Next: Analysis in the Up: MIDAS utilities for Previous: Fourier analysis . For the detection of smooth signals, e.g. sinusoids, use either SCARGLE/TSA or AOV/TSA with bins. ... SCARGLE/TSA -- . Scargle sine model: This command computes Scargle's (1982) periodogram for unevenly spaced observations x . ... In this way, the command can be used to perform a CLEAN-like analysis manually by removing individual oscillations one by one in the time domain (see Roberts et al. ... AOV/TSA -- . ...

... N. Kardashev and M. Popov informed the participants on the current IOC results. ... Kovalev). ... Agenda of the RadioAstron teleconference November 16, 2011 Corrections to the Agenda 1 2 3 4 5 6 IOC status and results Single Dish observation with RA VLBA observations to find best fringe search candidates Fringe search plan Early science program plan Tracking stations outside Russia N.Kardashev N. Kardashev / M.Popov V. Kostenko E.Fomalont M.Popov Y.Y. Kovalev / M.Popov /A.Alakoz ...

Next: Amplitude Distribution Previous: Gravitational Wave Background from . To get rid of the extragalactic GWB produced by binaries, one can use the above considerations to find the optimal detector halfwidth and frequency for observations. ... for the flat red end of the GWB, and . ... Equating to unity, one finds the critical detector halfwidth . ... In contrast, by observing the sky with a GW detector with a narrow enough halfwidth , one will not ``see'' the extragalactic GWB at frequencies . ...

WFPC2 . Images: version1 , version2 . Catalogs: Version 1 HDF-S , HDF-N ;Version 2 HDF-S . STIS . ... NICMOS . Images: Camera 3 , V2 of psf-convolved STIS 50CCD on NICMOS . ... Images: WFPC2 FF , STIS FF ; Version2: WFPC2 FF , STIS FF , NICMOS FF . Catalogs: Version2 WFPC2 FF , STIS FF , NICMOS FF . ... Check the instrument specific technical pages for a description of the data products and the implemented data reduction steps: STIS , WFPC2 , NICMOS , Flanking Fields . ...

... Pulsar timing in a nutshell" Measure the TOA, average over time and frequency, then correct for the motion of the Earth and the pulsar. ... They contain: unmodeled physics of the Earth and the pulsar motion, receiver noise and RFI (white) clock errors (quite red), calibration errors, particularly polarization (mostly white), interstellar-plasma mean-density fluctuations (red), interstellar-plasma scattering (white), pulsar rotational noise (pink), the effects of gravitational waves (quite red). ...

... Several attempts to discover the FICN signal in VLBI nutation series made during last years failed. ... We investigated several VLBI CPO series by means of spectral and wavelet analysis. It has been shown that there are several periodic signals with close amplitude around the expected FICN period without any prevailing one that can be reliably associated with the FICN. ... DATA ANALYSIS We analyzed several CPO series obtained in IVS analysis centers by means of spectral and wavelet analysis. ...

Next: Observations and Data Reduction Up: Coronal Hole Diagnostics out Previous: Coronal Hole Diagnostics out . ... Line width variations combined with simultaneous electron density estimates, provides a very powerful diagnostic for the solar corona. ... They find that for distances of a few arc seconds outside the solar limb, the average line of sight electron densities in the coronal holes are about a factor of 2 lower than in quiet sun regions. ... The Western limb data showed a similar trend. ...

... 13, Moscow 119992, Russian Federation, e-mail: busarev@sai.msu.ru; 2 Research Institute Crimean Astrophysical Observatory, p/o Nauchnyi, Crimea 334413, Ukraine, e-mail: prok@crao.crimea.ua Summary: We propose a combined method of astronomical investigations of small or distant planets incorporating registration of a set of integral spectra of an object and their frequency analysis. ... An application of the method is shown on example of asteroid 21 Lutetia. ... 6] Busarev V. V. (2002), Solar Sys. ...

The VLTI Calibrator Selector Tool is a tool intended to assist in the selection of suitable interferometric calibrators for VLTI observations with MIDI and AMBER. It uses a model of the VLTI and its instruments to assess the fringe visibility, given the observed bandpass, the geometry, spectrum, and coordinates of the target and the time at which the observations are to be made. ... The tool offers an HTML/Java based interface and consists of two pages. ... The quality flag depends on LDD_chi2. ...

... 2.3 Establishing the Extragalactic Distance Scale . ... 2.3.2 The Second Rung: Distances to stellar clusters . ... 2.3.4 Distances to Local Group Galaxies . ... The Luminosity Function of Planetary Nebulae . ... 3.2.2 Clusters of Galaxies . ... 4.2 Evidence for Dark Matter as a Function of Scale Size . ... 4.3 Other Dark Matter Indicators for Galaxies . ... What is the nature of the large-scale distribution of matter in the universe as traced by the three-dimensional galaxy distribution? ...

