PLANCK is a project of the European Space Agency to be launched in February 2007 by an ArianeV rocket with the Herschel Space Observatory . It is designed for imaging the temperature and polarization anisotropies of the millimetre and submillimetre radiation over the whole sky with unprecedented sensitivity, accuracy and angular resolution using 9 frequency channels ranging between 25 and 1000 GHz. The main source at these frequencies is the Cosmic Microwave Background (CMB), i.e. the radiation emitted by the early universe when, about 300000 years old, ionised hydrogen recombined and became transparent from the visible to radio frequencies of the electromagnetic spectrum. The main goal of the PLANCK mission is to retrieve the main cosmological parameters of the Universe with accuracies of a few percent from the observation and analysis of random small contrast (10–4) features in the CMB. The angular power spectrum of the CMB anisotropies is a function of the fundamental cosmological parameters. A proper measurement of all the angular frequencies of the CMB is essential for an accurate interpretation of the data. In consequence the optical performances of Planck will directly impact the ability of retrieving theses parameters. Recent results of the Willkinson Microwave Anisotropy Probe (WMAP) mission show that polarization information of CMB radiation is very challenging, and that the precise measurement of the CMB could completely change the knowledge we have on our universe ([1]). The focal plane assembly (FPA) of the PLANCK telescope is composed of two instruments. The High Frequency Instrument (HFI) of PLANCK is the most sensitive CMB experiment ever planned ([2]). Together with the Low Frequency Instrument (LFI), this will make a unique tool to measure the full sky and to separate various components of its spectrum. This paper describes the main performances of the HFI beams and compares results obtained with 2 different softwares: GRASP8 [3] and an home-made software developed at the Ireland National University of Maynooth [4]. Specials attention will be paid to polarized beams (100, 143, 217, 353 GHz) and multimoded channels (545 and 857 GHz).
A multimode horn differs from a single mode horn in that it has a larger sized waveguide feeding it. Multimode horns can therefore be utilized as high efficiency feeds for bolometric detectors, providing increased throughput and sensitivity over single mode feeds, while also ensuring good control of the beam pattern characteristics. Although a cavity mounted bolometer can be modelled as a perfect black body radiator (using reciprocity in order to calculate beam patterns), nevertheless, this is an approximation. In this paper we present how this approach can be improved to actually include the cavity coupled bolometer, now modelled as a thin absorbing film. Generally, this is a big challenge for finite element software, in that the structures are typically electrically large. However, the radiation pattern of multimode horns can be more efficiently simulated using mode matching, typically with smooth-walled waveguide modes as the basis and computing an overall scattering matrix for the horn-waveguide-cavity system. Another issue on the optical efficiency of the detectors is the presence of any free space gaps, through which power can escape. This is best dealt with treating the system as an absorber. Appropriate reflection and transmission matrices can be determined for the cavity using the natural eigenfields of the bolometer cavity system. We discuss how the approach can be applied to proposed terahertz systems, and also present results on how the approach was applied to improve beam pattern predictions on the sky for the multi-mode HFI 857GHz channel on Planck.
Multimode horn antennas can be utilized as high efficiency feeds for bolometric detectors, providing increased
throughput and sensitivity over single mode feeds, while also ensuring good control of beam pattern characteristics.
Multimode horns were employed in the highest frequency channels of the European Space Agency Planck Telescope,
and have been proposed for future terahertz instrumentation, such as SAFARI for SPICA. The radiation pattern of a
multimode horn is affected by the details of the coupling of the higher order waveguide modes to the bolometer making
the modeling more complicated than in the case of a single mode system. A typical cavity coupled bolometer system can
be most efficiently simulated using mode matching, typically with smooth walled waveguide modes as the basis and
computing an overall scattering matrix for the horn-waveguide-cavity system that includes the power absorption by the
absorber. In this paper we present how to include a cavity coupled bolometer, modelled as a thin absorbing film with
particular interest in investigating the cavity configuration for optimizing power absorption. As an example, the possible
improvements from offsetting the axis of a cylindrically symmetric absorbing cavity from that of a circular waveguide
feeding it (thus trapping more power in the cavity) are discussed. Another issue is the effect on the optical efficiency of
the detectors of the presence of any gaps, through which power can escape. To model these effects required that existing
in-house mode matching software, which calculates the scattering matrices for axially symmetric waveguide structures,
be extended to be able to handle offset junctions and free space gaps. As part of this process the complete software code
'PySCATTER' was developed in Python. The approach can be applied to proposed terahertz systems, such as SPICASAFARI.
KEYWORDS: Cryogenics, Control systems, Bolometers, Temperature metrology, Satellites, Space telescopes, Sensors, Thermography, Electronic filtering, Anisotropy
The core of the High Frequency Instrument (HFI) on-board the Planck satellite consists of 52 bolometric
detectors cooled at 0.1 Kelvin. In order to achieve such a low temperature, the HFI cryogenic architecture
consists in several stages cooled using different active coolers. These generate weak thermal fluctuations
on the HFI thermal stages. Without a dedicated thermal control system these fluctuations could produce
unwanted systematic effects, altering the scientific data. The HFI thermal architecture allows to minimise
these systematic effects, thanks to passive and active control systems described in this paper. The
passive and active systems are used to damp the high and low frequency fluctuations respectively. The
last results regarding the tests of the HFI passive and active thermal control systems are presented here.
The thermal transfer functions measurement between active coolers and HFI cryogenic stages will be
presented first. Then the stability of the temperatures obtained on the various cryogenic stages with PID
regulations systems will be checked through analysis of their power spectrum density.
We present the latest results of our fast physical optics simulations of the ESA PLANCK HFI beams. The main beams of both polarized and non-polarized channels have been computed with account of broad frequency bands for the final design and positions of the HFI horns. Gaussian fitting parameters of the broadband beams have been presented. Beam polarization characteristics and horn defocusing effects have been studied.
