PFS (Prime Focus Spectrograph), a next generation facility instrument on the 8.2-meter Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed over the 1.3 deg field of view. The spectrograph has been designed with 3 arms of blue, red, and near-infrared cameras to simultaneously observe spectra from 380nm to 1260nm in one exposure at a resolution of ~1.6 - 2.7Å. An international collaboration is developing this instrument under the initiative of Kavli IPMU. The project is now going into the construction phase aiming at undertaking system integration in 2017-2018 and subsequently carrying out engineering operations in 2018-2019. This article gives an overview of the instrument, current project status and future paths forward.
The Primordial Inflation Explorer is an Explorer-class mission to open new windows on the early universe through measurements of the polarization and absolute frequency spectrum of the cosmic microwave background. PIXIE will measure the gravitational-wave signature of primordial inflation through its distinctive imprint in linear polarization, and characterize the thermal history of the universe through precision measurements of distortions in the blackbody spectrum. PIXIE uses an innovative optical design to achieve background-limited sensitivity in 400 spectral channels spanning over 7 octaves in frequency from 30 GHz to 6 THz (1 cm to 50 micron wavelength). Multi-moded non-imaging optics feed a polarizing Fourier Transform Spectrometer to produce a set of interference fringes, proportional to the difference spectrum between orthogonal linear polarizations from the two input beams. Multiple levels of symmetry and signal modulation combine to reduce systematic errors to negligible levels. PIXIE will map the full sky in Stokes I, Q, and U parameters with angular resolution 2.6° and sensitivity 70 nK per 1° square pixel. The principal science goal is the detection and characterization of linear polarization from an inflationary epoch in the early universe, with tensor-to-scalar ratio r < 10−3 at 5 standard deviations. The PIXIE mission complements anticipated ground-based polarization measurements such as CMB- S4, providing a cosmic-variance-limited determination of the large-scale E-mode signal to measure the optical depth, constrain models of reionization, and provide a firm detection of the neutrino mass (the last unknown parameter in the Standard Model of particle physics). In addition, PIXIE will measure the absolute frequency spectrum to characterize deviations from a blackbody with sensitivity 3 orders of magnitude beyond the seminal COBE/FIRAS limits. The sky cannot be black at this level; the expected results will constrain physical processes ranging from inflation to the nature of the first stars and the physical conditions within the interstellar medium of the Galaxy. We describe the PIXIE instrument and mission architecture required to measure the CMB to the limits imposed by astrophysical foregrounds.
F. De Bernardis, J. Stevens, M. Hasselfield, D. Alonso, J. R. Bond, E. Calabrese, S. Choi, K. Crowley, M. Devlin, J. Dunkley, P. Gallardo, S. Henderson, M. Hilton, R. Hlozek, S. P. Ho, K. Huffenberger, B. Koopman, A. Kosowsky, T. Louis, M. Madhavacheril, J. McMahon, S. Næss, F. Nati, L. Newburgh, M. Niemack, L. Page, M. Salatino, A. Schillaci, B. Schmitt, N. Sehgal, J. Sievers, S. Simon, D. Spergel, S. Staggs, A. van Engelen, E. Vavagiakis, E. Wollack
In recent years there have been significant improvements in the sensitivity and the angular resolution of the instruments dedicated to the observation of the Cosmic Microwave Background (CMB). ACTPol is the first polarization receiver for the Atacama Cosmology Telescope (ACT) and is observing the CMB sky with arcmin resolution over 2000 sq. deg. Its upgrade, Advanced ACTPol (AdvACT), will observe the CMB in five frequency bands and over a larger area of the sky. We describe the optimization and implementation of the ACTPol and AdvACT surveys. The selection of the observed fields is driven mainly by the science goals, that is, small angular scale CMB measurements, B-mode measurements and cross-correlation studies. For the ACTPol survey we have observed patches of the southern galactic sky with low galactic foreground emissions which were also chosen to maximize the overlap with several galaxy surveys to allow unique cross-correlation studies. A wider field in the northern galactic cap ensured significant additional overlap with the BOSS spectroscopic survey. The exact shapes and footprints of the fields were optimized to achieve uniform coverage and to obtain cross-linked maps by observing the fields with different scan directions. We have maximized the efficiency of the survey by implementing a close to 24 hour observing strategy, switching between daytime and nighttime observing plans and minimizing the telescope idle time. We describe the challenges represented by the survey optimization for the significantly wider area observed by AdvACT, which will observe roughly half of the low-foreground sky. The survey strategies described here may prove useful for planning future ground-based CMB surveys, such as the Simons Observatory and CMB Stage IV surveys.
