Peter A Strittmatter

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Journals/Publications

• Doeleman, S. S., Fish, V. L., Schenck, D. E., Beaudoin, C., Blundell, R., Bower, G. C., Broderick, A. E., Chamberlin, R., Freund, R., Friberg, P., Gurwell, M. A., Ho, P. T., Honma, M., Inoue, M., Krichbaum, T. P., Lamb, J., Loeb, A., Lonsdale, C., Marrone, D. P., , Moran, J. M., et al. (2012). 1.3mm VLBI detections of M87 (Doeleman+, 2012). VizieR Online Data Catalog, 210, 33801.
• Doeleman, S. S., Fish, V. L., Schenck, D. E., Beaudoin, C., Blundell, R., Bower, G. C., Broderick, A. E., Chamberlin, R., Freund, R., Friberg, P., Gurwell, M. A., T., P., Honma, M., Inoue, M., Krichbaum, T. P., Lamb, J., Loeb, A., Lonsdale, C., Marrone, D. P., , Moran, J. M., et al. (2012). Jet-launching structure resolved near the supermassive black hole in M87. Science, 338(6105), 355-358.
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  PMID: 23019611;Abstract: Approximately 10% of active galactic nuclei exhibit relativistic jets, which are powered by the accretion of matter onto supermassive black holes. Although the measured width profiles of such jets on large scales agree with theories of magnetic collimation, the predicted structure on accretion disk scales at the jet launch point has not been detected. We report radio interferometry observations, at a wavelength of 1.3 millimeters, of the elliptical galaxy M87 that spatially resolve the base of the jet in this source. The derived size of 5.5 ± 0.4 Schwarzschild radii is significantly smaller than the innermost edge of a retrograde accretion disk, suggesting that the M87 jet is powered by an accretion disk in a prograde orbit around a spinning black hole.
• Duschl, W. J., & Strittmatter, P. A. (2012). The cosmogony of super-massive black holes. Journal of Physics: Conference Series, 372.
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  Abstract: We summarize our recent results on the evolution of super-massive black holes in the cores of galaxies. Our models are based on the viscous, Eddington-limited evolution of self-gravitating accretion disks. We find that, within this framework, one can explain the growth time scales and the luminosities of individual objects as well as the variation of these quantities for AGN with different black hole masses.
• Martin, H. M., Allen, R. G., Burge, J. H., Kim, D. W., Kingsley, J. S., Law, K., Lutz, R. D., Strittmatter, P. A., Su, P., Tuell, M. T., West, S. C., & Zhou, P. (2012). Production of 8.4 m segments for the Giant Magellan Telescope. Proceedings of SPIE - The International Society for Optical Engineering, 8450.
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  Abstract: Production of segments for the Giant Magellan Telescope is well underway at the Steward Observatory Mirror Lab. We report on the completion of the first 8.4 m off-axis segment, the casting of the second segment, and preparations for manufacture of the remaining segments. The complete set of infrastructure for serial production is in place, including the casting furnace, two 8.4 m capacity grinding and polishing machines, and a 28 m test tower that incorporates four independent measurement systems. The first segment, with 14 mm p-v aspheric departure, is by some measures the most challenging astronomical mirror ever made. Its manufacture took longer than expected, but the result is an excellent figure and demonstration of valuable new systems that will support both fabrication and measurement of the remaining segments. Polishing was done with a 1.2 m stressed lap for smoothing and large-scale figuring, and a series of smaller passive rigid-conformal laps for deterministic figuring on smaller scales. The interferometric measurement produces a null wavefront with a 3-element asymmetric null corrector including a 3.8 m spherical mirror and a computer-generated hologram. In addition to this test, we relied heavily on the new SCOTS slope test with its high accuracy and dynamic range. Evaluation of the measured figure includes simulated active correction using both the 160-actuator mirror support and the alignment degrees of freedom for the off-axis segment. © 2012 SPIE.
• Duschl, W. J., & Strittmatter, P. A. (2011). The cosmogony of supermassive black holes. Monthly Notices of the Royal Astronomical Society, 413(2), 1495-1504.
