EMCCD SPECKLE INTERFEROMETRY WITH THE 6 m TELESCOPE: ASTROMETRIC MEASUREMENTS, DIFFERENTIAL PHOTOMETRY, AND ORBITS

Abstract

Results of the EMCCD-based speckle interferometric observations and differential photometry for 46 visual binaries obtained in 2007 June and July with the 6 m telescope of the Special Astrophysical Observatory (Russia) are presented. First preliminary orbits for COU 401, COU 1281, and COU 1037 as well as improved orbits for CHR 137, COU 100, COU 1136, COU 798, CHR 51, CHR 55, COU 315, COU 206, and ADS 13961, along with their dynamical mass estimates, are reported. On the basis of dynamical parallax information, first distance estimates for COU 100, COU 1136, COU 798, COU 206, and COU 1037 are calculated.

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

“…Speckle imaging has contributed in both areas over its long history, and indeed the technique has seen a resurgence in recent years due to the more widespread use of electron-multiplying CCDs (EMCCDs) in speckle work (Tokovinin & Cantarutti 2008;Docobo et al 2010;Horch et al 2011;Balega et al 2013). In addition to opening new parameter space for the measurement of binary systems due to their sensitivity and readout speed, these devices have enabled the use of speckle imaging for faint (stellar) companion detection for stars thought to host exoplanets (Howell et al 2011(Howell et al , 2016Furlan et al 2017;Hirsch et al 2017).…”

A method for EMCCD multiplication gain measurement with comprehensive correction

“…(13-15): Measurement procedure. According to formulas (14) and 15, it is necessary to determine six factors in Table 1 for the comprehensive correction of the original image of the camera. The more the number of collected images, the smaller the random error of the mean image.…”

“…2, the mean value of slope k ave * A and intercept b ave can be obtained from formula (8). After the parameters in Table 1 are calculated, the comprehensive correction coefficient k total , b total are obtained by substituting them into formulas (14) and (15). Finally, k total , b total and the original output image are substituted into formula (13) as X i, j to get the camera output image with comprehensive correction.…”

“…At present, the research on non-uniformity correction mainly focuses on infrared imaging and common CCD imaging [4][5][6][7][8][9][10][11] . The related scientific research of EMCCD mainly concentrates on the application of weak light imaging in astronomical observation [12][13][14][15][16][17][18][19] , biomedical [20][21][22][23][24][25][26] and other fields. There are few literatures on the non-uniformity characteristics of EMCCD imaging and its correction.…”

A Method for Optical Tracking of On-Orbit Servicing Operations in Geostationary Orbit Using Speckle Interferometry

“…The binary star community exploited this approach enabling the measurement of gravitationally bound binary stars 6 with separations less than the atmospheric seeing disk, allowing large aperture telescopes to take advantage of their full resolution capabilities. [43], [44], [45] and for Lucky Imaging 7 [46]. Moderate sized instruments have also employed them [47] providing precision measurements on astronomical objects with accuracies of 0.05 arcseconds or better.…”