The Prime Focus Spectrograph (PFS) is an optical/near-infrared multifiber spectrograph with 2394 science fibers distributed across a 1.3-deg diameter field of view at the Subaru 8.2-m telescope. The wide wavelength coverage from 0.38 μm to 1.26 μm, with a resolving power of 3000, simultaneously strengthens its ability to target three main survey programs: cosmology, galactic archaeology and galaxy/AGN evolution. A medium resolution mode with a resolving power of 5000 for 0.71 μm to 0.89 μm will also be available by simply exchanging dispersers. We highlight some of the technological aspects of the design. To transform the telescope focal ratio, a broad-band coated microlens is glued to each fiber tip. A higher transmission fiber is selected for the longest part of the cable system, optimizing overall throughput; a fiber with low focal ratio degradation is selected for the fiber-positioner and fiber-slit components, minimizing the effects of fiber movements and fiber bending. Fiber positioning will be performed by a positioner consisting of two stages of piezo-electric rotary motors. The positions of these motors are measured by taking an image of artificially back-illuminated fibers with the metrology camera located in the Cassegrain container; the fibers are placed in the proper location by iteratively measuring and then adjusting the positions of the motors. Target light reaches one of the four identical fast-Schmidt spectrograph modules, each with three arms. The PFS project has passed several project-wide design reviews and is now in the construction phase.
The Primordial Inflation Explorer is an Explorer-class mission to measure the gravity-wave signature of primordial inflation through its distinctive imprint on the linear polarization of the cosmic microwave background. PIXIE uses an innovative optical design to achieve background-limited sensitivity in 400 spectral channels spanning 2.5 decades in frequency from 30 GHz to 6 THz (1 cm to 50 micron wavelength). Multi-moded non-imaging optics feed a polarizing Fourier Transform Spectrometer to produce a set of interference fringes, proportional to the difference spectrum between orthogonal linear polarizations from the two input beams. Multiple levels of symmetry and signal modulation combine to reduce the instrumental signature and confusion from unpolarized sources to negligible levels. PIXIE will map the full sky in Stokes I, Q, and U parameters with angular resolution 2.6 deg and sensitivity 0.2 µK per 1 deg square pixel. The principal science goal is the detection and characterization of linear polarization from an inflationary epoch in the early universe, with tensor-to-scalar ratio r < 10-3 at 5 standard deviations. In addition, PIXIE will measure the absolute frequency spectrum to constrain physical processes ranging from inflation to the nature of the first stars to the physical conditions within the interstellar medium of the Galaxy. We describe the PIXIE instrument and mission architecture with an emphasis on the expected level of systematic error suppression.
The Prime Focus Spectrograph (PFS) is an optical/near-infrared multi-fiber spectrograph with 2394 science fibers, which
are distributed in 1.3 degree diameter field of view at Subaru 8.2-meter telescope. The simultaneous wide wavelength
coverage from 0.38 μm to 1.26 μm, with the resolving power of 3000, strengthens its ability to target three main survey
programs: cosmology, Galactic archaeology, and galaxy/AGN evolution. A medium resolution mode with resolving
power of 5000 for 0.71 μm to 0.89 μm also will be available by simply exchanging dispersers. PFS takes the role for the
spectroscopic part of the Subaru Measurement of Images and Redshifts (SuMIRe) project, while Hyper Suprime-Cam
(HSC) works on the imaging part. HSC’s excellent image qualities have proven the high quality of the Wide Field
Corrector (WFC), which PFS shares with HSC. The PFS collaboration has succeeded in the project Preliminary Design
Review and is now in a phase of subsystem Critical Design Reviews and construction.
To transform the telescope plus WFC focal ratio, a 3-mm thick broad-band coated microlens is glued to each fiber tip.
