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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• Getting the Dispersion Solution
• Wavelength calibration
• Fitting the dispersion curve

... It lists the coefficients defining the colour transformations, the zero points for the different filters and the aperture radii used in the photometric calibration analysis. ... The AB system zero point of the filter FilterID is stored in the keyword ABM0 FilterID , e.g. the AB zero point of the the U-filter is stored in ABM0U. The flux conversion factor derived from White Dwarfs of the filter FilterID is stored in the keyword FCF FilterID . ... description . ... AB Flux conversion factor of U . ...

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... This paper describes various methods for the analysis of spectroscopic data, particularly as they relate to wavelength calibration of echelle­format spectra. ... A short introduction to robust regression by Least­Median of Squares is presented in Section 2. ... Wavelet transform can be useful in complementing robust techniques for mul­ tiresolution analysis, and Section 4 presents an application of the Mexican hat transform to the detection of spectral features. ... Robust Regression 2.1. ...

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• A Wavelet Parallel Code for Structure Detection
• In-Orbit Calibration of the Distortion of the SOHO/LASCO-C2 Coronagraph
• ADASS 2003 Conference Proceedings

HDF data were reduced with the same software as the standard HST pipeline (the STSDAS task calwp2), but with different calibration files, and with a slightly different treatment of the darktime. After pipeline processing, the data were stacked and cosmic rays were identified. Hot pixels were identified from dark frames and from the images themselves. ... A number of shortcuts were taken in the initial processing of the data. ...

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• Target Identification
• The Hubble Deep Field - Hot Pixel Removal
• Near Infrared Camera and Multi-Object Spectrometer Instrument Handbook for

Next: Imaging Polarimetry with NICMOS Up: NICMOS Data Calibration and Previous: The Photometric Performance of . ... NICMOSlook and Calnic C . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... NICMOSlook and Calnic-C are two programs that were designed to take advantage of the fact that the NICMOS grism mode typically consists of taking both a direct and a grism image. ...

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... 2014 June 9 . How to Identify that Light in the Sky . ... If so, and if you live near a city, the answer is typically an airplane, since planes are so numerous and so few stars and satellites are bright enough to be seen over the din of artificial city lights . If not, and if you live far from a city, that bright light is likely a planet such as Venus or Mars -- the former of which is constrained to appear near the horizon just before dawn or after dusk. ... Poll: Is APOD a Blog? ...

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• APOD: 2004 September 13 - Identify this Phenomenon
• APOD: 2009 July 9 - Fermi's Gamma ray Pulsars
• APOD: 2004 September 29 - HUDF: Dawn of the Galaxies

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• Astronomy HyperText Book: Stellar Clusters
• Digital Stellar Spectra

... Gravitational wave detection Timing residuals = unmodelled physical effects Spin-down irregularities No angular signature CSIRO. Gravitational wave detection Time standards · Most pulsar observations referred to TT(TAI) · Post-corrected time standard TT(BIPM2010) can be used · Requirement to fit for the pulsar's period and first derivative => a quadratic must be removed from the expected clock errors CSIRO. ... Simulate 10x expected TAI-TT(BIPM2010) in real pulsar data 5s CSIRO. ... CSIRO. ...

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• ATNF Daily Astronomy Picture
• Input Parameters to the Self-Calibration Tasks
• Self-Calibrating with Multiple Models

Application of IVOA software tools for radio sources investigation Zhelenkova O., Kopylov A., Chernenkov V. The interrelationship between the objects of astronomical catalogs in the different ranges of electromagnetic spectrum and their association into the real astrophysical source has obvious scientific interest. ... We used NVSS as the reference coordinate catalog. ... For 60% of radio sources identified with the objects of the radio catalogs we discovered optical candidates in SDSS survey. ...

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• Fabry-Perot Interferometer: Data cubes
• Radio sources identfification
• Introduction

Guest Editorial , May 2006 . Transforming SETI to METI . ... Those who propose, or oppose, sending Messages to Extra-Terrestrial Intelligence (METI) must contemplate the Hamlet-like question: "To send or not to send?" The science known as SETI deals with searching for messages from aliens. ... We therefore propose that, for solution to the various current METI problems, we consider transforming the familiar SETI search space to a METI search space. ... Where to search? ... When to search? ...

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• Atmospheric influence on the different radioengineering systems functioning.

... Left: Black hole systems with high mass companions in blue, black hole systems with low mass companions in green, X-ray pulsars in red, and non-pulsing neutron star systems in Magenta. ... Left: Black hole systems with low-mass companions in green; black hole systems with high-mass companions in blue. Right: Persistent black hole systems in blue; transient black hole systems in green. ... Bhaskar Balaji Unionville High School Summer 2012 . Robert Sylvia Medfield High School Summer 2011 . ...

