... 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. ...

... (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 [ ...

... 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 ) ...

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. ...

... 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 . ...

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. ...

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. ...

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 _ ...

... 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. ...

... 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. ...

... 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) . ...

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