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  Abstract: We report calculations of the evolution, under Reynolds viscosity, of the massive gaseous accretion discs thought to form in the centres of galaxies as a result of major galactic mergers at early epochs. Starting with the formation of such a disc and the postulated existence of a low-mass 'seed' black hole, we focus on the mass accretion rate, and hence luminosity, LGC, of a putative supermassive black hole (SMBH) in the galactic centre. Our computations cover a range of initial disc mass, Md, 0, and outer radius, smax, 0, and have been carried out under the assumption that cannot exceed the Eddington limit and that any excess mass supplied from the disc is lost from the system. Our purpose is to understand the extent to which such a model can account for the evolution with redshift of the observed properties of active galactic nuclei (AGNs). We show that within this framework: (i) the initial mass supply rate from the disc increases with Md, 0 and compactness, adjusts rapidly (on a viscous time-scale) to its peak value and decreases steadily thereafter; (ii) peak SMBH mass accretion rate and hence luminosity occurs when the (decreasing) disc flow rate equals the (increasing) black hole (BH) Eddington rate and is proportional to the BH mass, MEddBH, at that juncture; (iii) the fractional disc mass lost during the Eddington-limited phase increases with Md, 0 and compactness so strongly that, for given (large) Md, 0, the peak BH luminosity and corresponding mass occurs for some intermediate value of smax, 0 so that MEddBH declines for more compact initial discs; (iv) SMBHs with mass MBH≥ 109M⊙ and luminosity LGC≥ 3 × 1013L⊙ can form in a time t < 109 yr as required by the most luminous high-redshift quasi-stellar objects but the Eddington-induced mass-loss renders unlikely the creation of BHs of comparable or greater mass or luminosity in significantly shorter times; (v) the most luminous quasars form and die at the earliest epochs while those of lower luminosity occur over successively longer periods ranging up to the present time; (vi) in general, AGNs that are at an early evolutionary phase accrete at or close to their Eddington rate but evolve into the sub-Eddington regime later on. The proposed scenario appears capable of accounting for many of the features of the observed quasar and AGN luminosity distribution with redshift and seems to be a natural consequence of the formation of massive central discs following major galaxy mergers. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
• Fish, V. L., Doeleman, S. S., Beaudoin, C., Blundell, R., Bolin, D. E., Bower, G. C., Chamberlin, R., Freund, R., Friberg, P., Gurwell, M. A., Honma, M., Inoue, M., Krichbaum, T. P., Lamb, J., Marrone, D. P., Moran, J. M., Oyama, T., Plambeck, R., Primiani, R., , E., A., et al. (2011). 1.3 mm wavelength VLBI of sagittarius A^*: Detection of time-variable emission on event horizon scales. Astrophysical Journal Letters, 727(2 PART II).
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  Abstract: Sagittarius A*, the ∼4 × 106 M ⊙ black hole candidate at the Galactic center, can be studied on Schwarzschild radius scales with (sub)millimeter wavelength very long baseline interferometry (VLBI). We report on 1.3 mm wavelength observations of Sgr A * using a VLBI array consisting of the JCMT on Mauna Kea, the Arizona Radio Observatory's Submillimeter Telescope on Mt. Graham in Arizona, and two telescopes of the CARMA array at Cedar Flat in California. Both Sgr A* and the quasar calibrator 1924-292 were observed over three consecutive nights, and both sources were clearly detected on all baselines. For the first time, we are able to extract 1.3 mm VLBI interferometer phase information on Sgr A* through measurement of closure phase on the triangle of baselines. On the third night of observing, the correlated flux density of Sgr A* on all VLBI baselines increased relative to the first two nights, providing strong evidence for time-variable change on scales of a few Schwarzschild radii. These results suggest that future VLBI observations with greater sensitivity and additional baselines will play a valuable role in determining the structure of emission near the event horizon of Sgr A*. © 2011. The American Astronomical Society.
• Doeleman, S. S., Weintroub, J., E., A., Plambeck, R., Freund, R., P., R., Friberg, P., Ziurys, L. M., Moran, J. M., Corey, B., Young, K. H., Smythe, D. L., Titus, M., Marrone, D. P., Cappallo, R. J., Bock, D. C., Bower, G. C., Chamberlin, R., Davis, G. R., , Krichbaum, T. P., et al. (2008). Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre. Nature, 455(7209), 78-80.
