at spatial scales down to 60 km on the solar surface. Within an innovative and novel Multi-wavelength Imaging Setup (MWIS) in the BBC and the Blue Imaging Channel (BIC),  Halpha-Lyot/G-Band/Ca II K-Lyot Filters can gather now photospheric and chromospheric information concerning solar small scale structures and their dynamics simultaneously to the spectroscopic and spectropolarimetric data recorded in the NBC of the instrument. The Blue Imaging Solar Spectrometer (BLISS) will be a twin of the GFPI and will provide narrow-band Spectral Line Scanning and Broadband Imaging in the wavelength range 380-530 nm. It will replace the BIC of the GFPI in the near future. I completed the design for this instrument  in 2013.

Image under @copyright of Klaus Gerhard Puschmann - Click to enlarge

The GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope. The instrument is mounted in the 5th floor of the 1.5m GREGOR solar telescope building on five optical benches. The image shows part of the spectropolarimetric Narrow-Band Channel (NBC, 530-860 nm) and the Laser-Photomultiplier Channel for Etalon-Finesse adjustment. In the background one finds the BroadBand Channel (BBC, 530-860 nm), the Wight-Light Channel (WLC) for spectral calibration purposes, and the Blue Imaging Channel (BIC, 380-530 nm).

Image under @copyright of Klaus Gerhard Puschmann - Click to enlarge the image

The GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope. The core of the system are two tunable and computer controlled etalons for spectral line scanning in collimated mounting at the direct vicinity of the secondary pupil of the instrument.

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Optical design and setup of the GREGOR Fabry-Perot Interferometer including Halpha and Ca II K Lyot filter imaging.  I completed the optical design and setup in August 2013. Figure from right to left: Blue Imaging channel (BIC, blue light-beam), White-light channel (WLS, yellow light-beam), BroadBand Channel (BBC, light-red light beam), spectropolarimetric NarrowBand Channel (NBC, red light-beam), Laser/Photomultiplier Channel (Laser/MP, yellow light beam).  Halpha and Ca II K Lyot filter are denoted by orange color. Design based on calculations that I performed in geometrical optics. Graphic produced with Microsoft PowerPoint. 

Image @copyright Klaus Gerhard Puschmann. - Click to enlarge the image.

Deployed Lyot filters @ the GREGOR Fabry-Perot Interferometer. 

 

The Lyot filters are part of an innovative and novel multi-wavelength imaging system (MWIS) that gathers information about fine structure and dynamics in the solar photosphere and chromosphere simultaneously to the spectroscopic and spectropolarimetric measurements with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. I completed MWIS in August 2013. The Halpha Lyot-Filter is property of the Einsteinturm.

Click to enlarge the image

Between 2011 and 2013 I integrated the following Opto-mechanical Components into the GREGOR Fabry-Perot Interferometer (GFPI): Two Filter Sliders (upper left), each harbouring two interference filtersl; while in the narrow-band channel of the instrument, the filter slider allows the sequential scanning of spectral lines, the filter slider in the broadband channel allows the simultaneous recording of broadband images at the same wavelength range. 3-Mirror System (upper right) for observations > 650 nm, replacing the former pentaprism with a cutoff @ 650 nm; This allows for the first time the scanning of chromospheric sepctral lines like Halpha or Ca II IR. New Laser-Photomultiplier Channel (bottom) with a Laser-Beam Expander for better Finesse adjustment of the etalons (improved parallelicity of the etalon plates) and  improved spectral resolution of the instrument. The CAD-Designs have been perfromed and kindly provided by Dipl. Ing. S.M. Bauer (AIP).

 

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image
Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Snapshot of the GUI of the instrument control software (ICS) for the GREGOR Fabry-Perot Interferometer (GFPI). I developed the GFPI-ICS in collaboration with T. Seelemann (LaVision, Göttingen, Germany) between 2004 and 2013.

 

The GFPI-ICS provides an extended and complex Graphical User Interface (GUI) and completely automated alignment, calibration and observation procedures, dramatically simplifying the usage of the extremely complex instrument.

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

The GUI of the GREGOR Fabry-Perot Interferometer Control software: First Spectrum ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope that I recorded in 2012. 