The microlenses are molded glass, providing uniform lens dimensions and a variety of refractive-index selection. After
successful production of mechanical and optical samples, mass production is now complete. Following careful
investigations including Focal Ratio Degradation (FRD) measurements, a higher transmission fiber is selected for the
longest part of cable system, while one with a better FRD performance is selected for the fiber-positioner and fiber-slit
components, given the more frequent fiber movements and tightly curved structure. Each Fiber positioner consists of two
stages of piezo-electric rotary motors. Its engineering model has been produced and tested. After evaluating the statistics
of positioning accuracies, collision avoidance software, and interferences (if any) within/between electronics boards,
mass production will commence. Fiber positioning will be performed iteratively by taking an image of artificially back-illuminated
fibers with the Metrology camera located in the Cassegrain container. The camera is carefully designed so
that fiber position measurements are unaffected by small amounts of high special-frequency inaccuracies in WFC lens
surface shapes.
Target light carried through the fiber system reaches one of four identical fast-Schmidt spectrograph modules, each with
three arms. All optical glass blanks are now being polished. Prototype VPH gratings have been optically tested. CCD
production is complete, with standard fully-depleted CCDs for red arms and more-challenging thinner fully-depleted
CCDs with blue-optimized coating for blue arms. The active damping system against cooler vibration has been proven to
work as predicted, and spectrographs have been designed to avoid small possible residual resonances.
We describe the conceptual design of the camera cryostats, detectors, and detector readout electronics for the SuMIRe
Prime Focus Spectrograph (PFS) being developed for the Subaru telescope. The SuMIRe PFS will consist of four
identical spectrographs, each receiving 600 fibers from a 2400 fiber robotic positioner at the prime focus. Each
spectrograph will have three channels covering wavelength ranges 3800 Å - 6700 Å, 6500 Å - 10000 Å, and 9700 Å -
13000 Å, with the dispersed light being imaged in each channel by a f/1.10 vacuum Schmidt camera. In the blue and red
channels a pair of Hamamatsu 2K x 4K edge-buttable CCDs with 15 um pixels are used to form a 4K x 4K array. For
the IR channel, the new Teledyne 4K x 4K, 15 um pixel, mercury-cadmium-telluride sensor with substrate removed for
short-wavelength response and a 1.7 um cutoff will be used. Identical detector geometry and a nearly identical optical
design allow for a common cryostat design with the only notable difference being the need for a cold radiation shield in
the IR camera to mitigate thermal background. This paper describes the details of the cryostat design and cooling
scheme, relevant thermal considerations and analysis, and discusses the detectors and detector readout electronics.
The Prime Focus Spectrograph (PFS) of the Subaru Measurement of Images and Redshifts (SuMIRe) project has been
endorsed by Japanese community as one of the main future instruments of the Subaru 8.2-meter telescope at Mauna Kea,
Hawaii. This optical/near-infrared multi-fiber spectrograph targets cosmology with galaxy surveys, Galactic archaeology,
and studies of galaxy/AGN evolution.
Taking advantage of Subaru’s wide field of view, which is further extended with the recently completed Wide Field
Corrector, PFS will enable us to carry out multi-fiber spectroscopy of 2400 targets within 1.3 degree diameter. A
microlens is attached at each fiber entrance for F-ratio transformation into a larger one so that difficulties of spectrograph design are eased. Fibers are accurately placed onto target positions by positioners, each of which consists of two stages
of piezo-electric rotary motors, through iterations by using back-illuminated fiber position measurements with a widefield
metrology camera. Fibers then carry light to a set of four identical fast-Schmidt spectrographs with three color arms
each: the wavelength ranges from 0.38 μm to 1.3 μm will be simultaneously observed with an average resolving power
of 3000.
Before and during the era of extremely large telescopes, PFS will provide the unique capability of obtaining spectra of
2400 cosmological/astrophysical targets simultaneously with an 8-10 meter class telescope. The PFS collaboration, led
by IPMU, consists of USP/LNA in Brazil, Caltech/JPL, Princeton, and JHU in USA, LAM in France, ASIAA in Taiwan,
and NAOJ/Subaru.
External occulters provide the starlight suppression needed for detecting and characterizing exoplanets with
a much simpler telescope and instrument than is required for the equivalent performing coronagraph. In
this paper we describe progress on our Technology Development for Exoplanet Missions project to design,
manufacture, and measure a prototype occulter petal. We focus on the key requirement of manufacturing a
precision petal while controlling its shape within precise tolerances. The required tolerances are established
by modeling the effect that various mechanical and thermal errors have on scatter in the telescope image
plane and by suballocating the allowable contrast degradation between these error sources. We discuss the
deployable starshade design, representative error budget, thermal analysis, and prototype manufacturing.
