... Bojan Nikolic web pages (r. 329) . Galaxy Evolution . This pages illustrates some of the galaxies with close pairs which we identified in our study of star formation in interacting galaxies selected from the Sloan Digital Sky Survey (Nikolic et al 2004, see the publication list ) . ... This is 10 out of 114 of all of the galaxies in the volume limited sample at redshift smaller than 0.03 and with the first companion within 30 kiloparsecs. A gallery of interacting galaxies . ...

... rgsbadpix combines the calibration bad pixel data from the CCF with any hot pixels found by analyzing the raw telemetry for one CCD from an RGS exposure in spectroscopy mode. ... When the same bad pixel is identified by both the CCF and the telemetry analysis, the output bad pixel table mentions only the CCF version. CCF bad pixels that lie outside the telemetry window of the exposure are not included. ... A bad pixel identified by analysis of the telemetry. ...

Next: Non-classified objects Up: Non-emission-line objects Previous: Absorption-line galaxies . To separate the stars among the objects missing detectable emission lines we cross-correlated a list of the most common stellar features with the observed spectra. ... All of them were crudely classified in categories from definite A-stars to G-stars, with most of them intermediate between A and F. The data for these stars are presented in Table 7. ... 2001-06-08 ...

Automatic Classification of Sunspot Groups Using SOHO/MDI Magnetogram and White Light Images David Stenning March 29, 2011 1 Introduction and Motivation Although solar data is being generated at an unprecedented rate, the majority of sunspot classification is done manually by experts. ... This is to smooth the "white" areas in the magnetograms. ... Left: Inverse Magnetogram Right: "Opened" Inverse Magnetogram 6 Using the cleaned images, sunspot active-region "seeds" are obtain by thresholding. ...

Next: Sample Properties Up: Sample Identification Previous: Comments on Individual Sources . Previously known serendipitous sources were selected by cross-correlating WGACAT with a variety of optical and radio catalogs, including the Ver?n-Cetty & Ver?n (1996) and Hewitt & Burbidge (1993) quasar catalogs, the 1 Jy (Stickel et al. 1994) and S4 (Stickel & K?hr 1994) radio catalogs, and the BL Lac catalog of Padovani & Giommi (1995b). ... Details of these 97 objects are given in Table 6. ...

... Chapter 4: Solar System Targets > 4.2 Target Identification . ... The following information is required to identify and classify each target. ... For example, separate targets should be defined if you plan to take spectra of several different surface features on a planet, or if you plan to observe the same feature with different timing constraints. ... Description . PLANET . If the target is the center of a planet, enter PLANET followed by its name (e.g., PLANET JUPITER , PLANET SATURN ). ...

The Oct 10 discovery of this object was announced on MPEC:2004-T55 under the asteroid designation 2004 TU12. Mag 14 at discovery and with q=1.23 this object was clearly unusual in its large size. ... Animated image, please wait for all frames to load. ... It is now designated 162P/Siding Spring. Animated image, please wait . for all frames to load. ... Siding Spring Survey Main Page . ... Discoveries . ... Anglo-Australian Near Earth Asteroid Survey 1990-96 . ...

... Previous: Generalized Linear Multi-Frequency Imaging in VLBI . ... At Astronomical Observatory of Valencia University (OAUV), CCD observations of asteroids and big planets satellites are obtained since 2001 with a big format camera and several telescopes. ... Software for comparison of single and overlapped CCD fields obtained at different epochs has been developed. ... After images measurement in CCD field, catalogue stars are identified and adjusted with images. ...

... News . ... Star Atlas . ... A newly identified separate star cluster in front of the Orion Nebula Cluster . Astronomers identified the massive cluster of young stars NGC 1980 to be a clearly separate entity from the main cluster of the most-studied star formation region in the galaxy. ... For me, the most intriguing part is that the older sibling, the Iota Ori cluster, is so close to the younger cluster still forming stars inside the Orion Nebula," said JoУ?o Alves from the University of Vienna. ...

. Home . News . Gallery . Events . Twitter . Press Releases . Links . Contact Us . Calendar . Press & Web Coverage . Previous . Next . List . Taken on the 24th November by John McConnell. It shows the ISS and an unidentified satellite . Friday, 2 January 2009 23:14 . International Year of Astronomy, Ireland National Node . [Back To Top] .

