We report on the CCAT-prime Project, including the science program, the Fred Young Submillimeter Telescope (FYST), its instrumentation, and the schedule. FYST is a 6-m telescope sited at 5600 m elevation near the summit of Cerro Chajnantor in northern Chile. The site, together with its very large field-of-view optics, and high surface accuracy, low-emissivity surface enables pursuit of low surface brightness science over large fields. Our science goals include: tracing the formation and evolution of star forming galaxies from the epoch of reionization to the cosmic peak of star formation activity through wide-field, broad-band [CII] line imaging and dust continuum surveys; constraining thermodynamics and feedback in galaxy clusters through the Sunyaev-Zel’dovich effects on the CMB; improving constraints on primordial gravitational waves through precision removal of polarization foregrounds; and tracing local star formation processes through velocity-resolved spectroscopy at 15” spatial resolution over 110 scales in the Galaxy. These goals are realized through sensitive wide-field surveys. Our main instruments are Prime-Cam, a large FoV direct detection imager and CHAI, a multi-beam submillimeter heterodyne spectrometer. We have also built Mod-Cam which serves as a Prime-Cam test facility and/or first light camera. Prime-Cam has seven instrument modules, four now under construction: three polarimetric cameras (at 280, 350, and 850 GHz) and a 210-420 GHz Fabry-Perot imaging spectrometer, EoR-Spec. CHAI will have 128 pixels covering important lines in the short submillimeter windows. The CCAT-prime team is an international group of universities, led by Cornell University. FYST is being designed and built by CPI Vertex Antennentechnik, GmbH, Germany with first light expected in 2024.
For the telescope number and size of the PFI proposal (20 x 8m), the Q-band (around 25 μm) was shown to be an optimal complement to submm- and optical interferometry, to detect substructures in proto-planetary disks. Here, broadband medium-resolution heterodyne would be an appropriate option, considering recent experimental findings on a quantum-limit heterodyne detection (HD) scheme. Under high thermal background and the very small beam filling factors in interferometry, HD was shown to be more sensitive than direct detection for the same bandwidth for wavelengths larger 3-8 micron, depending on the conditions. A new class of heterodyne mixers based on graphene could extend the instantaneous IF-bandwidth up to hundred GHz, for which photonic correlators may be developed since a resolution of R=30000 would be sufficient at 10μm. Such large IF-bandwidths could then even be multiplied in “dispersed heterodyne receivers” using optical frequency combs and photonic techniques derived from the DWDM technology.
We describe a system being developed for measuring the shapes of the mirrors of the Fred Young Submillimeter Telescope (FYST), now under construction for the CCAT Observatory. “Holographic” antenna-measuring techniques are an efficient and accurate way of measuring the surfaces of large millimeter-wave telescopes and they have the advantage of measuring the wave-front errors of the whole system under operational conditions, e.g. at night on an exposed site. Applying this to FYST, however, presents significant challenges because of the high accuracy needed, the fact that the telescope consists of two large off-axis mirrors, and a requirement that measurements can be made without personnel present. We use a high-frequency (~300GHz) source which is relatively close to the telescope aperture (<1/100th of the Fresnel distance) to minimize atmospheric effects. The main receiver is in the receiver cabin and can be moved under remote control to different positions, so that the wave-front errors in different parts of the focal plane can be measured. A second receiver placed on the yoke provides a phase reference. The signals are combined in a digital cross-correlation spectrometer. Scanning the telescope provides a map of the complex beam pattern. The surface errors are found by inference, i.e. we make models of the reflectors with errors and calculate the patterns expected, and then iterate to find the best match to the data. To do this we have developed a fast and accurate method for calculating the patterns using the Kirchhoff-Fresnel formulation. This paper presents details of the design and outlines the results from simulations of the measurement and inference process. These indicate that a measurement accuracy of ~3μm rms is achievable.
