The search for extrasolar planets is fundamental for expanding our understanding of the Universe and investigating the likelihood that other worlds might harbour life. Among the several approaches employed for this purpose, the astrometric method offers significant advantages, as it provides an accurate estimate of the mass of the planet under consideration, which is not required to be necessarily aligned with the line of sight of the observer as for the transit or radial velocity techniques. This work aims at analysing the pointing manoeuvres required by a future spacecraft carrying an optical instrument such as RAFTER (Ring Astrometric Field Telescope for Exoplanets and Relativity) to properly fulfil the objectives of an exoplanet astrometric search mission. RAFTER is an annular field telescope conceived and proposed with the goal of achieving consistent optical response over a wide field of view, which exhibits a compact and scalable design and enforces circular symmetry for each optical element. A mathematical model describing the dynamics of the system and the evaluation of an appropriate optimal control strategy will be presented. At the end, the selection of proper actuators will also be discussed.
RAFTER (Ring Astrometric Field Telescope for Exo-planets and Relativity) is a TMA telescope concept aimed at astrometric missions, and providing a wide FOV and high optical response uniformity over an annular region around the optical axis. This paper describes and analyzes the process of miniaturization and implementation of this idea into a Cubesat for technology demonstration purposes, and to evaluate its feasibility by analysing the performance and challenging aspects of different designs, calculating their mechanical tolerances and thermal sensitivity. We outline the critical aspects of the payload that can be tested and optimized in the framework of a dedicated CubeSat mission, in order to demonstrate the enabling technological contributors crucial to the development of a future larger scale mission.
The CEntral (field) Three-mirror Anastigmat (CETA) telescope is designed on the specifications of the proposed Theia mission, aiming at high precision differential astrometry over a large field, for exo-planetary system characterization and dark matter /dark energy search through the dynamics of star clusters. Usually, Three Mirror Anastigmat designs are either off-axis in terms of field, or decentered in terms of pupil. We propose a family of solutions using fully centred optics and a large on-axis field, at the expense of a non negligible central obscuration. We analyse in particular a 1 m class compact telescope, with 15 m effective focal length, i.e. suited to small pixel (4-6 $micro$m) CMOS detectors operating in the visible and near IR. Due to the underlying symmetry, the resulting optical response is quite good over a 14 arcmin radius field, and it is of special interest to astrometry applications. Also, manufacturing, alignment and calibration can be expected to benefit significantly; some basic aspects are preliminarily considered.
AVU-GSR is a pipeline designed to solve the problem of the Global Astrometric Sphere Reconstruction of the Gaia ESA mission whose goal is to replicate the AGIS baseline process. The pipeline produces an independent solution using a different astrometric model and different algorithms for the solution of this problem, thus providing an effective way to assess the reliability of the solution, as it is called by the absolute character of the satellite measurements. It recently passed its qualification phase with real data, successfully solving the sphere reconstruction problem at the sub-mas level with Cycle 2 data. We review the context, the current status of the pipeline, and the development needed to cope with the goal of contributing to the forthcoming Gaia Data Release four.
Small and compact optics are a key element for future small missions, in particular cubesat. We started the miniaturization concept study in order to adapt the idea to the small cubesat envelope; lab tests on representative units are in progress, as part of a INAF Mini Grant awarded in 2022. In particular, we aimed at simplification of the initial design, in order to cope with costs and available space. Preliminary results are shown in this paper. We study standard reflective coatings and propose an innovative approach for future development of the design. We characterize the telescope and put it into the experimental perspective of a ground based instrument, trying to identify and solve the main issues towards the subsequent spatialization.
The opportunity given with cubesats opens new scenarios in the field of astronomy, due to (among the other advantages) the relatively low budget and the replicability features of such devices. This push the research efforts towards the miniaturization and compactness of the traditional optical devices and layouts. The possibility of having small telescopes in operation without the atmospheric disturbances allows newer possibilities for astronomical targets. In this paper, we will describe the coupling of newer astrometric techniques with specific optical layout in order to reach the maximum precision and reliability. We propose and describe a simple acquisition system with a multiple field of view (i.e. 4), to verify and prove the robustness of the astrometric techniques. In addition we study the use of a disperser element, in order to have fast and multiple spectra of the selected target.
The concept of a 3 lines of sight telescope for space astrometry is evaluated in terms of implementation feasibility and some science applications. The beam combination by pupil splitting exploits the Hipparcos concept, extending it to true large bidimensional angle. The PSF symmetry provides equivalent astrometric performance and immediate field identification on the common detector. Operation aspects are investigated in terms of field identification and observing strategy, in particular pointing constraints and sky density of reference bright stars. The approach, based on flat mirrors mounted on a pyramidal structure, provides a simple geometric framework, with immediate mechanical materialization and clear interface to metrology. The geometric arrangements considered place the lines of sight either along the (x, y, z) Cartesian axes, or in a planar layout for a Gaia-like astrometric mission. The application to a single head, multiple boresight star tracker is also outlined.
