Exoplanets can potentially be observed very close to stars using single-mode cross-aperture nulling interferometry, an optical-fiber based approach in which starlight rejection occurs as a result of a coupling mismatch between an antisymmetric stellar input field and a symmetric fiber mode. The input stellar point-spread function is first modified by passage through an appropriate upstream pupil-plane phase mask, such as a phase-knife mask, which provides a p-radian phase step, or equivalently, a relative field reversal, across a pupil bisector. Using a phase mask with a “crossed” halfwave plate structure to produce the desired relative field reversal, a narrowband null depth of 2.2 × 10-5 has been demonstrated in the laboratory, a rejection level that is sufficient for the detection of Hot Jupiters with large ground-based telescopes. Moreover, as is shown here, phase masks with slightly more complex spatial patterns can in theory lower the stellar leakage due to finite stellar diameters into the 10-9 to 10-10 range needed for terrestrial exoplanet observations. Because nulling performance improves with wavelength, near-infrared cross-aperture nulling may thus be able to serve as a long-wavelength complement to visible wavelength coronagraphy on future exoplanet missions such as the Habitable Worlds Observatory.
The presence of oceans on the outer solar system moons Europa and Enceladus poses the question of whether microbial life might be present on those bodies. One approach to answering that question could be a very compact, lightweight and robust microscope that is capable of rapidly imaging the contents of a 3-dimensional sample volume. To this end, we have been developing deployable digital holographic microscopes, which can also be used in the short term for terrestrial field work. A very stable “common-mode” microscope, in which two adjacent beams share several optics, has shown very good imaging performance, and has been deployed successfully to several field sites, including Greenland and Alaska. A more compact approach is our version of the lensless digital holographic microscope, which uses gradient index rod lenses to produce a pair of high numerical-aperture input beams. Sub-micron resolution has been obtained with both systems, and further performance improvements are possible.
We have been developing focal-plane phase-mask coronagraphs ultimately aiming at direct detection and characterization of Earth-like extrasolar planets by future space coronagraph missions. By utilizing photonic-crystal technology, we manufactured various coronagraphic phase masks such as eight-octant phase masks (8OPMs), 2nd-order vector vortex masks, and a 4th-order discrete (32-sector) vector vortex mask. Our laboratory experiments show that the 4th-order vortex mask reaches to higher contrast than the 2nd-order one at inner region on a focal plane. These results demonstrate that the higher-order vortex mask is tolerant of low-order phase aberrations such as tip-tilt errors. We also carried out laboratory demonstration of the 2nd-order vector vortex masks in the High-Contrast Imaging Testbed (HCIT) at the Jet Propulsion Laboratory (JPL), and obtained 10-8-level contrast owing to an adaptive optics system for creating dark holes. In addition, we manufactured a polarization-filtered 8OPM, which theoretically realizes achromatic performance. We tested the manufactured polarization-filtered 8OPM in the Infrared Coronagraphic Testbed (IRCT) at the JPL. Polychromatic light sources are used for evaluating the achromatic performance. The results suggest that 10-5- level peak-to-peak contrasts would be obtained over a wavelength range of 800-900 nm. For installing the focal-plane phase-mask coronagraph into a conventional centrally-obscured telescope with a secondary mirror, pupil-remapping plates have been manufactured for removing the central obscuration to enhance the coronagraphic performance. A result of preliminary laboratory demonstration of the pupil-remapping plates is also reported. In this paper, we present our recent activities of the photonic-crystal phase coronagraphic masks and related techniques for the high-contrast imaging.
