Triple-correlation subplane reconstruction of photon-address stellar images

Meng, Julian; Aitken, George J. M.; Hege, E. K.; Morgan, J. S.

doi:10.1364/josaa.7.001243

Cited by 61 publications

(41 citation statements)

References 7 publications

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“…For each target, the power spectrum is divided by the power spectrum of the point source calibrator to yield a fringe pattern, which contains information on the separation, relative position angle, and brightness of any pair of stars, or a pattern containing no significant fringes in the case of a single star. Using the methods described by Meng et al (1990), a reconstructed image of the target star and its surroundings is made from the power spectrum and bispectrum (the bispectrum contains the phase information to properly orient the position angle). We fit a model fringe pattern to the observations to determine the separation and position angle of any detected companion relative to the primary, as well as the magnitude difference between companion and primary encoded in the amplitude of the fringes.…”

Section: Speckle Interferometrymentioning

confidence: 99%

The Kepler Follow-Up Observation Program. I. A Catalog of Companions to Kepler Stars From High-Resolution Imaging

et al. 2017

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We present results from high-resolution, optical to near-IR imaging of host stars of Kepler Objects of Interest (KOIs), identified in the original Kepler field. Part of the data were obtained under the Kepler imaging follow-up observation program over six years (2009)(2010)(2011)(2012)(2013)(2014)(2015). Almost 90% of stars that are hosts to planet candidates or confirmed planets were observed. We combine measurements of companions to KOI host stars from different bands to create a comprehensive catalog of projected separations, position angles, and magnitude differences for all detected companion stars (some of which may not be bound). Our compilation includes 2297 companions around 1903 primary stars. From high-resolution imaging, we find that ∼10% (∼30%) of the observed stars have at least one companion detected within 1″ (4″). The true fraction of systems with close (4″) companions is larger than the observed one due to the limited sensitivities of the imaging data. We derive correction factors for planet radii caused by the dilution of the transit depth: assuming that planets orbit the primary stars or the brightest companion stars, the average correction factors are 1.06 and 3.09, respectively. The true effect of transit dilution lies in between these two cases and varies with each system. Applying these factors to planet radii decreases the number of KOI planets with radii smaller than 2 Å R by ∼2%-23% and thus affects planet occurrence rates. This effect will also be important for the yield of small planets from future transit missions such as TESS.

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Section: Speckle Interferometrymentioning

confidence: 99%

The Kepler Follow-Up Observation Program. I. A Catalog of Companions to Kepler Stars From High-Resolution Imaging

et al. 2017

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“…We compute near-axis sub-planes of the bispectrum for the science observation following their methodology. The phase of the object's Fourier transform is then computed from these, using the relaxation algorithm of Meng et al (1990). This is combined with the modulus estimate previously obtained to give the (complex) Fourier transform of the object.…”

Section: Speckle Data Reductionmentioning

confidence: 99%

Observations of Binary Stars with the Differential Speckle Survey Instrument. VII. Measures from 2010 September to 2012 February at the WIYN Telescope

Horch¹,

Casetti-Dinescu²,

Camarata³

et al. 2017

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We report on speckle observations of binary stars carried out at the WIYN Telescope over the period from 2010 September through 2012 February, providing relative astrometry for 2521 observations of 883 objects, 856 of which are double stars and 27 of which are triples. The separations measured span a range of 0.01-1.75 arcsec. Wavelengths of 562, 692, and 880 nm were used, and differential photometry at one or more of these wavelengths is presented in most cases. 66 components were resolved for the first time. We also estimate detection limits at 0.2 and 1.0 arcsec for high-quality observations in cases where no companion was seen, a total of 176 additional objects. Detection limits vary based on observing conditions and signal-to-noise ratio, but are approximately 4 mag at 0.2 arcsec and 6 mag at 1.0 arcsec on average. Analyzing the measurement precision of the data set, we find that the individual separations obtained have linear measurement uncertainties of approximately 2 mas, and photometry is uncertain to approximately 0.1 mag in general. This work provides fundamental, well-calibrated data for future orbit and mass determinations, and we present three first orbits and total mass estimates of nearby K-dwarf systems as examples of this potential.

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“…In the case of reconstructed images, the relaxation technique of Meng et al (1990) is used to generate a phase map of the object's Fourier transform, and this is combined with the object's modulus obtained by taking the square root of the power spectrum. By combining the modulus and the phase and inverse transforming, one arrives at the reconstructed image.…”

Section: Data Analysis and Self-calibrationmentioning

confidence: 99%

“…Apogee (2003), SBIG (2002) and Ethernaude (2001) constitute recent examples of this improvement, with the application of USB 2.0 and Ethernet interfaces to CCDs in the high-end amateur market. These kinds of initiative can supply readout rates typically 10 to 30 times faster than that offered by our port-parallel camera.…”

Section: New Ccds Improvementsmentioning

confidence: 99%

Application of fast CCD drift scanning to speckle imaging of binary stars

Fors¹,

Horch²,

Núñez³

2004

A&A

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Abstract.A new application of a fast CCD drift scanning technique that allows us to perform speckle imaging of binary stars is presented. For each observation, an arbitrary number of speckle frames is periodically stored on a computer disk, each with an appropriate exposure time given both atmospheric and instrumental considerations. The CCD charge is shifted towards the serial register and read out sufficiently rapidly to avoid an excessive amount of interframe dead time. Four well-known binary systems (ADS 755, ADS 2616, ADS 3711 and ADS 16836) are observed in to show the feasibility of the proposed technique. Bispectral data analysis and power spectrum fitting is carried out for each observation, yielding relative astrometry and photometry. A new approach for self-calibrating this analysis is also presented and validated. The proposed scheme does not require any additional electronic or optical hardware, so it should allow most small professional observatories and advanced amateurs to enjoy the benefits of diffraction-limited imaging.

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Triple-correlation subplane reconstruction of photon-address stellar images

Cited by 61 publications

References 7 publications

The Kepler Follow-Up Observation Program. I. A Catalog of Companions to Kepler Stars From High-Resolution Imaging

The Kepler Follow-Up Observation Program. I. A Catalog of Companions to Kepler Stars From High-Resolution Imaging

Observations of Binary Stars with the Differential Speckle Survey Instrument. VII. Measures from 2010 September to 2012 February at the WIYN Telescope

Application of fast CCD drift scanning to speckle imaging of binary stars

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