Next: The derived luminosity and Up: The galactic population of Previous: The galactic population of . Figure 16: The observed distribution of pulsar dispersion measures. Dotted curve is the total known population, solid curve is the Parkes survey. Figure 17: The observed distribution of pulsar distances above the galactic plane. ... Figure 18: The observed distribution of pulsar flux densities. ...

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• Australia Telescope National Facility
• Southern Cross Astrophysics Conference Series
• ATNF Colloquium

... Home Education Classes AAA Winter Astronomy Class: Measuring Distances in Space тАУ Dec 2015 тАУ Feb 2016 . ... Classes . AAA Fall Astronomy Class: Astronomy Basics тАУ October-November 2015 . AAA Winter Astronomy Class: Measuring Distances in Space тАУ Dec 2015 тАУ Feb 2016 . AAA Spring Astronomy Class: The Physics of Astronomy тАУ February - March 2016 . ... This MonthтАЩs Sky тАУ April 2016 . ... Dec. ... Observing Resources for Amateur Astronomers - Part 1: Beginning Observers . ...

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• Astronomy Workshop: Observing Variable Stars from the City ? February 15, 2015
• Observing-Events ? Amateur Astronomers Association of New York
• Observing Out-Of-Town ? Amateur Astronomers Association of New York

... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

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• ASP: A Taste of Real Astronomy ? The ESA/ESO Astronomy Exercises
• ASP: Mercury Summer 2011
• ASP: Good Astronomy Activities on the WWW

... According to the most popular cosmological paradigm, the greater part of the galaxy mass is accumulated in the dark matter halo. ... The polar ring galaxies (PRGs) reveal external rings or disks of gas, dust and stars rotating in a plane roughly perpendicular to the disk of the central galaxy. ... The shape of the dark halo in the model was chosen so as to achieve the best fit to the observed rotation of both galaxies themselves and their polar rings. ... The SPRC-7 galaxy. ...

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• Detection of Radio Transients and Variable Radio Sources Using the Archive Data
• HD965
• Detection of unique bright radio flare of X-ray binary

... Posts tagged ?distance measure? ... From arxiv/math.st:0708.0169v1 . Data-Driven Goodness-of-Fit Tests by L. Mikhail . ... ArXiv] Data-Driven Goodness-of-Fit Tests, Aug. ... Tags: consistency , distance measure , distribution , goodness-of-fit test , inverse problem , Neyman type , regularity condition , score . Category: arXiv , Fitting , Uncertainty | 1 Comment . ... Entries RSS . Comments RSS . ... vlk on [MADS] Parallel Coordinates . ... Entries (RSS) and Comments (RSS) . ...

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• Period Criteria
• The AstroStat Slog Blog Archive [ArXiv] Data-Driven Goodness-of-Fit Tests, Aug.
• Project Tanagra

The wavelength dependence of interstellar polarization due to dust in M31 has been observed along four sight lines. Only one sight line had been measured previously. ... The Serkowski law produces good fits for all the sight lines, although the relationship between K and ЮЛmax may be different from that found in the Galaxy. ... These are consistent with average values of ЮЛmax measured in the Galaxy and the Magellanic Clouds. ... ADS Citation Query . ... citations vs. year [year,citations] . ...

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• Observing Faint Targets Near Bright Objects
• Andy Fruchter's Homepage
• Processing of Observed Data

... Observers looking at an object that is moving away from them see light that has a longer wavelength than it had when it was emitted (a redshift), while observers looking at an approaching source see light that is shifted to shorter wavelength (a blueshift). ... By measuring the amount of the shift to the red, we can determine that the bright galaxy is moving away at 3,000 km/sec, which is 1 percent of the speed of light, because its lines are shifted in wavelength by 1 percent to the red. ... Part 2...

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• HyperLEDA documentation: parameter: vmaxg
• HyperLEDA documentation: compilation of cz measurements (a110)
• What was measured?

... A star was observed at different zenith distances during one night at the Engelgardt's Astronomical Observatory in the program of atmospheric extinction study at blue. ... The determination of the star's brightness was performed with the method of photon counting. ... Variable star. ... The brightness of the variable star was measured occasionally during the other nights, and moments of maximal values of brightness (15.59m) were received on nights 2­5, the 2nd table. ... JD 2452805. ...

