... Magnetic fields, subatomic particles, etc., traveling in different directions fill the universe. Do they deflect or otherwise affect one another? If so, isnт??t the information we get from them distorted? ... Neutrino astronomy, which is still in its infancy, is attractive because neutrinos interact so weakly with matter that few of these distorting effects occur. Get instant access to subscriber content on Astronomy.com! ...

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• Astronomy Magazine - Interactive Star Charts, Planets, Meteors, Comets,
• Does the time it takes different methods to create all the elements coincide
• Why do some stars appear to flash a variety of different colors when you look

... You are here: start €Ё lbaops €Ё lbajul2011 €Ё v255o . ... VLBI Schedule . ... Observer's Wiki . ... Other VLBI . ... lbaops:lbajul2011:v255o . ... Setup v255o.5cm: . ... IFP#1-LO 6642 - 6658 MHz USB RCP . ... Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255o . ... As for March the setup for the ICRF observations is to be 2 IFs with different polarizations. ... For Hobart the LOs should be set to 468 MHz (IFP#1) and 810 MHz (IFP#2) for the 4 x 16 MHz setup and 810 MHz for the 2 x 16 MHz setup....

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• lbaops:lbaapr2011:v255n [ATNF VLBI Wiki]
• lbaops:lbanov2011:v255p [ATNF VLBI Wiki]
• lbaops:lbajun2013:v490a [ATNF VLBI Wiki]

... HST . What overhead is required to change ACS detectors during an observing sequence? ... HST Peer Review Process . ... HST Overview . Overview . ... Cycle 24 Announcement . Cycle 23 Results . ... Mid Cycle Submission . ... Phase II Cycle 23 . ... Retrieving HST Data . ... Exposure Time Calculator### * What overhead do I incur if I change ACS detectors during an observing sequence? ... For a complete discussion of overheads, please read Chapter 9 in the ACS Instrument Handbook. ...

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• Changes to Recommended Buffer Time for COS TIME-TAG observations
• Change to COS FUV Pulse Height Filtering to Lower the Observed Dark Rate
• Changes in Treatment of STIS GO-WAVECAL Exposures (TARGET=WAVE)

An Ancient Universe: How Astronomers Know the Vast Scale of Cosmic Time . THE CHANGING UNIVERSE: EVOLUTION HAPPENS! ... Luckily nature has left a wide range of clues about evolution for us - at every scale of the universe - which we can uncover with some good astronomical detective work. a) Changes in the Solar System . ... An Ancient Universe - Table of Contents . ... The Universe: An Overview | ... The Changing Universe - Changes in the Solar System - Changes in Stars - Changes in the Universe | ...

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• ASP: An Ancient Universe - Changes in the Universe
• ASP: An Ancient Universe - Changes in Stars
• ASP: Guest Observer

... Science Users Information > Observing Facilities > La Silla Facilities > La Silla Science Operations . ... La Silla News . ... Internal Pages . La Silla Science Operations Department (LSO) is part of the La Silla Paranal Observatory and is in charge of the operations of the telescopes on La Silla. ... In the La Silla Science Operation pages, you should find all the information you need for your observations from the time you have an idea of observations until when you finish processing your data. ...

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• ESO - Observing conditions: definitions
• ESO - VLT Service Mode Guidelines
• Sub-arrays

If you have questions, need help, want to point out errors in this page, suggest improvements or give constructive criticisms regarding the observing system and this website, call Paulo Freire . Why CIMA? ... CIMA has become the default observing mode for pulsar observations at the Arecibo Observatory . ... The 4 Wideband Arecibo Pulsar Processors (WAPPs) have become the default back-ends for pulsar observations at the Arecibo Observatory. ... CIMA / WAPP observing page now available. ...

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• The CIMA Homepage
• CIMA Auto-Observing
• CIMA Command File Observing

Next: Reducing the observations Up: PEPSYS general photometry Previous: Influencing the plan . ... If the telescope and instrumentation are unfamiliar to you, you may have trouble keeping to the schedule for the first night or two, so try to work with a previous observer on the equipment for a night or two of training before your observing run. If you fall behind, try to keep as many low-altitude observations of extinction stars as you can, and drop some circumzenithal ones if necessary. ...

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• Selection criteria

... XMM-Newton SOC Home Page Conferences & Meetings . ... Data Analysis SAS News What is SAS? How to use SAS SAS Workshops SAS Version Changes Download and Install SAS Science Simulator (SciSim) . ... EPIC cameras optical loading . ... The PI is invited to cross-check the expected X-ray flux from the target source (and from any other potentially bright source in the target field of view), or to provide the SOC with her/his own estimate, if not originally specified in the proposal. ...

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• SAS version changes
• SciSim Release Track
• CIFBuild

... The greater the distance, the smaller the parallax. ... That triangle has the same proportions as the much larger triangle ABC, and therefore, if the distance B'C to the thumb is 10 times the distance A'B' between the eyes, the distance AC to the far landmark is also 10 times the distance AB. ... The most distant objects our eyes can see are the stars, and they are very far indeed: light which moves at 300,000 kilometers (186,000 miles) per second, would take years, often many years, to reach them. ...