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Flow chart of the communications between the GREGOR Fabry-Perot Interferometer control computer (DaVis) and internal and peripheral devices. PTU: programmable timing unit; CCD 1 & CCD 2: CCD detectors; FLC 1 & FLC 2: ferro-electric liquid crystals; CS100 (1) & CS100 (2): etalon controllers; FPI 1 & FPI 2 etalons; GTCS: GREGOR Telescope Central Server; GRIS: Grating Infrared Spectrograph.

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Optical Design for the Integration of the BLue Imaging Solar Spectrometer (BLISS, 380-530 nm, optical elements marked with "a") into the GREGOR Fabry-Perot Interferometer (GFPI, 530-860 nm).

 

BLISS is essentially a clone of the GFPI, optimized for the wavelength range 380-530 nm. The presented design is based on calculations that I performed in geometrical optics. I produced the graphics by means of Microsoft PowerPoint.

 

 

Below one finds context information to both GREGOR Fabry-Perot Interferometer (GFPI) and BLue Imaging Solar Spectrometer (BLISS):

 

 

September 2006:

 

"From the Göttingen Fabry-Perot Interferometer to the GREGOR Fabry-Perot Interferometer" - Workshop "Modern Solar Facilities - Advanced Solar Science". Presentation of the finished design for the "GREGOR Fabry-Perot Interferometer". Description of new cameras, etalons, control software, opto-mechanical components, optical design. Please download the document below.

puschmann_web-small.pdf
PDF-Dokument [3.9 MB]

November 2012:

 

Status report - GEGOR Fabry-Perot Interferometer  - Colloquium @ Instituto de Astrofísica de Canarias. Please click here to see the talk.

Status report - GEGOR Fabry-Perot Interferometer - A similar talk held @ Kiepenheuer Institut für Sonnenphysik (KIS) - Freiburg, November 2012
puschmann_kis_2012_short_final_small.pdf
PDF-Dokument [5.2 MB]

"The GREGOR Fabry-Perot Interferometer - Comissioning and Science Verification" - ePoster present during the 1st SOLARNET -3rd EAST/ATST Meeting in Oslo, 5-8 August 2013. A pdf-file of the presentation can be downloaded below.

The GREGOR Fabry-Perot Interferometer (GFPI) - Technical Innovations and Results achieved in 2013.

Abstract: The present contribution provides a summary of not yet published technical innovations to the GREGOR Fabry-Perot Interferometer (GFPI) at the 1.5m GREGOR Solar Telescope (Europe's largest solar telescope) that I implemented in 2013 as the Instrument Scientist of the GFPI. It also represents an overview of first important and not yet published observational results that I achieved with the GFPI in 2013. The results and achievements can be considered as a milestone in the scientific verification and further development of the Instrument. Please download the document below.

The GREGOR Fabry-Perot Interferometer (GFPI) - Technical Innovations and Results achieved in 2013.
DOI: 10.13140/RG.2.1.4175.9849, published July 2015 on Researchgate
Puschmann-2015-rg-small.pdf
PDF-Dokument [2.7 MB]

 

Observational Highlights: Imaging, Spectroscopy & Polarimetry with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope

First Context Imaging Data (G-band) @ full spatial sampling (corresponding to a spatial resolution of 60 km on the solar surface) that I observed in Spring 2013 with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. Subfield: Sunspot. The broad-band reconstruction has been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent Adaptive Optics correction, which is part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DP, the Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. e-Poster: "Synergies between ground and space based solar research", 1st SOLARNET meeting, Oslo, August 2013. For more details see Section Scientific Results 2012-2013 .

Raw image and Speckle reconstructed broad-band of the first context imaging Data (G-band) @ full spatial sampling (corresponding to a spatial resolution of 60 km on the solar surface) that I observed in Spring 2013 with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. Subfield: Quiet Sun. The broadband reconstruction has been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent Adaptive Optics correction, which is part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DP, the Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. e-Poster: "Synergies between ground and space based solar research", 1st SOLARNET meeting, Oslo, August 2013. For more details see Section Scientific Results 2012-2013 .

