H I Self-Absorption (HISA) arises from cold H I gas in front of warmer H I emission at the same velocity. HISA is thus a unique probe of the velocity and temperature structure of the Galactic ISM, from sub-parsec scales within clouds up to multi-kiloparsec scales across the disk. ... To address this question, a series of simple H I radiative transfer models of the Galaxy will be presented. ...

... The solid curve at the bottom show an approximation of the distribution by an exponential law, and the numbers give the scale height and its error. discussion in the text | next figure | previous figure . ...

Next: Structure of the Galaxy Up: Model of the Galaxy Previous: Model of the Galaxy . As discussed above (Section  6 ), galactic binary systems are assumed to be distributed logarithmically along their semi-major axis A (Abt and Levy, 1976[ 2 ]), . ... Figure 40: Number of binary stars per frequency decade. ... As the observed distribution of binary periods is flat (equation ( 15.3.1 )), the normalization constant is the total number of galactic binaries per frequency decade: . ...

... Subject and Problems of Stellar Astronomy. ... Plane of Galaxy, Methods of Its Location Determination. ... Stars Distances. ... Other Methods of Stars Distances Determination. ... Tangential Velocities, Their Determination by Self-Motions. ... Determination of Solar Apex and Spatial Velocity by Radial and Spatial Velocities of Stars. ... Features of Orientation and Parameters of Peculiar Stellar Velocities Ellipsoid. ... General and Selective Light Absorption in Galaxy. ... Darc Clouds in Galaxy. ...

Next: Spectral Extraction of Point Up: Spectral Analysis Previous: Structure of the Spectral . A pulse height distribution can be extracted from a QPOE file only if the event structure is `large', `region', or `full'. ... With the new RDF format files, the output from qpspec for most instruments is split into three files: . ... source off-axis histogram . ... background off-axis histogram . For Einstein IPC, there are no off-axis histogram files, but there is a BAL histogram file, _bal.tab. ...

... Next: Cheating Poisson: A Up: Statistical Analysis Previous: Spatial Models and . ... The spatial distribution of stars in the Local Group dwarf irregular galaxy NGC 6822 has been studied, using recent positions and deep photometry for about 15,000 stars in the galaxy. Based on photometrical data, OB stars and red stars could be studied separately. Spatial statistical tools have been applied to the analysis of the spatial structure. ... Figure: Model selection by the aid of CAIC . ...

... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

Our publications in 2001 year Kniazev, A. Y.; Engels, D.; Pustilnik, S. A.; Ugryumov, A. V.; Kniazeva, T. F.; Pramsky, A. G.; Brosch, N.; Hagen, H.-J.; Hopp, U.; Izotov, Y. I.; Lipovetsky, V. A.; Masegosa, J.; Marquez, I.; Martin, J.-M. Astronomy and Astrophysics, v.366, p.771-787 (02/2001) . ... Pustilnik, S.; Kniazev, A.; Lipovetsky, V.; Ugryumov, A. Astronomische Gesellschaft Abstract Series, Vol. ... N.; Soboleva, N. S.; Temirova, A. V. Astronomische Gesellschaft Abstract Series, Vol. ...

Galactic coordinate system based on multi-wavelength catalogues Ping-Jie Ding, Jia-Cheng Liu, and Zi Zhu School of Astronomy and Space Science, Nanjing University, China Outline Introduction: why we need to establish a new Galactic Coordinate System ( GalCS ) Data and methods used to find a proper GalCS Results and conclusion Discussion 2 Introduction: why we need to establish a new GalCS The Galactic coordinate ... 3 The GalCS is defined by three parameters p , p and . ...

T he Siding Spring Survey (SSS) is a Near-Earth Object search program that utilises the 0.5-m Uppsala Schmidt Telescope at Siding Spring Observatory, N.S.W., Australia. ... The mission of the Siding Spring Survey is to contribute to the inventory of near-earth objects (NEOs), or more specifically, the potentially hazardous asteroids (PHAs) and comets (PHOs) that may pose a threat of impact and thus harm to civilization. ... Based on the CSS Mission page . ... Siding Spring Survey Main Page . ...

