Nova Dissertation Tracking System

Nova Dissertation Tracking System-27
Diameter determinations from VINCI using global calibration solutions Poster presented at the workshop entitled: The power of optical/IR interferometry: recent scientific results and 2nd generation VLTI instrumentation held in Garching, Germany, 4-8 April 2005 View Abstract MIDI data reduction, analysis and science workshop 2004: Presentation on ESO MIDI Data Reduction System (pipeline) Presentation given 14 October 2004 in Leiden as part of MIDI data reduction workshop Conceptual Design Review PRIMA Astrometry Operations and Software through Presentation given concerning dispersion and fringe tracking between bands Includes the "famous" dispersion animations Data reduction, calibration, and stellar diameter results using VINCI J. Pereira, Andreas Quirrenbach, David Raban, Amir Vosteen View Abstract Proceedings SPIE v7734 Optical and Infrared Interferometry II, SPIE conference, San Diego, July 2010 Direct detection of the disk around HR 4049 Bakker, Eric J.; Meisner, Jeffrey A.; Percheron, Isabelle; Dominik, Carsten View Abstract Proceedings SPIE v5491, p35 Interferometry conference, Glasgow, July 2004 Scientific and technical results from VINCI using coherent estimation of fringe visibility J. Meisner View Abstract Proceedings of the workshop at JENAM 2002, The Very Large Telescope Interferometer: Challenges for the Future Astrophysics and Space Science, v286, p119 Direct detection of exoplanets using long-baseline interferometry and visibility phase J. Fringe Tracking and Group Delay Tracking Methods for MIDI Jeffrey Meisner View Abstract Published in the proceedings of the 36th Liege International Astrophysics Colloquim (2001): "From Optical to Millimetric Interferometry: Scientific and Technological Challenges" Spatial Filters for Astronomical Interferometry using Discrete Optical Components Jeffrey A. p.303 ("Working on the Fringe" conference, sponsored by JPL, May 24-27 1999, Dana Point, CA) Concentration of Starlight from Large Apertures into a Single Spatial Mode for Long-Baseline Interferometry Jeffrey Meisner ASP Conference Series #174, p193 (1999) (Contribution to symposium on interferometry and adaptive optics, ASP meeting, June 28 - July 1 1998, Albuquerque) Long unpublished Version in HTML format Estimation and tracking of atmospheric delay noise in a long-baseline optical stellar interferometer and determination of the expected estimation error, Ph. The NOVA Fringe Tracker: a second generation cophasing facility for up to six telescopes at the VLTI Jeffrey A. This instrument at the VLTI will enable the cophasing of up to 6 telescopes simultaneously.Meisner Annotated slides from a presentation made at the September 2003 Workshop Long Baseline Interferometry in the mid-infrared, Ringberg Castle near Munich. Meisner View Abstract Published in the proceedings for the NOVA/LEIDEN/NEVEC/ESO/ESA Workshop on Space and Ground Based Optical/Infra Red Interferometry, Leiden, The Netherlands, September 18-22, 2000 Coherent estimation of complex fringe visibility: a generalized approach, Jeffrey Meisner View Abstract Published in Proc. Using broad band optics with detection from 1.2 to 2.4 microns, a unique configuration is employed that eliminates so-called photometric crosstalk.

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Both issues were addressed and inclusion of escaping sample to the final fit led to an effective increase of statistics by 4% with best- fit measurements of $$\sin\theta^2_ = 0.504$$ and $$\Delta m^2_ = 2.45 \times 10^$$ e V$^2$.

The NOVA Fringe Tracker: a second generation cophasing facility for up to six telescopes at the VLTI Talk presented at SPIE conference 8445, Amsterdam, July 2012 View Abstract See also the paper submitted to SPIE, below.

This realization can simplify the choice and use of calibrator observations in an instrument benefiting from full spatial filtering.

Due to the exceptionally high intrinsic precision of the measurements, the demonstrated error in raw visibilities (but also in calibrated visibilities) could often be shown to steadily decrease in proportion to the square root of the observing time, rather than reaching a plateau due to systematic error sources as is more often the case.

Its parameters fluctuated over time requiring frequent (and troublesome) adjustment in order to obtain a high interferometric efficiency.

Polarization mismatch is believed to be mainly responsible for the fluctuating and sometimes poor interferometric efficiency, and this is a general concern in the case of single-mode (guided wave) optical systems accepting both polarizations.

Direct detection of exoplanets using long-baseline interferometry and visibility phase J. Le Poole View Abstract Proceedings SPIE v8445 Optical and Infrared Interferometry II, SPIE conference, Amsterdam, July 2012 The polarization-based collimated beam combiner and the proposed NOVA fringe tracker (NFT) for the VLTI Jeffrey A. SPIE 4006, pp 1068, Astronomical Interferometry, Proceedings of the conference "Interferometry in Optical Astronomy," held March 26 - 29, 2000, Munich, Germany Use of a Seeing Monitor to Determine the Velocities of Turbulent Atmospheric Layers Richard Roosen, Jeffrey Meisner View Abstract Working on the Fringe: Optical and IR Interferometry from Ground and Space. This refers to imbalance in the beam combiner which results in fluctuations of the incoming wavefronts and the proportion of power accepted by a spatial filter masquerading as a visibility, a common problem afflicting previous interferometric instruments and fringe trackers.

Meisner Presentation made in Leiden 27 June 2003 based on a poster presented at XIXth IAP Colloquium "Extrasolar Planets : Today and Tomorrow" held in Paris, 30 June - 4 July 2003 View Abstract The NOVA Fringe Tracker: a second generation cophasing facility for up to six telescopes at the VLTI Jeffrey A. Also proposed for use in science instruments (for the measurement of visibility), the Polarization-Based Collimated Beam Combiner, with its achievement of photometric symmetry in hardware, is particularly suited for combined use of the smaller AT (1.8 meter) telescopes with the UT (8 meter) telescopes involving a 20:1 intensity ratio of the interfering beams, and also for fringe tracking using highly resolved sources having a very small visibility.

155 stars were observed sufficiently to consider, some of which are rather dim or might not be properly fit using a UD visibility function.

The better half of this set, 77 stars, all had a median residual which was better than 1.2% of the visibility itself.

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