Peremennye Zvezdy", . ... We observed six primary minima: HJD 2454712.3808, 2454713.5038, 2454774.2700, 2454774.5549, 2454776.2386, 2454776.5200. ... We observed four primary minima: HJD 2454712.2847, 2454713.5099, 2454776.2531, 2454776.5584. ... We observed five primary minima: HJD 2454713.3051, 2454714.3669, 2454773.3070, 2454776.4822, 2454778.5956. ... We observed three primary minima: HJD 2454713.3508, 2454774.2818, 2454778.5807. ... Two observed primary minima: HJD 2454713.4729, 2454776.3105. ...

CATS home ] [ Back to CATS list ] [ ftp ] . ... 363Landau+ Fifty-five variable radio sources have been observed at 90 GHz, 22 of them for first time. ... The variability of those sources previously observed is somewhat greater than observed by Owen et al. (1978); some sources exhibited the lowest flux densities ever recorded at 90 GHz. ... The adopted 90-GHz flux density of DR21 is 17.7 Jy and is based on a 90-GHz brightness temperature of 183.4+-3.4 K for Jupiter (Ulich 1978). ...

... The scheduling routines assist in creating an observing list (stored in the startable) from scratch or from another list stored on disk, and computing the visibility of the stars in a specific night and array configuration. The date of observation is taken from the variable date , and the array name from the variable systemid . If these are not defined, defaults are used for date (the next night) and for array (NPOI). ... addstar , stars _char Add one or more stars to the startable. ...

... Observing . ... Home Education Workshops at Adorama Astronomy Workshop: Observing Variable Stars from the City ? February 15, 2015 . ... Beyond New York City . ... Observing Resources for Amateur Astronomers - Part 1: Beginning Observers . ... A History of the First Forty Years of the Amateur Astronomers Association . ... Presented by€а Adorama €аFor the Amateur Astronomers Association of New York . ... 2016 Amateur Astronomers Association of New York Designed by Press Customizr Powered by . ...

... Bright spot spectra have been constructed by differencing the mean spectra observed at pre- and post-eclipse orbital phases. These difference spectra contain ultraviolet absorption lines and show the Balmer jump in emission. ... Model disk spectra constructed as ensembles of stellar atmospheres provide poor descriptions of the observed post-eclipse spectra, despite the fact that UX UMa's light should be dominated by the disk at this time. ... huizinga@stsci.edu . ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . ... Information & tools for observers . ... Visiting Parkes radio telescope . ... The most striking feature of Fig.б  1 is the group of four parallel period-luminosity (PL) sequences (A,B,C,D) brighter than 13 and the sequence E which consists of stars on the first giant branch (it also has an extension between sequences C and D - see Wood et al....

XMMнNewton CCF Release Note XMMнCCFнRELн330 Astrometry: time variable boresight. ... A. Talavera and P. RodrТРguez October 7, 2015 1 CCF components Name of CCF VALDATE List of Blocks changed CAL VERSION XSCS flag XMM BORESIGHT 0025 2000н01н01T00:00:00 OM ANGVAR No EMOS1 ANGVAR EMOS2 ANGVAR EPN ANGVAR RGS1 ANGVAR RGS2 ANGVAR 2 Changes The XMMнNewton Time Variable Boresight was implemented in 2012. ... As explained in XMMнCCFнRELн290, the same o#sets obtained for EPIC can be used to process RGS data. ...

... Astrophysics Group . ... COAST . COAST Astronomical Results . ... Surface Imaging of Betelgeuse . ... This page highlights some astronomical results obtained with COAST over the years. These are listed in chronological order (most recent first). ... Measurements of cyclic variations in the angular diameter of Chi Cygni . ... The first infrared image from an aperture synthesis array . ... The images of Betelgeuse below were reconstructed from COAST data taken in early 2004. ...

Figure 1. Light curve measurements of several RR Lyrae variables are shown in this figure. These variables were selected for observation based on data taken from the Sloan Digital Sky Survey commissioning runs 94 (done on 19 Sep 98) and 259 (done on 17 Nov 98). ... In addition to having been observed by the SDSS and at MRO, these variables have also been observed in the LOENEOS data base. In the figure X marks denote LOENEOS data and + marks denote MRO data. ...

... During the analysis of the surveys carried out on RATAN-600, it was found that almost one fifth of the detected sources shows significant radio flux variations. ... We used the data from "Cold" radio surveys carried out with RATAN-600 in 1980-1994 to search for radio sources with significant flux variability. ... On possibility of detection of variable sources using the data of Cold surveys carried out on RATAN-600. ... Detection of Variable Sources Using the Data of "Cold" Surveys. ...