We present the detailed science case, and brief descriptions of the telescope design, site, and first light instrument plans for a new ultra-wide field submillimeter observatory, CCAT-prime, that we are constructing at a 5600 m elevation site on Cerro Chajnantor in northern Chile. Our science goals are to study star and galaxy formation from the epoch of reionization to the present, investigate the growth of structure in the Universe, improve the precision of B-mode CMB measurements, and investigate the interstellar medium and star formation in the Galaxy and nearby galaxies through spectroscopic, polarimetric, and broadband surveys at wavelengths from 200 m to 2 mm. These goals are realized with our two first light instruments, a large field-of-view (FoV) bolometer-based imager called Prime-Cam (that has both camera and an imaging spectrometer modules), and a multi-beam submillimeter heterodyne spectrometer, CHAI. CCAT-prime will have very high surface accuracy and very low system emissivity, so that combined with its wide FoV at the unsurpassed CCAT site our telescope/instrumentation combination is ideally suited to pursue this science. The CCAT-prime telescope is being designed and built by Vertex Antennentechnik GmbH. We expect to achieve first light in the spring of 2021.
The CCAT-prime telescope is a 6-meter aperture, crossed-Dragone telescope, designed for millimeter and sub-millimeter wavelength observations. It will be located at an altitude of 5600 meters, just below the summit of Cerro Chajnantor in the high Atacama region of Chile. The telescope’s unobscured optics deliver a field of view of almost 8 degrees over a large, flat focal plane, enabling it to accommodate current and future instrumentation fielding <100k diffraction-limited beams for wavelengths less than a millimeter. The mount is a novel design with the aluminum-tiled mirrors nested inside the telescope structure. The elevation housing has an integrated shutter that can enclose the mirrors, protecting them from inclement weather. The telescope is designed to co-host multiple instruments over its nominal 15 year lifetime. It will be operated remotely, requiring minimum maintenance and on-site activities due to the harsh working conditions on the mountain. The design utilizes nickel-iron alloy (Invar) and carbon-fiber-reinforced polymer (CFRP) materials in the mirror support structure, achieving a relatively temperature-insensitive mount. We discuss requirements, specifications, critical design elements, and the expected performance of the CCAT-prime telescope. The telescope is being built by CCAT Observatory, Inc., a corporation formed by an international partnership of universities. More information about CCAT and the CCAT-prime telescope can be found at www.ccatobservatory.org.
The 1.1 THz multi-pixel heterodyne receiver will be mounted in the Nasmyth A cabin of the 12 m APEX telescope on the Chajnantor plateau, 5000 meters altitude in northern Chile. The receiver will cover the spectral window of 1000 - 1080 GHz, where important spectral lines like CO 9-8 at 1036.9 GHz, a tracer of warm and dense gas and OH+ at 1033 GHz and NH+ at 1012.6 GHz, both important for the study of chemical networks in the ISM, are located. The multi-pixel receiver greatly enhances the science output under the difficult observing conditions in this frequency range. Two 9-pixel focal plane sub-arrays on orthogonal polarizations are installed in easily removable cartridges. We developed a new thermal link to connect the cartridges to the cryostat. Our thermal link is an all-metal design: aluminum and Invar. All the optics is fully reflective, thus avoiding the absorption and reflection losses of dielectric lenses and reducing standing waves in the receiver. To guaranty internal optics alignment, we employ a monolithic integrated optics approach for the cold optics and the Focal Plane Unit (FPU) optics modeled after the CHARM (Compact Heterodyne Array Receiver Module) concept. The receiver uses synthesizer-driven solid-state local oscillators (LO) and the mixers will be balanced SIS mixers, which are essentially based on the design of the on-chip balanced SIS mixers at 490 GHz developed in our institute. Singleended HEB mixers are used for the laboratory tests of the optics. The LO power distribution is accommodated behind the FPU optics. It is composed of the LO optics, which includes a collimating Fourier grating, and an LO distribution plate to supply LO signal to each of the 9 pixels of the sub-array. Different options for the LO coupling design and fabrication are being analyzed and will be based on in-house hybrid waveguide/planar technology. We summarize the receiver project with emphasis on the cryogenics and the optics and present laboratory test results of the cryogenics, including the thermal link's performance. Beam pattern measurements of the receiver optics are scheduled for the coming days, but unfortunately could not be included in the current paper.