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• http://www.issp.ac.ru/iao/2015/booklet/b11_ia15_p_en_b.pdf

The Sun is our nearest star and the source of energy for life on Earth. ... For centuries astronomers wondered whether they were clouds floating in the Sun's atmosphere, but we now know that they really are huge regions of magnetic field, about as intense as the field at the poles of an iron magnet. ... Such abrupt events were named solar flares , and what made them especially interesting was that occasionally, after a prominent flare, a magnetic storm would erupt on Earth. ...

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• Parallax
• TCV [Oulu]
• The Acceleration of the Aurora

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

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• Spatial distribution of X-ray binaries at the Galactic center after the
• Gravitational waves from supernova explosions
• Galactic potential

Over the coming weeks an international team, including Simon Jeffery , Vincent Woolf and Amir Ahmad of the Armagh Observatory, will use over fifteen different telescopes to make over one hundred nights of observations of just one star to learn about its internal structure. ... Although the approach has been used before, this may be the first time that a global asteroseismology project has tried to measure both light and spectrum variations at the same time for any star apart from the Sun. ...

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• Armagh Observatory
• Solar Eclipse Observed Armagh Observatory
• Broadening of Si VIII lines observed in the Solar polar coronal holes

M. ( / DIAS, Ireland), A. (ISDC, Switzerland) 1 - Key Question Only 3 binary systems regularly observed in TeV: PSR B1259-63 (young pulsar +Be star, P=3.4 y) LSI +61 303 (comp. source + Be star, P=26.42 d) LS 5039 (comp. source + O star, P=3.9 d) Origin of the high-energy emission? ... 2006; Neronov &Chernyakova 2007 4 3.4 years orbital period. e~0.87 Correlated variability with a sharp rise ( "two bumps structure" ) is seen in radio, X-ray (and TeV?) bands. ...

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• Fast search through RTT150 data archive
• GRANAT Home Page

... Bad Astronomy . Misconceptions . ... Bad Astronomy : The Moon only shows one face to us because it is not rotating. Better astronomy : The Moon only shows one face because it is rotating, once every time it revolves around the Earth. ... Place the Moon model on the table about 30 centimeters (one foot) away with the X facing the Earth model. ... You'll see that to keep the X facing the Earth model, you have to rotate the Moon model as it goes around the Earth model . ... 2008 Phil Plait. ...

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• Phil Plait's Bad Astronomy: Mad Science

... Science Users Information > Observing with ESO Telescopes > Phase 2 Preparation > Observing conditions . ... Service Mode Philosophy . ... The following definitions of the observing conditions are common between Phase 1 preparation and Phase 2 preparation, as well as between Service Mode and Visitor Mode observations. ... There are additional Service Mode Policies and Service Mode Guidelines regarding the observing conditions. ... Seeing (Phase 1) and Image quality (Phase2) constraints . ... Moon . ...

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• Homepage of Christian A. Hummel
• Titan Observed Through Nine Different Filters on November 26, 2002 | ESO
• FORS1 Photometric System Characterization

... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...

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• Introduction
• Extinction properties (transmitted radiation)
• Linear polarization: wavelength dependence

Diffuse interstellar bands (DIBs) and atomic lines are observed as interstellar absorptions in GALAH and other massive spectroscopic stellar surveys. By observing a given DIB toward many stars which are nearly in the same direction, but at different distances, one can reconstruct absorption sites along the line of sight. ...

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• http://www.mso.anu.edu.au/pfrancis/ObsTech/Ass4.pdf
• CHIAKI's Research

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

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... These structures are best observed at somewhat high latitudes so that they can be compared with other datasets, such as IRAS and H-alpha, without contamination by unrelated gas along the line of sight. HI structures like this have never been mapped with high angular resolution and sensitivity because nearly all HI sky maps have been done with angular resolution 36 arcmin. ... Part of the observing run. ...

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• http://www.naic.edu/vscience/schedule/tpfiles/GoldstontagA2187tp.pdf
• I-GALFA View of a Galactic Tangent Region
• Example Observing Projects

... 12c. Venus transit (1) . 12d. Venus transit (2) . 12e. Venus transit (3) . ... 1 The 2004 Venus transit . ... Kepler's third law allows one to evaluate the dimensions of the solar system in relative units, e.g. in " astronomical units " (AUs), where 1 AU is the mean Sun-Earth distance. ... Edmond Halley suggested using the transit of Venus across the Sun's disk, when it appears as a dark round spot --or to quote one observer of the 2004 transit, "like a blueberry in front of an orange." ...

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• The Sun
• Space Research Institute (IKI) Seminar
• Seasons of the Year

... 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 . ...

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