... THE DETAILS . ... proj> : This is just your project number (i.e. a9999) and it is used both for making the executable file name (a9999.exec) and for knowing the name of your .sls set-up files (assumed to be a9999.sls). start_lst(hh:mm) : The is the LST at which your observations will start. ... You tell the program which .sls file to use for a given observation by the target object's priority number -- a priority of 2 selects the "b" set-up file, while all other priorities select the "a" set-up file...

Catalogue of eclipsing variables (CEV) is the world's principal database of eclipsing binary systems with available classification. CEV contains identifications, classifications, photometry, periods, eclipses data, spectral types, references and notes for 7179 systems. Format of the current CEV . CEV main table (~1.0MB) . ... List of systems, erroneously classified as eclipsing binaries in GCVS (they are not included in the CEV main table) Download all files as a single archive (~0.6MB) . ...

... OH, = 18 cm Nancay Radio Telescope, OH 18-cm line observations , since 1969 F, Jy 6 4 2 0 0 -1 -2 0 -1 -2 0 -2 -4 -6 30 40 50 1612 MHz I HU Pup August 5, 2009 1665 MHz 4 2 0 0.5 0.0 - 0.5 -1.0 -1.5 1.0 0.5 0.0 - 0.5 4 3 2 1 0 -1 1667 MHz I I 1.0 0.5 0.0 0.5 0.0 22-meter telescope, Pushchino Radio Astronomy Observatory H2O F, Jy 1.0 0.5 0.0 0.4 0.2 0.0 -0.2 -0.4 0.4 0.2 0.0 -0.2 -0.4 -0.6 0.6 0.4 0.2 0.0 -0.2 -0.4 -70 -60 -50 -40 -30 -20 -10 0 Mira-type star R Leo. ...

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

... We have compiled the Catalogue of extragalactic supernovae using the GCVS card catalogue. ... Doubtful (?), or rejected (-) SN 8 A1 --- RemFlag [*] The '*' indicates a remark in sn_rem.dat 10- 19 A10 --- Gal Parent galaxy designation 21- 22 I2 h RAh Right Ascension 1950 of Parent galaxy 23- 24 I2 min RAm Right Ascension 1950 (minutes) 25- 28 F4.1 s RAs Right Ascension 1950 (seconds) 29 A1 --- DE- Declination 1950 (sign) 30- 31 I2 deg DEd Declination 1950 of Parent ...

... A star was observed at different zenith distances during one night at the Engelgardt's Astronomical Observatory in the program of atmospheric extinction study at blue. ... The determination of the star's brightness was performed with the method of photon counting. ... Variable star. ... The brightness of the variable star was measured occasionally during the other nights, and moments of maximal values of brightness (15.59m) were received on nights 2­5, the 2nd table. ... JD 2452805. ...

Over the coming weeks an international team, including Simon Jeffery , Vincent Woolf and Amir Ahmad of the Armagh Observatory, will use over fifteen different telescopes to make over one hundred nights of observations of just one star to learn about its internal structure. ... Although the approach has been used before, this may be the first time that a global asteroseismology project has tried to measure both light and spectrum variations at the same time for any star apart from the Sun. ...

... CEPHEID VARIABLE STARS: A Cepheid variable or Cepheid is a member of a particular class of very luminous, massive variable stars with pulsation periods of 1-70 days. ... The relationship is calibrated using data collected from Cepheids whose distances are determined by other means. ... Browse through the 68 CCD fits images he sent you, using ds9 and locate the Cepheid variable. ... Image credits: ESA - "http://sci.esa.int/science-e-media/img/20/cepheid-variables.jpg" . ...

... we show that the comparison between the calculated and observed numbers of the most ``fragile'' (from the point of view of the binary evolution scenario )   galactic binary types (such as X-ray low-mass X-ray binaries (LMXB), cataclysmic variables (CV),   Be-stars   with compact companions, relative number of visible binary radiopulsars   with normal and compact secondary components) impose certain constraints on the feasible initial ... Phenomenological Kick Velocity . ...

... Each point shows the 1 sigma photometric errors and the time span covered by the data; the dotted lines are the 3 sigma limits of each image. ... The solid thick lines are a fit obtained from a K-corrected, time-dilated SNIb light curve at z= 0.95 with tmax=34.0, E(B-V)=0.04 and omega=0.1. ... The three images on the left are the total HDF-N images by Williams et al. 1996 with a pixel scale of 0.04 arcsec/pixel. ... Each image is labelled by the filter and the time range of the observations in days....