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  • 김해콜걸출장마사지〖카톡:do26〗【doo26.com】☜김해콜걸김해▧출장소이스E2018-12-12-20-23┇콜걸샵김해김해♕김해xI미시출장안마오피♡♮
  • 양산출장소이스『카톡:mss41』{mss41.com}역출장안마양산2018-12-12-20-23출장맛사지★⇙출장가격SP⇂╋양산콜걸양산♘n78양산출장샵안내콜걸출장안마WOR양산광명출장업계위┌의왕출장오피⊿《구미안마(카톡:kow58)『kow58.com』⇩▨◊S2018-12-12-20-23출장외국인출장샵안내구미구미◊웃╤✿구미T0☂구미구미⊙》안동출장샵예약↘안산출장최강미녀─속초콜걸강추☽광주출장안마김해오피✑구미출장업소╘《영주출장맛사지(카톡:kn887)《kn887.net》출장샵추천영주p2018-12-12-20-23콜걸샵영주영주m출장안마야한곳Y♪ 영주⇗영주☪Z영주영주p34출장미인아가씨✏영주ax》오산출장안마추천◎청주안마♪ 김포콜걸출장마사지↛속초출장외국인
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    익산출장최강미녀¤남원출장샵추천☆《김해출장안마야한곳『카톡:do26』〖doo26.com〗출장미인아가씨↞2018-12-12-20-23£콜걸추천➻김해김해e출장맛사지╟김해콜걸업소김해oek콜걸fOM♥➼김해》청주출장코스가격◎여수출장맛사지♗마산오피걸♧김천콜걸출장마사지

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  • 남양주릉콜걸샵❖남양주콜걸출장마사지❃남양주콜걸↰남양주외국인출장만남☭남양주출장샵♪남양주출장샵추천

    The SDSS-III's Baryon Oscillation Spectroscopic Survey (BOSS) will map the spatial distribution of luminous red galaxies (LRGs) and quasars to detect the characteristic scale imprinted by baryon acoustic oscillations in the early universe. Sound waves that propagate in the early universe, like spreading ripples in a pond, imprint a characteristic scale on cosmic microwave background fluctuations. These fluctuations have evolved into today's walls and voids of galaxies, meaning this baryon acoustic oscillation (BAO) scale (about 150 Mpc) is visible among galaxies today. This concept is illustrated below (some of the relative scales have been exaggerated for illustration purposes).

  • 광주출장아가씨
  • 전주출장샵콜걸▀천안출장샵후기[《영천외국인출장만남[카톡:xo779]〖xo779.com〗ⓔa2영천tu출장만족보장출장시영천2018-12-12-20-23영천출장샵후기영천⇛⇪출장최강미녀영천모텔출장4출장소이스╬➻》창원출장오쓰피걸☼제주출장시☠진주콜걸출장안마═군산출장샵

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    거제출장연애인급┏원주출장색시미녀언니⇩《청주출장미인아가씨(카톡:do26)[doo26.com]☱✄☼청주흥출장안마오피흥출장안마청주청주1청주uT✉콜걸출장안마yI6콜걸출장마사지☃☍2018-12-12-20-23》김제외국인출장만남↓정읍출장샵강추①안산흥출장안마▀고양출장샵
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  • An illustration of the concept of baryon acoustic oscillations, which are imprinted in the early universe and can still be seen today in galaxy surveys like BOSS
    (Illustration courtesy of Chris Blake and Sam Moorfield).
    서산출장서비스
    Comparison of the power spectrum of SDSS-II LRGs and BOSS DR9 CMASS galaxies. Solid lines show the best-fit models. From 남양주출장연애인급 .

    These baryon acoustic oscillations have now been measured in the distribution of galaxies as illustrated on the right, where we show the power spectrum of galaxy fluctuations, as a function of scale (shown here as a wave number, k). We have removed the smooth component to more clearly show the oscillations, which are the BAO signal of interest. The two panels show the previous results from SDSS-II DR7 LRGs (top) and the new results from the z = 0.55 BOSS DR9 sample (CMASS, bottom). The reduction in errors and the better fit to the cosmological model (solid line) of the BOSS data compared to the SDSS-II is clearly evident. When the survey is completed, the errors on the BOSS measurements will be further reduced, and we will also measure the BAO at several other redshifts.

    Using the acoustic scale as a physically calibrated ruler, BOSS will determine the angular diameter distance with a precision of 1% at redshifts z = 0.3 and z = 0.55 using the distribution of galaxies. It will also measure the distribution of quasar absorption lines at z = 2.5, yielding a measurement of the angular diameter distance at that redshift to an accuracy of 1.5%. It will also measure the cosmic expansion rate H(z) with 1-2% precision at the same redshifts. These measurements will provide demanding tests for theories of dark energy and the origin of cosmic acceleration.

    BOSS at a glance
    Dark time observations
    Fall 2009 - Spring 2014
    출장업소 , resolution R~2000
    Wavelength: 360-1000 nm
    10,000 square degrees
    Redshifts of 1.5 million luminous galaxies to z = 0.7
    Lyman-α forest spectra of 160,000 quasars at redshifts 2.2 < z < 3
    거제모텔출장
    논산오피걸

    In addition to constraining cosmological models, BOSS will deliver an outstanding sample of galaxies and quasars ideally suited to probing the formation and evolution of galaxies in the Universe. For example, we show below an example z =0.56 galaxy spectrum for early BOSS data which shows the level of spectral detail we can expect on these intermediate redshift galaxies. By studying the various key absorption features in this spectrum (labeled and shown with red tickmarks), we can estimate the age and metallicity of the stars in these galaxies, and thus determine how and when they formed. The sheer size of BOSS, coupled with the BOSS spectrograph resolution, will greatly enhance this area of science.

    A randomly selected spectrum from the dr10 BOSS data, showing absorption (red) and emission (blue) lines. Click on the image to go to this object's page on SkyServer.

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