The Navy Precision Optical Interferometer (NPOI) is currently undergoing a fundamental renaissance in its functionality and capabilities. Operationally, its fast delay line (FDL) infrastructure is completing its upgrade from a VME/VxWorks foundation to a modern PC/RTLinux core. The Classic beam combiner is being upgraded with the New Classic FPGA-based backend, and the VISION beam combiner has been upgraded over this past summer with low-noise EMCCD cameras, resulting in substantial gains in sensitivity. Building on those infrastructure improvements, substantial upgrades are also in progress. Three 1-meter PlaneWave CDK1000 telescopes are being delivered to the site, along with their relocatable enclosure-transporters, and stations are being commissioned for those telescopes with baselines ranging from 8 meters to 432 meters. Baseline-wavelength bootstrapping will be implemented on the facility back-end with a near-infrared beam combiner under development. Collectively, these improvements mark substantial progress in taking the facility towards realizing its full intrinsic potential.
The New Classic instrument was built as a electronics and computer upgrade to the existing Classic beam combiner at the Navy Precision Optical Interferometer (NPOI). The classic beam combiner is able to record 32 of 96 available channels and has a data throughput limitation which results in a low duty cycle. Additionally the computing power of the Classic system limited the amount of fringe tracking that was possible. The New Classic system implements a high-throughput data acquisition system which is capable of recording all 96 channels continuously. It also has a modern high-speed computer for data management and data processing. The computer is sufficiently powerful to implement more sophisticated fringe-tracking algorithms than the Classic system, including multi-baseline bootstrapping. In this paper we described the New Classic hardware and software, including the fringe-tracking algorithm, performance, and the user interface. We also show some initial results from the first 5-station, 4-baseline bootstrapping carried out in January 2015.
A Michelson optical interferometer, such as an upgraded version of the Navy Precision Optical Interferometer, could image geosynchronous satellites (geosats) with resolution of roughly 1 m. Baselines that sample features as small as 0.2 m can be built, however, the fringes would be swamped by the resolved component. Recent observations have shown that small glints known as “glintchen,” aside from being a nuisance, serve to isolate and highlight the signal from these structures. Imaging of geosats during glintchen events can determine the dimensions of these structures and can also play a critical role in determining if these glintchen are due to a previously undetected companion satellite. An approach for performing this glint-aided imaging of geosats and the wealth of detail it would yield, is discussed.
We simulate the observations of a red supergiant star and an asteroid with an optical interferometer mounted on
a boom. This instrument has an advantage over more traditional interferometers because it significantly reduces
the number of reflections and surfaces, thus allowing one to combine a larger number of telescopes without a
significant loss of sensitivity. We investigate two telescope arrays distributed on a hexagonal pattern, one that
produces a non redundant coverage of the uv-plane and one that produces a redundant coverage of the uv-plane.
These simulated observations are combined with traditional aperture synthesis techniques to reconstruct images
and determine the accuracy of these images relative to the original ones.
Geostationary satellites are generally too small to image at high resolution with conventional single-dish tele-
scopes. An alternative to a 100+ m diameter telescope is to use an optical/infrared interferometer consisting
of multiple smaller telescopes in an array configuration. In this paper we focus on what is required to achieve
the required signal-to-noise ratio to image. We will look at the signal-to-noise ratio required to track fringes on
satellites on multiple baselines, a pre-requisite to imaging.We will also look at how to achieve the required signal-
to-noise required for image reconstruction. We compare these performance specifications to the performance of
existing interferometers as well as that of a new interferometer concept optimized for satellite imaging.
Even the longest geosatellite, at 40 m, subtends only 0.2 arcsec (1 microradian). Determining structure and
orientation with 10 cm resolution requires a 90 m telescope at visual wavelengths, or an interferometer. We de-
scribe the application of optical interferometry to observations of complex extended targets such as geosatellites,
and discuss some of its challenges. We brie
y describe our Navy Optical Interferometer (NOI) group's eorts
toward interferometric observations of geosatellites, including the rst interferometric detection of a geosatellite.
