To construct two-dimension distribution of minor planets user should specify elements/ parameters/ function that will be plotted as abscissas and ordinates. In three-dimension case one should add to them the element plotted on Z axis. ... Though you may choose elements plotted along different axes at will, often there is good reason to plot such elements as a, n, or n" along X axis (two-dimension distributions) and to plot them along Y axis in three-dimension case. ...

... We employ Stokes I and V LSD profiles of the co ol magnetic Ap star CrB, extracted for the elements Ti, Cr, Fe and Ba, to confirm systematic element-toelement differences in the longitudinal field variation of this star. ... 5 Mo deling the phase variations The longitudinal field and equivalent width variations of CrB potentially provide a useful method to probe the surface abundance distributions of this and other slowly-rotating magnetic stars. ...

Next: Pulsations Up: PHYSICAL CHARACTERISTICS Previous: PHYSICAL CHARACTERISTICS . The fundamental properties of RCBs may be deduced from their spectra at maximum light. ... The properties of a stellar atmosphere may be measured from both the large-scale features - the broad-band flux distribution - and the detailed spectrum of absorption lines. ... They show that, in general, hydrogen makes up less than one part per thousand down to less than one part per million of the stellar atmosphere. ...

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. ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

THE CHEMICAL COMPOSITION OF REGOLITH AT THE MOON'S SOUTH POLE, ACCORDING TO DATA OF LUNAR PROSPECTOR AND LUNAR RECONNAISSANCE ORBITER MISSIONS. ... Introduction: The article tells about the results of integrated study of the craters at the Moon's South Pole with permanently shadowed region of craters. ... We have compared the ultimate composition of the soil matters in the craters with "cold traps" in the Moon's South Pole with regard to thorium, ferric oxide and hydrogen contents (Fig. ...

... 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. ...

XMM­Newton CCF Release Note XMM­CCF­REL­135 EPIC MOS Spectral Response Distribution R. D. Saxton, S. Sembay 10 Dec 2002 1 CCF components Name of CCF VALDATE EVALDATE List of Blocks changed CAL VERSION XSCS flag EMOS1 REDIST 0020.CCF 1999­12­10 2000­07­15 CCD REDISTRIBUTION ­n 3.152 NO EMOS1 REDIST 0021.CCF 2000­07­15 2000­11­09 CCD REDISTRIBUTION ­n 3.152 NO EMOS1 REDIST 0022.CCF 2000­11­09 2001 ­04­18 ... Mos­1, epoch 1 (rev 62) imaging mode response, all patterns. ...

We have designed the laboratory model of static Fourier spectrometer for onboard usage for spectral study of atmosphere and ionosphere. The gain of model is to simulate onboard FS which will not have any moving elements (all its optical elements will be mounted at fused quartz monolithic construction), to compare experimental results with theoretical estimations and to measure MTF of CCD array. ... This fact connected with low frequency response of CCD array due to small format of it. ...

... The measured bolometric flux and corrected NPOI angular diameter yield an effective temperature of 8600+/-500 K. Least-squares comparisons of synthetic spectral energy distributions from 1220 Г: to 3.6 cm with the observations provide estimates for the effective temperature and the mass-loss rate of ~=8400+/-100 K and (8+/-3)Г-10-7 Msolar yr-1, respectively. ... ADS Citation Query . citations = 34 . citations vs. year [year,citations] . ...

... Posts tagged ?light curve? ... Posted by hlee . ... Tags: book , Brieman , cigar , Clinton , data mining , Friedman , Hastie , KDD , light curve , machine learning , SCMA , shaking hands , SN , statistical learning , Supernova , Tibshirani . Category: Algorithms , Cross-Cultural , High-Energy , Jargon , Methods , Quotes , Stat , Uncertainty | Comment . ... Click for what was appeared in arXiv this week. ... Category: arXiv , Data Processing , gamma-ray , Objects , Spectral , Timing , X-ray | ...