With a null precision of a few 10-4 at all azimuth angles inside a field-of-view extending from 35 to 275 mas, the
Palomar Fiber Nuller (PFN) is able to explore angular scales intermediate between those accessed by coronagraphic
imaging and by long baseline interferometry. We first briefly summarize the recent performance improvements of the
PFN (sensitivity, azimuthal coverage, duty cycle efficiency on-sky) over the 2011-2014 time period. Then we report on
recent K-band observations of the young pre-main sequence star AB Aurigae obtained with the PFN. It is shown that a
mean astrophysical null of 1.52% was detected around AB Aur at all probed azimuthal angles, and this inside a field-of-view
corresponding to projected separations between 5 and 40 AU. In addition, we also report a slight ±0.2% modulation
in addition to this average null level. The isotropic astrophysical null is indicative of circumstellar emission dominated
by an azimuthally extended source, possibly a halo or one or more rings of dust. The modest azimuthal variation may be
explained by some skewness or anisotropy of the spatially-extended source, e.g. with an elliptical or spiral geometry, or
clumping, but it could also be due to the presence of a point-source located at a separation of ~120 mas (17AU) and
carrying ~6*10-3 of the stellar flux.
The vortex coronagraph has already enabled high-contrast observations very close to bright stars on large ground-based telescopes, and it also has great potential for use on coronagraphic space missions aimed at exoplanet detection and characterization. As such, demonstrations of vortex coronagraph performance have recently been carried out in JPL’s High Contrast Imaging Testbed. Some of our recent results are presented here, including the suppression of a monochromatic, single-polarization point-source to below the 10-9 level over a dark hole covering both the 2-7 λ/D and 3-8 λ/D regions, as well as the suppression of a 10% band of white-light to approximately the 10-8 level over a 3-8 λ/D dark hole.
The Vector Vortex Coronagraph (VVC) is one of the most attractive new-generation coronagraphs for ground- and
space-based exoplanet imaging/characterization instruments, as recently demonstrated on sky at Palomar and
in the laboratory at JPL, and Hokkaido University. Manufacturing technologies for devices covering wavelength
ranges from the optical to the mid-infrared, have been maturing quickly. We will review the current status of
technology developments supported by NASA in the USA (Jet Propulsion Laboratory-California Institute of
Technology, University of Arizona, JDSU and BEAMCo), Europe (University of Li`ege, Observatoire de Paris-
Meudon, University of Uppsala) and Japan (Hokkaido University, and Photonics Lattice Inc.), using liquid
crystal polymers, subwavelength gratings, and photonics crystals, respectively. We will then browse concrete
perspectives for the use of the VVC on upcoming ground-based facilities with or without (extreme) adaptive
optics, extremely large ground-based telescopes, and space-based internal coronagraphs.
Arrays of single mode fibers can be used to form segmented pupils of almost arbitrary geometry. Such pupil arrays can
be used both for interferometric imaging, for example by non-redundant aperture masking or in direct imaging systems
such as the phased array coronagraph. Achieving control over the optical coupling, phase and dispersion for fiber arrays
of reasonable size is a technological challenge. Progress has been made using a monolithic block of single mode fibers,
lens arrays and masks, and mirror arrays. On one testbed, arrays of up to 37 beamlets are being combined to form a
single image. On a second testbed, control of dispersion between fibers of slightly different length is being evaluated.
The combination of the techniques being demonstrated has a range of potential uses in astronomy. In this paper we
discuss the initial testbed results.
The optical vortex coronagraph has great potential for enabling high-contrast observations very close to bright stars, and
thus for reducing the size of space telescopes needed for exoplanet characterization missions. Here we discuss several
recent developments in optical vortex coronagraphy. In particular, we describe multi-stage vortex configurations that
allow the use of on-axis telescopes for high-contrast coronagraphy, and also enable the direct measurement of the
amplitudes and phases of focal plane speckles. We also briefly describe recent laboratory demonstrations of the optical
properties of the dual-stage vortex, and of the broadband performance of single stage vortex masks. Indeed, the
demonstrated performance of the vector vortex phase masks already in hand, ≈ 10-8, is approximately that needed for an
initial coronagraphic mission, such as an exoplanet explorer, aimed at detecting exozodiacal light and jovian exoplanets.
Single-mode optical fibers are playing an increasing role in astronomical interferometry, e.g., in high-accuracy visibility
measurements and in nulling interferometry. However, such observing modes typically involve only small numbers of
fibers. On the other hand, some recently proposed observing techniques call for arrays of single mode fibers coupled to
arrays of sub-apertures within a large telescope pupil. The concepts include pupil-masked visibility measurements (non-redundant
masking), pupil-sheared nulling interferometry, and coronagraphic imaging using a fiber-linked phased-array
of small optical telescopes. The latter arrangement may also be relevant to optical communications. Here we provide an
overview of a number of recent novel applications of single-mode fibers and single-mode fiber arrays.