... Kerr et al. (2014) studied the emission from PSR J1717-4054 over intervals from single pulses to years using the Parkes radio telescope and the Australia Telescope Compact Array (ATCA). They identified and characterized nulling at three discrete time-scales: the pulsar emits during `active states' separated by nulls lasting many thousands of rotations, while active states themselves are interrupted by nulls with a bimodal distribution of durations - one to two rotations, or tens of rotations. ...

Every file and directory in the file system can be identified by a complete list of the names of the directories that are on the route from the root directory to that file or directory. ... usr/local/bin/ue . This gives the full pathname starting at the root directory and going down through the directories usr , local and bin to the file ue - the program for the MicroEMACS editor. You can picture the full pathname as looking like this: . root) | tmp usr | ... Relative pathnames . ...

Proposal Identification No.: ... Section IV - RFI Considerations 2 Frequency Ranges Planned 300 - 350 Section V - Observing List Target List 00:31:06.0 01:02:12.7 02:39:32.8 03:12:48.7 03:18:01.9 03:38:16.7 03:41:51.7 04:31:33.5 05:16:47.9 05:26:38.1 06 ... 07:11:38 06:12:48 10:13:29 15:48:36 01:31:12 06:32:31 12:12:43 35:55:47 36:52:56 12:13:13 26:05:07 07:02:53 07:07:24 Fermi2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL 2FGL ...

Download Izmccd (~2.7 MB). Solution of problems at identification of star field. ... 2) Scale is not correct. ... In this case algorithm of identification will revise all values of scale from twice smaller up to twice greater. ... There should be more than value of the field "Number of stars in frame". ... The star field is considered identified if number of the identified stars more or equally to this value. It is necessary to set value from 4 up to value of field "Number of stars in frame". ...

Next: References Up: No Title Previous: Observational data and reduction . ... A minor loss of information is due to the overestimation of the scattered light in the region of and to the broad emission lines and . On the diagrams are shown the blue-shifted absorption lines and the interstellar diffusion bands. ... In Table 1 are given only emission lines. Questionable features and the lines that fell within the gaps are not included in it, question-marks are for unreliable identification. ...

... Sternberg Astronomical Institute , Moscow University . ... Present edition unites two parts of Catalogue of interacting galaxies by B.A.Vorontsov-Velyaminov: the first part (Part 1) containing 355 systems was published in 1959 [1] and the second one (Part 2) with 497 objects - in 1976 [2].Thus two published parts of Catalogue include 852 interacting systems. ... All new of them (1162 by number) were taken from the comments to the galaxies in Morphological catalogue by Vorontsov-Velyaminov et al.[ ...

... The common identifier of this star system is G89-14. Initially, there were known just two close spectroscopic components in this system, A and B, orbiting around each other with a period of about 190 days (Carney et al., ... Subsequently, at a separation of 34 arc seconds from this spectroscopic pair, Allen et al. (2000) found its companion D with common proper motion (Fig.1, right, and Fig.2). ... The uniqueness of this star is that it is the most metal-poor quadruple system known to date. ...

Andreyev Yu.V., Dmitriev A.S. and Pustovoit V.I. Institue of RadioEngineering and Electronics of RAS . Efremova E.V. Moscow Institue for Physics and Technology . ... Separation of a sum of chaotic signals corrupted by Gaussian channel noise into the components with a method based on chaotic synchronous response is discussed. In order to establish the response, a procedure of iterating the maps, inverse to the maps that generate the chaotic signals, is proposed. ...

This Directory contains mean hourly, mean daily and mean monthly values of cosmic ray intensity recorded by World Network NM stations to the end of 2011. ... CD is created in WDC for STP, Moscow and IZMIRAN. ... This directiry contains catalogue Corrected for pressure and verificated data in WDC for STP, Moscow . This directiry contains catalogue Corrected only for pressure but Original data in WDC for STP, Moscow . ... 20 May - 22 July 1972, M., 1975 6. 27 March - 22 July 1972, M., 1975 7. ...

This diagram shows the effect of the 'separate' value of the 'border-collapse' property. The diagram shows a three column, two row table whose cells are subject to the separated borders model. The cells themselves have a grey background color and an 'inset' border style, which makes them appear to sink into the page. ... The table itself has a 10pt 'outset' border that gives one the impression the table is rising out of the page. ...