Since the publication of the HIPPARCOS catalog in 1997, and with its successor Gaia in operational phase since 2013 having already published 3 data releases, global astrometry has earned itself a prominent role in the field of astrophysics. Both missions rest on the well-established concepts of one-dimensional (or nearly one-dimensional) observations performed by a telescope that is continuously scanning the sky following a predefined scanning law. Moreover, Gaia heavily relies also on the concept of self-calibrating instrument. In this work we explore the possibility of exploiting two-dimensional observations performed by a pointed mission, discussing the feasibility of this concept, and its possible advantages.
High-precision astrometry well beyond the capacities of Gaia will provide a unique way to achieve astrophysical breakthroughs, in particular on the nature of dark matter, and a complete survey of nearby habitable exoplanets. In this contribution, we present the scientific cases that require a flexibly-pointing instrument capable of high astrometric accuracy and we review the best mission profiles that can achieve such observations with the current space technology as well as within the boundary conditions defined by space agencies. We also describe the way the differential astrometric measurement is made using reference stars within the field. We show that the ultimate accuracy can be met without drastic constrains on the telescope stability.
High precision astrometry aims at source position determination to a very small fraction of the diffraction image size, in high SNR regime. One of the key limitations to such goal is the optical response variation of the telescope over a sizeable FOV, required to ensure that bright reference objects to any selected target. The issue translates into severe calibration constraints, and/or the need for complex telescope and focal plane metrology. We propose an innovative system approach derived from the established TMA telescope concept, extended to achieve high filling factor of an annular field of view around the optical axis of the telescope. The proposed design is a very compact, 1 m class telescope compatible with modern CCD and CMOS detectors (EFL = 15 m). We describe the concept implementation guidelines and the optical performance of the current optical design. The diffraction limited FOV exceeds 1.25 square degrees, and the detector occupies the best 0.25 square degree with 66 devices.
The Astrometric Gravitation Probe mission is a modern version of the 1919 Dyson-Eddington-Davidson experiment, based on a space-borne telescope with a permanent built-in eclipse, provided by a coronagraphic system. The expected improvement on experimental bounds to General Relativity and competing gravitation theories is by at least two orders of magnitude. The measurement principle is reviewed, in particular the principle of Fizeau-like combination of a set of individual inverted coronagraphs simultaneously feeding a common high resolution telescope. Also, the payload has a dual field of view property, in order to support simultaneous observations of stellar fields either very close, or far away, from the Sun, i.e. fields affected by either high or low light bending. We discuss a set of solutions introduced in the optical design to improve on technical feasibility and robustness of the optical performance against perturbations, in particular induced by manufacturing and alignment tolerances, and launch stresses.
Astrometric Science and Technology Roadmap for Astrophysics (ASTRA) is a bilateral cooperation between China and Italy with the goal of consolidating astrometric measurement concepts and technologies. In particular, the objectives include critical analysis of the Gaia methodology and performance, as well as principle demonstration experiments aimed at future innovative astrometric applications requiring high precision over large angular separations (one to 180 degrees). Such measurement technologies will be the building blocks for future instrumentation focused on the "great questions" of modern cosmology, like General Relativity validity (including Dark Matter and Dark Energy behavior), formation and evolution of structure like proto-galaxies, and planetary systems formation in bio compatibles environments. We describe three principle demonstration tests designed to address some of the potential showstoppers for high astrometric precision experiments. The three tests are focused on the key concepts of multiple fields telescopes, astrometric metrology and very fine sub-pixel precision (goal: < 1/2000 pixel) in white light.
This paper, “Astrometry at micro-arcsec resolution: optical design aspects and technology issues," was presented as part of International Conference on Space Optics—ICSO 1997, held in Toulouse, France.
This paper describes the current opto-mechanical design of AGP, a mission designed for astrometric verification of General Relativity (GR) and competing gravitation theories by means of precise determination of light deflection on field stars, and of orbital parameters of selected Solar System objects. The optical concept includes a planar rear-view mirror for simultaneous imaging on the CCD mosaic detector of fields of view also from the direction opposite to the Sun, affected by negligible deflection, for the sake of real time calibration. The precision of astrometric measurements on individual stars will be of order of 1 mas, over two fields separated by few degrees around the Sun and observed simultaneously. We describe the optical design characteristics, with particular reference to manufacturing and tolerancing aspects, evidencing the preservation of very good imaging performance over the range of expected operating conditions.