The NIRCam instrument on the James Webb Space Telescope will have a Lyot coronagraph for high contrast imaging of
extrasolar planets and circumstellar disks at λ=2 - 5 μm. Half-tone patterns are used to create graded-transmission image
plane masks. These are generated using electron beam lithography and reactive ion etching of a metal layer on an antireflection
coated sapphire substrate. We report here on the manufacture and evaluation of the flight occulters.
A unique statistical data analysis method has been developed for reducing nulling interferometry data. The idea
is to make use of the statistical distributions of the fluctuating null depths and beam intensities to retrieve the
astrophysical null depth in the presence of fluctuations. The approach yields an accuracy much better than is
possible with standard data reduction methods, because the accuracy of the null depth is not limited by the
sizes of the phase and intensity errors but by the uncertainties on their statistical distributions. The result is
an improvement in the instrumental null depth measurement limit of roughly an order of magnitude. We show
in this paper that broadband null depths of 10-4 can be measured in the lab with our infrared Fiber Nuller
without achromatic phase shifters. On sky results are also dramatically improved, with measured contrasts up to
a couple of 10-4 with our instrument mounted on the Hale telescope at the Palomar Observatory. This statistical
analysis is not specific to our instrument and may be applicable to other interferometers.
The use of a rotating-baseline nulling interferometer for exoplanet detection was proposed several decades ago, but the
technique has not yet been fully demonstrated in practice. Here we consider the faint companion and exozodiacal disk
detection capabilities of rotating-baseline nulling interferometers, such as are envisioned for space-based infrared
nullers, but operating instead within the aperture of large single telescopes. In particular, a nulling interferometer on a
large aperture corrected by a next-generation extreme adaptive optics system can provide deep interferometric contrasts,
and also reach smaller angles (sub λ/D) than classical coronagraphs. Such rotating nullers also provide validation for an
eventual space-based rotating-baseline nulling interferometer. As practical examples, we describe ongoing experiments
with rotating nullers at Palomar and Keck, and consider briefly the case of the Thirty Meter Telescope.
We report on high-accuracy, high-resolution (< 20mas) stellar measurements obtained in the near infrared (
2.2 microns) at the Palomar 200 inch telescope using two elliptical (3m x 1.5m) sub-apertures located 3.4m
apart. Our interferometric coronagraph, known as the "Palomar Fiber Nuller" (PFN), is located downstream
of the Palomar adaptive optics (AO) system and recombines the two separate beams into a common singlemode
fiber. The AO system acts as a "fringe tracker", maintaining the optical path difference (OPD) between
the beams around an adjustable value, which is set to the central dark interference fringe. AO correction
ensures high efficiency and stable injection of the beams into the single-mode fiber. A chopper wheel and a fast
photometer are used to record short (< 50ms per beam) interleaved sequences of background, individual beam
and interferometric signals. In order to analyze these chopped null data sequences, we developed a new statistical
method, baptized "Null Self-Calibration" (NSC), which provides astrophysical null measurements at the 0.001
level, with 1 σ uncertainties as low as 0.0003. Such accuracy translates into a dynamic range greater than 1000:1
within the diffraction limit, demonstrating that the approach effectively bridges the traditional gap between
regular coronagraphs, limited in angular resolution, and long baseline visibility interferometers, whose dynamic
range is restricted to 100:1. As our measurements are extremely sensitive to the brightness distribution very
close to the optical axis, we were able to constrain the stellar diameters and amounts of circumstellar emission
for a sample of very bright stars. With the improvement expected when the PALM-3000 extreme AO system
comes on-line at Palomar, the same instrument now equipped with a state of the art low noise fast read-out near
IR camera, will yield 10-4 to 10-3 contrast as close as 30 mas for stars with K magnitude brighter than 6. Such
a system will provide a unique and ideal tool for the detection of young (<100 Myr) self-luminous planets and
hot debris disks in the immediate vicinity (0.1 to a few AUs) of nearby (< 50pc) stars.