The Stratospheric TeraHertz Observatory (STO) is a NASA funded, Long Duration Balloon (LDB) experiment designed to
address a key problem in modern astrophysics: understanding the Life Cycle of the Interstellar Medium (ISM). STO will
survey a section of the Galactic plane in the dominant interstellar cooling line [C II] (1.9 THz) and the important star
formation tracer [N II] (1.46 THz) at ~1 arc minute angular resolution, sufficient to spatially resolve atomic, ionic and
molecular clouds at 10 kpc. STO itself has three main components; 1) an 80 cm optical telescope, 2) a THz instrument
package, and 3) a gondola [1]. Both the telescope and gondola have flown on previous experiments [2,3]. They have been reoptimized
for the current mission. The science flight receiver package will contain four [CII] and four [NII] HEB mixers,
coupled to a digital spectrometer. The first engineering test flight of STO was from Ft. Sumner, NM on October 15, 2009.
The ~30 day science flight is scheduled for December 2011.
GREAT (German REceiver for Astronomy at Terahertz frequencies) has been selected as first-light instrument for the
early science flights of SOFIA, scheduled for early 2009. In its first-light configuration GREAT will allow observations
in two out of three FIR bands: two low frequency channels 1.25-1.5 THz and 1.82-1.92 THz for observations of, e.g.,
highly excited CO and of ionized carbon, and a 2.7 THz channel focusing on the ground-state transition of deuterated
molecular hydrogen HD. A forth channel, centered on the 4.7 THz transition of atomic oxygen will become available
later.
The observatory schedule asks for delivery of the instrument in early 2009. At the time of the conference system level
assembly, integration, and verification (AIV) is ongoing, and we report on the performance of the integrated system.
Shipment to NASA/DAOF (Dryden aircraft operations facility) in Palmdale/California for aircraft integration is currently
planned for mid December 2008.
We report on developments of submillimeter heterodyne arrays for high resolution spectroscopy with APEX. Shortly, we will operate
state-of-the-art instruments in all major atmospheric windows accessible from Llano de Chajnantor. CHAMP+, a dual-color 2×7 element heterodyne array for operation in the 450 μm and 350 μm atmospheric windows is in operation since late 2007. With its
state-of-the-art SIS detectors and wide tunable local oscillators, its cold optics with single sideband filters and with 3 GHz of processed IF bandwidth per pixel, CHAMP+ does provide outstanding observing capabilities. The Large APEX sub-Millimeter Array (LAsMA) is in the final design phase, with an installation goal in 2009. The receiver will operate 7 and 19 pixels in the lower submillimeter windows, 285-375 GHz and 385-520 GHz, respectively. The front-ends are served by an array of digital wideband Fast Fourier Transform spectrometers currently processing up to 32×1.5 (optionally 1.8) GHz of bandwidth. For CHAMP+, we process 2.8 GHz of instantaneous bandwidth (in 16.4 k channels) for each of the 14 pixels.
GREAT, the German REceiver for Astronomy at Terahertz frequencies, is a first generation SOFIA dual channel
heterodyne PI−instrument for high resolution spectroscopy. The system is developed by a consortium of German
research institutes. The receiver will allow simultaneous observations in two out of the following three far−infrared
frequency bands:
* a low−frequency (1.4−1.9 THz) channel for e.g. the fine-structure lines of ionized nitrogen [NII] at 205μm
and ionized carbon [CII] at 158μm;
* a mid−frequency (2.4−2.7 THz) channel for e.g. the 112μm transition of HD; and
* a high−frequency (4.7 THz channel) for the 63 μm fine−structure line of neutral atomic oxygen.