The main goal of the Astrometric Gravitation Probe mission is the verification of General Relativity and competing gravitation theories by precise astrometric determination of light deflection, and of orbital parameters of selected Solar System objects. The key element is the coherent combination of a set of 92 circular entrance apertures, each feeding an elementary inverted occulter similar to the one developed for Solar Orbiter/METIS.1 This provides coronagraphic functions over a relevant field of view, in which all stars are observed for astrometric purposes with the full resolution of a 1 m diameter telescope. The telescope primary mirror acts as a beam combiner, feeding the 92 pupils, through the internal optics, toward a single focal plane. The primary mirror is characterized by 92 output apertures, sized according to the entrance pupil and telescope geometry, in order to dump the solar disk light beyond the instrument. The astronomical objects are much fainter than the solar disk, which is angularly close to the inner field of view of the telescope. The stray light as generated by the diffraction of the solar disk at the edges of the 92 apertures defines the limiting magnitude of observable stars. In particular, the stray light due to the diffraction from the pupil apertures is scattered by the telescope optics and follows the same optical path of the astronomical objects; it is a contribution that cannot be eliminated and must therefore be carefully evaluated. This paper describes the preliminary evaluation of this stray light contribution.
AVU/BAM is the Gaia software for the Astrometric Verification Unit (AVU) devoted to the monitoring of the Basic Angle Monitoring (BAM), one of the metrology instruments onboard of the Gaia Payload. AVU/BAM is integrated and operative at the Data Processing Center of Turin (DPCT), since the beginning of the Gaia Mission. The DPCT infrastructure performs the ingestion of pre-elaborated data coming from the satellite and it's responsible of running the code of different Verification Packages. The new structure of the pipeline consists of three phases: the first is a pre-analysis in which a preliminary study data is performed, with the calculation of quantities needed to the analysis; the second one processes the interferograms coming from the instrument; the third phase analyzes the data obtained from the previous processing. Also it has been changed part of the long-term analysis and was added a phase of calibration of the data obtained from the processing.
The Gaia payload is a highly sophisticated system and much of its instrumental behaviour is tested to proper accuracy during the Commissioning and Early Operations phase. The Astrometric Instrument Modelling (AIM) belongs to the Core Processing, or CU3, software systems devoted to astrometric data processing, instrumental monitoring and calibration.; it was developed in the context of a special unit of CU3 devoted to Astrometric Verification. While waiting for nominal scientific operations, we present the challenges phased in the Gaia initial data treatment and real-time instrument health monitoring and diagnostic, during the non-standard conditions of the Commissioning phase. We describe the dedicated diagnostic and correction procedures implemented for Commissioning and Early Operations and we show some results obtain during still on-going Commissioning activities.
The Gravitation Astrometric Measurement Experiment (GAME) is a space mission for Fundamental Physics tests in the
Solar system, through coronagraphy and Fizeau interferometry for differential astrometry. The precision goal on the γ and β General Relativity PPN parameters is respectively in the 10-8 and 10-6 range. The design is focused on systematic
error control through multiple field simultaneous observation and calibration. The GAME instrument concept is based on
multiple aperture Fizeau interferometry, observing simultaneously regions close to the Solar limb (requiring the adoption
of coronagraphic techniques), and others away from the Sun. The diluted optics approach is selected to achieve an
efficient rejection of the scattered solar radiation, while retaining an acceptable angular resolution on the science targets.
The Interferometric Stratospheric Astrometry for Solar system (ISAS) project is a GAME technology demonstrator,
providing milli-arcsec level astrometry on the main planets of the Solar System. The ISAS technical goal is the
validation of basic concepts for GAME, in particular integration of Fizeau interferometry and coronagraphic techniques
by means of pierced silicon carbide (SiC) mirrors, intermediate angle dual field astrometry, smart focal plane
management for increased dynamic range and pointing correction. The ISAS instrument concept is a dual field, multiple
aperture Fizeau interferometer, using coronagraphy for observation of Solar System planets also close to the Sun. A
prototype SiC multi-aperture mirror was manufactured by Boostec (F), and has been investigated by thermo-elastic
analysis to define the applicability to both GAME and ISAS designs. We describe the development status of both
stratospheric and space options, as well as the current extrapolation of the SiC prototype characteristics to the GAME
and ISAS optical configurations.
KEYWORDS: Telescopes, Fringe analysis, Data processing, Space operations, Calibration, Signal processing, Satellites, Interferometry, Metrology, Space telescopes
The goal of the Gaia mission is to achieve micro-arcsecond astrometry, making Gaia the most important astro- metric space mission of the 21st century. To achieve this performance several innovative technological solutions have been realized as part of the satellite's scientific payload. A critical component of the Gaia scientific pay- load is the Basic Angle Monitoring device (BAM), an interferometric metrology instrument with the task of monitoring, to some picometers, the variation of the Basic Angle between Gaia's two telescopes. In this paper we provide an overview of the AVU/BAM software, running at the Italian Data Processing Center (DPCT), to analyze the BAM data and to recover the basic angle variations at the micro-arcosecond level. Outputs based on preliminary data from Gaia's Commissioning phase are shown as an example.
