A5012011601- Advanced Fiber Laser Technologies
- Photonic and Optical Devices
- Adaptive optics and wavefront sensing
- Spectroscopy and Laser Applications
- Photonic Crystal and Fiber Optics
- Advanced Fiber Optic Sensors
- Astronomy and Astrophysical Research
- Stellar, planetary, and galactic studies
- Semiconductor Lasers and Optical Devices
- Atmospheric Ozone and Climate
- Advanced Optical Sensing Technologies
- Optical Network Technologies
- Astronomical Observations and Instrumentation
- Calibration and Measurement Techniques
- History of Science and Medicine
- Plasma Diagnostics and Applications
- Historical Astronomy and Related Studies
- Gyrotron and Vacuum Electronics Research
- Mechanical and Optical Resonators
- Laser-induced spectroscopy and plasma
- Plasma Applications and Diagnostics
- Photocathodes and Microchannel Plates
- Environmental Monitoring and Data Management
- Advanced Fluorescence Microscopy Techniques
- CCD and CMOS Imaging Sensors
Leibniz Institute for Astrophysics Potsdam
2014-2024
Laboratoire Procédés, Matériaux et Energie Solaire
2012
Centre National de la Recherche Scientifique
2012
Ground-based near-infrared astronomy is severely hampered by the forest of atmospheric emission lines resulting from rovibrational decay OH molecules in upper atmosphere. The extreme brightness these lines, as well their spatial and temporal variability, makes accurate sky subtraction difficult. Selectively filtering with suppression instruments has been a long standing goal for spectroscopy. We have shown previously efficacy fibre Bragg gratings combined photonic lanterns achieving...
This paper describes an optical setup built to record Fourier transform infrared (FTIR) absorption spectra in atmospheric pressure plasma with a spatial resolution of 2 mm. The overall system consisted three basic parts: (1) components located within the FTIR sample compartment, making it possible define size beam (2 mm × over path length 50 mm) imaged at site by (2) interface positioned between spectrometer and reactor. Once through region, (3) retro-reflector module, behind reactor,...
Photonic Integrated Circuits (PIC) are best known for their important role in the telecommunication sector, e.g. high speed communication devices data centers. However, PIC also hold promise innovation sectors like life science, medicine, sensing, automotive etc. The past two decades have seen efforts of utilizing to enhance performance instrumentation astronomical telescopes, perhaps most spectacular example being integrated optics beam combiner interferometer GRAVITY at ESO Very Large...
The problem of atmospheric emission from OH molecules is a long standing for near-infrared astronomy. PRAXIS unique spectrograph which fed by fibres that remove the background and optimised specifically to benefit OH-Suppression. suppression achieved with fibre Bragg gratings, were tested successfully on GNOSIS instrument. uses same gratings as in its first implementation, will exploit new, cheaper more efficient, multicore second implementation. lines are suppressed factor ∼ 1000, expected...
In astronomical spectroscopy, optical fibers are abundantly used for multiplexing and decoupling the spectrograph from telescope to provide stability in a controlled environment. However, less than perfect components introduce complex effects that diminish overall throughput, efficiency, of instrument. We present novel numerical field propagation model emulates modal noise, scrambling, focal ratio degradation with rigorous treatment wave optics. demonstrate simulation near- far-field output...
Atmospheric emission from OH molecules is a long standing problem for near-infrared astronomy. PRAXIS unique spectrograph, currently in the build-phase, which fed by fibre array that removes background. The suppression achieved with Bragg gratings, were tested successfully on GNOSIS instrument. will use same gratings as first implementation, and new, less expensive more efficient, multicore second implementation. lines are suppressed factor of ~1000, expected increase signal-to-noise...
Abstract The wide‐field spectroscopic survey telescope (WST) is proposed to become the next large optical/near infrared facility for European southern observatory (ESO) once extremely (ELT) has operational. While latter optimized unprecedented sensitivity and adaptive‐optics assisted image quality over a small field of view, WST addresses need volumes in spectroscopy with light‐collecting power 10‐m class telescope. Its unique layout will feature combination multi‐object integral...
The problem of atmospheric emission from OH molecules is a long standing for near-infrared astronomy. We are now close to solving this the first time with PRAXIS instrument. unique spectrograph which fed by fibres that remove background, and optimised specifically benefit OH-Suppression. suppression achieved fibre Bragg gratings, were tested successfully on GNOSIS lines suppressed factor ~1000, leading reduction integrated background ≈9. A future upgrade multicore gratings will further...
We here report on recent progress astronomical optical frequency comb generation at innoFSPEC-Potsdam and present preliminary test results using the fiber-fed Multi Unit Spectroscopic Explorer (MUSE) spectrograph. The is generated by propagating two free-running lasers 1554.3 1558.9 nm through dispersionoptimized nonlinear fibers. centered 1590 comprises more than one hundred lines with an optical-signal-to-noise ratio larger 30 dB. A crystal used to double whole spectrum, which efficiently...