Hot electron bolometers (HEB) mixers provide state of the art sensitivity. A spectral resolving power of up to
108 is achieved with chirp transform spectrometers, and a total bandwidth of 4 GHz at 1 MHz resolution is
reached with wide band acousto-optical spectrometers. The modular concept of GREAT allows to observe with
any combination of two out of the three channels aboard SOFIA. A more complete frequency coverage of the
THz regime by adding additional GREAT channels is possible in the future. The adaptation of new LO−, mixer−
or backend−techniques is easily possible.
We describe details of the receiver and the results of first performance tests of the system at 1.9 THz. As an
outlook to future developments we show first results obtained with phase locking a quantum cascade laser, the
most promising option for future high power local oscillators in the Terahertz regime.
GREAT, the German REceiver for Astronomy at Terahertz frequencies, is a first generation SOFIA dual channel
heterodyne PI-instrument for high resolution spectroscopy. The system is developed by a consortium of German
research institutes. The receiver will allow simultaneous observations in two out of the following three far-infrared
frequency bands:
a 1.4-1.9 THz channel for e.g. the fine-structure line of ionized carbon [CII] at 158μm;
a 2.4-2.7 THz channel for e.g. the 112μm transition of HD; and
a 4.7 THz channel for the 63 μm fine-structure line of neutral atomic oxygen.
Hot electron bolometers (HEB) mixers provide state of the art sensitivity. A spectral resolving power of up to
108 is achieved with chirp transform spectrometers, and a total bandwidth of 4 GHz at 1 MHz resolution is
reached with wide band acousto-optical spectrometers. The modular concept of GREAT allows to observe with
any combination of two out of the three channels aboard SOFIA. A more complete frequency coverage of the
THz regime by adding additional GREAT channels is possible in the future. The adaptation of new LO-, mixer-
or backend-techniques is easily possible. We describe details of the receiver and the results of first performance
tests of the system at 1.9 THz.
We present the first astronomical results from DesertSTAR, a 7 pixel heterodyne array receiver designed for operation in the astrophysically rich 345 GHz atmospheric window. DesertSTAR was constructed for the 10m Heinrich Hertz Telescope located at 3150m elevation on Mt. Graham, Arizona. This receiver promises to increase mapping speed at the HHT by a factor of ~15 over the facility's existing single beam, dual polarization receiver. DesertSTAR uses tunerless, single-ended waveguide SIS mixers to achieve uncorrected receiver noise temperatures of ~60K. The instantaneous bandwidth is 2 GHz, with a 5 GHz Intermediate Frequency, offering 1600 km/s of velocity coverage. Cryogenic isolators are employed between the mixers and low noise amplifiers to assure a flat IF passband. The system uses a Joule-Thompson closed-cycle refrigerator with 180W capacity at 70K and 1.8W capacity at 4K. A novel reflective phase grating is used for Local Oscillator multiplexing, while a simple Mylar beamsplitter is used as an LO diplexer. Optics include only polyethelene mixer lenses and a single, cold, flat mirror, maximizing simplicity for high efficiency and easy optical alignment. The computer controlled bias system provides low noise bias for the SIS junctions, magnets and LNAs through a modular and hardware independent GUI interface, and allows remote operation and monitoring. We present measurements of receiver noise, beam quality, efficiency and stability in addition to astronomical observations obtained during engineering runs at the HHT.
The German REceiver for Astronomy at Terahertz frequencies (GREAT) is a first generation PI instrument for the SOFIA telescope, developed by a collaboration between the MPIfR, KOSMA, DLR, and the MPAe. The first three institutes each contribute one heterodyne receiver channel to operate at 1.9, 2.7 and 4.7 THz, respectively. A later addition of a e.g. 1.4 THz channel is planned.
The GREAT instrument is developed to carry two cryostats at once. That means that any two of the three frequencies can be observed simultaneously. Therefore, we need to be able to quickly exchange the optics benches, the local oscillator (LO) subsystems, and the cryostats containing the mixer devices. This demands a high modularity and flexibility of our receiver concept. Our aim is to avoid the need for realignment when swapping receiver channels.
