In order to calculate the line profile of a given absorption line for atomic species Z with a wavelength LAMBDA (in Angstroms) and a microturbulent velocity VT (in km/s). ... mode . ... 1) The input model may contain more than one model (i.e. it may be an entire grid of models). Spectrum will cycle through this grid NMOD times, omitting NSKIP-1 models from the . ... However, the input data following MODE must be repeated NMOD times in order to obtain equivalent results for each model in the grid. ...

... 3p5.3d . ... 1s.3p6.3d . ... 57558696 . ... 57559503 . ... 57561923 . ... 2p5.3p6.3d . ... 1.08e-01 . ...

... HST . ... Data . ... HST Peer Review Process . ... HST Overview . Overview . ... Phase I Proposing . ... Phase II Cycle 23 . ... Retrieving HST Data . ... Data Analysis . ... Column 1: Wavelength (in Angstroms) Column 2: Earthshine intensity (in erg/sec/cm^2/Angstrom/arcsec^2) Column 3: Zodiacal intensity (in erg/sec/cm^2/Angstrom/arcsec^2) Column 4: Total background intensity (sum of columns 2 and 3) 1000 4.8E-23 7.3E-29 4.8E-23 1100 8.8E-22 6.0E-27 8.8E-22 1200 8.0E-23 6.1E-26 8.0E-23 1400 8 ...

by I.M. Chertok, V.V. Fomichev, A.A. Gnezdilov, R.V. Gorgutsa, V.V. Grechnev, A.K. Markeev, R.W. Nightingale, and D.E. Sobolev . Fig. 2. Inverted TRACE images at 195 illustrating development of the EUV post-eruption arcade with the well-organized loop, two-ribbon, and spine structures. Note that the exposures have been rescaled to the same peak intensity to show the evolution of the bright elements. The field of view is 220.5 by 182 Mm. Back to paper .

Next: Wavelength calibration Up: Wavelength calibration Previous: Wavelength calibration . The detection of arc lines in the wavelength calibration frame .bdf is done by . SEARCH/MOS . ... PLOT/SEARCH . you will get a plot of the x-positions of all found arc lines versus the CCD rows. If you do not know the central wavelength and mean dispersion of the grism you used you have to identify at least two arc lines in any row of any slitlet. IDENTIFY/MOS . ... As frame it will use .bdf. ...

... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...

... The calibration of astrophysical spectra in wavelength based on calibration lamp data suffers from different kinds of uncertainties. Besides inaccuracies in the observational phase, common data reduction practice adds ``pixelation'' errors, due to the fact that the centering method does not use the correct PSF. These model mismatch errors depend, for a given feature, on the sub-pixel location of the line center (David & Verschueren, private communication). ...

... Observatory . ... Science . ... Science Users Information > Data Handling and Products > Data Reduction FAQ > There are few ThAr lines in my wavelength calibration spectra, what do I do? ... Observing Facilities . ... Observing with ESO Telescopes . ... Data Pipelines and Calibrations . ... ESO Data . ... In order to obtain a good wavelength solution with CRIRES, you should have at least two or three ThAr lines visible on each detector, preferably well spaced, at least for a 2nd order polynomial. ...

... The minimum precision occurs at x = 0.1 and is approximately equal to precision(1d0)-1. subroutine getBBfluxPerMetre(angstromValues, kelvin, powerValues) real(double), intent(in) :: angstromValues(:), kelvin real(double), intent(out) :: powerValues(size(angstromValues)) end subroutine getBBfluxPerMetre function bbFluxPerMetre(angstroms, kelvin) result(power) real(double), intent(in) :: angstroms, kelvin real(double) :: power end function bbFluxPerMetre . ...