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  PMID: 18769434;Abstract: The cores of most galaxies are thought to harbour supermassive black holes, which power galactic nuclei by converting the gravitational energy of accreting matter into radiation. Sagittarius A* (Sgr A*), the compact source of radio, infrared and X-ray emission at the centre of the Milky Way, is the closest example of this phenomenon, with an estimated black hole mass that is 4,000,000 times that of the Sun. A long-standing astronomical goal is to resolve structures in the innermost accretion flow surrounding Sgr A*, where strong gravitational fields will distort the appearance of radiation emitted near the black hole. Radio observations at wavelengths of 3.5 mm and 7 mm have detected intrinsic structure in Sgr A*, but the spatial resolution of observations at these wavelengths is limited by interstellar scattering. Here we report observations at a wavelength of 1.3 mm that set a size of microarcseconds on the intrinsic diameter of Sgr A*. This is less than the expected apparent size of the event horizon of the presumed black hole, suggesting that the bulk of Sgr A* emission may not be centred on the black hole, but arises in the surrounding accretion flow. ©2008 Macmillan Publishers Limited. All rights reserved.
• Duschl, W. J., & Strittmatter, P. A. (2008). The cosmogony of super-massive black holes. ESO Astrophysics Symposia, 2008, 129-133.
• Krichbaum, T. P., Graham, D. A., Witzel, A., Zensus, J. A., Greve, A., Grewing, M., Bremer, M., Doeleman, S., Phillips, R. B., Rogers, A. E., Fagg, H., Strittmatter, P., & Ziurys, L. (2007). Towards the event horizon: High resolution VLBI imaging of nuclei of active galaxies. ESO Astrophysics Symposia, 2007, 189-190.
• Martin, H. M., Angel, J. R., Burge, J. H., Cuerden, B., Bavison, W. B., Johns, M., Kingsley, J. S., Kot, L. B., Lutz, R. D., Miller, S. M., Shectman, S. A., Strittmatter, P. A., & Zhao, C. (2006). Design and manufacture of 8.4 m primary mirror segments and supports for the GMT. Proceedings of SPIE - The International Society for Optical Engineering, 6273 I.
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  Abstract: The design, manufacture and support of the primary mirror segments for the GMT build on the successful primary mirror systems of the MMT, Magellan and Large Binocular telescopes. The mirror segment and its support system are based on a proven design, and the experience gained in the existing telescopes has led to significant refinements that will provide even better performance in the GMT. The first 8.4 m segment has been cast at the Steward Observatory Mirror Lab, and optical processing is underway. Measurement of the off-axis surface is the greatest challenge in the manufacture of the segments. A set of tests that meets the requirements has been defined and the concepts have been developed in some detail. The most critical parts of the tests have been demonstrated in the measurement of a 1.7 m off-axis prototype. The principal optical test is a full-aperture, high-resolution null test in which a hybrid reflective- diffractive null corrector compensates for the 14 mm aspheric departure of the off-axis segment. The mirror support uses the same synthetic floatation principle as the MMT, Magellan, and LBT mirrors. Refinements for GMT include 3-axis actuators to accommodate the varying orientations of segments in the telescope.
• Martin, H. M., Angel, J. R., Burge, J. H., Miller, S. M., Sasian, J. M., & Strittmatter, P. A. (2002). Optics for the 20/20 telescope. Proceedings of SPIE - The International Society for Optical Engineering, 4840, 194-205.
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  Abstract: We present a plan for making the optics of a 21 m telescope that builds on advances in mirror design and fabrication developed for the Large Binocular Telescope (LBT) and other large telescopes. The 21 m telescope, with a fast f/0.7 primary mirror made of only seven large honeycomb-sandwich segments and an adaptive secondary with matching segments, is much suffer than other designs and offers simpler and more accurate wavefront control. It can be a powerful stand-alone telescope, or one of a pair that move on a circular track to achieve coherent imaging with baselines up to 120 m (the 20/20 telescope). Each segment of the 21 m primary mirror is similar to an 8.4 m LBT primary, and each segment of the 2.1 m adaptive secondary mirror is similar to an LBT secondary. The off-axis segments of both mirrors can be made with the same methods and equipment currently used at the Steward Observatory Mirror Lab, and can be polished with the same stressed-lap polishing system used for the LBT mirrors. A change in algorithm to accommodate the asymmetric surface is required, but no new hardware development is needed because the lap bending is similar to that for the LBT mirrors. Each segment can be measured interferometrically, with a combination reflective and diffractive null corrector producing an accurate aspheric template wavefront and alignment references for the segments.
