... About ATNF overview . ... Both are consistent with earlier estimates, computed for the population of optically selected galaxies. This consistency occurs because, although the distribution of optical central surface brightnesses among galaxies is flat, we fail to find a population of galaxies with central surface brightnesses fainter than 24б  B - , even though there is no observational selection against them. Keywords: Galaxies: Luminosity Function, Mass Function; Surveys . ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... Астронет | ... Переменные Звезды | ... Микролинзирование . ... На протяжении последних нескольких лет в рамках проекта MACHO проводятся наблюдения микролинзирования звезд Большого Магелланова Облака - спутника нашей Галактики. Эффект микролинзирования заключается в гравитационной фокусировке света звезды массивным объектом, находящимся на луче зрения между звездой и наблюдателем. ... Согласно некоторым гипотезам, линзами могут являться реликтовые черные дыры или "нейтралинные звезды". ...

... 2001 June 14 . Around The Arches Cluster . Credit: X-ray; NASA / CXC / Northwestern / F. Zadeh et al., IR; NASA/ HST /NICMOS, . ... Explanation: The most compact cluster of stars known in our galaxy, the Arches cluster , boasts 100 or so massive, young stars contained within a diameter of one light-year. ... Astronomers consider the tightly packed and relatively nearby Arches cluster, an analog of the furious star forming regions in galaxies millions of light-years away. ... About APOD | ...

... Science Activities > PhD Thesis Topics offered by ESO Faculty Members > Thesis Topic: Dynamical models of multiple globular cluster populations around massive galaxies . ... Different techniques have been devised to separate multiple GC populations and perform dynamical analyses. ... Within this project, the PhD candidate will examine mock models of multiple GC populations around massive galaxies, devising `blinded' functional tests and comparing the possible sources of bias in different techniques....

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

Dust emission from the Type II supernova SN 2002hh in NGC 6946 has been detected at mid-infrared wavelengths by the Spitzer Space Telescope from 590 to 758 days after outburst and confirmed by higher angular resolution Gemini North mid-IR observations. ... The minimum emitting radius of 1.1У?1017 cm is too large for the emitting dust to have been formed in the supernova ejecta. ... ADS Citation Query . citations = 25 . ... 2006,6][2007,4][2008,2][2009,4][2010,2][2011,3][2012,1][2013,2][2015,1] . ...

... According to the most popular cosmological paradigm, the greater part of the galaxy mass is accumulated in the dark matter halo. ... The polar ring galaxies (PRGs) reveal external rings or disks of gas, dust and stars rotating in a plane roughly perpendicular to the disk of the central galaxy. ... The shape of the dark halo in the model was chosen so as to achieve the best fit to the observed rotation of both galaxies themselves and their polar rings. ... The SPRC-7 galaxy. ...

I will present theresults from a deep, extended, planetary nebulae survey in a 0.5 sqdeg region centered on the brightest cluster galaxy NGC 4486 (M87) in the Virgo cluster core, carried out with SuprimeCam@Subaru and FLAMES-GIRAFFE@VLT. ... A substructure detected in the projected phase-space of the line-of-sight velocity vs. major axis distance for the M87 halo planetary nebulae provides evidence for the recent accretion event of a satellite galaxy with luminosity twice that of M33. ...

... Resembling a gigantic hubcap in space, a 3,700 light-year-diameter dust disk encircles a 300 million solar-mass black hole in the center of the elliptical galaxy NGC 7052. ... Because the front end of the disk eclipses more stars than the back, it appears darker. ... Despite its size, the disk is 100 times less massive than the black hole. ... The bright spot in the center of the disk is the combined light of stars that have crowded around the black hole due to its strong gravitational pull. ...

... St Petersburg 23, September 2014 1 Motivation · Origin of Martian moons? ... Considered error sources: ­ Phobos a priori ephemerides; ­ Phobos a priori GM value; ­ measurements noise; ­ different strategies; · Methods: ­ real data analysis; ­ simulations. ... St Petersburg 23, September 2014 8 Simulations: sensitivity of the measurements to the a priori GM value Simulations: zero noise+ IMCCE a priori ephemerides +GMPH = 7.16 * 105 m3/sec2. ... St Petersburg 23, September 2014 14 Thank you! ...