The NIRCam instrument on the James Webb Space Telescope will provide coronagraphic imaging from λ =1-5 μm of
high contrast sources such as extrasolar planets and circumstellar disks. A Lyot coronagraph with a variety of circular
and wedge-shaped occulting masks and matching Lyot pupil stops will be implemented. The occulters approximate
grayscale transmission profiles using halftone binary patterns comprising wavelength-sized metal dots on anti-reflection
coated sapphire substrates. The mask patterns are being created in the Micro Devices Laboratory at the Jet Propulsion
Laboratory using electron beam lithography. Samples of these occulters have been successfully evaluated in a
coronagraphic testbed. In a separate process, the complex apertures that form the Lyot stops will be deposited onto
optical wedges. The NIRCam coronagraph flight components are expected to be completed this year.
We report the status of JPL and JDSU ongoing technological developments and contrast results of the vector
vortex coronagraph (VVC) made out of liquid crystal polymers (LCP). The first topological charge 4 VVC was
tested on the high contrast imaging testbed (HCIT) around 800 nm, under vacuum and with active wavefront
control (32x32 Xinetics deformable mirror). We measured the inner working angle or IWA (50% off-axis transmission)
at ~ 1.8λ/d. A one-sided dark hole ranging from 3λ/d to 10λ/d was created in polarized light, showing
a mean contrast of ~ 2 × 10-7 over a 10% bandwidth. This contrast was maintained very close in (3 λ/d) in
a reduced 2% bandwidth. These tests begin to demonstrate the potential of the LCP technology in the most
demanding application of a space-based telescope dedicated to extrasolar planet characterization. The main limitations
were identified as coming from incoherent sources such as multiple reflections, and residual chromaticity.
A second generation of improved masks tackling these issues is being manufactured and will be tested on the
HCIT in the coming months.
A rotating nulling coronagraph has been built for use on ground-based telescopes. The system is based on the concept of sub-aperturing the pupil of the telescope with two elliptical apertures and combining the resulting two input beams on a single-mode fiber. By a relative π phase shift of the beams, the starlight can be nulled and a relatively faint companion star can be detected. Rotation of the aperture mask on the telescope pupil results in a signal similar to that expected from a space-borne telescope system such as the proposed TPF/Darwin interferometer. The design of the nulling coronagraph and the ancillary systems that are needed, such as the fringe tracker, are described and the potential for observations on telescopes such as the Palomar 200" is discussed. Results of a nulling experiment using a single mode fiber as a beam combiner for broadband light between 1.50 μm and 1.80 μm are shown.
The basic advantage of single-mode fibers for deep nulling applications resides in their spatial
filtering ability, and has now long been known. However, and as suggested more recently, a single-mode
fiber can also be used for direct coherent recombination of spatially separated beams, i.e. in a
"multi-axial" nulling scheme. After the first successful demonstration of deep (<2e-6) visible
LASER nulls using this technique (Haguenauer & Serabyn, Applied Optics 2006), we decided to
work on an infrared extension for ground based astronomical observations, e.g. using two or more
off-axis sub-apertures of a large ground based telescope. In preparation for such a system, we built
and tested a laboratory infrared fiber nuller working in a wavelength regime where atmospheric
turbulence can be efficiently corrected, over a pass band (~1.5 to 1.8 micron) broad enough to
provide reasonable sensitivity. In addition, since no snapshot images are readily accessible with a
(single) fiber nuller, we also tested baseline rotation as an approach to detect off-axis companions
while keeping a central null. This modulation technique is identical to the baseline rotation
envisioned for the TPF-I space mission. Within this context, we report here on early laboratory
results showing deep stable broad-band dual polarization infrared nulls < 5e-4 (currently limited
by detector noise), and visible LASER nulls better than 3e-4 over a 360 degree rotation of the
baseline. While further work will take place in the laboratory to achieve deeper stable broad-band
nulls and test off-axis sources detection through rotation, the emphasis will be put on bringing such a
system to a telescope as soon as possible. Detection capability at the 500:1 contrast ratio in the K
band (~2.2 microns) seem readily accessible within 50-100 mas of the optical axis, even with a first
generation system mounted on a >5m AO equipped telescope such as the Palomar Hale 200 inch, the Keck, Subaru or Gemini telescopes.