• Duschl, W. J., Strittmatter, P. A., & Biermann, P. L. (2000). A note on hydrodynamic viscosity and selfgravitation in accretion disks. Astronomy and Astrophysics, 357(3), 1123-1132.
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  Abstract: We propose a generalized accretion disk viscosity prescription based on hydrodynamically driven turbulence at the critical effective Reynolds number. This approach is consistent with recent re-analysis by Richard & Zahn (1999) of experimental results on turbulent Couette-Taylor flows. This new β-viscosity formulation is applied to both selfgravitating and non-selfgravitating disks and is shown to yield the standard α-disk prescription in the case of shock dissipation limited, non-selfgravitating disks. A specific case of fully selfgravitating β-disks is analyzed. We suggest that such disks may explain the observed spectra of protoplanetary disks and yield a natural explanation for the radial motions inferred from the observed metallicity gradients in disk galaxies. The β-mechanism may also account for the rapid mass transport required to power ultra luminous infrared galaxies.
• Hill, J. M., Angel, J. R., Lutz, R. D., Olbert, B. H., & Strittmatter, P. A. (1998). Casting the first 8.4 meter borosilicate honeycomb mirror for the large binocular telescope. Proceedings of SPIE - The International Society for Optical Engineering, 3352, 172-181.
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  Abstract: We report on the casting of the first 8.4 meter diameter borosilicate honeycomb mirror at the Steward Observatory Mirror Laboratory. This blank will become the world's largest monolithic glass telescope mirror, and is the first of two mirrors for the Large Binocular Telescope Project. The honeycomb 8.4 meter mirror was cast from 21 tons of E6 borosilicate glass manufactured by Ohara. This glass is melted into a mold constructed of aluminosilicate fiber to produce a honeycomb structure with roughly 20% of solid density. The 1662 hexagonal voids that form the honeycomb structure are produced by ceramic fiber boxes bolted to the bottom of the mold with SiC bolts. The furnace rotates at 6.8 rpm during the casting process to produce the F/1.14 paraboloid on the front surface. This shaping minimizes the amount of glass which must be removed during the grinding process. The front faceplate of the mirror will be 28 mm thick after generating and the back faceplate will be 25 mm. The overall thickness of the finished honeycomb blank is 89 cm at the outer edge and 44 cm at the central hole. The first 8.4 meter mirror blank was cast in January 1997. During the casting, two tons of glass leaked from the mold inside the spinning furnace. After a three month annealing cycle the furnace was opened for inspection. As a result of the leakage about 2 square meters of the faceplate near one edge of the mirror was too thin to be polished. In April 1997, an additional two tons of glass was loaded on top of the intact honeycomb structure. In June 1997, after heating slowly back to the annealing temperature, this extra glass was flash melted onto the front of the blank to assure that the faceplate was of sufficient thickness. After a further three month annealing cycle, the furnace was re-opened to reveal a superb casting with low bubble content and little trace of the fusion boundary. The blank has been removed from the furnace using a fixture glued to the upper surface of the blank. It will soon be stripped of its mold material in preparation for polishing.
• Martin, H. M., Allen, R. G., Angel, J. R., Burge, J. H., Davison, W. B., DeRigne, S. T., Dettmann, L. R., Ketelsen, D. A., Kittrell, W. C., Miller, S. M., Strittmatter, P. A., & West, S. C. (1998). Fabrication and measured quality of the MMT primary mirror. Proceedings of SPIE - The International Society for Optical Engineering, 3352, 194-204.
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  Abstract: The primary mirror for the Multiple Mirror Telescope Conversion is the first 6.5 m honeycomb sandwich mirror cast and polished by the Steward Observatory Mirror Lab. We describe the optical fabrication and testing of the f/1.25 paraboloid, and present the final measurements of figure accuracy and inferred image quality. Figuring was performed with a 1.2 m stressed lap-which bends under active control to match the local curvature of the optical surface-and a variety of small passive tools. The mirror was pressurized to compensate for polishing loads and thereby eliminate print-through of the honeycomb structure. The net results is a smoother surface on scales of 5-20 cm than has been achieved on previous honeycomb sandwich mirrors. The figure was measured with IR and visible interferometers, using refractive null correctors to compensate 810 microns of aspheric departure. The final measurements were used to calculate synthetic stellar images in a variety of seeing conditions.
