The Comet Interceptor mission has been adopted by the European Space Agency (ESA) Science Programme Committee in June 2022 as the first ”F” mission in the Science Programme. The aim of the mission is to increase the knowledge on comets and on the Solar System formation by encountering and exploring a Dynamically New Comet (DNC) or an Interstellar Object (ISO) originating at another star. EnVisS (Entire Visible Sky) is an all-sky camera designed to fly on Comet Interceptor and whose scientific task is to study the radiance and the polarization properties of the comet coma in the visible spectrum. The camera is composed of an optical head, a filter strip assembly and a detector. The Institute for Photonics and Nanotechnologies (CNR-IFN) of Padova and Leonardo SpA (Campi BisenzioFlorence) are in charge of the design of the filter package, which currently consists of three filter strips glued side by side. The central strip is a high transmission broadband (BB) filter in the range 550–800 nm with no polarization properties, while the side ones are linear polarization filters with the same transmission bandpass as the BB and with polarization axis at 45° from one another. In the CNR-IFN laboratories different types of polarizers have been tested to establish which one has the most fitting properties for EnVisS’s purposes. The analyzed filters are Moxtek Visible Light Polarizer RCV8N2EC and Ultra BroadBand Polarizer UBB01A, and Polarcor Wide Band Polarizer. For each type of polarizing filter, both transmissivity and reflectivity have been measured and compared both with those of the other filters as well as data provided by the manufacturer. Overall, measurements of the filters’ transmissivity and reflectivity agree with those provided by the supplier and mostly fit EnVisS’ purposes. Thanks to its optimal performance and the fused silica substrate, Moxtek UBB01A is considered the best candidate filter for the instrument between the polarizers that have been characterized.
Rosetta is one of the cornerstone missions of the European Space Agency for having a rendezvous with the comet 67P/Churyumov-Gerasimenko in 2014. The imaging instrument on board the satellite is OSIRIS (Optical, Spectroscopic and Infrared Remote Imaging System), a cooperation among several European institutes, which consists of two cameras: a Narrow (NAC) and a Wide Angle Camera (WAC).
The WAC optical design is an innovative one: it adopts an all reflecting, unvignetted and unobstructed two mirror configuration which allows to cover a 12° × 12° field of view with an F/5.6 aperture and gives a nominal contrast ratio of about 10–4.
The flight model of this camera has been successfully integrated and tested in our laboratories, and finally has been integrated on the satellite which is now waiting to be launched in February 2004.
In this paper we are going to describe the optical characteristics of the camera, and to summarize the results so far obtained with the preliminary calibration data. The analysis of the optical performance of this model shows a good agreement between theoretical performance and experimental results.
JANUS (Jovis, Amorum ac Natorum Undique Scrutator) is the visible camera selected for the ESA JUICE mission to the Jupiter system. Resources constraints, S/C characteristics, mission design, environment and the great variability of observing conditions for several targets put stringent constraints on instrument architecture. In addition to the usual requirements for a planetary mission, the problem of mass and power consumption is particularly stringent due to the long-lasting cruising and operations at large distance from the Sun. JANUS design shall cope with a wide range of targets, from Jupiter atmosphere, to solid satellite surfaces, exosphere, rings, and lightning, all to be observed in several color and narrow-band filters. All targets shall be tracked during the mission and in some specific cases the DTM will be derived from stereo imaging. Mission design allows a quite long time range for observations in Jupiter system, with orbits around Jupiter and multiple fly-bys of satellites for 2.5 years, followed by about 6 months in orbit around Ganymede, at surface distances variable from 104 to few hundreds km. Our concept was based on a single optical channel, which was fine-tuned to cover all scientific objectives based on low to high-resolution imaging. A catoptric telescope with excellent optical quality is coupled with a rectangular detector, avoiding any scanning mechanism. In this paper the present JANUS design and its foreseen scientific capabilities are discussed.
We have designed Aqueye+, an instrument for the Copernicus 182 cm Asiago Telescope, with two channels, one devoted to ultrafast photometry based on four single photon avalanche photodiodes, the second dedicated to stellar coronagraphy based on innovative optical vortex coronagraph system. The OVC requires a very good image quality, therefore an adaptive optic system AO was designed for the instrument. The peculiarity of this AO system is that there is no wavefront sensors, but the feedback for the deformable mirror is instead given by the photometric channel of Aqueye+.
In recent years, we developed two very high speed single photon photometers, Aqueye and Iqueye, as prototypes for “quantum” photometers for the Extremely Large Telescopes of the next decade. These instruments, based on single photon avalanche photodiodes and a 4-fold split-pupil concept, have been successfully used to obtain data of the highest quality on optical pulsars. Subsequently, we performed an attempt to utilize the Orbital Angular Momentum and associated Optical Vorticity to achieve high performance stellar coronagraphy. Presently, we are making a synergic effort in building Aqueye Plus, a new instrument for the 1.8 m telescope of the Asiago - Cima Ekar Observatory, which combines both functions, namely high speed simultaneous multicolor photon counting photometry and stellar coronagraphy. The innovative capability of Aqueye Plus is to take advantage of the two parallel outputs (NIM and TTL) of the four high time accuracy photon counting sensors. The NIM output preserves the best timing capability, while the TTL output drives a deformable 32-element mirror in a sort of quadrant detector to correct for defocus and tip/tilt aberrations of the stellar image on the phase mask discontinuity. This paper describes the Aqueye Plus instrument main characteristics and its foreseen performance.