This paper describes a concept study for a simple and cost effective approach to upgrade of existing infrastructures. A conventional monolithic telescope can be endowed with a set of identical small telescopes combined coherently to enhance the resolution. The solid telescope represent a convenient solution for a simple and replicated small telescope. The solid telescope is intrinsically suited to be used in diffraction limited mode down to visible wavelengths. This may allow a viable dual feed mode for both guiding and phase referenced imaging. In this paper we analyze some of the critical engineering aspects and outline a possible implementation approach.
Gaia is ESA's next-generation space mission aimed at global astrometry at the microarcsecond level. Its science
case is devoted to the understanding of our Galaxy's structure, evolution and composition. The GAIA payload
includes two identical telescopes separated by a Basic Angle whose variations in time must be measured with
very high accuracy, to fulll the astrometry goal. To this purpose, an interferometric sub-system, the Basic
Angle Monitoring Device (BAMD), has been introduced. The BAMD optical concept is based on a pair of
laser beams per telescope, producing fringes on a dedicated CCD. The basic measurement principle of BAMD
consists in monitoring the stability of the fringe pattern phase. We are developing a demonstrator of the BAMD
for educational purposes, considered representative of the driving design concept for the Gaia microarcsecond
astrometry. In this paper we describe the design guidelines and analyze some of the key elements related to the
demonstration of the basic angle monitoring concept.
The Interferometric Stratospheric Astrometry for Solar system (ISAS) project is designed for high precision
astrometry on the brightest planets of the Solar System, with reference to many field stars, at the milli-arcsec
(mas) level or better. The science goal is the improvement on our knowledge of the dynamics of the Solar System,
complementing the Gaia observations of fainter objects. The technical goal is the validation of basic concepts for
the proposed Gamma Astrometric Measurement Experiment (GAME) space mission, in particular, combination
of Fizeau interferometry and coronagraphic techniques by means of pierced mirrors, intermediate angle dual field
astrometry, smart focal plane management for increased dynamic range and pointing correction. We discuss
the suitability of the stratospheric environment, close to space conditions, to the astrometric requirements. The
instrument concept is a multiple field, multiple aperture Fizeau interferometer, observing simultaneously four
fields, in order to improve on the available number of reference stars. Coronagraphic solutions are introduced
to allow observation of internal planets (Mercury and Venus), as well as of external planets over a large fraction
of their orbit, i.e. also close to conjunction with the Sun. We describe the science motivation, the proposed
experiment profile and the expected performance.
Medium to large angle observations, e.g. for global astrometry, can be implemented in space by means of either a
common telescope, fed by a Beam Combiner (as in Hipparcos), or by individual telescopes set in a rigid geometry
(as in Gaia). We investigate the applicability of auto-collimation and cophasing techniques for implementation of
a monitoring system alternative to more conventional point-to-point metrology. Apart different implementation
constraints, the most relevant difference consists in the auto-collimation approach characteristics of monitoring
simultaneously comparably large sections of the optical system, thus evaluating collective properties closer to
those experienced by the stellar beams.
In astrometric instrumentation a laser subsystem may be used for precise metrology of instrumental response.
Such subsystems do not require diraction limited imaging, but can be tailored to specic application needs.
We describe an interferometric arrangement for high precision monitoring of telescope line of sight and evaluate
its performance as a function of some design parameters. We deduce that good sensitivity can be achieved over
a signicant range of e.g. focusing conditions, provided proper cautions are adopted for detection and data
processing.
Modern astronomical instrumentation is often developed through non traditional congurations and free form
optics. Recent technological development allows the manufacturing of exotic surfaces, sometimes very far away
from rotationally symmetric geometries. We propose new developments of the solid telescope concept using
multiple re
ections between the faces of a single lens. Taking advantage of modern materials and manufacturing
solutions, a compact, robust, and easily replicable optical subsystem could represent an optimal solution for small
telescopes tailored to specic applications. In this paper we describe the solution for an instrument devoted to
the fast transients detection and tracking.
GAME is a recent concept for a small/medium class mission aimed at Fundamental Physics tests in the Solar
system, by means of an optimised instrument in the visible, based on smart combination of coronagraphy and
Fizeau interferometry. The targeted precision on the γ and β parameters of the Parametrised Post-Newtonian
formulation of General Relativity are respectively in the 10-7-10-8 and 10-5-10-6 range, improving by one or two orders of magnitude with respect to the expectations on current or near future experiments. Such precision
is suitable to detect possible deviations from the unity value, associated to generalised Einstein models for
gravitation, with potentially huge impacts on the cosmological distribution of dark matter and dark energy from
a Solar system scale experiment. The measurement principle is based on the differential astrometric signature on
the stellar positions, i.e. based on the spatial component of the effect rather than the temporal component as in
the most recent experiments using radio link delay timing variation (Cassini). The instrument concept is based
on multiple field, multiple aperture Fizeau interferometry, observing simultaneously regions close to the Solar
limb (requiring the adoption of coronagraphic techniques), and others in opposition to the Sun. The diluted
optics approach is selected for achieving an efficient rejection of the scattered solar radiation, while retaining
an acceptable angular resolution on the science targets. The multiple field observation is aimed at cost-effective
control of systematic effects through simultaneous calibration. We describe the science motivation, the proposed
mission profile, the instrument concept and the expected performance.