• Roger, J., Hill, J. M., Strittmatter, P. A., Salinari, P., & Weigelt, G. (1998). Interferometry with the large binocular telescope. Proceedings of SPIE - The International Society for Optical Engineering, 3350, 881-889.
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  Abstract: The Large Binocular Telescope (LBT) has been designed for optical/infrared interferometry that combines high sensitivity and resolution. Key scientific projects will be deep, wide field infrared images of the Hubble Deep Field, with nearly ten times the resolution of the Hubble telescope, and the study of planets and dust in extra-solar systems, from their formation onward. A basic requirement for interferometry of faint objects is that the aberrations across the two 8.4 m telescopes be corrected for atmospheric phase errors. This will be done at the telescopes' secondary mirrors, so as to preserve the very low emissivity of the direct beam combination optics. Sodium lasers projected co-axially from above each secondary will allow wavefront sensing for correction of even the faintest objects. The two telescopes are rigidly mounted close together on a single alt-azimuth mount, to cover a large fraction of the u-v plane in a single exposure, with baselines continuous from 0 to 23 m. Field rotation during the night completes the cover, to allow recovery of images with the full resolution of a diffraction limited 23 m telescope. The beam combining optics will be cryogenically cooled to maintain the very low thermal background from only 3 warm reflections in total (primary, adaptive secondary, tertiary). For wide field imaging, the beams will be combined and stabilized so that in a long exposure every source across a ∼ 1 arcminute field is crossed by nterference fringes. From a set of such exposures the resultant deep image will have a resolution 0.02 arcsec in the 2.2.μm K band. For high contrast studies of exo-planetary systems, a Bracewell nulling system will be used with superposition by division of amplitude, for 99.99% suppression of the stellar radiation. ©2004 Copyright SPIE - The International Society for Optical Engineering.
• Strittmatter, P. A. (1996). Mt Graham and the environment [3]. Nature, 379(6568), 765-.
• Walsh, B., Angel, R., & Strittmatter, P. (1994). Endangered telescopes or species?. Nature, 372(6503), 215-216.
• Strittmatter, P. (1990). Columbus Project telescope. Proceedings of SPIE - The International Society for Optical Engineering, 1236 pt 1, 71-84.
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  Abstract: The design for the Columbus binocular telescope has been completed and the project is now proceeding to the construction phase. The two 8 meter f/1.2 borosilicate honeycomb mirrors will give an effective collecting area of 11.3 m and a baseline of 22 m for interferometry. The optics are supported on an exceedingly compact and rigid 'C-ring' mount with a lowest eigen frequency of around 10 Hz. The system will be housed in a corotating enclosure and will be located on Mt. Graham in southeastern Arizona. Instrumentation priorities have been established for the telescope and conceptual designs are now under development. The Columbus Project is a collaboration between the Osservatorio Astrofisico di Arcetri, Italy, the Ohio State University and the University of Arizona.
• Angel, J. R., Hill, J. M., Martin, H. M., & Strittmatter, P. A. (1989). Recent progress on the Columbus Project and the Miror Laboratory program. Astrophysics and Space Science, 160(1-2), 55-70.
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  Abstract: This paper summarizes recent advances on the Columbus Project telescope and in the University of Arizona Mirror Lab. The Columbus telescope structure has been re-optimized to allow rapid changes between foci, while still maintaining high rigidity. Room has been made to translate secondary and tertiary spiders out of the light path to the center. A bill allowing construction of the telescope on Mt. Graham, Arizona, has been passed by Congress and signed into law. Two alternative enclosure designs, one with a co-rotating building and a second which opens like a flower, are being explored. A common baseline design for the 8 m honeycomb mirrors for both the Columbus and Magellan telescopes has been developed. It has stiffness comparable to that of the Palomar 200 inch mirror. The Mirror Lab has successfully cast two 3.5 m honeycomb blanks and expects to begin casting at the 6.5 and 8 m scale at the end of 1990. Interferometric tests of the Vatican f/1 1.8 m borosilicate honeycomb mirror show good stability of figure with the air jet ventilation system. A 60 cm stressed lap has been completed, and will be used to parabolize this mirror which is now polished as an f/1 sphere. Plans for a polishing facility to house two 8 m machines and a test tower are complete, with construction starting in April 1989. © 1989 Kluwer Academic Publishers.
