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... HST Phase II Proposal Instructions for Cycle 20 > Chapter 12: Cosmic OriginsSpectrograph (COS) > REFERENCE INFORMATION > 12.14 COS Spectral Elements and Central Wavelengths . ... Table 12.3: COS Spectral Elements and Central Wavelengths . ... Spectral Element . Central Wavelengths (Angstroms) . ... MIRRORA 2 . ... MIRRORB 3 . ... The MIRRORA spectral element positions a flat mirror in the beam to produce an image of the sky with a field of view slightly larger than the diameter of the aperture. ...

Next: An overview Up: The discovery of pulsars Previous: Identification with rotating neutron . unsuccessful optical search for PSR 1919+21 . optical pulsations from the Crab pulsar [ 9 ] . optical data before radio discovery not analysed [ 36 ] . ... X-ray data before radio discovery not analysed [ 10 ] . Figure 3: The Crab pulsar. This pair of photographs was taken using a stroboscopic technique, showing the pulsar on (left) and off (right). ...

... Observatory . ... Science . ... Science Users Information > Data Handling and Products > Data Reduction FAQ > How can I 'extract' lines from the arc and match them to wavelengths? ... Science Users Information . Observing Facilities . La Silla Paranal Observatory . Paranal Facilities . La Silla Facilities . ... Observing with ESO Telescopes . ... Science Data Products Forum . ... Science Archive Facility . ... ESO Data . ... ESO Data Access Policy . ... ESO Science Newsletter . ...

Diffuse interstellar bands -- a survey with precise wavelengths . ... We present an atlas of 271 diffuse interstellar bands (DIBs) between 4460 and 8800A based on echelle spectra (R=45,000), more than 100 of which are new DIB discovered in this survey. It is restricted mostly to narrow features and we describe the tests for an interstellar origin. ... new . ... new W-type . figure10, figure11 . ... figure11 . ... figure13, figure14 . ... figure14 . ... figure19 . ... figure21 . ...

Building the Foundation for U.S . Astronomy at m/cm Wavelengths in 2010 and Beyond Community Workshop (*) Workshop SOC/LOC Robert Brown (NAIC) Chris Carilli (NRAO) Jim Cordes (US SKA Consortium) Dale Frail (NRAO) B. Murray Lewis (NAIC) K. Y. Lo (NRAO) Emmanuel Momjian (NAIC) Yervant Terzian (US SKA Consortium) (Special thanks to Billie Rodriguez, Jill Tarbell and Joan Martin) * Support provided by NSF, NRAO, and NAIC R. L ...

... Optical depth at 100 MHz 122-127 F6.4 --- e_Tau ? ... The highest absorption is observed in the direction of G0.0+0.0. ... G0.9+0.1 is a classic example of a composite, two-component SNR including an extended (8') source with a steep (a=-0.64) spectrum and a central, more compact, component (2') with a flat spectrum (a=-0.1) [49]. ... The highest absorption was observed for four sources in the direction of the galactic central region: 1, 2, 3, and the unidentified source G0.4+0.1 [t(100MHz)=6-0.8]. ...

Classroom Activity: Making a Rainbow . ... When white light from the Sun or a light bulb passes through a prism, the light splits into its component wavelengths. ... Red, blue, green colored filters - if possible, cut 1x4-inch pieces of the filters for each student . ... Many students have the misconception that filters somehow dye the light a certain color. ... Younger students can draw the rainbow and make up a mnemonic for remembering the order of the colors (such as, ROY G. BIV). ...

The CHIANTI database consists of 4 primary ASCII files for each ion in the database. contains the energy levels in cm^(-1) It includes both experimental data and theoretical values of the levels energies. References: %observed energy levels: Fuhr et al, 1999, NIST Atomic Spectra Database Version 2.0 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Ken Dere May 3 2001 . ... contains the spline fits to the scaled proton collision strengths. ...