We also present our metrology system and methodology for verifying that the petal shape meets the contrast
requirement. Finally, we summarize the progress to date building the prototype petal.
The Primordial Inflation Explorer is an Explorer-class mission to measure the gravity-wave signature of primordial
inflation through its distinctive imprint on the linear polarization of the cosmic microwave background. PIXIE
uses an innovative optical design to achieve background-limited sensitivity in 400 spectral channels spanning 2.5
decades in frequency from 30 GHz to 6 THz (1 cm to 50 μm wavelength). Multi-moded non-imaging optics
feed a polarizing Fourier Transform Spectrometer to produce a set of interference fringes, proportional to the
difference spectrum between orthogonal linear polarizations from the two input beams. The differential design
and multiple signal modulations spanning 11 orders of magnitude in time combine to reduce the instrumental
signature and confusion from unpolarized sources to negligible levels. PIXIE will map the full sky in Stokes I,
Q, and U parameters with angular resolution 2.°6 and sensitivity 0.2 μK per 1° square pixel. The principal
science goal is the detection and characterization of linear polarization from an inflationary epoch in the early
universe, with tensor-to-scalar ratio r < 10-3 at 5 standard deviations. We describe the PIXIE instrument and
mission architecture needed to detect the signature of an inflationary epoch in the early universe using only 4
semiconductor bolometers.
We present an analysis of the Occulting Ozone Observatory (O3) - a $1 billion class mission dedicated to finding
extra-solar planets down to Earth size, performing photometric characterizations of planets and disks, detecting
the presence of ozone, and general astrophysics. We present trade studies for the observatory, composed of a 1
to 2 m telescope based on heritage imaging systems and a complementary sized, free-flying occulter spacecraft,
to maximize the expected science yield for this mission class. Using a camera with four filters each in the 250-
550 nm and 500-1100 nm bands, this modest-size telescope can detect atmospheric ozone in Earth-like planets,
methane in gas giants, determine planetary spin rotation periods, characterize the surface composition of rocky
planets and determine or constrain the values of basic orbital elements. We present multiple different mission
designs along with the expected number of planetary detections and photometric characterizations.
ACCESS is one of four medium-class mission concepts selected for study in 2008-9 by NASA's Astrophysics Strategic
Mission Concepts Study program. ACCESS evaluates a space observatory designed for extreme high-contrast imaging
and spectroscopy of exoplanetary systems. An actively-corrected coronagraph is used to suppress the glare of diffracted
and scattered starlight to contrast levels required for exoplanet imaging. The ACCESS study considered the relative
merits and readiness of four major coronagraph types, and modeled their performance with a NASA medium-class space
telescope. The ACCESS study asks: What is the most capable medium-class coronagraphic mission that is possible with
telescope, instrument, and spacecraft technologies available today? Using demonstrated high-TRL technologies, the
ACCESS science program surveys the nearest 120+ AFGK stars for exoplanet systems, and surveys the majority of
those for exozodiacal dust to the level of 1 zodi at 3 AU. Coronagraph technology developments in the coming year are
expected to further enhance the science reach of the ACCESS mission concept.
The Primordial Inflation Explorer (PIXIE) is an Explorer-class mission to map the absolute intensity and linear
polarization of the cosmic microwave background and diffuse astrophysical foregrounds over the full sky from
frequencies 30 GHz to 6 THz (1 cm to 50 μm wavelength). PIXIE uses a polarizing Michelson interferometer with 2.7 K
optics to measure the difference spectrum between two orthogonal linear polarizations from two co-aligned beams.
Either input can view either the sky or a temperature-controlled absolute reference blackbody calibrator. The multimoded
optics and high etendu provide sensitivity comparable to kilo-pixel focal plane arrays, but with greatly expanded
frequency coverage while using only 4 detectors total. PIXIE builds on the highly successful COBE/FIRAS design by
adding large-area polarization-sensitive detectors whose fully symmetric optics are maintained in thermal equilibrium
with the CMB. The highly symmetric nulled design provides redundant rejection of major sources of systematic
uncertainty. The principal science goal is the detection and characterization of linear polarization from an inflationary
epoch in the early universe, with tensor-to-scalar ratio r << 10-3. PIXIE will also return a rich data set constraining
physical processes ranging from Big Bang cosmology, reionization, and large-scale structure to the local interstellar
medium.