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Multi-wavelenght Imaging System (MWIS) - GREGOR Fabry-Perot Interferometer (GFPI) @ the 1.5m GREGOR Solar Telescope. Simultaneus Observations in 5 different channels: GFPI Narrow Band Channel (NBC) - spectroscopy & polarimetry; GFPI Broad Band Channel (BBC)- Imaging; GFPI Halpha Lyot Channel (HLC) -imaging, GFPI Gband - CaIIK Lyot Channel (Bue Imaging Channel, BIC). For more details see Section Scientific Results 2012-2013 and Breaking News 2015

 

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Observational Targets - August 2013 - GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope in spectroscopic and spectropolarimetric mode, accompanied by an innovative and novel multi-wavelength imaging setup (MWIS), including a G-band Interference filter and a Halpha- and CaIIK Lyot filter, respectively. The broadband reconstructions have been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent correction of Adaptive Optics, which is part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DPImaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. Targets: Sunspots and a quiet solar region at different heliocentric angles. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Still image of a time series of the first Stokes I spectra @ full spatial sampling (corresponding to an unique spatial resolution of 60 km on the solar surface) that I recored with the GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope  on 14 August 2013. The spectral observations have been  accompanied by context imaging obtained within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope, thus recording simultaneously photospheric and chromospheric small scale structure and their dynamics. From left to right and from top to bottom: Speckle reconstructed Broadband Image (630 nm; BB-SP) of the sunspot under investigation; Speckle-Deconvolved Narrowband Continuum Image (Fe I 630.2 nm line; NB-Cont), Narrowband Line-Core Image (Fe I 630.2 nm line; NB-Core), Line-of-Sight Velocity (Fe I 630.2 nm line; LoS Vel), Full-Width @ Half-Maximum (Fe I 630.2 nm line; FWHM) and Equivalent Width (Fe I 630.2 nm line; EQW); Speckle reconstructed G-band, Halpha Lyot- and CaIIK Lyot Images. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

From 16 to 19 August 2013, I performed the first spectropolarimetric observations ever recorded with the GREGOR Fabry-Perot Interferometer  @ the 1.5m GREGOR Solar TelescopeThe spectropolarimetric observations have been  accompanied by context imaging obtained within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope, simultaneously recording photospheric and chromospheric small scale structures, their dynamics and related magnetic fields. The processing of the data is in progress. However, due to the alt-azimuthal mount of GREGOR, a time-dependent telescope model is required in addition for a precise calibration of the spectropolarimetric observations. The available model (developed by a former AIP colleague) unfortunately turned out to be immature/incomplete at this point. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Polarimetric Calibration Measurement with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope (August 2013), demonstrating the excellent performance of the vector polarimetric mode of the instrument, including the new and automated instrumental calibration procedure that has been implemented in the instrument control software within a collaboration of La Vision Göttingen and myself. However, due to the alt-azimuthal mount of GREGOR, a time-dependent telescope model is required in addition for a precise calibration of the spectropolarimetric observations. The available model (developed by a former AIP colleague) unfortunately turned out to be immature/incomplete at this point. For details of the related observations see Section: Scientific Work 2012-2013

Image @copyright Klaus Gerhard Puschmann - Click to enlarge the image

Breakthrough - 8 October 2013: First Ca II IR spectra ever observed with the GREGOR Fabry-Perot Interferometer. I accompanied my spectroscopic observations by context imaging within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. Until today, the context imaging data  are exclusively retained by the AIP. Not even within an extremely costly juridical fight of more than a year I received copies of my observational data.  The broadband reconstructions have been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent correction of Adaptive Optics. The narrow-band data have been deconvolved using a modified version of a code developed by Krieg et al., 1999, A&A 343, 983 and K. Janssen, 2003, PHD-Thesis, which is based on the method of Keller & v.d. Luehe, 1992, A&A 261, 321. The codes are part of the GFPI-Datapipeline (Puschmann & Beck, 2011,A&A 533,21)

iSPOR-DP, Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

Angular resolution comparison between spectroscopic Ca II IR (854.2 nm) observations performed with CRISP/SST and GFPI/GREGOR (2013).