... Up: Data Analysis and Processing Techniques . ... Also, a method for quality control of CCD observations is suggested. ... Everyone who observes a celestial object using a CCD detects moving celestial objects as a ``by product''. ... We hope that our investigations may be useful for near-Earth space control and also for searches of the moving celestial objects through analysis of old and new CCD frames obtained at any amateur or professional astronomical observatory. ...

... A radio galaxy is a galaxy that emits an unusually big amount of energy at radio wavelengths. ... Inside of each galaxy with an active nucleus (radio galaxies are among them) there must be a system of a "central machine" responsible for the colossal amount of the emitted energy from radio to gamma ranges. ... Sometimes a radio source in an active galaxy may flare again if the needed conditions appear (a new portion of matter would fall into the furnace of the "central machine"). ...

Proposal Identification No.: ... Proposal Type: General Category: Observation Category: Time Requested this semester: Hours Next Semester: Hours already used for this pro ject : Additional Hours required to complete pro ject : Minimum Useful Time : Expected Data Storage: Prop osal Title: ABSTRACT: Large Pulsars Extragalactic 185 185 680 1500 1.5 hours less than 100 GB The North American Nanohertz Observatory for Gravitational Waves Direct detection of gravitational ...

ES 255: DETECTION AND ESTIMATION THEORY & APPLICATIONS (Fall 2005) Teaching Staff Prof. Patrick J. Wolfe (Instructor) Office Hours: Tuesdays 2:30-4pm or by appointment, Maxwell-Dworkin 129 E-mail: patrick@deas.harvard.edu Tel: 617.496.1448 (Teaching Fellow TBA) Logistics Location: Maxwell Dworkin 221 Meeting Time: Tu., ... Tuesday Oct 25: M-ary detection in white Gaussian noise, Sensitivity. ... Tuesday Nov 1: Non-Linear Estimation (continued), Introduction to colored noise problem. ...

The VIRGO project is a physics experiment; its aim is the detection of gravitational waves. ... It has not yet been possible to detect directly the gravitational waves: it remains one of the major challenges of experimental physics. ... Interferometric antennas for gravitational waves Gravitational waves distort space-time: along two perpendicular directions, the distances between fixed points will increase (resp. decrease), at the arrival of a gravitational wave. ... Publications from our Group . ...

... Flux density at 1 GHz (/Jy): 33 . ... Notes: This is the remnant of the SN of AD 1181. ... Point sources: Central pulsar. ... Green et al. ... ADS . ... WSRT at 610 MHz (58''?64''), 1.4 GHz (24''?27'') and 5 GHz (7''?8''). ... van den Bergh 1978, ApJ, 220, L9. Optical observations. ... Green 1986, MNRAS, 218, 533. 151 MHz observations (1'.2?1'.3: S=36?4 Jy), plus 2.7 GHz (4''), plus Einstein observations for limit on shell. ... Green 1987, MNRAS, 225, 11P. Flux density increase at 408 MHz. ...

... Prof. G.A. Mikhailov, corr.-member of the Russian Academy of Science . ... Prof. B.A. Kargin . ... Marchuk G.I., Mikhailov G.A., Kargin B.A. et al. 1980) The Monte Carlo Methods in Atmospheric Optics. ... Mikhailov G.A. (1992) Optimization of Weighted Monte Carlo Methods. ... Mikhailov G.A. (1998) New approach to constructing and substantiating weight "path estimates" in Monte Carlo method. ... Optics of Atmosphere and Ocean , v.12, p.238-245. ...

The close position of main satellite and subsatellite (distance between them about 1000 km) and using the similar sets of Faraday cups (VDP and VDP-S) with high resolution measurements (up to 16 Hz for the main satellite and up to 10 Hz for the subsatellite) allow us to determine the small-scale variations of the magnetopause shape and position and to estimate the velocity of the magnetopause motion. ... Two point observation of the magnetopause motion: the INTERBALL project. ...

... They were determined as a result of orbit improving on the base of all kinds of optical observations available in the catalog of observations of the Minor Planet Center on March 16, 2014 (radar observations have not been used at this stage). ... As the MPC orbits do not all were improved simultaneously with EMP orbits, only 383866 sets of elements were used for data comparison (for selected sets of elements process of improvement had started with the use of the same observations). ...

... This step is done mostly interactively and uses some basic ad-hoc IDL procedures, mainly for testing and checking of the consistency of the results.Once the observations have been selected and the count spectra extracted, the available spectra of each background level are accumulated. ... Average QUALITY such that QUALITY =0|1 Exposure times are added and the total is written in the EXPOSURE keyword of the header of the output FITS file. Finally, the CCFs are built from these templates. ...