The six-meter Atacama Cosmology Telescope (ACT) in Chile was built to measure the cosmic microwave background
(CMB) at arcminute angular scales. We are building a new polarization sensitive receiver for ACT
(ACTPol). ACTPol will characterize the gravitational lensing of the CMB and aims to constrain the sum of the
neutrino masses with ~ 0.05 eV precision, the running of the spectral index of inflation-induced fluctuations,
and the primordial helium abundance to better than 1 %. Our observing fields will overlap with the SDSS BOSS
survey at optical wavelengths, enabling a variety of cross-correlation science, including studies of the growth of
cosmic structure from Sunyaev-Zel'dovich observations of clusters of galaxies as well as independent constraints
on the sum of the neutrino masses. We describe the science objectives and the initial receiver design.
An occulter is an instrument designed to suppress starlight by diffraction from its edges; most are designed
to be circular, with a set of identical "petals" running around the outside. Proposed space-based occulters
are lightweight, deployed screens tens of meters in diameter with challenging accuracy requirements. In
this paper we describe the design of an occulter for the THEIA mission concept. THEIA consists of a
4-meter telescope diffraction limited to 300 nm, and a 40-meter external occulter to provide high-contrast
imaging. Operating from 250 to 1000 nm, it will provide a rich family of science projects, including exoplanet
characterization, ultraviolet spectroscopy, and very wide-field imaging. Originally conceived of as a hybrid
system employing both an occulter and internal coronagraph, THEIA now uses a single occulter to achieve
all of the starlight suppression but at two different distances from the telescope in order to minimize size and
distance. We describe the basic design principles of the THEIA occulter, its final configuration, performance,
and sensitivity.
An occulter is an instrument designed to suppress starlight by diffraction from its edges; most are designed
to be circular, with a set of identical "petals" running around the outside. Proposed space-based occulters
are lightweight, deployed screens tens of meters in diameter with challenging accuracy requirements. We
describe a general method for modifying the shape of an occulter to accommodate engineering considerations
and show how to calculate the resulting wavefront. This method can be used to place hinges and tensioning
elements between petals, to reduce tolerancing requirements by allowing gaps between petals to be moved
elsewhere, and to potentially reduce the number of petals required on an occulter.
We use our automated Design Reference Mission construction framework to evaluate the performance of multiple
direct exoplanet imager mission concepts on a variety of metrics including: total number of planetary detections,
number of unique planets found, number of target stars observed and number of successful spectral characterizations.
We evaluate designs of self-contained coronagraphs and co-orbiting occulters. Performance is evaluated
on simulated universes with differing frequencies of planets and varying expected occurrence rates of different
planet types.
The Atacama Cosmology Telescope (ACT) is designed to measure temperature anisotropies of the cosmic microwave background (CMB) at arcminute resolution. It is the first CMB experiment to employ a 32×32 close-packed array of free-space-coupled transition-edge superconducting bolometers. We describe the organization of the telescope systems and software for autonomous, scheduled operations. When paired with real-time data streaming and display, we are able to operate the telescope at the remote site in the Chilean Altiplano via the Internet from North America. The telescope had a data rate of 70 GB/day in the 2007 season, and the 2008 upgrade to three arrays will bring this to 210 GB/day.
The Millimeter Bolometer Array Camera (MBAC) was commissioned in the fall of 2007 on the new 6-meter
Atacama Cosmology Telescope (ACT). The MBAC on the ACT will map the temperature anisotropies of the
Cosmic Microwave Background (CMB) with arc-minute resolution. For this first observing season, the MBAC
contained a diffraction-limited, 32 by 32 element, focal plane array of Transition Edge Sensor (TES) bolometers
for observations at 145 GHz. This array was coupled to the telescope with a series of cold, refractive, reimaging
optics. To meet the performance specifications, the MBAC employs four stages of cooling using closed-cycle
3He/4He sorption fridge systems in combination with pulse tube coolers. In this paper we present the design of
the instrument and discuss its performance during the first observing season. Finally, we report on the status
of the MBAC for the 2008 observing season, when the instrument will be upgraded to a total of three separate
1024-element arrays at 145 GHz, 220 GHz and 280 GHz.