Breakthrough - 7 October 2013: First  Halpha spectra ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. I accompanied my spectroscopic observations by context imaging within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope. Until today, the context imaging data  are exclusively retained by the AIP. Not even within an extremely costly juridical fight of more than a year I received copies of my observational data.  The broad-band reconstructions have been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent correction of Adaptive Optics. The narrow-band data have been deconvolved using a modified version of a code developed by Krieg et al., 1999, A&A 343, 983 and K. Janssen, 2003, PHD-Thesis, which is based on the method of Keller & v.d. Luehe, 1992, A&A 261, 321. The codes are part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DPImaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the 

Imaging Spectropolarimetric Parallel Organized Reconstruction Server. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

@copyright Klaus Gerhard Puschmann

Breakthrough October 2013! Time series of specific Halpha line-parameters calculated from my observations of a sunspot observed on 7 October 2013 with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope. Upper pannels - from left to right: Bisector Velocity @ 90% and 17% Line Depression; Bisector Width @ 17% Line Depression. Lower panels - from left to right: Broad-Band Intensity, Line-Wing Intensity, Intensity @ 50% Line Depression. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. Most remarkable feature despite the perfectly resolved sunspot fine structure: Running umbral/penumbral waves. For more details see Section Scientific Results 2012-2013 and Breaking News 2015

 

Observational Highlights: Imaging, Spectroscopy & Polarimetry with the GREGOR Fabry-Perot Interferometer still deployed @ the German Vacuum Tower Telescope (VTT)

 

Time series of Halpha narrow-band spectra and broad-band images that I observed in 2006 with the GREGOR Fabry-Perot Interferometer (GFPI) @ the German Vacuum Tower Telescope (VTT). The presented movies are the results of a common investigation of Bruno Sanchez Andrade Nuno and myself under my directive and instructions. The broad-band reconstructions have been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Goettingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent correction of Adaptive Optics. The narrow-band data have been deconvolved using a modified version of a code developed by Krieg et al., 1999, A&A 343, 983 and K. Janssen, 2003, PHD-Thesis, which is based on the method of Keller & v.d. Luehe, 1992, A&A 261, 321. The codes are part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DP, the Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. Upper Panel: Speckle-deconvolved Halpha line-core images; Middle Panel: Speckle-deconvolved Halpha line-wing images; Lower panel: Speckle-reconstructed Broad-band images @656 nm. B. Sanchez Andrade Nuno, K.G. Puschmann, Kneer, F. 2007, 2007msfa.conf..273S.

Time series of line parameters from spectropolarimetric observations of the Fe I 525 nm line I performed with the GREGOR Fabry-Perot Interferometer GFPI @ the German Vacuum Tower Telescope (VTT) in 2006. The broad-band reconstructions have been performed with a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) accounting for the field dependent correction of Adaptive Optics. The narrow-band data have been deconvolved using a modified version of a code developed by Krieg et al., 1999, A&A 343, 983 and K. Janssen, 2003, PHD-Thesis, which is based on the method of Keller & v.d. Luehe, 1992, A&A 261, 321. The codes are part of the GFPI-Datapipeline (Puschmann & Beck, 2011, A&A 533, 21) iSPOR-DP, the Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. From left to right: Speckle reconstructed broad-band image; Speckle deconvolved narrow-band continuum intensity image; LOS-velocity map, Line-core intensity map, effective magnetic field map from weak field approximation. Region of interest: Dynamics of a magnetic network patch and the surrounding quiet Sun region (Puschmann et al. 2007, msfa.conf, 151p).

 

 

Spectral Line Inversion, Numerical Analysis, Mathematical Modeling

Results from a 3D geometrical semi-empirical modeling of an inner penumbral region of a sunspot subsequently applied to spectral line inversions of spectropolarimetric data obtained with the Solar Optical Telescope (SOT) onboard the Japanese Hinode Satellite: Electrical current density, twist, helicity, Wilson depression, plasma beta, total energy flux and the real geometrical height distribution of different physical parameters in a 2D FOV. The results have been obtained in collboration with Basilio Ruiz Cobo (IAC).

"A geometrical height-scale for sunspot penumbrae"; Seminar held @ AIP in May 2010
Potsdam_web.pdf
PDF-Dokument [2.9 MB]
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