The NOI observes in 16 spectral channels (550{850 nm) using up to six 12-cm apertures, with baselines (separa-
tions between apertures) of 16 to 79 m. We detected the geosatellite DirecTV-9S during glint seasons in March
2008 and March 2009, using a single 16 m baseline (resolution 1:6 m). Fringes on a longer baseline were too
weak because the large-scale structure was over-resolved. The fringe strengths are consistent with a combination
of two size scales, 1:3 m and & 3:5 m. Our near term NOI work is directed toward observing geosatellites with
three or more 10 to 15 m baselines, using closure phase measurements to remove atmospheric turbulence eects
and coherent data averaging to increase the SNR. Beyond the two- to three-year time frame, we plan to install
larger apertures (1.4 and 1.8 m), allowing observations outside glint season, and to develop baseline bootstrap-
ping, building long baselines from chains of short baselines, to avoid over-resolution while increasing maximum
resolution. Our ultimate goal is to develop the design parameters for dedicated satellite imaging interferometry.
The increase in the number of satellites and space debris in low Earth orbit (LEO) makes tracking these objects
and avoiding collisions a major endeavor. A particularly important issue is the determination of the altitude
of these objects, which in many cases is not known with a precision better than 1 km. Here we present the
idea of using simultaneous observations by 2 optical telescopes, separated by a few hundred km, to refine the
altitude measurement of these objects to a precision of 10 m. We discuss the requirements for such a system,
like aperture, timing precision, and the precision to which one needs to know the positions of the telescopes and
background stars.
Intensity interferometry, in which intensity fluctuations at separate apertures are measured and then correlated,
is an attractive technique for high angular resolution measurements because of its simplicity. There is no
need to transport light beams from the telescopes of the interferometer array to a beam combiner, and the
telescope optics need not be precise. Michelson interferometry, in which light beams are brought together
and the interference pattern is measured, is significantly more difficult, requiring precision optics and precise
pathlength control, but it has a great advantage in sensitivity, requiring milliseconds to make a detection that
might require hours with an intensity interferometer. However, for interferometry with a large number of array
elements, the sensitivity of Michelson interferometry suffers from the fact that the light beams must be shared
among many correlations, thereby reducing the sensitivity of each measurement. We explore these and other
influences on the relative sensitivities of these techniques to determine under what circumstances, if any, their
sensitivities become comparable.
We simulate observations of geostationary satellites using different optical interferometer array configurations.
We test several array designs, including the typical Y shaped array, a couple of circular arrays, telescopes mounted
on a linear movable boom, and a couple of arrays of 30 telescopes on a non redundant and a redundant hexagonal
grid. We use aperture synthesis techniques to reconstruct images from the simulated observations. We compared
the performance and reliability of the different arrays, and find that the image quality increases with the number
of telescopes being used. We also find that short baselines, with lengths of ~2m are needed in order to recover the
large scale structure of the satellite. Some of the best results are produced by the non redundant and redundant
arrays on a hexagonal grid. Considering that the satellite appearance changes with illumination, the boom array
is not a good design, since it requires too much time to observe at different angles.
KEYWORDS: Interferometers, Satellites, Telescopes, Optical fibers, Wavefront sensors, Signal to noise ratio, Space telescopes, Sensors, Interferometry, Imaging systems
This paper presents the results of a study designed to test the feasibility of imaging satellites in geostationary
orbit from the ground. We argue that the instrument should be an interferometer consisting of > 30 telescopes
mounted on a common, steerable boom. Light from the telescopes is fed to the beam combiner with optical
fibers. The delays are equalized by steering the boom and stretching the fibers. The feed system and delay lines
are replaced with single mode fibers.
This system should be better throughput than the optical interferometers in use today and should be able
to reach the sensitivity needed to image these targets with meter-scale telescopes. Calculations supporting this
claim and a system design are presented.