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• The Face on Mars
• The Acceleration of the Aurora
• The Wind Spacecraft

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

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• The Face on Mars
• Changing your IP address is easy, but...
• The Discovery of the Galilean Satellites

... Bad Astronomy . ... I think I will break from my usual format of Bad Astronomy/ Good Astronomy by saying that the way we define seasons currently is not strictly bad, but I feel (in my opinion!) that it could be better. The definition of when the seasons begin is at the moment of solstice or equinox; that is, winter (in the north) starts on December 22 nd and summer starts on June 22 nd . ... Now imagine breaking up the Sun's 46 degree up-and-down yearly swing into 1 day intervals. ...

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Next: Scattering properties Up: Polarization properties (transmitted radiation) Previous: Linear polarization: wavelength dependence . Traditionally, the main problem considered in connection with circular interstellar polarization is the meaning of the wavelength where changes the sign . ... This is also demonstrated by Fig. 19 (lower panel) which shows the wavelength dependence of the factors of linear and circular polarization for particles of magnetite as was done by Shapiro ([ 1975 ]). ...

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• Linear polarization: wavelength dependence

Next: Mission Element Points-of-Contact . Previous: Mission Operations Data Transfer . ... Each mission element should ensure that their contact information remains current and notify the RSOG of any changes. ... Non-RSOG mission elements will also use the "dit" list to notify the RSOG (and all other mission elements) of unexpected events that may impact operations elsewhere, e.g., if a tracking station discovers that the spacecraft is in an unexpected configuration. ...

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• Description of the RadioAstron project, english version
• RSOG Pre-Observation Products

ATMoB "Double Star Award " Guidelines Purpose: To promote observing among the membership of the Amateur Telescope Makers of Boston ­ in particular, double, triple, and multiple stars. Introduction: Double, triple, and multiple stars are the "Rodney Dangerfields" of the night sky. ... W hile they can be observed under a variety of sky conditions, double stars ­ especially close ones ­ are best viewed on nights when the seeing is steady. ... The direction from a star to Polaris is north. ...

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• http://www.atmob.org/about/observing/awards/files/open_cluster_instructions_2011-02-01.pdf
• http://www.atmob.org/about/observing/awards/files/globular_cluster_instructions_2011-02-01.pdf
• Amateur Telescope Makers of Boston

... The most precisely determined characteristic for accreting neutron stars (NS's) is their period. ... Period changes show fluctuations. ... Some applications of stochastic processes in astrophysics especially in accreting systems were discussed in Lipunov (1987),Hoshino Takeshima (1993) and Lipunov (1992).In Hoshino Takeshima (1993) the authors, using simple models of MHD turbulence, try to explain aperiodic changes in X-ray luminosity of X-ray pulsars. ... Here, -constant angular momentum. ...

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• Semi-major axis change
• The COOC Criterion (Criterion of Observations versus Calculations)
• Contents

... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2014 October 15 . Mysterious Changing feature on Titan . Image Credit: Cassini Radar Mapper , Cornell , JPL , ESA , NASA . Explanation: What is that changing object in a cold hydrocarbon sea of Titan? ... Subsequent observations in 2014 found the object remained -- but had changed! ... About APOD | ... A service of: ASD at NASA / GSFC . ...

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• APOD: 2008 July 14 - Changes in Angular Mars
• APOD: April 13, 1998 - The Sun Changes
• APOD: 2005 July 4 - A Panorama from Mauna Kea

Peremennye Zvezdy ( Variable Stars ) 26 , No. ... Moscow 119992, Russia . ... 84/32, Moscow 117997, Russia . ... Our CCD observations compared to times of minima derived from the archival photographic plates and from the NSVS and ASAS-3 data clearly show that the orbital period of the system is variable. ... The phased light curve for the light elements . ... CCD, Moscow . ... and for the current linear light elements (in excellent agreement with the NSVS, ASAS, and our CCD observations): . ...

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• XWare > APOD

We model the spectral chanages of late oxygen-rich Miras observed in different pulsation phases. From a combination of variable near-IR spectra and UKIRT spectrophotometry of the 9.7 \mu m silicate dust emission feature in different phases we study the influence of the changing atmospherical circumstances on the conditions in the circumstellar dust shell. ... A comparision with the modelling results for another long period Mira U Ori is also provided. ...

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• Armagh Observatory
• Want to observe? Read the guide given by Tolis | International Year of
• Terry Mosely's Bulletins

... Operations of the Hubble Space Telescope (HST) require the creation of stable and efficient observation schedules in an environment where inputs to the plan can change daily. ... A process and software architecture is presented which achieves stable and efficient observation schedules by dividing the task into long term and short term components. ... However, the resulting long range plan would be unstable as unscheduled observations in a week bin would have to be rescheduled. ...

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• ETCs and Observations Simulation at the VLT
• Nightly Scheduling of ESO's Very Large Telescope
• The Ground Support Facilities for the BeppoSAX Mission

Next: References Up: A Method of Integrating Previous: Description of algorithm . In April 1996 the described method was included in the software of automatic data acquisition complex "Continuous". ... The measuring of sensibility by observing at the wave lengths of 1.38cm and 2.7cm. The measuring of sensibility by observing at the wave lengths of 3.9cm and 7.6cm. wave lengths. The measuring of sensibility by observing at the wave lengths of 13.0cm and 31cm. wave lengths. ...

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• Fabry-Perot Interferometer: Data cubes
• Instrumentation
• di_eks