We present the optomechanical design of Potsdam Arrayed Waveguide Spectrograph (PAWS), which is first on-sky demonstrator an integrated photonic spectrograph specifically designed and optimized for astronomy. The instrument based on arrayed waveguide grating (AWG) that was by custom fabricated innovation center innoFSPEC Potsdam. commissioning planned at Calar Alto 2:2m Telescope in southern Spain. core AWG-chip as primary dispersive element. AWG device coupled to telescope module via a...
WST - Widefield Spectroscopic Telescope: We summarise the design challenges of instrumentation for a proposed 12m class Telescope that aims to provide large (>2.5 square degree) field view and enable simultaneous Multi-object (> 20,000 objects) Integral Field spectroscopy (inner 3x3 arcminutes view), initially at visible wavelengths. For MOS mode, includes fiber positioning units, runs high (R~40,000) low (R~3,000 4,000) resolution spectrographs. MUSE like Spectrograph, this relay from Focal...
The 4-Metre Multi-Object Spectrograph Telescope (4MOST) is a second-generation instrument build for ESO's VISTA telescope in Chile, enabling large-scale spectroscopic surveys of the night sky. 4MOST will complement several European space-based observatories and future ground-based survey facilities, furthering our understanding universe. uses over 2 400 science optical fibres to collect transmit light simultaneously from various astronomical targets three spectrographs. Two thirds go...
The wide-field spectroscopic survey telescope (WST) is proposed to become the next large optical/near infrared facility for European Southern Observatory (ESO) once Extremely Large Telescope (ELT) has operational. While latter optimized unprecedented sensitivity and adaptive-optics assisted image quality over a small field-of-view, WST addresses need volumes in spectroscopy with light-collecting power of 10 m class telescope. Its unique layout will feature combination multi-object integral...
BlueMUSE is a novel instrument under development for the ESO VLT, that builds on legacy of MUSE, however with blue wavelength range, larger field-of-view (FoV), and higher spectral resolution. Driven by high-profile unique science cases, requirements present new challenges to instrument, although fundamental layout will be based successful modular structure classical MUSE. In order achieve expected mean resolution R=3600 radial velocity measurement accuracy better than 1 km/s, as well...
The accurate characterization of the field at output optical fibres is relevance for precision spectroscopy in astronomy. modal effects fibre translate to illumination pupil spectrograph and impact on resulting point spread function (PSF). A Model presented that based Eigenmode Expansion Method (EEM) calculates from a given different manipulations input field. design modes calculation are done via commercially available Rsoft-FemSIM software. We developed Python script apply EEM. Results...
Photonic Integrated Circuits (PIC) are best known for their important role in the telecommunication sector, e.g. high speed communication devices data centers. However, PIC also hold promise innovation sectors like life science, medicine, sensing, automotive etc. The past two decades have seen efforts of utilizing to enhance performance instrumentation astronomical telescopes, perhaps most spectacular example being integrated optics beam combiner interferometer GRAVITY at ESO Very Large...
The Potsdam Arrayed Waveguide Spectrograph (PAWS) is based on an integrated photonic spectrograph designed and developed by innoFSPEC to work in the astronomical H‐band. PAWS demonstrates how a traditional bulk optics can be miniaturized additionally serves as tool for testing in‐house astrophotonical devices. main element second‐generation Grating (AWG) with unprecedented performance terms of spectral resolution throughput that fiber‐coupled works first dispersive component. pre‐dispersed...
Abstract For near‐infrared ground and space‐based astronomy, compact photonic devices can replace the large bulk optical components in spectrographs, frequency combs, beam combiners, sky subtraction filters, thus saving cost, reducing volume, weight, power requirements. Photonic integrated circuits (PICs), analogous to (IC) electronics, are particularly powerful address innovative miniaturized solutions. Here, we demonstrate two new instrument prototypes: Potsdam Arrayed Waveguide...
To better understand the impact of avalanche gain applied in detector technology and apply this our in-house astrophotonic projects, we have characterized a C-RED One camera produced stable reliable method for calculating system at any desired setting. We observed that depending on how is obtained, multiplying times may not accurately produce conversion factor from electrons to ADUs. Since acquisition photon transfer curve (PTC) was possible different levels, several PTCs low levels were...
Abstract To better understand the impact of avalanche gain applied in detector technology and apply this our in‐house astrophotonic projects, we have characterized a C‐RED One camera produced stable reliable method for calculating system at any desired setting. We observed that depending on how is obtained, multiplying times may not accurately produce conversion factor from electrons to ADUs. As acquisition photon transfer curve (PTC) was possible different levels, several PTCs low levels...
Dear Readers, Friends, The “Scientific Detector Workshop 2022” (SDW2022) was held during September 4–9, 2022 on the Telegrafenberg Campus of Leibniz-Institut für Astrophysik Potsdam (AIP) in Potsdam, Germany. This seventh meeting SDW series that initiated 1996 at European Southern Observatory (ESO) by James Beletic, following previous conferences organized Sandro D'Odorico, also ESO. motivation behind is creation an open and collaborative venue exchange information about high-performance...