We report a tentative interferometric detection of an earth-orbiting artificial satellite using optical interferometry. We
targeted four geosynchronous communications satellites with the Navy Prototype Optical Interferometer (NPOI) near
Flagstaff, AZ, and obtained interferometric fringes on one of them, DIRECTV-9S. We used an east-west 15.9-meter
baseline of the NPOI and took data in 16 spectral channels covering the 500-850 nm wavelength range. Observations
took place during the "glint season" of 28 February to 3 March 2008, when the geometry of the solar panel arrays and the
Sun's position creates glints as bright as 2nd magnitude of a few minutes' duration each night. We detected fringes on
the satellite at approximately the 2 σ level on 1 March at magnitude 4.5. Subsequent analysis shows that the fringe
amplitudes are consistent with a size scale of 2 meters (50 nanoradians at geosynchronous orbit) in an east-west
direction. This detection shows that interferometric detection of satellites at visual wavelengths is possible, and suggests
that a multi-baseline interferometer array tailored to the angular size and brightness of geosynchronous satellites could
lead to images of these satellites.
In this paper we will discuss the current status of coherent integration with the Navy Prototype Optical Interferometer
(NPOI). Coherent integration relies on being able to phase reference interferometric measurements, which in turn relies on making measurements at multiple wavelengths. We first discuss the generalized group-delay approach, then the meaning of the resulting complex visibilities and then demonstrate how coherent integration
can be used to perform very precision measurement of stellar diameters. The phase of the complex visibility is
particularly attractive as a data product because it is not biased in the same way as visibility amplitudes. We
discuss the relative SNR of triple-product phases and single-baseline phases. We then demonstrate how singlebaseline
phases can be used to make accurate measurements of magnitude differences and separations of binary stars.
We present the results of Navy Prototype Optical Interferometer observations of the binary stars θ2 Tauri and
HR7955. These data are reduced using standard methods, as well as coherent integration, and were fitted using
three different methods to measure the separation and position angle of the components, and their magnitude
differences. We used the traditional technique of fitting the V2's, triple amplitudes and triple phases, we also
fitted the baseline phases obtained through coherent integration, and measured the separation of the components
directly on images reconstructed using complex visibilities and phase self calibration. We find that fitting baseline
phases produces the highest precision. The results obtained from imaging are similar to these, although with
higher uncertainties, while the traditional method has the lowest precision. We attribute this result to the fact
that the traditional method combines multiple measurements, e.g. triple phases, thus increasing the errors and
reducing the amount of information that can be fitted. We also obtain a preliminary fit to the orbit of HR7955.
We have detected a satellite via optical interferometry for the first time, using a 16 m baseline of the Navy
Prototype Optical Interferometer (NPOI) to observe the geostationary communications satellite DirecTV-9S
during the "glint" seasons of February-March 2008 and 2009 when the sun-satellite-NPOI geometry was favorable
for causing specular reflections from geostationary satellites. We used the US Naval Observatory Flagstaff
Station 1 m telescope to generate accurate positions for steering the NPOI. Stars are the easiest targets for
optical/infrared interferometers because of their high surface brightness. Low surface brightness targets are
more difficult: if they are small enough not to be resolved out by typical baselines, they are likely to be too faint
to produce detectable fringes in an atmospheric coherence time. The 16 m NPOI baseline, the shortest available
at the time of our observations, resolves out structures larger than ~ 1.5 m at the geostationary distance, while
a typical size for the solar panel arrays is 2 m x 30 m. Our detection indicates that a small fraction of the
satellite glinted, not surprising given that the solar panels are not accurately flat. Our fringe data are consistent
with a two-component image consisting of a 1 to 1.3 m higher surface brightness component and a significantly
larger lower surface brightness component. The brightness of the glints (2.m 4 and ~ 1.m 5 for the two detections in March 2009) and the size scale suggest that the compact component has an albedo of 0.06 to 0.13, while the
larger-scale component is much darker, if circular geometry is assumed.
