REPEATABILITY OF THE FOS G130H GRATING EXTERNAL WAVELENGTH ZEROPOINT ANURADHA KORATKAR and IAN EVANS Space Telescope Science Institute,3700 San Martin Drive, Baltimore, MD 21218 Abstract. Measurements of the position of the geo­coronal Lyff are used to determine the repeata­ bility of the G130H grating and the external wavelength zeropoint for the first time since launch. ... The 1oe repeatability of the wavelength calibration is 0.159 љ A (0.64 pixels or 39 kms \Gamma1 ). ...

Next: Reduction procedure Up: Extinction and transformation Previous: Strategy . Standard stars can be included in the extinction solution, if one is careful. The problem is that there are usually appreciable ``conformity errors'' due to mismatch between the instrumental and the standard passbands [ 16 ]. ... Thus, it is wrong to assume that the transformation between the instrumental system and the standard system is exact, even if there were no measurement error in either system [ 1 ]. ...

For solar wind dials without any explanatory text, see this page . ... There are three logs, one for each condition index ( K P , Solar Wind ,and NOAA/SEC .) ... More about the solar wind's recent behavior can be found on my Current Solar Wind Conditions page. ... Other items of interest include NOAA/SEC Current Conditions , my composite current Auroral Images page, Windows on the Universe: Space Weather , and Public Outreach Index, Department of Space Physics and Astronomy, Rice University . ...

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

... 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). ...

... Based on the measurements of the Stokes parameters in the continuum and in the broad 0.6563 nm hydrogen emission line obtained with the 6-m telescope for the Seyfert galaxy Mkn 6, secular variability of the hydrogen line profile polarization was discovered; a time lag of less than 2 days between the continuum flux and the polarized continuum emission was determined which corresponds to the size of the region where the polarization of the continuum occurs, less than 0.001 pc. ...

... Research . ... The major problem in HVC research is the unknown distance towards most of the HVCs. ... Thilker et al. (2004) used the Green Bank Telescope (GBT) to map an area of $7^{\circ} \times 7^{\circ}$ around M31 in H i . They discovered a population of HVCs located within a projected distance of about $50~\mathrm{kpc}$ from M31. ... 2004). ... The remaining HVCs around M31 are isolated in position and velocity and may represent primordial, dark-matter-dominated clouds. ...

... P2068 Date Received: 2005-Feb-01 11:09:13 Technical Page Proposal Type: General Category: Observation Category: Total Time Requested: Prop osal Title: ABSTRACT: Regular Pulsars Galactic 18 Hours High-precision timing of two recycled pulsars We request 18 hours of observing time to continue regular timing observations of two recycled pulsars spanning a 12-month baseline. ... Measurements of the prop er motion of b oth J1829+2456 and J1944+0907 will allow their intrinsic Pdots to b e determined. ...

The period of this variable was first determined by Tony Vanmunster (Center of Backjard Astrophysics). We have taken the observations with CCD ST-7 and 60-cm reflector of SAI Crimean station. ... The longest set was taken at night of 2000 February 12 including 291 R 60 second long frames with the magnitude limit of 18. Summing all these frames in a single one I have taken a "deep sight" of this region having the limit of 21.7R. The effective exposition is 4 h. 51 m. Look at this frame! ...

Next: First CCD Observations of Up: Highlights Previous: Origin of Stars Contents . Subdwarf B stars are highly evolved stars which pulsate non-radially in several modes with different frequencies. ... Over 60,000 images were obtained, which when played in sequence show the star's oscillations in red, green and ultraviolet light. ... Figure 3: ULTRACAM light curve for PG0014+067, from 2004 August 20 to 2004 August 25 (top to bottom). ...

Peremennye Zvezdy ( Variable Stars ) 33 , No. ... The new variable star HD 305629, with a Cepheid-like light curve, is demonstrated, from our optical observations and ASAS-3 data, to actually be an ellipsoidal variable star on a highly eccentric orbit. ... During a systematic search of variable stars in the publicly available ASAS-3 database (Pojmanski 2002), apparent variability was found in the star HD 305629 (10 51 34 35, -60 47 57 4, J2000.0; Fig. ... The light curve and color curves of HD 305629. ...

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. ...

... The experience of determination of the link between radio sources and dynamical reference frames is presented. To obtain this connection we used a series of very long baseline interferometry (VLBI) observations of the spacecraft Phobos-2 and angularly nearby quasars. ... The dynamical reference frame is determined by equator and equinox of these ephemerides. ... References . ... The relative orientation of the radio and dynamical reference frames can be described by a sequence of three rotations . ...

... The most precisely determined characteristic for accreting neutron stars (NS's) is their period. ... Period changes show fluctuations. ... Some applications of stochastic processes in astrophysics especially in accreting systems were discussed in Lipunov (1987),Hoshino Takeshima (1993) and Lipunov (1992).In Hoshino Takeshima (1993) the authors, using simple models of MHD turbulence, try to explain aperiodic changes in X-ray luminosity of X-ray pulsars. ... Here, -constant angular momentum. ...

... Determining the nominal roll angle for stable intervals . ... We found the necessary information in a file 'rh*.ao', which has a binary extension table for each obi. ... Unlike the question of determining the nominal roll angle, we know of no a priori indication of this problem (although the guide star configuration may be the cause, or at least associated with this condition): it is necessary to examine the source position for each obi. ... The guide star record is at the end of the 'anc file'. ...

... Development of Ideas of Structure and Evolution of Stars. Integral Features of Stars, Which Determine Their Structure, Direction and Rate of Evolutuion. ... Connection between Potential and Thermal Energy of Star. ... Structure of a Main Sequence Star. Features of Massive Stars Evolution on the Main Sequence. Internal Structure of the Sun. ... White Dwarfs, Their Features. ... Evolution from the Main Sequence of Massive Stars. ... Evolution of Small Mass Stars till White Dwarfs Sequence. ...

... Resolved Stellar Populations Globular Clusters . Galaxies are made of stars, gas and the illusive dark matter. ... Star clusters are the simplest form of the stellar population. ... Old globular clusters are easily observed at great distances and can be used as probes of the early stages of star formation history in galaxies where individual stars cannot be resolved. My research interests are centered on the studies of resolved stellar populations and (old) star clusters in nearby galaxies. ...

Aristarch is Copernic of Classic World. ... First Aristarch determined the fact for how many times the Sun was father then the Moon and then he compared the Sun and the Moon with the Earth. ... Only the Moon rotates around the Earth. ... Gipparch suggested that the Sun turned around the Earth steady and in circumference but the Earth is displaced according its centre. ... The orbit point in which the Sun is nearer to the Earth Gipparch called perigee and the most remote one he called apogee . ...

... 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? ...

... The bright supernova (hereafter SN) in the galaxy NGC 4527 was first sighted by S. Knight (USA) on April 13.17UT at magnitude ~14.0v. The report of the sighting was subsequently forwarded by phone to the AAVSO. ... SN 1991T. The galaxy NGC 4527 is an Sb(s)II type galaxy with an apparent Blue magnitude of 11.32 (Shapley-Ames, 1981). ... An analysis of this event utilizing visual observations by amateurs, plus a light curve is presented.. ... THE LIGHT CURVE: . ... ISN SN 1991T web page . ...