The Astrometric Instrument Model system comprises several monitoring and diagnostic tasks for the astrometric
instrument aboard Gaia. It is a hierarchy of dedicated software modules aimed at decreasing the parameter degeneration
of the relation linking the observations to the instrumental behavior, and optimize the estimation process at the CCD and
field-of-view crossing level. Critical for the system is the definition and maintenance of a physical instrument model
fitting the science data, and able to accommodate non nominal configurations. Precise modeling of the astrometric
response is required for optimal definition of the data reduction and calibration algorithms, and to ensure high sensitivity
to both instrumental and astrophysical source parameters.
Micro-arcsecond precision must rely on the detailed knowledge of instrument parameters and observing conditions for
optimal definition of data reduction and calibration procedures. The variation of instrumental response over the field of
view with wavelength and in time is potentially critical and often unavoidable. This work addresses selected topics in
modeling of the astrometric instrument of the Gaia mission, evidencing their role in the data reduction strategy.
Discussion is extended to how the modeling will impact on the data quality and to how the science data can be used to
trace directly the instrument response. Finally mention is provided of the actual implementation of our recipe into the
Astrometric Instrument Model, a software tool which will be used during the processing of Gaia data.
We present a new design of a four mirrors telescope for astrometric measurement to be used in the GAME
mission, currently under study at the Astronomical Observatory of Turin, Italy. The main aim of GAME -
Gamma Astrometric Measurement Experiment - is to measure the γ parameter of the Parameterized Post-
Newtonian formulation by looking at the deflection of light produced by the Sun's gravitational curvature, as in
the Dyson, Eddington et al. 1919 experiment, using a dedicated, space based dual-field telescope. A first design
has been presented in recent years, based on a Cassegrain scheme with a mask in front of the primary mirror to
realize multiple aperture Fizeau interferometry. The new design still implements a Fizeau interferometer, but the
telescope layout is based on a Korsch-like scheme with four conical mirrors, long focal length, and without the
use of exotic surfaces (aspheric or polynomial) as adopted in other long focal astrometric instruments. A different
combination scheme of the two lines of sight makes the dimensioning of the primary mirror more relaxed allowing
us to work with smaller surfaces and therefore to achieve a more compact payload configuration. The design
of the instrument and the masked interferometry approach allow us to maximize the astrometric performances
and at the same time to improve the baffling, minimizing the amount of stray light from the Sun. In this
paper we describe the mission profile, the observation principle, the new instrument layout and the expected
performances.
KEYWORDS: Mirrors, Telescopes, Space telescopes, Photons, Signal to noise ratio, Nanoimprint lithography, Sensors, Space operations, Calibration, Astronomy
Improvement of our understanding of Fundamental Physics is more and more based on high precision measurements
over significant fractions of our Universe. Among the crucial tests of General Relativity and competing theories is the
detection of gravitational waves, which is the subject of advanced modern experiments (LISA, VIRGO, LIGO). Our
investigation is focused on a novel concept for pointed observations of selected astronomical objects in our Galaxy, like
compact binary systems, neutron stars and compact white dwarf binaries, which are expected to be sources of
gravitational waves in the Very Low Frequency range, i.e 10-4 Hz < fg < 10-1 Hz. The detection mechanism is based on
indirect astrometric observations by a spaceborne dedicated instrument, monitoring the astrometric light deflection of the
photons crossing the buffer zone of the gravitational source at the microarcsecond level accuracy. We discuss the class of
potential candidates, the mission concept and its high level specifications; furthermore, we present an implementation
concept including basic instrument characteristics (system configuration, telescope size and constraints, operating
wavelength, detector, operation).
KEYWORDS: Sun, Stars, General relativity, Solar processes, Aerospace engineering, Current controlled current source, Precision measurement, Berkelium, Telescopes, Satellites
The GAME mission concept is aimed at very precise measurement
of the gravitational deflection of light by the Sun, by an
optimized telescope in the visible and launched in orbit
on a small class satellite. The targeted precision on the γ parameter of the Parametrized Post-Newtonian formulation of General Relativity is 10-6 or better, i.e. one to two orders of magnitude better than the best current results. Such precision is suitable to detect possible deviations from unity value, associated to generalized Einstein models for gravitation, with potentially huge impacts on the cosmological distribution of dark matter and dark energy.
The measurement principle is based on differential astrometric
signature on the stellar positions, i.e. on the spatial component
of the effect rather than the temporal component as in recent
experiments using radio link delay timing. Exploiting the observation strategy, it is also possible to target other interesting scientific goals both in the realm of General Relativity and in the observations of extrasolar systems. The instrument is a dual field, multiple aperture Fizeau interferometer, observing simultaneously two regions close to the Solar limb. The diluted optics approach is selected for efficient rejection of the solar radiation, while retaining an acceptable angular resolution on the science targets.