... Variation of systematic errors for USNO A2 (in mas per year) 23 .914 0.082 0.250 0.418 0.586 0.753 0.921 1.089 1.257 1.425 1.593 4 4. 3. 3. 3. 3. 3. 3. 3. 3. 3. 15 ± 7± 1± 3± 3± 10 ± 10 ± 11 ± 6± 10 ± 12 ± and their errors USNO UCAC USNO UCAC A2.0 2 3 B1.0 4 (1998) (2006) (2003) (2012) 37 27 11 4 732 529 778 501 050 078 775 387 (34 610 829) (17 209 447) (9 744 401) () Distribution of observations ( ...

... The MMT optical spectra of SBS 0335-052W were obtained on 1996 January 19 with the Red Channel of the MMT Spectrograph. ... The linear scale is 1 = 263 pc at the distance to SBS 0335-052W of 54.1 Mpc. ... In Table 1, the observed line intensities and intensities corrected for interstellar extinction for SBS 0335-052W are shown along with extinction coefficient C (H ), observed flux of the H emission line, the equivalent width EW (H ) and equivalent width of absorption Balmer hydrogen lines EW (abs)....

... This represents the first HI selected sample covering the core and the outskirts of a local cluster of galaxies. ... Optically selected samples miss a considerable number of low luminosity, low surface brightness galaxies underestimating by almost a factor 2 the number of HI rich galaxies present in the cluster volume. ... Right: The g band luminosity function for galaxies in the A1367 volume as obtained from the optically (circles) and HI (histogram) selected sample. ...

The antenna element Ravi ATNF, Narrabri 1. ... Miriad works out the radio Parabolic reflector: A parabolic reflector adds all the fields from a surface = aperture at a focal point. ... Feeds are `compact' and `corrugated' horns The inner profile is curved The inner surface has grooves Cross-section of a horn Sub-reflector 28 main-reflector Feed horn O `optical axis' The feed horn adds all the rays that come from the 28 deg. wide sub-reflector. The feed down-weights rays that come off-axis. ...

... We have developed an integrated system that performs astronomical observations in Near Infrared bands operating two-dimensional instruments at the Italian National Infrared Facility's ARNICA and LONGSP . ... The user interface is organized as widget-based X11 client. ... 1993; Di Giacomo et al. 1993). ... Moreover, if the interprocess communication interface includes support for networking, the software immediately becomes network distributed software. ... DESQview/X User Guide 1993, Quarterdeck . ...

DIGITAL WDC EXCHANGE FORMAT . FOR OBSERVATORY 1.0 MINUTE VALUES 1. ... DATA-1 .. DATA-60 are 1-minute values of the given element for that hour. ... Typically, digital 1-minute values received by WDCs from organizations operating automatic magnetic observatory instruments are averages of more frequendy sampled values, e.g. 10-second point samples. ... If the method used to obtain 1-minute average values is important to a user, the WDC will assist in determining the exact procedure applied. ...

... 2002 August 20 . The Universe in Hot Gas . ... Explanation: Where is most of the normal matter in the Universe? ... The above image derives from a computer simulation showing an expected typical distribution of hot gas in a huge slice of the universe 2.7 billion light-years across and 0.3 billion light years thick. The distribution of much more abundant dark matter likely mimics the normal matter, although the composition of the dark matter remains mysterious. ... About APOD | ...

... The accuracy of calculation of both INTERBALL spacecraft (SC) motion has been estimated at the IKI. ... The 30 days measuring intervals were used during the Tail probe (TP) orbital data treatment, and 15 days intervals - during the Auroral probe (AP) orbit determination. ... http://www.iki.rssi.ru/vprokhor/indap.htm for the Auroral probe; . http://www.iki.rssi.ru/vprokhor/indtp.htm for the Tail probe . ... http://www.iki.rssi.ru/vprokhor/ssc.htm , or http://www.iki.rssi.ru/vprokhor/amisan.htm . ...

An Ancient Universe: How Astronomers Know the Vast Scale of Cosmic Time . ... d) The Age of the Chemical Elements . ... Some isotopes (forms of the element with different numbers of neutrons in the nucleus) of these elements are radioactive; they change into other isotopes at a rate that can be measured accurately in the laboratory. ... The Ancient Universe - The Age of the Expanding Universe - The Age of the Oldest Stars - The Age of Light From Distant Galaxies - The Age of the Chemical Elements | ...