After an overview of the common GREAT optics, a detailed description of several parts (optics benches, calibration units, diplexer, focal plane imager) is given. Special emphasis is given to the LO optics of the KOSMA 1.9 THz channel, because its backward wave oscillator has an astigmatic output beam profile, which has to be corrected for. We developed astigmatic off-axis mirrors to compensate this astigmatism. The mirrors are manufactured in-house on a 5 axis CNC milling machine. We use this milling machine to obtain optical components with highest surface accuracy (about 5 microns) appropriate for these wavelengths. Based on the CNC machining capabilities we present our concept of integrated optics, which means to manufacture optical subsystems monolithically. The optics benches are located on three point mounts, which in conjunction with the integrated optics concept ensure the required adjustment free optics setup.
We present the opto-mechanical layout of KOSMA's (Kolner Observatorium fur SubMillimeter Astronomie) submillimeter and terahertz heterodyne array receiver STAR (SOFIA Terahertz Array Receiver) which is derived from SMART (Sub-Millimeter Array Receiver for Two frequencies). To reduce the alignment effort, SMART, for the first time, uses an integrated optics concept with no adjustable optical components inside the receiver dewar. For STAR this successful design concept will be extended and adapted for 1.9 THz and for use aboard SOFIA (Stratospheric Observatory For Infrared Astronomy).
The design of STAR's cryostat and cryogenic optics is described. Emphasis is laid on the required accuracy for 4x4 spatially multiplexed Terahertz heterodyne receivers. The proposed design of the local oscillator, a frequency-tripled BWO (Backward Wave
Oscillator), is outlined. The presentation comprises the scheme
for multiplexing the local oscillator, dense arrangement of mixer elements in a cryogenic focal plane and manufacturing techniques of integrated optics units for reduction of optical adjustment efforts in astronomical submillimeter and terahertz receivers.
We are developing a 1.4 THz receiver to explore the far infrared
universe, such as probing high mass star forming regions using,
e.g., the high J transitions of CO, investigating the warm
interstellar medium in N+ or probing cold and dense stellar cores in H2D+. Due to the poor atmospheric transmission at these frequencies we are planning to use this modular receiver on high altitude ground based observatories, for example the Atacama Pathfinder EXperiment (APEX), and as an additional channel for the German Receiver for Astronomy at Terahertz Frequencies (GREAT) on the Stratospheric Observatory For Infrared Astronomy (SOFIA) located on an airplane. To allow successful astronomical observations under poor atmosphere transmission a low receiver noise temperature and a high receiver stability are mandatory. To achieve a low receiver temperature the main effort is directed to develop phonon-cooled NbTiN HEB mixers. For optimum coupling with the telescope beam and easier alignment we are focussing on waveguide mixers. A phase locked Gunn (114-135 GHz) and three multipliers will be used as the Local Oscillator (LO) of 1370-1500 GHz. A liquid He Dewar will be used for operation on SOFIA and a closed-cycle system with a pulse-tube cooler on APEX. Initially, we are aiming for 1 GHz IF bandwidth (214 kms-1 at 1.4 THz) sufficient for galactic
observations. First tests and astronomical observations with a similar but lower frequency HEB at 800 GHz have yielded encouraging results.
We present the concept for KOSMA's 16 element 1.9 THz heterodyne array
STAR (SOFIA Terahertz Array Receiver) which is being developed for
SOFIA. The instrument will consist of two interleaved sub-arrays of 8
pixels each. Together we will have a 4 × 4 pixel array with a beam spacing on the sky of approximately 1.5 times the beam size of 15 arcsec (FWHM). The receiver is mainly targeted at measuring the fine structure transition of ionized atomic carbon at 1.9 THz (158 microns). STAR's optics setup is modeled after the successful design used in KOSMA's SMART receiver. It will contain a K-mirror type beam rotator, a Martin-Puplett diplexer for LO coupling and an LO multiplexer using imaging Fourier gratings. Complete optical sub-assemblies will be machined monolithically as integrated optics units, to reduce the need for optical alignment. STAR will probably use waveguide mixers with diffusion cooled hot electron bolometers, which are being developed at KOSMA. The receiver backends will be KOSMA Array-AOSs. Local oscillator power will be provided by a backward wave oscillator (BWO), followed by a frequency tripler.