We describe the science motivation, the proposed mission profile, the payload concept and the expected performance from recent results.
The implementation of the simultaneous combination of several telescopes (from four to eight) available at
Very Large Telescope Interferometer (VLTI) will allow the new generation interferometric instrumentation
to achieve interferometric image synthesis with unprecedented resolution and efficiency. The VLTI Spectro
Imager (VSI) is the proposed second-generation near-infrared
multi-beam instrument for the Very Large
Telescope Interferometer, featuring three band operations (J, H and K), high angular resolutions (down to
1.1 milliarcsecond) and high spectral resolutions. VSI will be equipped with its own internal Fringe Tracker
(FT), which will measure and compensate the atmospheric perturbations to the relative beam phase, and in
turn will provide stable and prolonged observing conditions down to the magnitude K=13 for the scientific
combiner. In its baseline configuration, VSI FT is designed to implement, from the very start, the minimum
redundancy combination in a nearest neighbor scheme of six telescopes over six baselines, thus offering better options for rejection of large intensity or phase fluctuations over each beam, due to the symmetric set-up.
The planar geometry solution of the FT beam combiner is devised to be easily scalable either to four or eight
telescopes, in accordance to the three phase development considered for VSI. The proposed design, based
on minimum redundancy combination and bulk optics solution, is described in terms of opto-mechanical
concept, performance and key operational aspects.
In this paper we present the status of different experiments set up at Turin Observatory on novel techniques
for multiple beam combination, adopting mostly bulk optics. The goal of these experiments is to find the
best scheme able to perform efficient fringe tracking operation on a densely populated (N>4) interferometer,
while at the same time maximizing optical throughput and sensitivity on faint sources. One of these concepts
has been proposed for the VSI fringe tracker (see Corcione et al, this conference). The schemes proposed
have also the advantage of being in principle easily adapted to a large number of beams.
The VLTI Spectro Imager project aims to perform imaging with a temporal resolution of 1 night and with a maximum
angular resolution of 1 milliarcsecond, making best use of the Very Large Telescope Interferometer capabilities. To
fulfill the scientific goals (see Garcia et. al.), the system requirements are: a) combining 4 to 6 beams; b) working in
spectral bands J, H and K; c) spectral resolution from R= 100 to 12000; and d) internal fringe tracking on-axis, or off-axis
when associated to the PRIMA dual-beam facility.
The concept of VSI consists on 6 sub-systems: a common path distributing the light between the fringe tracker and the
scientific instrument, the fringe tracker ensuring the co-phasing of the array, the scientific instrument delivering the
interferometric observables and a calibration tool providing sources for internal alignment and interferometric
calibrations. The two remaining sub-systems are the control system and the observation support software dedicated to the
reduction of the interferometric data.
This paper presents the global concept of VSI science path including the common path, the scientific instrument and the
calibration tool. The scientific combination using a set of integrated optics multi-way beam combiners to provide high-stability
visibility and closure phase measurements are also described. Finally we will address the performance budget of
the global VSI instrument. The fringe tracker and scientific spectrograph will be shortly described.
KEYWORDS: Telescopes, Stars, Spectral resolution, Spatial resolution, Interferometry, Integrated optics, Space telescopes, Visibility, Image restoration, Signal to noise ratio
The VLTI Spectro Imager (VSI) was proposed as a second-generation instrument of the Very Large Telescope Interferometer
providing the ESO community with spectrally-resolved, near-infrared images at angular resolutions
down to 1.1 milliarcsecond and spectral resolutions up to R = 12000. Targets as faint as K = 13 will be imaged
without requiring a brighter nearby reference object; fainter targets can be accessed if a suitable reference is
available. The unique combination of high-dynamic-range imaging at high angular resolution and high spectral
resolution enables a scientific program which serves a broad user community and at the same time provides the
opportunity for breakthroughs in many areas of astrophysics. The high level specifications of the instrument are
derived from a detailed science case based on the capability to obtain, for the first time, milliarcsecond-resolution
images of a wide range of targets including: probing the initial conditions for planet formation in the AU-scale
environments of young stars; imaging convective cells and other phenomena on the surfaces of stars; mapping
the chemical and physical environments of evolved stars, stellar remnants, and stellar winds; and disentangling the central regions of active galactic nuclei and supermassive black holes. VSI will provide these new capabilities
using technologies which have been extensively tested in the past and VSI requires little in terms of new
infrastructure on the VLTI. At the same time, VSI will be able to make maximum use of new infrastructure as it
becomes available; for example, by combining 4, 6 and eventually 8 telescopes, enabling rapid imaging through
the measurement of up to 28 visibilities in every wavelength channel within a few minutes. The current studies
are focused on a 4-telescope version with an upgrade to a 6-telescope one. The instrument contains its own
fringe tracker and tip-tilt control in order to reduce the constraints on the VLTI infrastructure and maximize
the scientific return.