• Strittmatter, P. A. (1988). Mt Graham Observatory [1]. Nature, 336(6197), 302-.
• Cromwell, R. H., Strittmatter, P. A., Allen, R. G., Hege, E. K., Kuehr, H., Marien, K. -., Funk, H. W., & Frank, K. (1985). PROXIMITY-FOCUSED IMAGE INTENSIFIER FOR ASTRONOMY.. Advances in Electronics and Electron Physics, 64 A, 77-92.
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  Abstract: Progress in the development of a proximity intensifier for astronomy is very encouraging. A few samples have now been produced that exhibit good blue response, resolution, gain, dark emission (when cooled), and freedom from field emission. Manufacturing yield of such samples is still low. In the next year we expect to see improved yield and performance through continued refinements. An important next step is to discover and eliminate the cause of lost counting efficiency, observed in several diode intensifiers.
• Drummond, J. D., Cocke, W. J., Hege, E. K., Strittmatter, P. A., & Lambert, J. V. (1985). Speckle interferometry of asteroids. I. 433 eros. Icarus, 61(1), 132-151.
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  Abstract: Analytic expressions for the semimajor and semiminor axes and an orientation angle of the ellipse projected by a triaxial ellipsoid (an asteroid) and of the ellipse segment cast by a terminator across the ellipsoid as functions of the dimensions and pole of the body and the asterocenteric position of the Earth and Sun are derived. Applying these formulae to observations of the Earth-approaching asteroid 433 Eros obtained with the speckle interferometry system of Steward Observatory on December 17-18, 1981, and January 17-18, 1982, the following dimensions are derived: (40.5 ± 3.1 km) × (14.5 ± 2.3 km) × (14.1 ± 2.4 km) Eros' north pole is found to lie within 14° of RA = 0h16m Dec. = +43° (ecliptic longitude 23°, latitude +37°). Other than knowing the rotation period of Eros, these results are completely independent of any other data, and in the main confirm the results obtained in the 1974-1975 apparition by other methods. These dimensions, together with a lightcurve from December 18, 1981, lead to a geometric albedo of 0.156 ± 0.010. A series of two-dimensional power spectra and autocorrelation functions of the resolved asteroid clearly show it spinning in space. © 1985.
• Beckers, J. M., Hege, E. K., & Strittmatter, P. A. (1984). OPTICAL INTERFEROMETRY WITH THE MMT.. Proceedings of SPIE - The International Society for Optical Engineering, 444, 85-91.
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  Abstract: By adjustment of the optical pathlengths of the MMT telescopes, it is possible to make the MMT into a phased array with a 680 cm baseline. The authors describe experiments in speckle interferometry and spectroscopy which have been done this way using 2 and 3 of the MMT telescopes. Planned adjustments are described of the optical configuration of the MMT to achieve coherent operation over a large field of view with all six telescopes phased simultaneously.
• Beckers, J. M., Hege, E., Low, F. J., McCarthy, D. W., & Strittmatter, P. A. (1984). USE OF THE MULTIPLE MIRROR TELESCOPE AS A PHASED ARRAY.. Proceedings of SPIE - The International Society for Optical Engineering, 440, 136-142.
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  Abstract: We summarize the experiments which have used the Multiple Mirror Telescope (MMT) subapertures as a phased array in the optical, infrared, and submillimeter spectrum regions. Those experiments exploit the unique, very high angular resolution of the MMT being equivalent to that of a conventional telescope 686 cm in diameter. The operation of the MMT as a phased array is not only important for obtaining high angular resolution but also for obtaining the higher detection sensitivity which results from the better discrimination against the sky emission background for infrared diffraction limited images. We describe future plans to make the MMT into a phased telescope.
• Hege, E. K., Cocke, W. J., Strittmatter, P. A., Worden, S. P., & Booth, W. C. (1984). HIGH-SPEED DIGITAL SIGNAL PROCESSING FOR SPECKLE INTERFEROMETRY.. Proceedings of SPIE - The International Society for Optical Engineering, 445, 469-476.
• Macklin, R. H., Hege, E. K., & Strittmatter, P. A. (1983). REAL-TIME PHOTOELECTRON EVENT-DETECTING VIDEO SYSTEM.. Proceedings of SPIE - The International Society for Optical Engineering, 359, 135-138.