ACCESS (Actively-Corrected Coronagraph for Exoplanet System Studies) develops the science and engineering case for
an investigation of exosolar giant planets, super-earths, exo-earths, and dust/debris fields that would be accessible to a
medium-scale NASA mission. The study begins with the observation that coronagraph architectures of all types (other
than the external occulter) call for an exceptionally stable telescope and spacecraft, as well as active wavefront
correction with one or more deformable mirrors (DMs). During the study, the Lyot, shaped pupil, PIAA, and a number
of other coronagraph architectures will all be evaluated on a level playing field that considers science capability
(including contrast at the inner working angle (IWA), throughput efficiency, and spectral bandwidth), engineering
readiness (including maturity of technology, instrument complexity, and sensitivity to wavefront errors), and mission
cost so that a preferred coronagraph architecture can be selected and developed for a medium-class mission.
This paper summarizes our work designing optimal shaped pupils for high-contrast imaging. We show how any effective apodization can be created using shaped pupils and present a variety of both one-dimensional and azimuthally symmetric pupil shapes. Each pupil has its own performance advantage and we discuss the tradeoffs among various designs. Optimizations are typically performed by maximizing a measure of system throughput under constraints on contrast and inner working angle. We mention the question of sensitivity to aberrations. Controlling aberrations will be critical for any implementation of a planet-finding coronagraph. Finally, we present our first laboratory results testing a shaped pupil coronagraph.
The Princeton University Terrestrial Planet Finder (TPF) has been working on a novel method for direct imaging of extra solar planets using a shaped-pupil coronagraph. The entrance pupil of the coronagraph is optimized to have a point spread function (PSF) that provides the suppression level needed at the angular separation
required for detection of extra solar planets. When integration time is to be minimized, the photon count at the planet location in the image plane is a Poisson distributed random process. The ultimate limitation of these high-dynamic-range imaging systems comes from scattering due to imperfections in the optical surfaces of the collecting system. The first step in correcting the wavefront errors is the estimation of the phase aberrations. The phase aberration caused by these imperfections is assumed to be a sum of two-dimensional sinusoidal functions. Its parameters are estimated using a global search with a genetic algorithm and a local optimization with the BFGS quasi-Newton method with a mixed quadratic and cubic line search procedure.
The Princeton University Terrestrial Planet Finder (TPF) group has been working on a novel method for direct imaging of extra solar planets using a shaped-pupil coronagraph. The entrance pupil of the coronagraph is optimized to have a point spread function (PSF) that provides the suppression level needed at the angular separation required for detection of extra solar planets. When integration time is to be minimized, the photon count at the planet location in the image plane is a Poisson distributed random process. The ultimate limitation of these high-dynamic-range imaging systems comes from scattering due to imperfections in the optical surfaces of the collecting system. The first step in correcting the wavefront errors is the estimation of the phase aberrations. The phase aberration caused by these imperfections is assumed to be a sum of two-dimensional sinusoidal functions. Assuming one uses a deformable mirror to correct these aberrations, we propose an algorithm that
optimally decreases the scattering level in specified localized areas in the image plane independent of the choice of influence function of the deformable mirror.
Motivated by the desire to image exosolar planets, recent work by us and others has shown that high-contrast imaging can be achieved using specially shaped pupil masks. To date, our masks have been symmetric with respect to a cartesian coordinate system but were not rotationally invariant, thus requiring that one take multiple images at different angles of rotation about the central point in order to obtain high-contrast in all directions. In this talk, we present two new classes of masks that have rotational symmetry and provide high-contrast in all directions with just one image. These masks
provide the required 10-10 level of contrast to within 4 λ/Δ of the central point. They are also well-suited for use on ground-based telescopes, and perhaps NGST as well, since they can accommodate central obstructions and associated support spiders.
An experimental proof using two liquid crystal spatial light modulators in conjunction with a white light Michelson interferometer to correct amplitude error in telescopes is presented.The principle is reviewed,and then the experiment for a monochromatic closed loop is detailed.