We report an interferometric detection of an earth-orbiting artificial satellite using optical interferometry. We targeted
four geosynchronous communications satellites with the Navy Prototype Optical Interferometer (NPOI) near Flagstaff,
AZ, and obtained interferometric fringes on one of them, DIRECTV-9S. We used an east-west 15.9-meter baseline of
the NPOI and took data in 16 spectral channels covering the 500-850 nm wavelength range. Observations took place
during the "glint season" of 28 February to 3 March 2008, and then again in February - March 2009, when the geometry
of the solar panel arrays and the Sun's position creates glints as bright as 2nd magnitude of a few minutes' duration each
night. We detected fringes on the satellite at approximately the 2 sigma level on 1 March at magnitude 4.5. Subsequent
analysis shows that the fringe amplitudes are consistent with a size scale of 2 meters (50 nanoradians at GEO) in an east-west
direction. This detection shows that interferometric detection of satellites at visual wavelengths is possible, and
suggests that a multi-baseline interferometer array tailored to the angular size and brightness of geosynchronous
satellites could lead to images of these satellites.
In this paper we will discuss the current status of coherent integration with the Navy Prototype Optical Interferometer
(NPOI).1 Coherent integration relies on being able to phase reference interferometric measurements,
which in turn relies on making measurements at multiple wavelengths.We first discuss the generalized group-delay
approach, then the meaning of the resulting complex visibilities and then demonstrate how coherent integration
can be used to perform very precision measurement of stellar properties. For example, we demonstrate how we
can measure the diameter of a star to a precision of one part in 350, and measure properties of binary stars. The
complex phase is particularly attractive as a data product because it is not biased in the same way as visibility
amplitudes.
Recovering images from optical interferometric observations is one of the major challenges in the field. Unlike
the case of observations at radio wavelengths, in the optical the atmospheric turbulence changes the phases on
a very short time scale, which results in corrupted phase measurements. In order to overcome these limitations,
several groups developed image reconstruction techniques based only on squared visibility and closure phase
information, which are unaffected by atmospheric turbulence. We present the results of two techniques used by
our group, which employed coherently integrated data from the Navy Prototype Optical Interferometer. Based
on these techniques we were able to recover complex visibilities for several sources and image them using standard
radio imaging software. We describe these techniques, the corrections applied to the data, present the images of
a few sources, and discuss the implications of these results.
The instrumental status of the Navy Prototype Optical Interferometer (NPOI) since the last SPIE meeting in 2006 is
summarized, along with the results of the current science programs. The commissioning of new stations and plans for
greatly increased telescope apertures are discussed, along with other instrumentation upgrades. Recent results in the
areas of wide-angle astrometry, binary stars, physical modeling of the circumstellar disks of early-type stars,
improvements in coherent averaging, and phase-reference imaging are also reviewed.
In this paper we use coherently integrated visibilities (see separate paper in these proceedings1) to measure the
properties of binary stars. We use only the phase of the complex visibility and not the amplitude. The reason
for this is that amplitudes suffer from the calibration effect (the same for coherent and incoherent averages) and
thus effectively provide lower accuracy measurements. We demonstrate that the baseline phase alone can be used
to measure the separation, orientation and brightness ratio of a binary star, as a function of wavelength.
We report on the results of an experiment to characterize the fringe scanning stroke on the Navy Prototype
Optical Interferometer (NPOI) Fast Delay Line (FDL) strokes. The measurements were carried out during three
days April 11-13, 2005 at the NPOI site near Flagstaff, AZ. The NPOI uses a heterodyne metrology laser system
in its operations. It consists of a HeNe laser with a 2 MHz heterodyne component generated by an Acousto-Optic
Modulator (AOM). One polarization is used as the 2 MHz clock, and the other is sent through the feed system
twice and bounces off the piezo stroke modulators. We sampled both signals at 50 MHz, and obtained stroke
and cart combined motion at the frequency of the stroke modulated 2 MHz heterodyne signal. By counting
zero-crossings in the reference and feed system signals, a rough position (to a wavelength) can be obtained. This
can be further refined to the few-nanometer level by measuring the relative phases of the reference and feed
system signals. This results in approximately 4000 positions measurements per 2 ms stroke with a precision of
approximately 1 nm. We recorded stroke positions for approximately 500 strokes (1 s), for all but one of the six
FDLs, under a variety of conditions: different stroke amplitudes, different cart speeds, and different cart positions
in the FDLs. We then analyzed these data from a total of 100 tests to understand the deviation of the actual
stroke from the ideal stroke. We found that the mean stroke differs from the ideal stroke, and that consecutive
strokes differ from each other. We computed the effect of the non-ideal stroke on the science data. A non-ideal
stroke results in leakage of fringe power between fringe frequencies. This leakage is not significant during most
normal operations of the NPOI. However, when the squared visibilities of baselines on the same spectrograph
differ by large amounts (a factor of 10), care should be taken. Ideally, High- and low-visibility baselines should
be placed on different spectrographs.