The Terrestrial Planet Finder Interferometer (TPF-I) concept is being studied at the Jet Propulsion Laboratory and the TPF-I Planet Detection Testbed has been developed to simulate the detection process for an earthlike planet orbiting a star within about 15 pc. The testbed combines four beams of infrared light simulating the operation of a dual chopped Bracewell interferometer observing a star and a faint planet. This paper describes the results obtained this year including nulling of the starlight on four input beams at contrast ratios up to 250,000 to 1, and detection of faint planet signals at contrast ratios with the star of 2 million to 1.
We will report on the details of the ANITA instrument. This instrument is fundamentally a broadband antenna, which is arrayed and constructed in such a way as to be optimized for the detection and characterization of high-energy neutrino cascades. The requirement to maximize the detector view of the Antarctic ice fields implies low gain antennas yet the need for maximum sensitivity dictates using the highest gain possible. Since the Cherenkov signal increases quadratically at higher frequencies suggesting that the optimal selection is an antenna with constant gain as a function of frequency. The baseline design will be a linearly polarized log-periodic zigzag (LPZZ) antenna.
S. Barwick, James Beatty, David Besson, John Clem, Stephane Coutu, Michael DuVernois, Paul Evenson, Peter Gorham, Francis Halzen, Abram Jacobson, David Kieda, John Learned, Kurt Liewer, Stephen Lowe, Charles Naudet, Allen Odian, David Saltzberg, David Seckel
The ANITA project is designed to investigate ultra-high energy (>1017 eV) cosmic ray interactions throughout the universe by detecting the neutrinos created in those interactions. These high energy neutrinos are detectable through their interactions within the Antarctic ice sheet, which ANITA will use as a detector target that effectively converts the neutrino interactions to radio pulses. This paper will give an overview of the project including scientific objectives, detection description and mission design.
We report on results from 80 hours of livetime with the Goldstone Lunar Ultra-high energy neutrino Experiment (GLUE). The experiment searches for microwave pulses (width ≤ 10 ns) from the lunar regolith, appearing in coincidence at two large radio telescopes separated by 22 km and linked by optical fiber. Such pulses would arise from subsurface electromagnetic cascades induced by interactions of up-coming ~ 100 EeV neutrinos in the lunar regolith.
Triggering on a timing coincidence between the two telescopes significantly reduces the terrestrial interference background, allowing operation at the thermal noise level. No unambiguous candidates are yet seen. We report on limits implied by this non-detection, based on new Monte Carlo estimates of the efficiency.
KEYWORDS: Interferometers, Detection and tracking algorithms, Metrology, Space operations, Cameras, Visibility, Ferroelectric materials, Sensors, Servomechanisms, Control systems
StarLight, a NASA/JPL mission originally scheduled for launch in 2006, proposed to fly a two spacecraft visible light stellar interferometer. The Formation Interferometer Testbed (FIT) is a ground laboratory at JPL dedicated to validating technologies for StarLight and future formation flying spacecraft such as Terrestrial Planet Finder. The FIT interferometer achieved first fringes in February 2002. In this paper we present our status and review progress towards fringe tracking on a moving collector target.
Separated spacecraft interferometry is a candidate architecture
for several future NASA missions. The Formation Interferometer
Testbed (FIT) is a ground based testbed dedicated to the
validation of this key technology for a formation of two
spacecraft. In separated spacecraft interferometry, the residual
relative motion of the component spacecraft must be compensated
for by articulation of the optical components. In this paper, the design of the FIT interferometer pointing control system is described. This control system is composed of a metrology pointing loop that maintains an optical link between the two spacecraft and two stellar pointing loops for stabilizing the stellar wavefront at both the right and left apertures of the instrument. A novel feedforward algorithm is used to decouple the metrology loop from the left side stellar loop. Experimental results from the testbed are presented that verify this approach and that fully demonstrate the performance of the algorithm.
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