The database contains references to the papers, data files and links to the Internet resources related to measurements and calculations of the optical constants in the wavelength interval from X-rays to radio domain. ... References to some useful books and reviews on the subject (e.g. the classical handbooks edited by E.D.Palik) and links to Internet collections of optical constants and personal WWW pages with related software were also placed in the database. You have arrived at our welcome page. ...

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• Database of Optical Properties -- Level: subsubpage
• Database of Optical Properties -- Level: subpage
• Database of Optical Properties -- Level: subsubsubpage

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

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Chair of solid state physics . ... The Physics of Phonons . ... In the first part of the course “The Physics of Phonons” the dynamics of atoms in one- and three- dimensional crystalline lattices is considered in detail. The quasiparticle conception in solids, taking phonons as an example, is discussed; creation and annihilation operators of phonons, main properties of acoustic and optical phonons dispersion laws, density of phonon states. ... Crystalline state. ... Acoustic and optical phonons. ...

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• Laboratory for Spectroscopy of Molecular Structures

Atmospheric influence on the different radio-engineering system functioning . ESTIMATION OF ATMOSPHERIC OPTICAL CHARACTERISTICS AND REMOTELY SANSED IMAGE CORRECTION . ... Direct transmittance estimation results for 12 channels of the spectrometer CHRIS. ... We have managed to develop a direct method of estimating the discrete Normalized Atmospheric Point Spread Function (NAPSF) from available images alone, not using any external sources of information about the atmosphere. ... IRE RAS 1996-20 11 ...

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At Arecibo we have a variety of optical instruments that we use to study terrestrial airglow emissions. ... As a complement to the airglow instrumentation we also maintain a set of optical instruments, called lidars, used for "active" remote sensing of the atmosphere. That is, we generate our own source signal using lasers and measure the characteristics of the light scattered back from the atmosphere. ... An operations manual for the Optical Laboratories is currently under major revision. ...

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• The AO Optical Laboratories National Astronomy and Ionosphere Center (Arecibo
• Figures for Scattering Paper
• radar

... Archives . ... If you do not mind the time predictor, it is hard to believe that this is a light curve, time dependent data. ... It?s hard to say this data set is designed for time series analysis apart from the complication in statistical inference due to measurement errors. How to design the statistical study with measurement errors, huge gaps in time, and unequal time intervals is complex and unexplored. ... The following is R output without measurement errors. ... Chandra Blog . ...

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• The AstroStat Slog ANOVA
• The AstroStat Slog flux

... In order to disentangle the effects of different climate variables on tree-ring growth rates of different species, and to explore the possibility that more than one species could improve the accuracy of the reconstructions of climate using tree rings, a methodical study of trees in close proximity to the Armagh Observatory climate station was initiated together with Ana Maria Garc?a Su?rez, and continued as part of the latter's PhD thesis with John Butler and Professor Mike Baillie (QUB). ...

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• Armagh Observatory

... User Guide ] Task: colden Purpose: calculates column densities for linear molecules Categories: map analysis COLDEN is a MIRIAD task to calculate column densities. ... Key: method Three possibilities: (1) Give one optically thin transition and the kinetic temperature (Assumes tau=0). ... Default=1. Key: in1 The first input image contains the most abundant isotope (e.g. 12CO). ... No default Key: in2 For method 1, give the kinetic temperature in the first plane. ... Key: cut Two values. ...

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• Australia Telescope National Facility
• Reducing 3-mm ATCA observations
• OH_maser

This is the homepage of Andrew Fruchter, an astronomer on the staff of the Space Telescope Science Institute . ... Here you can look at an HST images of the optical counterparts of gamma-ray bursts and their host galaxies. ... Therefore, substantial information on the fine scale structure of objects can be obtained by offsetting the pointing of the telescope between exposures and then combining these "dithered" exposures into a single image. ...

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• Near Infrared Camera and Multi-Object Spectrometer Instrument Handbook for
• Gratings and Optical Elements
• The Opacity of Spiral Galaxy Disks. VIII. Structure of the Cold ISM

... A molecular cloud in the interstellar medium may be considered as spherical and of uniform density and fixed temperature as it undergoes expansion or contraction. Assume the opacity of material in the molecular cloud has a value . ... How will this affect cloud fragmentation? (e) In the stages of collapse of a gas cloud before it becomes optically thick, its temperature is determined by the balance between compressional heating and radiation of energy from the cloud. ...

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• Clearing the library. Note the different floor levels. There were at least 4
• Wavelengths
• Things are very different for small planets

... This is the truly fun part, observing molecular and atomic gas in star-forming regions with a variety of telescopes. Depending on the temperature and density of the gas, different observations are necessary to study the components of star-forming regions. Because stars form in cool gaseous regions, I most often use radio and sub-mm observations, but I also look for opportunities to make complementary observations using infrared and optical telescopes. ... Copyright 2015 Adele Plunkett. ...