We present the results of differential phase experiments done with data from the Navy Prototype Optical Interferometer (NPOI). We take advantage of the fact that this instrument simultaneously records 16 spectral channels in the wavelength range 550-850nm, for multiple baselines. We discuss the corrections applied to the data, and show the results obtained for Vega and the Be star β Lyrae.
We report on experiments in multi-wavelength phase referencing using the Navy Prototype Optical Interferometer (NPOI). In these experiments we use the unique capability of the NPOI to simultaneously observe 16 spectral channels covering 512-850 nm on multiple baselines simultaneously. We present observations of the well-known Be star ζ Tauri using custom filters which allow us to isolate the Hα line in a single spectral channel while the other channels observe the stellar continuum. Since the central star is unresolved, we can use the data in the continuum channels to calibrate the spectral line data. Using the phase information recovered in this way, it is possible for the first time to use standard techniques to construct simple images of the line-emitting region around the star.
Atmospheric turbulence is a major impediment to ground-based optical interferometry. It causes fringes to move
on ms time-scales, forcing very short exposures. Because of the semi-random phase shifts, the traditional approach
averages exposure power spectra to build signal-to-noise ratio (SNR). This incoherent average has two problems:
(1) A bias of correlated noise is introduced which must be subtracted. The smaller the visibility/the fainter the
target star, the more diffcult bias subtraction becomes. SNR builds only slowly in this case. Unfortunately, these
most difficult small visibility baselines contain most of the image information. (2) Baseline phase information is
discarded. These are serious challenges to imaging with ground based optical interferometers. But if we were able
to determine fringe phase, we could shift and integrate all the short exposures. We would then eliminate the bias
problem, improve the SNR, and we would have preserved most of the phase information. This coherent averaging
becomes possible with multi-spectral measurements. The group delay presents one option for determining phase.
A more accurate approach is to use a time-dependent model of the fringe. For the most interesting low-visibility
baselines, the atmospheric phase information can be bootstrapped from phase determinations on high-visibility
baselines using the closure relation. The NPOI, with 32 spectral channels and a bootstrapping configuration,
is well-suited for these approaches. We will illustrate how the fringe modeling approach works, compare it to
the group-delay approach, and show how these approaches can be used to derive bias-free visibility amplitude
and phase information. Coherent integration provides the highest signal-to-noise (SNR) improvement precisely
in the situations where SNR builds most slowly using incoherent averaging. Coherent integration also produces
high-SNR phase measurements which are calibration-free and thus have high real uncertainties as well. In this
paper we will show how to coherently integration on NPOI data, and how to use baseline visibilities and calibrate coherently integrated visibility amplitudes.
The technical status of the Navy Prototype Optical Interferometer (NPOI) since the last
SPIE meeting is summarized along with the current science programs. The instrument is
operated in an automatic observational mode, obtaining over 10,000 stellar observations
in the period, June 2004 through March 2006. The scientific program has been directed
at astrometry, TPF candidate stars, binary stars and other interesting targets such as Be
stars. A significant database of NPOI observations obtained in 1997-2004 is being
analyzed for binaries and single stars such as rapid rotating stars: Altair and Vega.
We describe recent science projects that the Navy Prototype Optical Interferometer (NPOI) scientific staff and collaborators are pursuing. Recent results from the wide angle astrometric program and imaging programs (rapid rotators, binaries and Be stars) will be summarized. We discuss some of the technology that enables the NPOI to operate routinely as an observatory astronomical instrument.