We examine several different approaches to achieving high contrast imaging of extrasolar planets. Rather than controlling the diffracted light by masking the star's image as in a classical coronagraph, we use the pupil's transmission function to focus the starlight. There are two broad classes of pupil coronagraphs examined in this paper: apodized pupils with spatially varying transmision functions and shaped pupils, whose transmission values are either 0 or 1. The latter are much easier to manufacture to the needed tolerances. This paper introduces several new shaped pupils and applies integration time and other metrics to them as well as to apodized pupils. These new designs can achieve nearly as high a throughput as the best
apodized pupils and perform significantly better than the apodized square aperture design. The new shaped pupils enable searches of 50% -100% of thedetectable region, suppress the star's light to below 10-10 of its peak value and have inner working distances as small as 2.8 λ/D.
Eclipse is a proposed Discovery-class mission to perform a sensitive imaging survey of nearby planetary systems, including a complete survey for Jupiter-sized planets orbiting 5 AU from all stars of spectral types A-K to distances of 15 pc. Eclipse is a coronagraphic space telescope concept designed for high-contrast visible wavelength imaging and spectrophotometry. Its optical design incorporates essential elements: a telescope with an unobscured aperture of 1.8 meters and optical surfaces optimized for smoothness at critical spatial frequencies, a coronagraphic camera for suppression of diffracted light, and precision active optical correction for suppression of light scattered by residual mirror surface irregularities. For reference, Eclipse is predicted to reduce diffracted and scattered starlight between 0.25 and 2.0 arcseconds from the star by at least three orders of magnitude compared to any HST instrument. The Eclipse mission offers precursor science explorations and critical technology validation in
support of coronagraphic concepts for NASA's Terrestrial Planet Finder (TPF). A baseline three-year science mission would provide a survey of the nearby stars accessible to TPF before the end of this decade, promising fundamental new insights into the nature and evolution of possibly diverse planetary systems associated with our Sun's nearest neighbors.
A new method is presented for amplitude and phase control using two liquid crystal spatial light modulators in conjunction with a white light Michelson interferometer. Preliminary proof-of-concept measurements are given showing the prospect of using this method for correction of amplitude errors in telescopes.
KEYWORDS: Planets, Stars, Signal to noise ratio, Space telescopes, Hubble Space Telescope, Coronagraphy, Wavefronts, Exoplanets, Telescopes, Point spread functions
Recent advances in deformable mirror technology for correcting wavefront errors and in pupil shapes and masks for coronagraphic suppression of diffracted starlight enable a powerful approach to detecting extrasolar planets in reflected (scattered) starlight at visible wavelengths. We discuss the planet-finding performance of Hubble-like telescopes using these technical advances. A telescope of aperture of at least 4 meters could accomplish the goals of the Terrestrial Planet Finder (TPF) mission. The '4mTPF' detects an Earth around a Sun at five parsecs in about one hour of integration time. It finds molecular oxygen, ozone, water vapor, the 'red edge' of chlorophyll-containing land-plant leaves, and the total atmospheric column density -- all in forty hours or less. The 4mTPF has a strong science program of discovery and characterization of extrasolar planets and planetary systems, including other worlds like Earth. With other astronomical instruments sharing the focal plane, the 4mTPF could also continue and expand the general program of astronomical research of the Hubble Space Telescope.
David Wittman, J. Anthony Tyson, Ian Dell'Antonio, Andrew Becker, Vera Margoniner, Judith Cohen, D. Norman, D. Loomba, G. Squires, Gillian Wilson, Christopher Stubbs, J. Hennawi, David Spergel, P. Boeshaar, A. Clocchiatti, M. Hamuy, G. Bernstein, A. Gonzalez, Puragra Guhathakurta, W. Hu, U. Seljak, Dennis Zaritsky
The Deep Lens Survey (DLS) is a deep BV Rz' imaging survey of seven 2°×2° degree fields, with all data to be made public. The primary scientific driver is weak gravitational lensing, but the survey is also designed to enable a wide array of other astrophysical investigations. A unique feature of this survey is the search for transient phenomena. We subtract multiple exposures of a field, detect differences, classify, and release transients on the Web within about an hour of observation. Here we summarize the scientific goals of the DLS, field and filter selection, observing techniques and current status, data reduction, data products and release, and transient detections. Finally, we discuss some lessons which might apply to future large surveys such as LSST.
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