Next: Selection and Multi-Source/Multi-Frequency Datasets Up: Visibility Data Concepts Previous: Selecting UV Data in . A Miriad visibility dataset can contain simultaneous observations at multiple spectral bands, or spectral windows. ... When there are multiple spectral windows, channels are still numbered from 1 to N , where channel 1 is the first channel of the first spectral window, and channel N is the last channel of the last spectral window. ... line=channel,1 . ...

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• Handling large spectral bandwidths
• Spectral Line Processing and RPFITS files
• Spectral Line Processing and FITS files

... Table: List of Templates in the Kinney-Calzetti Atlas File Name Spectral coverage Comments (angstroms) elliptical_template 1235 - 9935 - bulge_template 1235 - 7545 - s0_template 1235 - 9940 - sa_template 1235 - 9940 - sb_template 1235 - 9940 - sc_template 1235 - 7660 - starb1_template 1235 - 9945 starburst with E( B-V ) 0.1 starb2_template 1235 - 9945 starburst with 0.11 E( To the KINNEY-CALZETTI Spectral Atlas of Galaxies . ...

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• An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies
• L and M dwarf spectral standards
• Spectral Types

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

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• Structure of the Spectral Package
• Notes on IPC and PSPC Spectral Fitting
• *upspecrdf, downspecrdf* - Transform between RDF and pre-RDF spectral tables

The following files list line and continuum emissivities from the Arcetri Spectral Code. ... Ne = 10^8 g-zipped file (phot cm^3 s^-1); Ne = 10^8 g-zipped file (erg cm^3 s-1) . ... File format (html): File format for the continuum files . ... File format (html): File format for binned line emission files The following files list transitions whose emissivities have values greater than a fixed amount (10^-19 phot s^-1 cm^+3 and 10^-30 erg s^-1 cm^+3 respectively): . ...

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• The Arcetri Spectral Code - E.Landi and M.Landini (2002)
• The Arcetri Spectral Code - E.Landi and M.Landini (1998)
• The Arcetri Spectral Code - E.Landi and M.Landini (2001)

... Thomson's multiple window method of spectral estimationthomson provides a very good estimate of the power spectrum by measuring the energy contained within a collection of rectangular shaped frequency intervals. ... Often, much of the fine structure of a spectral estimate is due to noise. It should be stressed that while other methods of spectral estimation (such as the Welchoppenheim method) exist, the Thomson method is particularly noteworthy for its precisely defined rectangular frequency bins. ...

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... Spectral extraction is implemented in the task omgrism , which runs over all sources in the source list (created by omdetect ), cross-identifies the zero- and first-order spectra and decides which of them are usable for extraction. ... Omgrism allows spectral extraction using three possible algorithms: simple summing of counts above background in the cross-dispersion direction; one-dimensional Gaussian fit; and Optimal Extraction (Horne's algorithm [ 2 ]). ...

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• OGIP spectral products

... Подставки под телевизоры и Hi-Fi . ... Теплая детская шапка-бини Reima Auva идеально подойдет для прогулок в прохладное время года. ... Современный дизайн и расцветка делают эту шапку модным и стильным предметом детского гардероба. ... Цвет: разноцветный . Коллекция: Весна-лето 2016 . ... Пол: Мужской . ... Цвет: мультиколор. ... Сезон: Весна-лето 2016. ... Цвет: черный . ... Цвет: белый . ... Пол: Женский . ... Цвет: синий . ... Barkan 34.C.B 4D кронштейн - Barkan - Barkan . ...

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Next: Conclusions Up: Selection Effects Previous: Inconsistent (or Inconsistently Applied) . Another possible bias, present in this as well as all other surveys which use spectral indices based upon nonsimultaneous data in their selection process, is due to variability. ... In order to minimize the effect of non-simultaneous radio survey data upon our samples, we decided to expand the common definition of flat-spectrum radio sources to extend to (instead of 0.5). ...

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• ESO - Improvement to FLAMES Spectral Resolution and Sensitivity
• ESO - New GIRAFFE Spectral Resolutions Characterised For All Settings
• ESO - Availability of Science Grade UVES and X-shooter 1D Spectral Data...

... 41Kulkarni+ J/A+AS/82/41 Spectral index for B3 radio sources (Kulkarni+ 1990) ================================================================================ Spectral index distribution for a sample of sources from the B3 catalogue. ... For 429 of these sources flux density measurements at 1410MHz are also presented. ... This file table1 70 770 List of the observed sources, their flux densities and spectral indices table3 44 22 The median spectral index {alpha}_med_ values for different samples. ...