Iqueye is a single photon counting very high speed photometer built for the ESO 3.5m New Technology Telescope
(NTT) in La Silla (Chile) as prototype of a 'quantum' photometer for the 42m European Extremely Large Telescope (E-ELT).
The optics of Iqueye splits the telescope pupil into four portions, each feeding a Single Photon Avalanche Diode
(SPAD) operated in Geiger mode. The SPADs sensitive area has a diameter of 100 μm, with a quantum efficiency better
than 55% at 500 nm, and a dark count less than 50 Hz. The quenching circuit and temperature control are integrated in
each module. A time-to-digital converter (TDC) board, controlled by a rubidium oscillator plus a GPS receiver, time tags
the pulses from the 4 channels. The individual times are stored in a 2 TeraByte memory. Iqueye can run continuously for
hours, handling count rates up to 8 MHz, with a final absolute accuracy of each time tag better that 0.5 ns. A first very
successful run was performed in Jan 2009; both very faint and very bright stars were observed, demonstrating the high
photometric quality of the instrument. The first run allowed also to identify some opto-mechanical improvements, which
have been implemented for a second run performed in Dec 2009. The present paper will describe the first version, the
improvements implemented in the second one, and some of the obtained astronomical results.
Almost all astronomical instruments detect and analyze the first order spatial and/or temporal coherence properties
of the photon stream coming from celestial sources. Additional information might be hidden in the second
and higher order coherence terms, as shown long ago by Hanbury-Brown and Twiss with the Narrabri Intensity
Interferometer. The future Extremely Large Telescopes and in particular the 42 m telescope of the European
Southern Observatory (ESO) could provide the high photon flux needed to extract this additional information.
To put these expectations (which we had already developed at the conceptual level in the QuantEYE study for the
100 m OverWhelmingly Large Telescope to experimental test in the real astronomical environment, we realized
a small prototype (Aqueye) for the Asiago 182 cm telescope. This instrument is the fastest photon counting
photometer ever built. It has 4 parallel channels operating simultaneously, feeding 4 Single Photon-Avalanche
Diodes (SPADs), with the ability to push the time tagging capabilities below the nano-second region for hours
of continuous operation. Aqueye has been extensively used to acquire photons from a variety of variable stars,
in particular from the pulsar in the Crab Nebula. Following this successful realization, a larger version, named
Iqueye, has been built for the 3.5 m New Technology Telescope (NTT) of ESO. Iqueye follows the same optical
solution of dividing the telescope pupil in 4 sub-pupils, imaged on new generation SPADs having useful diameters
of 100 micrometers, time jitter less than 50 picoseconds and dark-count noise less than 50 counts/second. The
spectral efficiency of the system peaks in the visible region of the spectrum. Iqueye operated very successfully at
the NTT in January 2009. The present paper describes the main features of the two photometers and present
some of the astronomical results already obtained.
The WAC is a telescope developed by University of Padova for the OSIRIS experiment, mainly composed by two instruments, Narrow Angle Camera and Wide Angle Camera, and the related electronics. The payload will fly on board of the Rosetta ESA scientific mission, that will be flown to encounter Comet Wirtanen after about 10 years of flight in 2013. WAC main scientific objectives are to follow structure evolution in the coma and monitor their dynamics. To fulfill scientific requirements, the optical characteristics of the WAC telescope may be summarized as follows: wide field of view of 12° X 12°, focal length of 140 mm, operate in the wave-length range 240-1000nm after 10 years in space, Encircled Energy greater than 70% over the entire FoV, contrast ratio of 10-4 to detect coma activities against a bright nucleus, minimum exposure time of 10 msec with a repeatability better than 1/500, scattered light rejection for sources inside and outside FoV. This paper deals with the design optimization of critical parts and acceptance test campaign performed to validate the thermo-structural behavior of the WAC. The functional and performance tests carried out at experiment and system level demonstrated the overall capability of the telescope to satisfy the system and scientific requirements.
A new concept of electromechanical shutter has been designed and qualified for the OSIRIS imaging system to fly onboard the Rosetta Mission, whose main scientific goal are the randez-vous and the study of the Comet Wirtanen. The shutter, is composed by two blades, driven by dedicated four-bar linkages, that are moved independently by two torque motors each mounted on the same shaft of an high resolution optical encoder. A dedicate fail safe mechanism is also integrated in order to make the shutter single point failure proof. The mechanism has been designed in order to fulfil high reliability with high performance. Reliability has been verified by life testing over 100000 cycles (factor 2 on expected operative cycles). Performance verified by calibration show that the minimum exposure time with a uniformity of 1/500 is 10 ms over a large sensitive area (about 30x30 mm). The exposure time can vary from 10ms to 5s. Scope of this paper is to present the mechanism and to demonstrate that it accomplishes the sciences and interfaces requirements.
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