... JWST . ... Science Blog . ... JWST Science . ... Early Release Science Program . JWST Science Corner . ... The following graphics illustrates that all of the expected science and calibration areas are well represented in the SODRM 2012. ... Total Time [days] . Percentage of Total Time . ... NIRSpec Multi-Object Spectroscopy . ... Total Spectroscopy . ... The distribution of non-moving sources from all the SODRM programs is shown in galactic coordinates. ... Science Programs Summaries . ...

... Tonight's Sky . ... Constructing a 3-D map of the large-scale structure of the universe . ... Using the Subaru Telescope s new Fiber Multi-Object Spectrograph (FMOS), the team s 3-D map includes 1,100 galaxies and shows the large-scale structure of the universe 9 billion years ago. ... The current 3-D map of 1,100 galaxies shows the large-scale structure of the universe 9 billion years ago, spanning 600 million light-years along the angular direction and 2 billion light-years in the radial direction...

... Galaxies which were observed in the project . Location of vortex centers . Laboratory simulations . ... Vortex structure of NGC 157 . Vortex structure of our Galaxy . ... Line-of-sight velocity fields of gas with high precision and resolution are planned to be obtained for the sample of galaxies with regular spiral structure to reveal systematic deviation from circular rotation and to analyze it on the base of hydrodynamical models, which are in progress. ... Back to Laboratory Home Page. ...

B?rbel Koribalski (ATNF) + HIPASS and ZOA teams . Velocities are color coded in bins of 1000 km/s: . dark blue . ... light blue . cross . 1000 . green . ... HVCs? ... All the new galaxies, most of which are at |b| All the new galaxies are marked in blue, HI clouds in green and HVCs in orange. (plot by Malte Marquarding, aips++). bkoribal @ atnf.csiro.au ...

Large-Scale Structure of the local Universe with INTEGRAL observatory >200-300 , . ... It is now widely accepted, that practically every galaxy in the local Universe has supermassive black hole and some of these black holes are AGNs. ... 136 ( ) 49- . ... The map of the survey is shown on the left. ... Using Hard X-ray all-sky survey such important properties of nearby Universe as energetics of accretion to the supermassive black holes and large-scale mass distribution of matter were studied. ...

... Spectral energy distributions (SEDs) for active galactic nuclei (AGN) are made publicly available by computing self-consistent 2-phase AGN torus models. ... Dust extends from the dust evaporation radius, typically located between pc/10 Heymann Siebenmorgen (2012). We consider fluffy dust particles ( Kr gel Siebenmorgen , 1994). ... As an example we show below the SEDs of an AGN computed with diffuse ISM dust ( Siebenmorgen et al 2014) and fluffy grains ( Kr gel Siebenmorgen 1994) . ...

... The file names' construction . The flight (m) stage's file set . ... the orbital data used for the flight operation monthly (m) long-term planning, . ... The orbital calculations are based on the initial orbital data determined by KIAM RAN using the orbital radio measurements treatment.The determined initial orbital data are presented as a state vector (satellite position and velocity) in the J2000 reference. ... Accept the file with extension '.bgr', where the Moscow time (MT=UT+3h) is used. ...

... For an input list of EBOXDETECT source locations, simultaneous maximum likelihood PSF fits to the source count distribution are performed in all energy bands of each EPIC telescope. A description of the main properties of the detection algorithm may be found in Cruddace, Hasinger, Schmitt (1988). ... Note, that =1 in the case of the individual energy band detection likelihoods listed in source table rows with ID_BAND 0 and is equal to the total number of energy bands in the ID_BAND=0 summary rows. ...

... spectrum . ... The photons we detect originate in the outermost layers, or atmosphere, of the star. In order to interpret stellar spectra, it is necessary to construct models which accurately represent the structure of a stellar atmosphere and the transfer of radiation from the stellar interior into interstellar space. For the study of helium stars and other stellar remnants, we in Armagh use several computer programs, of which sterne and spectrum are the most important. sterne . ...

The above image is a computer simulation of the distribution of mass in a Dark Matter dominated Universe. ... Structure (\eg density enhancements) clearly forms at the intersection of these filaments. ... What is Dark Matter? ... Testing for the presence of dark matter in the solar neighborhood now becomes an accounting problem The possible sources of this mass in the solar neighborhood are 1) luminous stars, 2) interstellar gas, 3) stellar remnants (mostly white dwarfs) and 4) dark matter: . ...