We have enhanced the spectral resolution of the Navy Prototype Optical Interferometer (NPOI) at the H-alpha line to 3 nm (FWHM). We use customized filters that suppresses light in the ~600-725 nm window except for light at the H-alpha wavelength (656.3 nm). The bands shortward of 600 nm and longward of 725 nm are used for fringe tracking and for calibrating the system fringe visibility. We have used these filters to observe H-alpha emission from circumstellar material around Be stars. Closure phases from our initial observations of the Be star zeta Tau with three array elements suggest that the H-alpha emission is not centered on the star. We will show these three-element results, as well as recently-acquired data from the NPOI using 4, 5, and 6 stations.
The Navy Prototype Optical Interferometry (NPOI) group has started an astrometric search for planets in binary star systems based on the idea of using the binary components as position references for one another and looking for deviations from Keplerian motion.
Our search will complement the radial velocity (vR) searches in three ways. We will observe stars of all spectral types; vR searches are limited to the FGKM range, where stars exhibit narrow spectral lines. We will search for planets in relatively large orbits (more than about 4 AU) where our method is most sensitive; vR searches are most sensitive to close-in planets. Finally, we will examine binary star systems, which with a few exceptions have been excluded from vR surveys.
Our targets are binaries with both components in the interferometric field of view, producing a periodic variation in the fringe visibility (V2) across the (u,v) plane. Past NPOI results from closer binaries (separations in the tens of mas) show residuals of tens of microarcseconds about the best-fit orbits. The larger separations we are observing produce more V2 oscillations across the (u,v) plane, offering the possibility of higher precision. We discuss the level of precision in test observations and the steps that will be needed to convert precision into accuracy.
At the Navy Prototype Optical Interferometer (NPOI), during stellar fringe acquisition and tracking, optical stations along the NPOI vacuum line array remain in passive mode. Optical drift amplitude and rate must remain below certain limits lest stellar acquisition and fringe tracking become unachievable. Subsequent to each observation, relay mirrors are reconfigured within the long delay line stations to provide appropriate constant delays. The placement of these mirrors must be reliable and repeatable within certain tolerances. We describe the results of drift tests conducted on the current long delay line stations.
At the Navy Prototype Optical Interferometer (NPOI) we have developed a two-stage method for preparation and installation of the optical feed relay stations (elevators). This method reduces contamination, increases consistency, and allows greater management in testing and upgrades. In stage one, we prepare a pre-alignment facility in a laboratory. Using this facility we accurately position the feed stations, internal optics and detector optics relative to the NPOI array line-of-sight. The feed station is cleaned, assembled, internally aligned, tested and placed in its vacuum canister. It is stored under vacuum until transported to the array. In stage two, we align the station on the array by global five-axis adjustments of the vacuum canister. No further independent internal alignments are necessary. The canister is continuously under vacuum during global alignments. We describe the methodology and techniques for installing the optical feed stations.
We have developed a method for performing long coherent integrations
with the Navy Prototype Optical Interferometer (NPOI), which is based
on fitting a model fringe pattern to the NPOI data frames. The
procedure is quite computationally intensive, but gives a better
estimation of the phase than the conventional method of location the
peak of the group delay power. We mention briefly some of the most
important past work on coherent integration, and then describe our
method. We conclude that the fitting approach produces a phase with
fewer outliers than the Fourier-transform group delay approach. We
show how the instrumental squared visibility varies as a function of
the fringe model used, and show that it provides a better SNR than the
FT method. The phase determination will always be imperfect, and thus
cause a reduction in the visibility amplitude relative to the true
instrumental visibility. We illustrate a method for calibrating the
visibility amplitude. With long coherent integrations the phase of the
visibility can be extracted. We show examples of visibility phases and
how to correct them for phase variations in the instrument. Finally,
we illustrate a method for measuring stellar diameters very precisely,
to one part in at least several hundred.
