... DEC - As above . LII - Galactic longitude computed from the RA above . BII - Galactic latitude computed from the DEC above . M_STD_COL - The standard M magnitude that was calculated when the standard COL colour was calculated (M stands for one of the filters and COL the instrumental colour that was used - NB THE FILTERS FOR ALL COLOURS ARE THE XMM CODES LISTED EARLIER). ERR_M_STD_COL - The error of the standard M magnitude. ...

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... (FIRPO-TIRGO) w/error AR, Sun Aug 24 10:34:33 MET DST 1997 ############################################################# Sp:K4 irc10007 J 1.509 0.028 irc10007 J 1.65+/- 0.06 [ 0.05 ] 0.14 0.09 irc10007 H 0.961 0.006 irc10007 H 1.03+/- 0.04 [ 0.04 ] 0.07 0.05 irc10007 K 0.606 0.040 irc10007 K 0.85+/- 0.05 [ 0.03 ] 0.24 0.09 Sp:M2 irc10024 J 2.099 0.028 irc10024 J 2.31+/- 0.04 [ ...

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• CHIANTI atomic database
• The Arcetri Spectral Code file format
• CHIANTI: c_4_elvl

... User Guide ] Task: clstats Purpose: Calculate dispersions, masses, etc for each clump from clfind file Categories: utility The mass is calculated in the following way; we define X such that, X * (sum T) * delv = column density of molecular hydrogen in units of 10^20 cm-2 which implies that to convert to a mass, multiply by 10^20 * meanmol * m(H_2) * Area Key : in file name of data cube (no default ) ...

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• casacore: DerivedMC_module
• colden
• casacore: casa::UDFMSCal Class Reference

Using Ly alpha line profiles generated from a grid of M dwarf model atmospheres we calculate the attenuation factor [i.e. Ly alpha (obs)/ Ly alpha (intrin)] due to the interstellar medium as a function of hydrogen column density. ... The major uncertainty in this work has been the interstellar hydrogen column density, emphasizing the need for further work in this area and in particular an accurate model of its variation in all directions. ...

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... We cannot use for this purpose equivalent widths and profiles of HI lines (well known criteria of atmospheric conditions for normal supergiants), since these lines are strongly distorted in the spectrum of IRAS04296 as seen in Fig. ... Figure: Upper: iron abundance FeI (circles) and FeII (crosses) calculated for IRAS04296+3429 with model parameters , and using lines with different excitation potentials EP of a low level; bottom: the same as a function of the equivalent width W . ...

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This diagram shows the six superimposed "layers" of the CSS table model. This diagram illustrates the algorithm for calculating a cell's final background. ... The diagram shows how, looking down on the six rectangles, one may compute the background color of each cell. ... A cell without a background color in the top layer is depicted as a "window" onto the lower layers, which give its final background color. ...

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Next: *upspecrdf, downspecrdf* - Transform Up: Spectral Analysis Previous: *grid_plot* - Plot Results . The conversion of count rate to flux depends on the intrinsic spectrum of the source, so xflux must be used in conjunction with fit . Fit generates a table of the best fit intrinsic spectrum ( _int.tab extension). xflux uses this table to calculate either the integrated flux between two energy limits or the flux density at a specific energy. ... This produces ``..._obs.tab'' file. ...

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• *tprint* - Reading a Table File Created by imcnts

CALSPEC: 2004 June 15 . ... CDBS Files of the Flux Standards with Columns in Order of Preference(1) ------------------------------------------------------------------------------- Star name V B-V CDBS name Model STIS FOS+Oke IUE+Oke (1) (2) (3) (4) (5) (6) (7) (8) AGK+81D266 11.94 -0.34 AGK_81D266 _ STIS_001 _ 005 ALPHA-LYR 0.03 0.00 ALPHA_LYR _STIS_002 _004 BD+17D4708 9.47 0.44 BD_17D4708 _ STIS_001 BD+25D4655 9.69 -0.31 BD_25D4655 _002 BD+28D4211 10.51 -0.34 BD_28D4211 _ STIS_001 _ FOS_003 _ ...

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• Analysis of in B-Type Stars
• Correcting ETC Calculations of CCD Spectral Observations for CTE Effects
• Update to the COS FUV Dark Rates and Impact on ETC Calculations for Background

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

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• Enhancements of MKRMF

... The first column gives the star identification number, followed by X, Y positions in mm. The zero point of these offsets is star number 1 which lies at 21:24:20.52 +36:30:25.6 (equator and equinox 2000). Next are relative proper motions (muX and muY) and their errors (ex and ey) in 10**4 arcsec/yr, followed by calculated V magnitudes. The final column gives the calculated membership probabilities in percent. ...

