Contact

Dr. Klaus Gerhard Puschmann

------------------------------------
Julius-Pfister-Ring 14d
63755 Alzenau

Bavaria

Germany

------------------------------------

Phone: +49 6023 7061001
Mobile: +49 1522 1517880

E-Mail: kgp@live.de

Dr. Klaus Gerhard Puschmann
Dr. Klaus Gerhard Puschmann

Breaking News 2015

 

This Section provides outstanding results from observations with the GREGOR Fabry Perot Interferometer (Imaging Spectropolarimeter) @ the 1.5m GREGOR Solar Telescope (Europe’s largest Solar Telescope) that I performed already in August and October 2013. Due to my violent expulsion from the Leibniz Institute for Astrophysics Potsdam (AIP) no earlier reduction and investigation of these outstanding and innovative observational data sets have been possible. Not even after an extremely costly juridical I possess all copies of my extraordinary and proof-finding data sets.

 

Nevertheless, in my opinion the results below depict the impressive potential of the above instrument as well as its precise performance and function already by 2013. Interestingly, the respective group leader and his employees apparently have not been able to produce any comparable data or scientific results until today. Apparently a tremendous waste of public money (3 Million Euros for the Instrument, 20 Million Euros for the Telescope) likely due to the personal and private political ambitions of the respective group leader that is supported by his institution and a frequent number of national and international scientists and institutions. The AIP still withholds part of my observational data, very likely to hamper any outreach of my technical innovations and observational results, as well as their importance and excellence.

 

As a first example, I present below results obtained on 9 June 2015.  These results are based on the first full spatial resolution Stokes I spectra ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope that I already recorded on 14 August 2013! These spectral observations, have been accompanied by an innovative and novel Multi-wavelength Imaging Setup (MWIS) that I implemented in 2013, covering simultaneously the small scale structure and dynamics of the solar Photosphere and Chromosphere by means of a G-band Interference filter and a CaIIK Lyot Filter (loan from the spectrograph of the German Vacuum Tower Telescope, VTT) in the Blue Imaging Channel (BIC) and an additional  Halpha Lyot Filter (former property of the Einstein Tower) in the BroadBand Channel (BBC) of the instrument. Also in 2013 and certainly also with the help of others, I replaced the former pentaprism with a cut-off at 650nm in front of the primary focus of the instrument by an innovative 3-mirror systems that provides now the entire spectral range 380-860nm for the instrument.

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

Figure: Deployed Halpha- and CaIIK Lyot Filters in the BroadBand Channel (BBC) and Blue Imaging Channel (BIC) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope as part of an innovative and novel Multi-Wavelength Imaging Setup (MWIS).

Figure: Left Panel - Old Setup with the GRIS-GFPI Pentaprism with a cut-off @ 650 nm infront of the primary focus of the instrument. Right Panel - innovative 3-mirror system, providing the entire spectral range 380-860nm for the instrument.

 

The achieved results are a milestone in the verification of the instrument and telescope as well as in solar physics research and solar instrumentation. The Leibniz Institute for Astrophysics Potsdam (AIP) retained the respective data exclusively over several months. It needed a long and extremely costly juridical fight to obtain at least most of my observational data also thanks to my lawyers and the respective judge in charge.

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

Figure: Still image of a time series of the first Stokes I spectra @ full spatial sampling  ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope that I recorded 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 instrument, thus recording simultaneously photospheric and chromospheric small scale structures 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.

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 narrowband 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 Spectropolarimteric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server that I purchased and configured thanks to the financial support of a friend who likes to be kept anonymous.

 

Despite the extremely detailed umbral and penumbral fine structure and flow field of the Sunspot under observations, an apparently penumbral magnetic field reconnection (penumbral flash) seems to leave its fingerprints exclusively within the Halpha Lyot- and CaIIK Lyot filter images, corresponding to upper photospheric and chromospheric layers. Just within approx. 20 minutes, one observes a remarkable brightening at the respective location in the penumbra that subsequently directs inwards and outwards the sunspot penumbra. The inward flow finally forms an arc of umbral dots at high atmospheric layers. The entire physical process is detailed in the figure below and will be studied and analyzed in more detail in the near future.

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

Figure: Temporal evolution (from left to right) of photospheric and chromospheric fine structure obtained from a time series of Stokes I spectra and context imaging data obtained within an innovative and novel Multi-wavelength Imaging Setup (MWIS) of the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope on 14 August 2013. 