The GAME mission concept aims at the very precise measurement of the gravitational deflection of light by the
Sun, by means of an optimised telescope operating in the visible and launched in orbit on a small class satellite.
The targeted precision on the γ parameter of the Parametrised Post-Newtonian formulation of General Relativity
is 10-6 or better, i.e. one to two orders of magnitude better than the best currently available results. Such
precision is suitable to detect possible deviations from the unity value, associated to generalised Einstein models
for gravitation, with potentially huge impacts on the cosmological distribution of dark matter and dark energy.
The measurement principle is based on the differential astrometric signature on the stellar positions, i.e., based
on the spatial component of the effect rather than the temporal component as in the most recent experiments
using radio link delay timing. The observation strategy also allows some additional scientific objectives related
to other tests of General Relativity and to the study of exo-planetary field, multiple aperture Fizeau interferometer, observing simultaneously two regions close to the Solar
limb. The diluted optics approach is selected for achieving an efficient rejection of the scattered solar radiation,
while retaining an acceptable angular resolution on the science targets. We describe the science motivation, the
proposed mission profile, the possible payload implementation and the expected performance.
In ground based interferometric observations, fringe stabilization over long integration times is a mandatory task in order
to achieve useful performances even on faint sources. This is done by dedicated instruments which search the maximum
of the fringe envelope and consequently correct the optical path of the interfering beams. Localization of the fringe
maximum position is corrupted by noise coming both from turbulent atmosphere and instruments. Atmospheric
fluctuations are corrected at telescope level, but high frequency disturbance, as well as inter-telescope one, still remain.
These residuals must be recognized and separated from the source signal, in order to properly model the instrument
behaviour. Moreover, algorithms for fringe tracking must be strong enough to tolerate residual noise and instrument
model inaccuracy.
We provide some examples of noise performance of both calibration and fringe maximum localization based on
laboratory experiments.
One of the concepts of radio interferometry which is very difficult to apply to the visible domain is phase closure. The main difficulty is the spatial requirement, namely that all pencil beams will interfere with all other beams on a flat detector. We use a pair-wise combination method using anamorphic stretching of the beams. All beams are lined up, imaged through a cylindrical lens into a square where each beam is now spread into a parallel line. The comb of lines is made to interfere with a copy of itself rotated at 90°. A rotation shear interferometer is employed for that stage, and the cross pattern of apertures is imaged on the detector. The diagonal shows interference of each beam with itself, for intensity calibration purposes. An extended source clearly reduces contrast on some off-axis patterns, in a symmetric manner. We have already tested two designs in the laboratory using lasers and white light.
VLTi Spectro-Imager (VSI) is a proposition for a second generation VLTI instrument which is aimed at providing
the ESO community with the capability of performing image synthesis at milli-arcsecond angular resolution. VSI
provides the VLTI with an instrument able to combine 4 telescopes in a baseline version and optionally up to
6 telescopes in the near-infrared spectral domain with moderate to high spectral resolution. The instrument
contains its own fringe tracker in order to relax the constraints onto the VLTI infrastructure. VSI will do
imaging at the milli-arcsecond scale with spectral resolution of: a) the close environments of young stars probing
the initial conditions for planet formation; b) the surfaces of stars; c) the environment of evolved stars, stellar
remnants and stellar winds, and d) the central region of active galactic nuclei and supermassive black holes. The
science cases allowed us to specify the astrophysical requirements of the instrument and to define the necessary
studies of the science group for phase A.
The VLTI system foresees two generations of fringe sensor: FINITO and PRIMA FSUs. The former is dedicated to H band; it controls the internal OPD with a temporal modulation with an external reference OPD. The latter, working with the ABCD model and in K band, is based on the introduction of known phase offsets for the interferometric signal (spatial phase modulation) and on the measurement of the corresponding combined power. Simulation models for both FSUs are developed with Matlab. Instrumental parameters, i.e. phase, transmission, visibility, are tabulated for ease of maintenance and to speed execution time. For the use of siderostats, due to fast turbulence, the need for intensity calibration arises. Assuming slow intensity variations with respect to phase variations, different algorithms can apply, yielding to numerical control of perturbations as a function of model parameters.
The design and performance of a Fizeau interferometer with long focal length and large field of view are discussed. The optical scheme presented is well suited for very accurate astrometric measurements from space, being optimised, in terms of geometry and aberrations, to observe astronomical targets down to the visual magnitude mV=20, with a measurement accuracy of 10 microarcseconds at mV=15.
This study is in the context of the next generation astrometric space missions, in particular for a mission profile similar to that of the Gaia mission of the European Space Agency.