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... The less then 5 degree value of the relative geocentric angular distance between the footprints of the SC is used as a criterion of the magnetic conjugation. ... On the last column of the file is shown the magnetic field model version ( MOD IOPT ) used during magnetic mapping. ... The difference between CMLT values of the Sat.1 and Sat.2 (see as well column 11) . ... dcorlat = dla (deg) . The difference between CORLAT values of the Sat.1 and Sat.2 (see as well column 12) . ... AnD (deg) . ...

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• STDA files

... Индексы солнечной активности . ... Наблюдения NGDC . Солнечные регионы . ... Среднегодичные индексы солнечной активности . Визуальные индексы солнечной активности по версии Национального центра геофизических данных . ... 0.06 . ...

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• The Sunspot Observer - Visual indices of solar activity - NGDC
• The Sunspot Observer - Average annual indices of solar activity
• Солнечное Обозрение - Среднегодичные индексы солнечной активности

pshistogram - Bin data and plot histograms pshistogram file -Jx xscale [/ yscale ] -W bin _ width [ -2 ] [ -A ] [ -B tickinfo ] [ -C ] [ -E azimuth / elevation ] [ -G fill ] [ -H[ nrec ] ] [ -I[o] ] [ -K ] [ -L pen ] ... [r] ] [ -S ] [ -U[ / dx / dy / ][ label ] ] [ -V ] [ -X x - shift ] [ -Y y - shift ] [ -Z type ] [ -c copies ] [ -bi[s][ n ] ] pshistogram reads the first column from file [or standard input ] and calculates ... L Draw bar outline using the specified pen thickness. ...

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• Calculation of binary NS coalescence rates
• The COOC Criterion (Criterion of Observations versus Calculations)
• Results of calculations

... AVERAGE/AVERAGE Compute simple average of all pixels in a subimage . AVERAGE/COLUMN Compute average of image columns . AVERAGE/IMAGE Calculate the average of images . AVERAGE/ROW Compute average of image rows . ... COMPUTE/COLUMN Perform arithmetic expression on image column . COMPUTE/IMAGE Compute arithmetic expression of images . COMPUTE/PIXEL Perform arithmetic operations on images using . ... COMPUTE/ROW Compute arithmetic expression on image scan lines . COMPUTE/.. ...

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• HyperLEDA documentation: parameter: bt
• Documentation: LEDA: parameter:
• Emission-line galaxies

... 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 ( ...

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• Structure of the database files
• Datafile structure

... Here is another interesting aspect of the A1863 data. ... The delta columns show the difference between the entries in the current row and the previous row: *AST* *Cal * *delta AST* *delta Cal * 67856 0.05 68302 0.02 446 -0.03 68749 -0.01 447 -0.03 69197 -0.04 448 -0.03 69643 -0.05 446 -0.01 70090 -0.02 447 0.02 70538 0.01 448 0.03 70985 0.04 447 0.03 71954 0.04 969 0.01 The time intervals are very evenly spaced at about 7min27sec with fairly consistent steps. ...

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• http://www.naic.edu/~gibson/galfa/igalfa/docs/poster_2014_aas_hughes_full.pdf
• Alfa_ang - IDL procedure for calculating the optimum rotation angle for ALFA
• Rotang - IDL procedure for calculating the optimum rotation angle for ALFA

... SiD workshop, Fermilab, April 9-11 2007 April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 1 Topics 1. ... What and how was simulated What and was One column clusters effects Accepted background density Hit reconstruction efficiency Hit efficiency How to improve efficiency Conclusions April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 2 What is this April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 3 Marty's idea Shift charge in neighboring columns in opposite directions. ...

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• QSO Absorption Lines and Other Cosmological Probes
• THE HUBBLE LAW JAVA APPLET
• Redshift Tutorial

... ОТЧЕТЫ СТУДЕНТОВ О ПРАКТИКЕ В САО . Лето 2001 года . ОТЧЕТ . ... Золотухина Ивана . ... 0.07 . ...

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... R P is the perigalactic radius and R a , the apogalactic radius. Z max is the maximum deviation of the star from the Galactic plane. THe dotted curve shows the position of the Galactic plane. The hatched horizontal band shows schematically the band in Z , where the probability of that location of the star was calculated. The vertical band shows the width of the column in which we reconstruct the star distribution in Z . ... next figure | previous figure . ...

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• Vladimir Marsakov Abstracts

... Classes . ... Class List . Class Hierarchy . Class Members . Dust :: AttSlab . include < attslab.hxx > . Collaboration diagram for Dust::AttSlab: . ... AttSlab ( RadField *InputRF, BNLib::UnaryDD *AbsXSect) . RadField * . MkRF (double n) . Calculate the attenuated radiation field as a function of column density . RadField * Dust::AttSlab::MkRF . double . ... Return the radiation field at column density n into the slab . ... attslab.hxx . attslab.cxx . ...

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• Command line interface to libAIR and water vapour column retrieval Bojan
• A Calculation of derivatives
• Zernike Polynomials Bojan Nikolic web pages (r. 329)