The future ESA space mission Planck Surveyor mission will measure the Cosmic Microwave Background temperature and polarisation anisotropies in a frequency domain comprised between 30GHz and 1THz. On board two instruments, LFI based on HEMT technology and HFI using bolometric detectors. We present the optical solutions adopted for this mission, in particular the focal plane design of HFI, concept which has been applied already to other instruments such as the balloon borne experiment Archeops.
Michel Piat, Jean-Michel Lamarre, Julien Meissonnier, Jean-Pierre Torre, Philippe Camus, Alain Benoit, Jean-Pierre Crussaire, Peter Ade, James Bock, Andrew Lange, Ravinder Bhatia, Bruno Maffei, Jean Puget, Rashmi Sudiwala
KEYWORDS: Sensors, Bolometers, Optical filters, Connectors, Control systems, Cryogenics, Signal to noise ratio, Signal detection, Temperature metrology, Spatial resolution
The Planck-High Frequency Instrument (HFI) will use 48 bolometers cooled to 100mK by a dilution cooler to map the Cosmic Microwave Background (CMB) with a sensitivity of ΔT/T~2.10-6 and an angular resolution of 5 minutes of arc. This instrument will therefore be about 1000 times more sensitive than the COBE-DMR experiment. This contribution will focus mainly on the thermal architecture of this instrument and its consequences on the fundamental and instrumental fluctuations of the photon flux produced on the detectors by the instrument itself. In a first step, we will demonstrate that the thermal and optical design of the HFI allow to reach the ultimate sensitivity set by photon noise of the CMB at millimeter wavelength. Nevertheless, to reach such high sensitivity, the thermal behavior of each cryogenic stages should also be controlled in order to damp thermal fluctuations that can be taken as astrophysical signal. The requirement in thermal fluctuation on each stage has been defined in the frequency domain to degrade the overall sensitivity by less than 5%. This leads to unprecedented stability specifications that should be achieved down to 16mHz. We will present the design of the HFI thermal architecture, based on active and passive damping, and show how its performances were improved thanks to thermal simulations.
The High Frequency Instrument of the Planck satellite is dedicated to the measurement of the anisotropy of the Cosmic Microwave Background (CMB). Its main goal is to map the CMB with a sensitivity of ΔT/T=2.10-6 and an angular resolution of 5 arcmin in order to constrain cosmological parameters. Planck is a project of the European Space Agency based on a wide international collaboration, including United States and Canadian laboratories. The architecture of the satellite is driven by the thermal requirements resulting from the search for low photon noise. Especially, the passively cooled telescope should be at less than 50K, while a cascade of cryo-coolers will ensure the cooling of the HFI bolometers down to 0.1K. This last temperature will be produced by a gravity insensitive 3He/4He dilution cooler. This will be achieved at the L2 Lagrangian point of the Sun-Earth system. The whole sky will be observed two times in the 14 months mission with a scanning strategy based on a 1RPM rotation of the satellite. In addition to the cosmological parameters that can be derived from the CMB maps, Planck will deliver nine high sensitivity submillimeter maps of the whole sky that will constitute unique data available to the whole astronomical community.
As one of the four cornerstones of its scientific program Horizon 2000, the European Space Agency is studying a far-infrared and submillimeter space telescope (FIRST) that will open to astronomical observations the 100-μm to 1-mm spectral region, virtually unexplored with a subarcminute angular resolution. The 3- to 4-m-diam telescope will be diffraction limited at λ = 300 μm or less. The expected lifetime of this system in orbit is five years or more. The model payload is composed of two focal instruments. The multifrequency heterodyne spectrometer will give a very high spectral resolution in the 400- to 630-μm wavelength range and around 300 μm. The far-infrared receiver (FIR) will be an imaging spectrometer covering the 100- to 400-μm range with spectral resolutions ranging from 3 to 104 obtained with a set of Fabry-Pérot interferometers and filters. Arrays of photoconductors and bolometers are cooled at 1.5 and 0.15 K, respectively, by an open-cycle 3He/4He dilution + Joule-Thomson expansion system developed to operate at zero gravity.
As one of the four Cornerstones of its scientific program 'Horizon 2000', the European Space Agency ESA is studying a Far Infrared and Submillimeter Space Telescope (FIRST). FIRST will open to astronomical observations the 100 micrometers to 1mm spectral region, virtually unexplored with a sub-arcmin angular resolution. The 3 - 4 m diameter telescope will be diffraction limited at (lambda) equals 300 micrometers or less. The fabrication of a single dish of composite materials is considered as the baseline. The expected life time of this system in orbit is five years or more. The Model Payload, defined in order to allow a realistic system study and an evaluation of the possible scientific return, is composed of two focal instruments. The Multifrequency heterodyne spectrometer will give a very high spectral resolution in the 400 to 630 micrometers wavelength range and around 300 micrometers . The Far Infrared Receiver will be an imaging spectrometer covering the 100 - 400 micrometers range with spectral resolutions ranging from 5 to 104 obtained with a set of Fabry-Perot interferometers and filters. FIRST is expected to give unprecedented information on the physics, chemistry and dynamics of interstellar, circumstellar, planetary and cometary gas and dust. Extragalactic physics and deep surveys of cosmological interest will also benefit from this project.
The setup and results of the experiment AROME to measure the 3.3 micron feature in diffuse galactic emission attributed to PAHs using stratospheric balloons are described. The main balloon project, Pronaus, consists of a 2 m telescope with two focal plane instruments: a submillimeter photometer dedicated to the measurement of very faint sources and a high resolution heterodyne spectrometer that measures water vapor and other species not observable from the ground.
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