 

From top to bottom: Speckle reconstructed photospheric BroadBand Image (630 nm; BB-SP); photospheric Speckle-Deconvolved NarrowBand Line-Core Image (Fe I 630.2 nm line; NB_Core); upper photospheric and chromospheric Speckle-reconstructed Halpha Lyot and CaIIK Lyot Filter Images. 

As a second example, I present below results obtained 21-24 June 2015.  These results are based on some of the first fully spatially sampled Stokes I spectra ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope that I already recorded on 15 August 2013! Like on 14 August 2013, the spectral observations have been accompanied by an innovative and novel Multi-wavelength Imaging Setup (MWIS), covering simultaneously the small scale structure and dynamics of the solar Photosphere and Chromosphere by means of a G-band Interference filter and a CaIIK Lyot Filter (loan from the spectrograph of the German Vacuum Tower Telescope, VTT) in the Blue Imaging Channel (BIC) and an additional  Halpha Lyot Filter (former property of the Einstein Tower) in the BroadBand Channel (BBC) of the instrument.

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

Figure: Still image of a time series of some of the first Stokes I spectra @ full spatial sampling  ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope that I recorded on 15 August 2013. The spectral observations have been accompanied by context imaging obtained within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the instrument, thus recording simultaneously photospheric and chromospheric small scale structures 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.

Figure: Still image of a time series of some of the first Stokes I spectra @ full spatial sampling  ever observed with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR Solar Telescope that I recorded on 15 August 2013. The spectral observations have been accompanied by context imaging obtained within an innovative and novel Multi-Wavelength Imaging Setup (MWIS) of the instrument, thus recording simultaneously photospheric and chromospheric small scale structures 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.

Already on 30 December 2014, I achieved another tremendous breakthrough in solar physics and instrumentation, by presenting outstanding results related to the first Ca II IR spectra ever observed with the GREGOR Fabry-Perot Interferometer (GFPI) and the first Halpha-spectra ever observed with the instrument @ the 1.5m GREGOR Solar Telescope, which I recorded on 7 and 8 October 2013. See also my related LinkedIn-post Tremendous Breakthrough in Solar Physics.These observations have been possible due to an innovative and novel 3-mirror system in front of the instrument, which I installed during the second half of 2013 and which replaces now the limiting pentaprism with a cutoff at 650 nm that has been installed before. The spectral observations have been accompanied by the innovative and novel Multi-Wavelength Imaging Setup (MWIS), although the recorded data sets are still exclusively retained on purpose by the Leibniz Institute for Astrophysics Potsdam (AIP). Not even after an extensive and costly juridical fight for more than one year I have been able to receive copies of this data.

@copyright Klaus Gerhard Puschmann - Click to enlarge the image

Figure: Breakthrough December 2014! Reconstruction of the First Ca II IR spectra ever observed with the GREGOR Fabry-Perot Interferometer that I recorded on 8 October 2013. 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. Crosses in the above-presented average spectral profile depict the individual spectral positions scanned.

@copyright Klaus Gerhard Puschmann - Click to enlarge the image

Figure: Breakthrough December 2014! Reconstruction of the first Halpha-Spectra ever observed with the GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope that I recorded on 7 October 2013. The broadband 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, Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. Crosses in the above-presented average spectral profile depict the individual spectral positions scanned.

@copyright Klaus Gerhard Puschmann

Figure: Breakthrough December 2014! Time series of specific Halpha line-parameters calculated from observations of a sunspot that I performed on 7 October 2013 with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope. Upper panels - 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 dominating with increasing height.

@copyright Klaus Gerhard Puschmann

Figure: Breakthrough December 2014! Time series of specific Halpha line-parameters calculated from observations of a sunspot that I performed on 7 October 2013 with the GREGOR Fabry-Perot Interferometer @ the 1.5m GREGOR solar telescope. Upper panels - from left to right: Bisector Width @ 33% Line Depression; Full-Width @ Half-Maximum; Bisector Width @ 83% Line Depression. Lower panels - from left to right: Intensity @ 70% and 83% Line Depression; Line-Core Intensity. 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.

@copyright Klaus Gerhard Puschmann

Figure: HMI Context-Information - Animation showing the temporal evolution of the Magnetic-Field Configuration of the above Sunspot. Upper panels - from left two right: unsigned Magnetic-Field Strength; Magnetic-Field Inclination; Magnetic Line-of-Sight Velocity; Magnetic-Field Azimuth. Lower panels - from left to right: Intensity; Magnetic-Field Polarity; Line-of-Sight Velocity; AIA 304nm Intensity. HMI data are courtesy of NASA/SDO and the HMI science team. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server.