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• Comparison of the central part of the Milky Way at different wavelengths
• Different X-ray Spectra
• Colours and magnitudes

To main of Laboratory . The research work and design of optical and optical-electronic devices are carries out by laboratory staff: . ... Lens: . ... In the layout 1 prism systems perform functions of dispersive element, corrector of aberrations, optical reducer. ... Spectral range 200 - 400 nm; . ... Back Forward . ... The main corrector's function are compensation of field aberrations of the main spherical mirror of a telescope (diameter of 600 mm, f'=1200 mm) and increase aperture ratio. ...

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... May 11, 1999 . Molecular Cloud Barnard 68 . ... Explanation: Where did all the stars go? What used to be considered a hole in the sky is now known to astronomers as a dark molecular cloud . ... One of the most notable of these dark absorption nebulae is a cloud toward the constellation Ophiuchus known as Barnard 68, pictured above . ... It is not known exactly how molecular clouds like Barnard 68 form, but it is known that these clouds are themselves likely places for new stars to form. ...

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• APOD: 2014 December 14 - Molecular Cloud Barnard 68
• APOD: 2012 January 29 - Molecular Cloud Barnard 68
• APOD: 2006 April 9 - Molecular Cloud Barnard 68

Next: Wavelength calibration Up: Getting Started Previous: Detecting lines in . ... and the Calibration Starting Row will be used for the lines identifications. ... After setting these parameters, click the button. to pop up the Identify window. ... The identification starts by clicking on , which plots one row of the spectrum in the graphic window, indicates the position of the detected arc lines with blue vertical traces and gives a cursor. ... Figure: Lines Identification Window . ...

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• Optical spectroscopy
• Equations of condition
• HyperLEDA documentation: parameter: objname

Since the light from galaxies represents the integrated contribution of its consitutient stars, then we can learn about stellar populations in galaxies by modelling their light by summing up individual stellar spectra for different kinds of stars. ... The data cover the wavelength range 3500 - 9000 angstroms. ... Retrieve Digital Stellar Spectra Click on the appropriate spectral type. ... Note that the designation V means main sequence, IV means subgiants, III means giants, I means supergiant. ...

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• Lecture V.
• Astronomy HyperText Book: Stellar Evolution
• Astronomy HyperText Book: Interstellar Medium

... This matter may absorb the radiation from the source, scatter it or in fact emit fur ther radiation. ... For the case of a homogeneous cloud with a constant source function and optical depth with initial incident intensity , the emergent intensity is This makes a lot of sense: the emergent radiation is the sum of the incident intensity attenuated by the total optical depth plus the sum of each section of cloud emission attenuated by the optical ...

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• http://www.mrao.cam.ac.uk/~kjbg1/lectures/lect5.pdf
• Data Format Session at 2001 IAU WG Meeting
• Relic radiolines of hydrogen at decimeter and meter wavelength band

Determination of the physical parameters of molecular clouds Riccardo Cesaroni INAF­Osservatorio Astrofisico di Arcetri, Firenze, Italy E-mail: cesa@arcetri.astro.it The most common methods to derive some of the physical parameters of Galactic molecular clouds are described in this lecture. Special attention is devoted to the derivation of the (column) density, mass, and temperature. ... In particular, we will discuss the derivation of the velocity field, temperature, (column) density, and mass. ...

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• IBIS - Flat Fielding
• Arcetri Guaranteed Time
• The Arcetri Spectral Code files

... Russian KOI8 . ... Radio galaxies and cosmology [in Russian]) . ... The book is devoted to investigations of powerful radio galaxies in the different wavelength ranges. ... The history of study for radio galaxies is given and the outlook on radio galaxy exploring is considered. ... The cosmological tests to check the Universe evolution parameters constructed on the observational data of radio galaxies are considered in details. ... List of detected misprints (in Russian). ...

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• Informational system "Evolution of RG"

... A detector map is used to provide a grid of positions over which to calculate and flux weight the ARF. The default detector map is 'flat' which has a weighting of 1.0 for each detector map pixel and is rectangular having sides which just encompass the region specified in the DSS. Only detector map pixels falling within the source region are included in the ARF calculation, e.g. for a circular source box, the pixels in the corners of the detector map will be ignored. ... flat : . ...

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• Selection of observations of empty RGS files
• Description
• CAL_getRGAObscure

... In one situation, we can use light from quasars to probe the material between us and them because that light may pass through one or more galaxies or gas clouds on its way to us. The gas inside the galaxies or the intergalactic clouds acts then as a filter, absorbing selected wavelengths from the quasar light. ... Light from a quasar must pass through clouds of gas and even faint galaxies -- each leaving its imprint on the light -- before we receive it here on Earth. ... Gravitational lensing . ...

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• ASP: Good Astronomy Activities on the WWW
• ASP: Using Multicultural Dimensions to Teach Astronomy
• ASP: Responsible Exploration