GREAT - a heterodyne instrument for high-resolution spectroscopy aboard SOFIA is developed by a consortium of German research institutes. The first-light configuration will allow parallel observations in two far-infrared frequency bands. We will have a choice of back-ends, including a broad-band acousto-optical array and a high-resolution chirp transform spectrometer. We describe the structural and quasi-optical design of the receiver, update on the front-end and back-end developments and discuss the data acquisition system.
We present the first results obtained with our new dual frequency SIS array receiver SMART The instrument is operational since September 2001 at the KOSMA 3m telescope on Gornergrat near Zermatt/Switzerland. The receiver consists of two 2×4 pixel subarrays. One subarray operates at a frequency of 490 GHz, the other one at 810 GHz. Both subarrays are pointed at the same positions on the sky. We can thus observe eight spatial positions in two frequencies simultaneously. For the first year of operation we installed only one half of each subarray, i.e. one row of 4 mixers at each frequency.
The receiver follows a very compact design to fit our small observatory. To achieve this, we placed most of the optics at ambient temperature, accepting the very small sensitivity loss caused by thermal emission from the optical surfaces. The optics setup contains a K-mirror type image rotator, two Martin-Puplett diplexers and two solid state local oscillators, which are multiplexed using collimating Fourier gratings. To reduce the need for optical alignment, we machined large optical subassemblies monolithically, using CNC milling techniques. We use the standard KOSMA fixed tuned waveguide SIS mixers with Nb junctions at 490 GHz, and similar Nb mixers with Al tuning circuits at 810 GHz.
We give a short description of the front end design and present focal plane beam maps, receiver sensitivity measurements, and the first astronomical data obtained with the new instrument.
DesertSTAR is a 7 beam, 345 GHz heterodyne array receiver for the Heinrich Hertz Telescope (HHT) on Mt. Graham, AZ. The instrument uses fixed-backshort Superconductor-Insulator-Superconductor (SIS) mixers with a broadband waveguide probe. Instantaneous bandwidths greater than 2 GHz can be achieved over the entire 345 GHz atmospheric window. A cryostat with a Joule-Thompson (JT) mechanical refrigerator allows continuous operation and 1.8W of cooling capacity at 4K, and provides the needed temperature stability for low-noise operation. Local Oscillator (LO) distribution is accomplished with a novel phase grating that yields high efficiency and power uniformity in a hexagonally symmetric geometry. The computer controlled bias system is an evolution of a proven design that is simple and portable to any computer platform. The 2 GHz Intermediate Frequency (IF) bandwidth allows the future addition of a wideband backend optimized for extragalactic observations, with ~1700 km/s of velocity coverage. We present measurements of receiver performance and plans for integration on the HHT.
We have used digital photogrammetry to accurately measure the surface of the KOSMA 3m-telescope's primary mirror. The method uses a large number of optical photographs of the telescope, taken from many different viewing angles to reconstruct the three-dimensional mirror surface. Thin retro-reflective targets are applied to the mirror in the places of interest. With a large format, high resolution metric CCD-camera a series of pictures is taken under many different viewing angles. A computer program compares the image data and constructs a three dimensional model of the target positions. We used approximately 100-230 targets distributed over the primary mirror and about 50 exposures to reconstruct the KOSMA telescope surface. The measurement accuracy is approximately 10 μm (RMS). The measured mean deviation between the initial surface setup and the ideal parabola was confirmed independently by planetary observations at 345, 492, 660, and 810 GHz. The frequency dependence of the beam efficiencies, derived from scans on Jupiter, follows the Ruze-formula for an initial surface error of 35±5 microns. This error was reduced by subsequent adjustments using surface maps of the deviations derived from the photogrammetric data sets. New observations of Jupiter to confirm this improvement are pending.