Beyond the accuracy goal, the great effort in optical aberrations reduction, particularly distortion, aims at the optimal exploitation of data acquisition done with CCD arrays working in Time Delay Integration mode. The design solution we present reaches the astrometric goals with a field of view of 0.5 square degrees.
FINITO is the first generation VLTI fringe sensor, optimised for three beam observations, recently installed at Paranal and currently used for VLTI optimisation. The PRIMA FSU is the second generation, optimised for astrometry in dual-feed mode, currently in construction. We discuss the constraints of fringe tracking at VLTI, the basic functions required for stabilised interferometric observations, and their different implementation in the two instruments, with remarks on the most critical technical aspects. We provide an estimate of the expected performance and describe some of their possible observing and calibration modes, with reference to the current scientific combiners.
We describe a software tool developed to simulate the behaviour of the angle between two lines of sight in a dual view telescope assembly (usually referred to as basic angle) due to optical misalignments induced by thermo-mechanical fluctuations. The tool applies to a variety of reflective optical designs. In principle, not only the basic angle behaviour can be simulated, but also other optical parameters. As a practical example, we present and discuss results obtained from application of our software to the case of the Gaia baseline optical design. We show that the final error can be severely degraded by fluctuations of the basic angle due to thermo-mechanical effects.
M. Bisi, L. Bonino, Massimo Cecconi, Stefano Cesare, Fabrizio Bertinetto, Giovanni Mana, D. Carollo, Mario Gai, Mario Lattanzi, Enrico Canuto, F. Donati
Within a Technology Research Program funded by the European Space Agency, a team led by Alenia Aerospazio has investigated and started the development of some technologies which are considered fundamental for the achievement of the scientific objectives of the future astrometric mission GAIA. The activities have been focused on the design of a two-aperture optical interferometer and of a system for the active stabilization of its configuration within few picometers. A laboratory prototype of the active stabilization system has been implemented and tested. The results achieved in the laboratory tests proved that the very challenging requirements imposed by the GAIA astrometric goal of 10 micro-arcsec accuracy can be fulfilled.
KEYWORDS: Data acquisition, Sensors, Electronics, Cameras, Data processing, Digital signal processing, Astronomy, Detection and tracking algorithms, Analog electronics, Infrared astronomy
We discuss the present implementation of the data acquisition electronics and the planned upgraded version, together with the related algorithms, of the new Torino IR camera: TC-MIRC. A detailed description of the camera is available in M. Robberto et al., 1994, presented in this SPIE meeting. The electronic structure of TC-MIRC is based on a PC-compatible host computer, using IDL/Windows, and a transputer network for detectors management and data processing; the engineering advantages of an intrinsically distributed environment and the computational scalability are discussed. The data acquisition procedures (standard algorithms for coadding and nondestructive readout, and their use in normal operations) are evaluated, with respect to their present performance and to the upgrade needed to fulfill the design requirements.
KEYWORDS: Telescopes, Sensors, Cameras, Infrared cameras, Data acquisition, Electronics, Digital signal processing, Control systems, Channel projecting optics, Infrared telescopes
Following the availability on the market of IR arrays able to perform ground-based astronomical observations in the atmospheric windows longward of 2.5 micrometers , we started at the Torino Astronomical Observatory a new project aimed at the construction of a thermal IR camera to be installed at the TIRGO telescope. Located in the Swiss alps at 3100 m a.s.l., this Italian facility (1.5 m f/20 IR optimized) provides during the winter months a relatively high number of nights (20%) with first-rate conditions (low temperature and emissivity) for medium-IR observations. In order to fully exploit this potential, we designed an instrument, named Two-Channel Medium IR Camera (TC-MIRC) operating over the entire 1 to 14 micrometers region and optimized for the 2.5 to 14 micrometers thermal bands. TC-MIRC covers such a broad range of wavelengths using two IR array detectors: an InSb device for the 1 to 5 micrometers region and a Si:Ga device for the 8 to 14 micrometers band. The main characteristic of the camera is that both arrays can simultaneously observe the same region. In this way, we can not only approach an almost double observing efficiency (time really spent `on target'), but also use both detectors for correlated observations and testing of unconventional acquisition techniques. It follows that TC-MIRC is a complex instrument presenting several interesting features. Thanks to the presence of two independent optical channels, the user can change the filters, adjust the focus and vary the optical scale on a channel without affecting the acquisition running on the other array. In particular, the possibility of adjusting the optical scale on each detector during the observations allows the user to select the most convenient sampling and field of view on the basis of the actual seeing or diffraction conditions, background level and scientific needs. Moreover, the adopted cryogenic system is entirely based on a mechanical closed-cycle cooler and allows very low-cost operations and easy maintenance on the mountain for long periods of time. In this paper we present the opto/mechanical design and construction, the general structure of the control system and the software architecture. We report the performances reached by the most critical parts of the instrument during the test carried out in the laboratory and at the telescope during the first engineering run in January 1994.
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