RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

Meyer, R. D.; Horch, Elliott; Ninkov, Zoran; Altena, W. F. van; Rothkopf, Constantin A.

doi:10.1086/498222

Cited by 11 publications

(4 citation statements)

References 17 publications

(24 reference statements)

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“…Horch et al (2009) state that the 562 and 692 nm DSSI filters' central wavelengths are close to those of the V and R of the Johnson U BV RI system. For observations from the RIT-Yale Tip-tilt Speckle Imager (RYTSI) (Meyer et al 2006) reported in Horch et al (2010Horch et al ( , 2012, ∆550 measurements were adopted as ∆V , ∆698 were adopted as ∆R, and ∆754 nm measurements were adopted as ∆I. The ∆814 measurements reported in Reid et al (2001) were assumed to be ∆I.…”

Section: Deblending Photometrymentioning

confidence: 99%

The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc

Henry²,

et al. 2019

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We present results of the largest, most comprehensive study ever done of the stellar multiplicity of the most common stars in the Galaxy, the red dwarfs. We have conducted an all-sky volume-limited survey for stellar companions to 1120 M dwarf primaries known to lie within 25 pc of the Sun via trigonometric parallaxes. In addition to a comprehensive literature search, stars were explored in new surveys for companions at separations of 2 ′′ to 300 ′′ . A reconnaissance of wide companions to separations of 300 ′′ was done via blinking archival images. I−band images were used to search our sample for companions at separations of 2 ′′ to 180 ′′ . Various astrometric and photometric methods were used to probe the inner 2 ′′ to reveal close companions. We report the discovery of 20 new companions and identify 56 candidate multiple systems.We find a stellar multiplicity rate of 26.8±1.4% and a stellar companion rate of 32.4±1.4% for M dwarfs. There is a broad peak in the separation distribution of the companions at 4 -20 AU, with a weak trend of smaller projected linear separations for lower mass primaries. A hint that M dwarf multiplicity may be a function of tangential velocity is found, with faster moving, presumably older, stars found to be multiple somewhat less often. We calculate that stellar companions make up at least 17% of mass attributed to M dwarfs in the solar neighborhood, with roughly 11% of M dwarf mass hidden as unresolved companions. Finally, when considering all M dwarf primaries and companions, we find that the mass distribution for M dwarfs increases to the end of the stellar main sequence.

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Section: Deblending Photometrymentioning

confidence: 99%

The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc

Henry²,

et al. 2019

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“…In 2001, we began using a system exclusively designed for CCD-based speckle imaging, RYTSI, designed and built primarily by Reed Meyer, two of us (E.H. and W.vA.), and Zoran Ninkov (Meyer et al 2006). As we gained greater experience with this system, we began to push the limits of the device, including observing some binaries when they were known to be below the diffraction limit.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Observations of Binary Stars With the Differential Speckle Survey Instrument. Iii. Measures Below the Diffraction Limit of the Wiyn Telescope

Horch

Altena

Howell

et al. 2011

The Astronomical Journal

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In this paper, we study the ability of CCD-and electron-multiplying-CCD-based speckle imaging to obtain reliable astrometry and photometry of binary stars below the diffraction limit of the WIYN 3.5 m Telescope. We present a total of 120 measures of binary stars, 75 of which are below the diffraction limit. The measures are divided into two groups that have different measurement accuracy and precision. The first group is composed of standard speckle observations, that is, a sequence of speckle images taken in a single filter, while the second group consists of paired observations where the two observations are taken on the same observing run and in different filters. The more recent paired observations were taken simultaneously with the Differential Speckle Survey Instrument, which is a two-channel speckle imaging system. In comparing our results to the ephemeris positions of binaries with known orbits, we find that paired observations provide the opportunity to identify cases of systematic error in separation below the diffraction limit and after removing these from consideration, we obtain a linear measurement uncertainty of 3-4 mas. However, if observations are unpaired or if two observations taken in the same filter are paired, it becomes harder to identify cases of systematic error, presumably because the largest source of this error is residual atmospheric dispersion, which is color dependent. When observations are unpaired, we find that it is unwise to report separations below approximately 20 mas, as these are most susceptible to this effect. Using the final results obtained, we are able to update two older orbits in the literature and present preliminary orbits for three systems that were discovered by Hipparcos.

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“…A practical example is useful for setting context and objectives for fiber multiplexing. For this exercise we adopt the WIYN 3.5-m telescope as a reference, given its 1 degree diameter FOV, its tradition in speckle imaging with the Rochester Institute of Technology-Yale Tip-Tilt Speckle Imager (RYTSI), DSSI and NESSI systems [5,6,9], as well as its history of multifiber spectroscopy with the Hydra fiber positioner [10]. We explore its potential use for a comprehensive, diffraction-limited imaging follow-up survey of targets for NASA's Transiting Exoplanet Survey Satellite (TESS).…”

Section: Multiplexing Factor Versus Fiber Fovmentioning

confidence: 99%

Speckle Imaging Through a Coherent Fiber Bundle

Davidson¹,

Horch²,

Majewski³

2018

Preprint

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Speckle imaging is a well known method to achieve diffraction-limited (DL) imaging from ground-based telescopes. The traditional observing method for speckle has been to observe a single, unresolved, source per telescope pointing over a relatively small field of view (FOV). The need for large DL surveys of targets with high sky density motivates a desire for simultaneous speckle imaging over large FOVs, however it is currently impractical to attain this by covering the entire focal plane with fast readout detectors. An alternative approach is to connect a relatively small number of detector pixels to multiple interesting targets spanning a large FOV through the use of optical fibers, a technique employed in spectroscopy for decades. However, for imaging we require the use of coherent fiber bundles (CFBs). We discuss various design considerations for coherent fiber speckle imaging with an eye toward a multiplexed system using numerous configurable CFBs, and we test its viability with a prototype instrument that uses a single CFB to transport speckle images from the telescope focal plane to a traditionally designed, fast readout speckle camera. Using this device on University of Virginia's Fan Mountain Observatory 40-inch telescope we have for the first time successfully demonstrated speckle imaging through a CFB, using both optical and NIR detectors. Results are presented of DL speckle imaging of well-known close (including subarcsecond) binary stars resolved with this fiber-fed speckle system and compared to both literature results and traditional speckle imaging taken with the same camera directly, with no intervening CFB.

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RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

Cited by 11 publications

References 17 publications

The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc

The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc

Observations of Binary Stars With the Differential Speckle Survey Instrument. Iii. Measures Below the Diffraction Limit of the Wiyn Telescope

Speckle Imaging Through a Coherent Fiber Bundle

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