Previous work by Hindsley and Mozurkewich (2001) showed that analysis of the Modulation Transfer Function (MTF) demonstrated the proportionality of signal-to-noise in a sparse aperture to the fill factor of the aperture. Analysis of the MTR also could enumerate the noise amplification characteristics of particular sparse apertures. However, such image quality metrics as the General Image Quality Equation (GIQE) also include edge effects, basically due to ringing and reduction in the edge sharpness. Here we report on our analysis of the MTF in order to quantify the relationship between the other terms in the GIQE and the structure of the MTF. We find that, for a fixed amount of optical surface, the image quality will improve with decreasing fill fraction due to an increase in resolution. Apodization of the Wiener Filter used to restore the image, as advocated by Hindsley and Mozurkewich, does not result in an improved image quality; use of the traditional unapodized Wiener Filter is highly favored. While the GIQE does not appear very sensitive to input signal-to-noise ratio (SNR), the input SNR does limit the ability to successfully reconstruct the image and is the ultimate limiting constraint on the fill fraction.
We review the theory of rotating stars, first developed 80 years ago. Predictions include a specific relation between shape and angular velocity and between surface location and effective temperature and effective gravity. Seen at arbitrary orientation rapidly rotating stars will display ellipsoidal shapes and possibly quite asymmetric intensity distributions. The flattening due to rotation has recently been detected at PTI and VLTI. With the increasing baselines available in the visible and the implementation of closure phase measurements at the NPOI it is now possible to search for the surface brightness effects of rotation. Roche theory predicts only large scale deviations from the usual centro-symmetric limb-darkened models, ideal when the stellar disks are only coarsely imaged as now. We report here observations of Altair and Vega with the NPOI using baselines that detect fringes beyond the first Airy zero in both objects. Asymmetric, non-classical intensity distributions are detected. Both objects appear to be rotating at a large fraction of their breakup velocity. Vega is nearly pole on, accounting for its low apparent rotational velocity. Altair's inclination is intermediate, allowing high S/N detection of all the predicted features of a Roche spheroid. We describe how these objects will test this fundamental theory and how Vega's role as a standard will need reinterpretation.
We describe the development of a portable NRL seeing monitor which consists of a 12 inch Meade f/10 telescope with a Dalsa Cad6 260x260 camera having 10 micron pixels. This seeing monitor is capable of up to 700 frames per second. We have three different techniques to measure Fried's r0 parameter: full aperture, two-hole mask, and two-hole mask with in-line intensifier. For the observations done at the Anderson Mesa, Arizona site in January-July 2004, we present comparison of Fried's r0 obtained. Calibration, observing techniques, and data analysis techniques are described. Comparison of the three different techniques is discussed.
The Navy Prototype Optical Interferometer has recently been equipped with specially-designed filters that pass Hα emission in a 2.5 nm band, suppress the continuum 50 nm to either side, and pass the continuum further from the Hα line. These filters allow fringe tracking on continuum light while taking data at Hα. Five- and six-aperture NPOI configurations have also been implemented recently. The improvement in U-V coverage with these configurations promises greater image fidelity in multi-spectral imaging as well as in specific lines, such as the very interesting Hα line. Using an array simulator operating in the AIPS++ environment, we simulate observations of Hα emission, assuming approximate source structure taken from earlier work in the literature. These simulations demonstrate the increased imaging capability of multi-aperture arrays and help define optimum Hα observation strategies.
We are now extending the studies of the angular diameters and limb darkening of K giant stars to K supergiants and dwarfs using the Navy Prototype Optical Interferometer (NPOI). Our goal is to compare our diameters with those predicted from model atmosphere calculations. The K supergiants, (epsilon) Peg, (zetz) Cep, and (xi) Cyg, as well as the K2 dwarf, (epsilon) Eri, have been observed with three elements of the astrometric sub-array. The diameters for giants are in good agreement with model predictions; while the results for supergiants agree less well, the extinction corrections make the comparison more uncertain. The measured diameter for (epsilon) Eri is significantly larger than that predicted by the models. These results show the power of the NPOI for testing fundamental astrophysical theory.
We examine our measured Cepheid diameters and the uncertainties as estimated from observations of calibrators and check stars, using (delta) Cephei, for which we have the most data, as our example. The mean limb-darkened diameter of (delta) Cep is 1.520 +/- 0.014 mas. The pulsation is only weakly seen, if at all, a tantalizing result that however does not determine the distance with useful precision. The longer baselines currently under construction will provide both high-precision diameters and a post-facto check of our uncertainty estimates.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.