... People . Posts tagged ?wavelength? ... One of the biggest culprits is the unit of energy, [keV], Continue reading ?keV vs keV [Eqn]? Tags: Angstrom , Boltzmann , EotW , Equation , Equation of the Week , erg , Kelvin , keV , Planck , temperature , units , wavelength . ... 1 Comment . ... Entries RSS . ... vlk on [MADS] Parallel Coordinates . upvc windows on [MADS] Parallel Coordinates . ... Alfred Inselberg on [MADS] Parallel Coordinates . ... Entries (RSS) and Comments (RSS) . ...

Main Page Data Structures File List Data Fields Globals . Data for OI_WAVELENGTH FITS table. ... int . ... char . ... float * . eff_wave . ... eff_band . Data for OI_WAVELENGTH FITS table. int _oi_wavelength::revision . char _oi_wavelength::insname[FLEN_VALUE] . int _oi_wavelength::nwave . float* _oi_wavelength::eff_wave . float* _oi_wavelength::eff_band . The documentation for this struct was generated from the following file: . ...

... This file table3 82 660 Observed wavelengths, laboratory values and identifications -------------------------------------------------------------------------------- Byte-by-byte Description ... Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- SpOrd Spectrum order 5- 12 F8.3 0.1nm SolLam Wavelength determination of all solar and telluric lines measurable on the ... Note (6): J: Junkes et al., ...

False-color image of the dark cloud Barnard 68, prepared using data from the Herschel Space Telescope at different far-infrared wavelengths. ... This could be a cloud fragment in collision with Barnard 68. The wavelengths for the images are 100, 160, 250, and 350 micrometers, respectively. The image colors show the intensity of the radiation received at that wavelength, from purple and blue at low intensity to high intensities in red and white. ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Tips on holding a viewing night . ... Multi-Wavelength View of the Interstellar Medium in the Large Magellanic Cloud . ... The Large Magellanic Cloud (LMC) has been surveyed in optical emission lines, X-rays, radio continuum, H I , and CO lines. ... Keywords: Magellanic Clouds - galaxies: ISM - ISM: general - ISM: structure - ISM: bubbles - supernova remnants . ... Structures of the Interstellar Medium in the LMC ...

Multi-Wavelength investigations of the Sun and modern problems of solar activity . ... Conference participants: . ... Altyntsev A.T. altyntsev@iszf.irk.ru . ISZF . ... Ussuriysk Astrophysical Observatory RAS . ... Pulkovo Observatory . ... Vasil'eva V.V. solar@narzan.com . MAS Pulkovo Observatory . ... Crimean Astronomical Observatory . ... grechnev@iszf.irk.ru . ... vgrig@iszf.irk.ru . ... Grigor'eva S.A. sgrig@iszf.irk.ru . ... Gubin A.V. gubin@iszf.irk.ru . ... ivanoff@iszf.irk.ru . ...

. Multi-Wavelength investigations of the Sun and modern problems of solar activity . SAO RAS . Nizhnij Arkhiz, September 28 - October 2, 2006. HOME . ORGANIZERS . REGISTRATION . PROGRAM . ABSTRACTS . PARTICIPANTS . CONTACTS . LOCATION . 1ST ANNOUNCEMENT . This page is not prepared yet. Copyright © 2006 SAO RAS . | RFBR | RAS | SAO RAS | MAO RAS | RATAN-600 |

... 1419.977 . ... 1419.978 . ... NaN . 0.00E+00 . ... 1420.021 . ... 1420.023 . ... 1420.024 . ... 1419.976 . ...

... Sum in visible - 500 k R . ... 16.4 nsec . ... Auroral, . ... 0.2 . ... Sum - 10-100 . 250 . ... Sum - 20-400 . ... sum –500 . ... Sum - <10R . ...

spaceweb@oulu.fi - last update: 12 February 1999, 1015 UT . Sun emits radio energy with a slowly varying intensity. This radio flux, originating from atmospheric layers high in the Sun's chromosphere and low in its corona, changes daily with the sunspot number, and thus also follows the solar cycle . This is seen from the figure displaying the flux at 2800 MHz or 10.7 cm wavelength over the entire solar disk (in here, monthly averages, although daily values exist too). ...

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