Orbital intersection . ... Structure of Taurid stream . ... Meteoroid swarm and Taurid fireballs . ... The following four diagrams schematically show four different Taurid orbits and the orbits of Earth and Jupiter. ... The Taurid stream contains particles (small, solid grains) at different stages of their precession cycles. ... The study of when a meteor stream can produce a meteor shower is the study of when precession brings orbits to intersection with Earth, or e.g. with Mars . ...

Space Cowboys Odissey: Beyond the Gould Belt S e r g e i P o p o v, B e t t in a P o s s e lt (co-authors: F. Haberl, R. Neuhauser, J. Truemper, R. Turolla) astro-ph/0609275, 0710.1547 and work in progress The new zoo of neutron stars During last >10 years it became clear that neutron stars can be born very different. ... Solid ­ new abundances, old mass Dotted ­ old abundances, old mass Dashed ­ new abundances, new mass 13 Population synthesis ­ II. recent improvements 3. ... These sources are hot. ...

... This talk focuses on exploring the connection between Ly absorbers and galaxies. The theorist view of gas in the low z universe is based on the filamentary structures that are evident in simulations based on the CDM paradigm. ... The observer's view of gas in the low-z universe is based on the Ly absorbers which have column densities as low as 10 cm , while galaxies are at column densities of 10 cm . ... The absorber has N cm . ... Can examine LSS defined by gas-rich galaxies around absorbers. ...

... Visible Distribution of Galaxies. ... Features of Elliptical, Lens-Shaped, Spiral and Irregular Galaxies. Galaxies with Bar. ... Distribution of Surface Brightness of Surface and Spiral Galaxies. ... Color Characteristics of Galaxies. ... Methods of Galaxies' Mass Determination. ... Hidden Mass of Spiral Galaxies. ... Features of Dark Matter Distribution in E and SO Galaxies. ... The Whole Number of Galaxies and Their Density by the Results of Observation on the 'Hubble' Space Telescope. ...

Dust around Herbig Ae/Be Stars: Porous, Cometary-like Grains? ... This brings up the question, which we try to answer here, of how the grain porosity affects the observational manifestations of the dust shells of HAeBe stars: the excess infrared emission, anomalous extinction in the ultraviolet, and the peculiar behaviour of colour indices and linear polarization during deep brightness minima observed for about 25% of HAeBe stars (UX Ori, WW Vul, etc). ...

Our publications in 1996 year . Lindner, U.; Einasto, M.; Einasto, J.; Freudling, W.; Fricke, K.; Lipovetsky, V.; Pustilnik, S.; Izotov, Y.; Richter, G. Astronomy and Astrophysics, v.314, p.1-12 (10/1996) . Thuan, Trinh X.; Izotov, Yuri I.; Lipovetsky, Valentin A . ... Edited by Daniel Kunth, B. Guiderdoni, M. Heydari-Malayeri, and Trinh Xu Thuan, 1996., p.607 . ... Edited by Daniel Kunth, B. Guiderdoni, M. Heydari-Malayeri, and Trinh Xu Thuan, 1996., p.587 . ... Thuan, Trinh Xuan; Izotov, Yu. ...

The LCDM paradigm: successes and challenges on scales of galaxies Anatoly Klypin (NMSU) LCDM · · · · DM profiles, concentrations, .. Clustering of galaxies: P(k) and correlation functions Satellites: abundance, number-density profiles Galaxies and Dark Matter: abundances Dwarfs. ... Springel et al 2008. ... Klypin et al 2010. ... Observations - LCDM: just enough Magellanic Clouds Observations LCDM Vmax > 50 km/s Busha et al 2010 Dark matter profiles: standard LCDM Aquarius simulation. ...

... What are the fluxes of the stars? ... Volume sampled is no longer 4/3 pi r cubed due to curved space-time Want to derive population properties brightness, size, etc - as function of distance (therefore, cosmic time) But - biases in sample Biases NUMBER OF STARS VS MASS Eddington Bias: in astronomy, there are always more little faint things than big bright things. ... Suppose there are 10 stars of mass 0.5 and 100 stars of mass 0.4, and you have a 20 percent error on measuring the mass. ...

Scale-heights of the Galactic disk subsytems with different ages and metallicities . V.Marsakov & Yu. ... It is based on the fact, that all stars cross the disk plane several times during their Galactic orbital period. ... We have used our representative sample of nearby disk F2-G2 stars Marsakov & Shevelev (1995) in which fundamental stellar parameters was determined on the basis of published date on uvby-photometry, proper motion and radial velocities. ... Marsakov V.A., Shevelev Yu.G. Bull. ...