We describe the receiver concept for KOSMA's planned second generation SOFIA instrument STAR (SOFIA Terahertz Array Receiver). The receiver will contain a 4 X 4 element heterodyne mixer array for the frequency range from 1.7 to 1.9 THz (158 to 176 microns). Its main scientific goal is large scale mapping of the 158 micron fine structure transition of singly ionized carbon. The design frequency range covers this line out to moderate red shifts and also allows to observe a variety of other spectral lines.
We present a new type of phase grating, the Fourier grating, to be used as local oscillator beam multiplexer in heterodyne receivers. The device has been developed for the SOFIA Terahertz Array Receiver (STAR). In contrast to the binary phase gratings (Dammann gratings), which are being used in many array receivers, our gratings have a smooth surface structure without any sharp edges.
A consortium of German research laboratories has been established for the development of a modular dual-channel heterodyne instrument (GREAT: German Receiver for Astronomy at Terahertz Frequencies) for high-resolution spectroscopy aboard SOFIA. The receiver is scheduled to be available in time for SOFIA's very first astronomical mission in late 2002. The first-flight version will offer opportunities for parallel observations in two frequency bands. We will have a choice of backends, including an acousto-optic array (4 X 1 GHz) and a high-resolution chirp transform spectrometer.
We describe frontend concepts for the future heterodyne array instruments of the KOSMA 3-m telescope and for SOFIA. For KOSMA we are currently developing a dual frequency (400 - 500, 800 - 900 GHz) SIS mixer array of four elements per frequency band. For SOFIA, we are planning an up to 4 X 4 element array for 1.6 - 2.0 THz using superconducting hot-electron bolometers. The small number of pixels allows us to keep the optics relatively compact. For the same reason, a single sideband filter is not included. The local oscillator power will be distributed using Dammann gratings. Motivated by the excellent beam characteristics of waveguide horns we are planning to extend the range of our waveguide mixers to 2 THz. The mixers are based on the wideband tunerless mixers that have been successfully used in single element telescope receivers at KOSMA. The mixers will be standard building blocks mounted at the back of waveguide horns integrated into the optical setup. Local oscillators for 400 - 900 GHz are solid state sources, for the Terahertz array we are developing several alternative local oscillator concepts.
The Kolner Observatorium fur Submillimeter-Astronomie (KOSMA) has recently been equipped with a new 3 m submm telescope. The new telescope dish has a CFRP backstructure and aluminum panels with a mean surface accuracy of the individual panels of well below 10 micrometer. The 18 panels of the primary reflector have been adjusted to a surface rms of at present about 30 micrometer with the help of a holographic phase retrieval algorithm developed for and previously used at the JCMT. The present main beam efficiency derived from observations of Jupiter and Saturn is approximately 45% at 660 GHz. The new telescope features a chopping secondary and 2 Nasmyth ports. The excellent atmospheric transmission during winter time at the telescope site, Gornergrat near Zermatt, Switzerland, allow us flexible operation up to the highest atmospheric submm windows. We present the current status of the new telescope, in particular with regard to its surface alignment, and first astronomical results at 660 and 690 GHz.
A new versatile system for the measurement of time-resolved fluorescence emission spectra of biomolecules is presented. Frequency doubling and tripling of a Ti:Sapphire laser allows excitation over a wide wavelength range. The influence of increasing the spectral resolution on the time resolution has been investigated. System performance can be optimized for best resolution in the spectral or time domain, respectively. System performance can be optimized for best resolution in the spectral or time domain, respectively. The currently achieved temporal resolution is 6 psec, and the best spectral resolution is 3 nm. Long fluorescence decays can be resolved with optimal time resolution by way of taking into account the flyback of the streak camera. With the system described, the core complex ((alpha) (beta) )3APCLC8.9 of the phycobilisome from the photosynthetic cyanobacteria Mastigocladus laminosus has been analyzed. Lifetime analysis clearly demonstrated the influence of the linker polypeptide on the phycobiliprotein complex and the identity of native and reconstituted complex.
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