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• Spectral types
• Spectral properties of X-ray loud e/g sources
• Spectral observations and data reduction

. Next: A Quick Look Up: Spectral-Line Observing at AO Previous: THE SOURCE LIST . This section describes using the AO-Control GUI - a graphical user interface (GUI) to the Arecibo observing/datataking system - for spectral line observations. If you would like more information on the general properties of the GUI, go to http://www.naic.edu/ aoui . Subsections . A Quick Look . The Details . Useful Stuff . koneil@naic.edu

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• spectral jumps vs A/D and pshift levels
• INTRODUCTION to Spectral Line Observing at AO
• spectral_jumps_at_powers_of_2

Next: Methods for Structuring and Searching Very Large Catalogs . ... We have explored two automated classification methods: supervised classification using Artificial Neural Networks (ANN) and unsupervised classification using Self Organized Maps (SOM). These methods are used to classify IUE low-dispersion spectra of normal stars with spectral types ranging from O3 to G5. This paper describes the application of automated methods to the problem of the classification of stellar spectra. ...

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• ADASS 2003 Conference Proceedings
• Automated Spectral Reduction in the IRAF Fabry-Perot Package
• ADASS 2002 Conference Proceedings

... Three or four lectures on isoperimetric inequalities in infinite groups (October) . ... Nash inequalities are useful tools to estimate the rate of decay of return probabilities in term of the spectral geometry of the space (isospectral profile). ... The isospectral profile can be estimate with purely geometric tools: isoperimetric inequalities and Folner couples. 3) Isoperimetric inequalities. ... The Erchler-Gromov isoperimetric inequality for wreath products is an entropic inequality. ...

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• Spectral theory (Spring 2003)
• Workshop on geometric analysis and spectral theory. Abstracts
• Workshop on geometric analysis and spectral theory. Schedule

... December 21, 1997 . ... Advantages are briefly discussed of gaining in spectral resolution, which is accompanied by losses in signal level, as compared with the attempts to improve the accuracy of measurement of line parameters by means of rising the S/N ratio alone with increasing the exposure time. To partially solve the problem of observations of faint objects at the BTA a new design echelle spectrometer is proposed. high resolution spectroscopy . ...

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• Spectral energy distribution
• Feed cabine #2 for spectral observations
• Spectral Devices

... The Wide Field Spectral Imager ( WISPI ) seen here in the Roll Roof Facility provides visible and near-infrared spectra of the sky across 4 degree fields. ... A computer controlled mounting automates the acquisition of 2-D rastered spectral images. ... Light from the sky enters the large 400mm lens at top center, is imaged on the slit, collimated by the smaller 180 mm lens, and diffracted by the grating at the bottom toward the 200mm lens and CCD camera on the right. ... Camera - 200mm f/2 Nikor ED ...

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• WISPI Optical Specifications

... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2004 April 18 . Stellar Spectral Types: OBAFGKM . ... Explanation: Astronomers divide stars into different spectral types . ... The seven main spectral types OBAFGKM are shown above with the spectrum of a single "O" star at the top followed by two spectra each from the progressively cooler designations, respectively. ... About APOD | ...

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• APOD: 2001 May 30 - Stellar Spectral Types: OBAFGKM

... The TESIS is a set of solar imaging instruments developed by the Lebedev Physical Institute of the Russian Academy of Science, and launched aboard the Russian spacecraft CORONAS-PHOTON on January 30, 2009. The main goal of the TESIS is to provide complex observations of solar active phenomena from the transition region to the inner and outer solar corona with high spatial, spectral and temporal resolution in the EUV and Soft X-ray spectral bands. ... Solar activity hits a new low . ...

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... Credit: KPNO 0.9-m Telescope , AURA , NOAO , NSF Explanation: Astronomers divide stars into different spectral types . ... A few types that best describe the temperature of the star remain in use today. The seven main spectral types OBAFGKM are shown above with the spectrum of a single "O" star at the top followed by two spectra each from the progressively cooler designations, respectively. ... Publications with keywords: stars - spectrum . Publications with words: stars - spectrum . ...

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• Астронет > Stellar Spectral Types: OBAFGKM
• Journal "Peremennye Zvezdy"
• XWare > APOD

. FLARES . LIMB FLARES . POST FLARE LOOPS . ACTIVATED PROMINENCES FILAMENTS . QUIET PROMINENCES FILAMENTS . 2004 Yu. Kupryakov .

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• Y.Kupryakov, SAI, MSU
• MSSA results

... The spectrum of the Sgr B2 molecular cloud has been surveyed between 215 and 265 GHz towards 3 positions, the dense cores Sgr B2(N)and Sgr B2(M), and the quiescent core Sgr B2(NW). ... The Sgr B2 molecular cloud, located approximately 100 pc from the Galactic Centre and with a mass of , is one of the most extreme cases among star formation sites ( Lis & Goldsmith (1991) ). ... Of the 3 observed positions Sgr B2(N) has the strongest line emission in most molecular species with a few exceptions. ...

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• G111.7-2.1
• G74.0-8.5

... Solar flare activity is produced by the processes of accumulation and release of energy in an active region. ... In the framework of study of solar active regions, producing powerful flares the researchers from the RATAN-600 radio telescope have detected sources with features in the form of a sharp drop in the intensity of polarized radiation in various parts of the recorded frequency range (2-16GHz), sometimes changing the sign of polarization. ...

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• IRAS01005+7910
• Study of radio spectra and variability of GPS sources
• Hardware sector, archive 2011