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

Figure: Breakthrough December 2014! Reconstruction of the first Halpha-Spectra ever observed with the GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope that I recorded on 7 October 2013. The broadband 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, Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. Panels: BB-SP - Broadband Speckle Image: NB-W - Deconvolved Narrow-band Line-Wing Images at increasing distance / spectral positions [p7]-[p16]  from the deconvolved Narrow-band Line-Core Image [p0]. Crosses in the above-presented average spectral profile depict the individual spectral positions scanned.

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

Figure: Breakthrough December 2014! Reconstruction of the first Halpha-Spectra ever observed with the GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope that I recorded on 7 October 2013. The broadband 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, Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. Panels: BB-SP - Broadband Speckle Image: NB-W - Deconvolved Narrow-band Line-Wing Images at increasing distance / spectral positions [p8]-[p16]  from the deconvolved Narrow-band Line-Core Image [p0]. Crosses in the above-presented average spectral profile depict the individual spectral positions scanned.

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

Figure: Breakthrough December 2014! Reconstruction of the first Halpha-Spectra ever observed with the GREGOR Fabry-Perot Interferometer @ 1.5m GREGOR Solar Telescope that I recorded on 7 October 2013. The broadband 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, Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline. The data have been processed on iSPOR-S, the Imaging Spectropolarimetric Parallel Organized Reconstruction Server. Panels: BB-SP - Broadband Speckle Image: NB-W - Deconvolved Narrow-band Line-Wing Images at increasing distance / spectral positions [p7]-[p16]  from the deconvolved Narrow-band Line-Core Image [p0]. Crosses in the above-presented average spectral profile depict the individual spectral positions scanned.

The GREGOR Fabry-Perot Interferometer Data Pipeline iSPOR-DP (Imaging Spectropolarimetric Parallel Organized Reconstruction Data Pipeline) is based on a modified version (Puschmann & Sailer, 2006, A&A 454, 1011) of the Göttingen broadband reconstruction code (de Boer, 1993, PHD-Thesis) and a modified version of a narrow-band deconvolution code developed by Krieg et al., 1999, A&A 343, 983 and K. Janssen, 2003, PHD-Thesis, which further bases on the method of Keller & v.d. Luehe, 1992, A&A 261, 321. As an alternative option also the Multi-Frame Multi-Object Blind-Deconvolution code (MOMFBD; M. Löfdahl, 2002, SPIE 4792, 146; M. van Noort et al. 2005, Solar Physics 228 ,19) can be applied instead. Details to this data-pipeline can be found in Puschmann & Beck 2011, A&A 533, 22. C. Beck (NSO) supplied me with his codes for the polarimetric calibration and analysis of spectropolarimetric data. Image: left-hand side - Broadband Raw-Image 656nm; right hand side - Speckle-reconstructed Broadband Image 656nm, with clearly improved contrast and spatial resolution after the application if iSPOR. By means of the Speckle reconstructed broadband images, one is able to deconvolve the narrow-band images, thus also further improving the spatial resolution and contrast of the corresponding spectra.

Unfortunately and as mentioned above, the AIP still exclusively retains on purpose the Gband-, Halpha Lyot- and CaIIK Lyot context imaging data that I observed on 7 and 8 October 2013 (see my related LinkedIn-post) and further denies to hand over copies of these novel and proof-finding data sets. These context data sets have been observed under even better seeing conditions than those presented above from August 2013.

 

Moreover, within a marginal publication in 2014, the institute violated the creator ship concerning these data, by publishing part of my observations without my permission or any appropriate citation, therefore misappropriating the impact of my contribution and my observational results. For detailed information on this concern and other shocking details  see my related LinkedIn-post. Subsequently, the AIP even announced to delete part of these data.  In order to prevent this marginal act, I asked for another court hearing. Surprisingly, I lost the hearing, which equals to the end of scientific freedom and thus makes science as a profession ridiculous and questionably.  The institute's proper pettifogger has become the cornerstone of AIP's research strategy and activity and representation to outside although he apparently did not possess any scientific knowledge or any knowledge on basic scientific facts and his reasoning was full of contradicting fabrications and false constructions.

 

 

All technical innovations and observational results to the GREGOR Fabry-Pérot interferomter at the 1.5m GREGOR Solar Telescope that I achieved in 2013 are summarized within the article cited below that I published in 02/2016:

 

****************************************************

 

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

 

Klaus Gerhard Puschmann

 

2016arXiv160205783P


****************************************************
 

Druckversion Druckversion | Sitemap
© Dr. Klaus Gerhard Puschmann