The Milky Way's Center . ... Credit Copyright: NASA , COsmic Background Explorer (COBE) Project . Explanation: NASA's COBE satellite scanned the heavens at infrared wavelengths in 1990 and produced this premier view of the central region of our own Milky Way Galaxy. The Milky Way is a typical spiral galaxy with a central bulge and extended disk of stars. However, gas and dust within the disk obscure visible wavelengths of light effectively preventing clear observations of the center . ...

... A radio galaxy is a galaxy that emits an unusually big amount of energy at radio wavelengths. ... Inside of each galaxy with an active nucleus (radio galaxies are among them) there must be a system of a "central machine" responsible for the colossal amount of the emitted energy from radio to gamma ranges. ... Sometimes a radio source in an active galaxy may flare again if the needed conditions appear (a new portion of matter would fall into the furnace of the "central machine"). ...

is split into spectral colours, corresponding to wavelength. Red light has long wavelengths, blue light has short wavelengths. from hot objects are continuous , like a rainbow . atoms only emit light of specific colours, revealing their fingerprints as a line spectrum . atoms in front of a hot object absorb light at these colours, giving an absorption spectrum . are predominantly absorption spectra . next

True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... Description: large, diffuse, X-ray and radio brighter in northern half . Radio . ... Radio Images Page . ... Exposure uf . ... Exposure uf Exposure time of unfiltered event file . Exposure f Exposure time of filtered event file . ... Event 2 FITS File . ... AUX file . ... 0.3 - 10.0 . ... see fit detail page for more about the fit. see chandra spectrum page for region used. ... True Color Image . ... Radio Images . ...

Astronotes Armagh Planetarium's Stellar Blog! ... Stars . ... Starbursts are short-lived events, stars are forming so quickly that the reservoirs of interstellar gas from which stars are coalescing would be used up on a timescale much shorter than the age of the galaxy . ... Strong stellar winds from giant new stars in the starburst region combine with the blasts of supernovae to push a mighty flood of extremely hot gas, a ?superwind? from the galaxy thousands of light years into intergalactic space. ...

. Cambridge . MRAO . Bojan Nikolic web pages home . Next: Science at Q-band meeting, Manchester . Previous: European Radio Interferometry School 2009 | . This is the lecture I gave at the European Radio Interferometry School: . http://www.mrao.cam.ac.uk/~bn204/publications/2009/NikolicERIS2009.pdf . Please enable JavaScript to view the comments powered by Disqus. blog comments powered by Disqus . Copyright 2012, Bojan Nikolic feedback welcome

... 2001 December 28 . Starlight Reflections . ... Explanation: Interstellar dust grains often find themselves in a reflective "mood". Near a bright star, clouds of these dust particles scatter short wavelengths of visible starlight more readily than long wavelengths, producing lovely blue reflection nebulae. ... Along the bottom are NGC 2023 ( near the Horsehead), NGC 7023 ( Iris Nebula ), and finally bright star Merope surrounded by a veil of dust ( NGC 1435 ). ... About APOD | ...

This enormous section of the Milky Way galaxy is a mosaic of images from NASA's Wide-field Infrared Survey Explorer. ... The colors used in this image represent specific wavelengths of infrared light. Blue and cyan (blue-green) represent light emitted at wavelengths of 3.4 and 4.6 microns, which is predominantly from stars. Green and red represent light from 12 and 22 microns, respectively, which is mostly emitted by dust. ...

... The large-scale chains visible on the inverted SOHO/EIT images (a-c) at three wavelengths of 171, 195 and 284 as well as on the normal MLSO/HAO He I 10830 spectroheliogram (d) of December 16, 1997. ...

... 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). ...

... Under certain conditions, like those in the nucleus of a QSO, all atoms can be made to emit light at particular wavelengths. ... If that source is approaching the observer, the wave is squashed up onto itself making the wavelength shorter. ... This is redshift. ... You can see how the section of the QSO spectrum which we observe changes with redshift. ... We then see how far we had to slide the observed spectrum along the scale to make it match and that is the objects redshift. ... The 2QZ team . ...