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• http://hea-www.harvard.edu/AstroStat/SolStat2012/jack_ireland.pdf
• The AstroStat Slog Blog Archive different views
• The Orion OB1 Association

... Science . ... Science Users Information > Data Handling and Products > Data Reduction FAQ > I want to process MOS data of the same target from different nights together - how can I do that? ... Observing Facilities . ... Observing with ESO Telescopes . ... However, if you want to process science data from different nights together you should limit the available calibrations to those from one night as the pipeline assumes that the calibration data were taken without mask movement in between. ...

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• Sample Identification
• Colours and magnitudes
• ESO - Why do the flats in my data have different exposure times and how do I

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... The low-resolution, Cassegrain mounted, FORS spectropolarimeter of the ESO Very Large Telescope is being extensively used for magnetic field surveys. Some of the new discoveries suggest that relatively strong magnetic fields may play an important role in numerous physical phenomena observed in the atmospheres as well as in the circumstellar environments of certain kinds of stars. ...

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• Influence of Climate Variables on Tree-Ring Widths of Different Species
• Serendipitous Discovery of a Double Helium-rich Subdwarf
• ULTRACAM Observations of Subdwarf B Stars

... Apache HTTP Server Version 2.4 . Apache > HTTP Server > Documentation > Version 2.4 > Modules . ... Description: . ... This module is designed for the use in test suites and large networks which have to deal with different httpd versions and different configurations. ... IfVersion [[!] operator ] version > .. ... httpd version is equal . ... Questions on how to manage the Apache HTTP Server should be directed at either our IRC channel, #httpd, on Freenode, or sent to our mailing lists . ...

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• K-band Arcetri Obscured Supernova Search - Detection technique
• mod_setenvif - Apache HTTP Server
• mod_authn_core - Apache HTTP Server

... Clearing the library. Note the different flooтАж . Sidebar Left . Sidebar Top . ... Title: Clearing the library. Note the different floor levels. There were at least 4 different levels of underfloor in the library. Description: NOTE: All images and movies are copyright and must not be reproduced or mirrored in any form without written permission. ... NOTE: All images and movies are copyright and must not be reproduced or mirrored in any form without written permission. ...

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• Things are very different for small planets
• Wavelengths
• GSAOI Orion Nebula Cluster Science Page

... For these observations night-time is required. Begin ­ End Interval­Interval ­ ­ ­ ­ 2 Days Needed at This Interval Time Constraints (Must Be Justified in the Prop osal Text) LST 0700 0700 0930 1715 Range - 1145 - 1300 - 1300 - 2000 Nights Notes 19 NGC 2577/UGC 4375 + Leo I Group 6 NGC 2577/UGC 4375 + Leo I Group + Abell 1367 51 Leo I Group + Abell 1367 89 Local Void (complete in second semester ) Constraints on scheduling: The Turn On Galfa Survey ( TOGS ) operates commensally with ...

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• http://www.naic.edu/vscience/schedule/2014Spring/DenevatagP2860.pdf
• http://www.naic.edu/vscience/schedule/tpfiles/NowakowskitagP2115tp.pdf
• http://www.naic.edu/vscience/schedule/2015Spring/MinchintagA2048.pdf

. There are several different shells available for Unix; the most popular are described here. You can use any one of these shells if they are available on your system. And you can switch between the different shells once you have found out if they are available. Bourne shell (sh) . C shell (csh) . TC shell (tcsh) . Korn shell (ksh) . Bourne Again SHell (bash) .

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• Using a different printer
• Divisions
• Example of using a different printer

... During the analysis of the surveys carried out on RATAN-600, it was found that almost one fifth of the detected sources shows significant radio flux variations. ... We used the data from "Cold" radio surveys carried out with RATAN-600 in 1980-1994 to search for radio sources with significant flux variability. ... On possibility of detection of variable sources using the data of Cold surveys carried out on RATAN-600. ... Detection of Variable Sources Using the Data of "Cold" Surveys. ...

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• important11-15_en
• GRB090726

Next: The Scenario Machine: Operational Up: Evolution of Magnetic Rotators Previous: Ejector-propeller hysteresis . ... The length of this segment is determined by the eccentricity. ... In this case no hysteresis occurs and transitions E -- P and the reverse take place in symmetrical points of the orbit. ... Here EP means a mixed state of the rotator at which it is in the ejector state during one part of the orbit, and in the propeller state during the rest of the orbital cycle. ...

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• Detection rate of binary compact star merging
• Cyg X-1 as a Progenitor of BH+PSR Binaries
• Introduction

The preliminary version of documentation of the format for the interchange of calibrated optical/IR data being developed by Tom Pauls of NRL and John Young of COAST was presented and a number of issues discussed. The proposed format is in the general form of a relational database with different components stored in FITS binary tables. ... Should there be a single data table type that includes all data types, or multiple table types, one per data type? What data types are needed? ...

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• OptInt PmWiki : PmWiki / Access Keys
• OptInt PmWiki : Access Keys
• ALMA Phase Calibration Techniques at the Cavendish Astrophysics Group