• Hege, E. K., Hubbard, E. N., Drummond, J. D., Strittmatter, P. A., Worden, S. P., & Lauer, T. (1982). Speckle interferometric observations of Pluto and Charon. Icarus, 50(1), 72-81.
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  Abstract: We report speckle interferometric observations of Pluto and its moon (1978 P1) Charon obtained on 5 June 1980 with a single 1.8-m mirror of the Multiple Mirror Telescope. Our observations yield a separation of 0″.31 (±0″.05) between Pluto and Charon at position angle 285° (±7°) for JD 2444395.75. This result and other direct observations indicate an adjustment of +4.0 hr to the orbital epoch of R. S. Harrington and J. W. Christy [Astron.J.86, 442-443 (1981)]. Our observation, which represents the first resolution of the system near minimum separation, also suggests that the inclination of the orbit to the plane of the sky should be increased by 3°; this will delay the onset of the predicted eclipsee season by one apparition to 1984 or 1985. Our data are consistent with Pluto diameter 0″.14 (±0″.02) = 3000 (±400) km and Charon diameter 0″..05 (±0″.03) = 1100 (±600) km. © 1982.
• McCarthy, D. W., Strittmatter, P. A., Hege, E. K., & Low, F. J. (1982). PERFORMANCE OF THE MULTIPLE MIRROR TELESCOPE (MMT) - 8. MMT AS AN OPTICAL-INFRARED INTERFEROMETER AND PHASED ARRAY.. Proceedings of SPIE - The International Society for Optical Engineering, 332, 57-64.
• Carswell, R. F., & Strittmatter, P. A. (1973). Redshift of OH471. Nature, 242(5397), 394-395.
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  Abstract: THE purpose of this letter is to draw attention to the very high redshift, z = 3.40, of the QSO OH471. © 1973 Nature Publishing Group.
• Strittmatter, P. A. (1972). British astronomy. Nature, 239(5373), 475-.
• Burbidge, G. R., & Strittmatter, P. A. (1968). Pulsed radio sources. Nature, 218(5140), 433-434.
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  Abstract: The bursts of radio waves at decametric wavelengths emitted by Jupiter suggest a model for producing the signals from the pulsating radio sources. This mechanism includes polarization of the signals and structure within the pulses. © 1968 Nature Publishing Group.
• Saslaw, W. C., Faulkner, J., & Strittmatter, P. A. (1968). Rapidly pulsing radio sources. Nature, 217(5135), 1222-1227.
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  Abstract: The gravitational lens effect associated with a neutron star binary gives results which agree well with recent observations of a new class of rapidly pulsing radio sources. Further tests of the theory are proposed. © 1968 Nature Publishing Group.
• Strittmatter, P., Faulkner, J., & Walmsley, M. (1966). Evidence for a correlation between the position and red-shift of quasars [1]. Nature, 212(5069), 1441-1442.

Proceedings Publications

• Martin, H. M., Angel, J. R., Angeli, G., Burge, J. H., Gressler, W., Kim, D. W., Kingsley, J. S., Law, K., Liang, M., Neill, D., Sebag, J., Strittmatter, P. A., Tuell, M. T., West, S. C., Woolf, N. J., & Xin, B. (2016, July). Manufacture and final tests of the LSST monolithic primary/tertiary mirror. In Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II, Proc. SPIE 9912.
• Martin, H. M., Burge, J. H., Davis, J. M., Kim, D. W., Kingsley, J. S., Law, K., Loeff, A., Lutz, R. D., Merrill, C., Strittmatter, P. A., Tuell, M. T., Weinberger, S. N., & West, S. C. (2016, July). Status of mirror segment production for the Giant Magellan Telescope. In Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II, Proc. SPIE 9912.
• Doeleman, S., Fish, V. L., Schenck, D., Beaudoin, C., Blundell, R., Bower, G. C., Broderick, A. E., Chamberlin, R., Freund, R., Friberg, P., Gurwell, M. A., Ho, P. T., Honma, M., Inoue, M., Krichbaum, T., Lamb, J. W., Loeb, A., Lonsdale, C. J., Marrone, D. P., , Moran, J. M., et al. (2013, jan). Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87. In American Astronomical Society Meeting Abstracts, 221, #123.07.