DOCSLIB.ORG

Cosmography of the Local Universe SDSS-III Map of the Universe

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Cosmography of the Local Universe SDSS-III Map of the Universe Cosmography of the Local Universe SDSS-III map of the universe Color = density (red=high) Tools of the Future: roBotic/piezo fiBer positioners AstroBot FiBer Positioners Collision-avoidance testing Echidna (for SuBaru FMOS) Las Campanas Redshift Survey The first survey to reach the quasi-homogeneous regime Large-scale structure within z<0.05, sliced in Galactic plane declination “Zone of Avoidance” 6dF Galaxy Survey, Jones et al. 2009 Large-scale structure within z<0.1, sliced in Galactic plane declination “Zone of Avoidance” 6dF Galaxy Survey, Jones et al. 2009 Southern Hemisphere, colored By redshift 6dF Galaxy Survey, Jones et al. 2009 SDSS-BOSS map of the universe Image credit: Jeremy Tinker and the SDSS-III collaBoration SDSS-III map of the universe Color = density (red=high) Millenium Simulation (2005) vs Galaxy Redshift Surveys Image Credit: Nina McCurdy and Joel Primack/University of California, Santa Cruz; Ralf Kaehler and Risa Wechsler/Stanford University; Klypin et al. 2011 Sloan Digital Sky Survey; Michael Busha/University of Zurich Trujillo-Gomez et al. 2011 Redshift-space distortion in the 2D correlation function of 6dFGS along line of sight on the sky Beutler et al. 2012 Matter power spectrum oBserved by SDSS (Tegmark et al. 2006) k-3 Solid red lines: linear theory (WMAP) Dashed red lines: nonlinear corrections Note we can push linear approx to a Bit further than k~0.02 h/Mpc Baryon acoustic peaks (analogous to CMB acoustic peaks; standard rulers) keq SDSS-BOSS map of the universe Color = distance (purple=far) Image credit: Daniel Eisenstein and the SDSS-III collaBoration Cosmological Analysis of BOSS galaxies 13 Correlation function Power spectrum P(k)-Psmooth(k) / Psmooth(k) BOSS DR12 - 0.5 <z<0.75 BOSS DR12 NGC - 0.5 <z<0.75 BOSS DR12 NGC - 0.5 <z<0.75 150 0.2 0.2 100 0.1 0.1 50 ] ] 1 1 − − Mpc] 1 0 0.0 0.0 Mpc Mpc − h h h [ [ [ s 50 k k − 0.1 0.1 − − 100 along line of sight − 150 0.2 0.2 − 150 100 50 0 50 100 150 − 0.2 0.1 0.0 0.1 0.2 − 0.2 0.1 0.0 0.1 0.2 − − − 1 − − 1 − − 1 s [h− Mpc] k [h Mpc− ] k [h Mpc− ] ⊥ ⊥ ⊥ 80 40 0 40 80 120 3.5 3.7 3.9 4.1 4.2 4.4 4.6 4.8 0.3 0.2 0.1 0.0 0.1 0.2 0.3 0.4 0.5 − − 2 2 2 3 3 − − − s ξ(s ,s )[h− Mpc ] log10 [P (k ,k )/(h− Mpc )] [P (k ,k ) Psmooth(k ,k )]/Psmooth(k) ⊥ ⊥ ⊥ − ⊥ Figure 5. The measured pre-reconstruction correlation function (left)on the sky and power spectrum (middle) in the directions perpendicular and parallel to the line of sight, shown for the NGC only in the redshift range 0.50 <z<0.75. In each panel, the color scale shows the data and the contours show the prediction of the best-fit model. The anisotropy of the contours seen in both plots reflects a combination of RSD and the AP effect, and holds most of the information used to separately constrain DM (z)/rd, H(z)rd, and fσ8. The BAO ring can be seen in two dimensions on the correlation function plot. To more clearly show the anisotropic BAO ring in the power spectrum, the right panel plots the two-dimensional power-spectrum divided by the best-fit smooth component. The wiggles seen in this panel are analogous to the oscillations seen in the top left panel of Fig 3. BOSS results, Alam et al. 2016, arXiv:1607.03155 Table 4. Summary table of pre-reconstruction full-shape constraints on the parameter combinations D r /r , H r /r , and fσ8(z) derived M ⇥ d,fid d ⇥ d d,fid in the supporting papers for each of our three overlapping redshift bins Measurement redshift Satpathy et al. Beutler et al. (b) Grieb et al. Sanchez´ et al. ⇠(s) multipoles P (k) multipoles P (k) wedges ⇠(s) wedges D r /r [Mpc] z =0.38 1476 33 1549 41 1525 25 1501 27 M ⇥ d,fid d ± ± ± ± D r /r [Mpc] z =0.51 1985 41 2015 53 1990 32 2010 30 M ⇥ d,fid d ± ± ± ± D r /r [Mpc] z =0.61 2287 54 2270 57 2281 43 2286 37 M ⇥ d,fid d ± ± ± ± H r /r [km s 1Mpc 1] z =0.38 79.3 3.382.5 3.281.2 2.382.5 2.4 ⇥ d d,fid − − ± ± ± ± H r /r [km s 1Mpc 1] z =0.51 88.3 4.188.4 4.187.0 2.490.2 2.5 ⇥ d d,fid − − ± ± ± ± H r /r [km s 1Mpc 1] z =0.61 99.5 4.497.0 4.094.9 2.597.3 2.7 ⇥ d d,fid − − ± ± ± ± fσ8 z =0.38 0.430 0.054 0.479 0.054 0.498 0.045 0.468 0.053 ± ± ± ± fσ8 z =0.51 0.452 0.058 0.454 0.051 0.448 0.038 0.470 0.042 ± ± ± ± fσ8 z =0.61 0.456 0.052 0.409 0.044 0.409 0.041 0.440 0.039 ± ± ± ± ods is consistent with what we observe in mocks (see Section 7.2 and Fig. 10). In all cases the µ-wedges analyses give significantly tighter constraints than the multipole analyses, in both configura- tion space and Fourier space. The consensus constraints, described in 8.2 below, are slightly tighter than those of the individual wedge § analyses. At all three redshifts and for all three quantities, mapping distance, expansion rate, and the growth of structure, the 68% con- fidence contour for the consensus results overlaps the 68% confi- dence contour derived from Planck 2015 data assuming a ⇤CDM cosmology. We illustrate the combination of these full shape results with the post-reconstruction BAO results in Fig. 11 below. c 2016 RAS, MNRAS 000, 1–38 Results from BOSS galaxy clustering analysis Alam et al. 2016, arXiv:1607.03155 1987ApJ...313...59D Tully-Fisher relation Fundamental Plane Absolute magnitude Djorgovski & Davis 1987 Tully & Fisher 1977 Effective radius ComBination of velocity dispersion and surface Brightness Width of HI line profile in velocity units Velocity power spectrum Dashed line: Planck prediction Black solid lines: Binned scaled angular power spectrum Johnson et al 2014 (6dGFS-v) Cosmological constraints from peculiar velocities + redshift-space distortions LCDM parameters Scale-dependent modifications to GR Johnson et al 2016 Johnson et al 2014 (6dGFS-v) Cosmic Flows CMBR Dipole: The One Peculiar Velocity We Know Very Well We are moving wrt. to the CMB at ~ 620 km/s towards b=27°, l=268° This gives us an idea of the probable magnitude of peculiar velocities in the local universe. Note that at the distance to Virgo (LSC), this corresponds to a ~ 50% error in Hubble velocity, and a ~ 10% error at the distance to Coma cluster. Real and Simulated Galaxies Scale sensitivity of various cosmological proBes Dynamical measurements (temporal potential) Light propagation measurements (spatial potential) Johnson et al 2014 (6dGFS-v).
Load more

Recommended publications
  • An Analysis Including the Latest Local Measurement of the Hubble Constant
    Eur. Phys. J. C (2017) 77:882 https://doi.org/10.1140/epjc/s10052-017-5454-9 Regular Article - Theoretical Physics Constraints on inflation revisited: an analysis including the latest local measurement of the Hubble constant Rui-Yun Guo1, Xin Zhang1,2,a 1 Department of Physics, College of Sciences, Northeastern University, Shenyang 110004, China 2 Center for High Energy Physics, Peking University, Beijing 100080, China Received: 21 June 2017 / Accepted: 8 December 2017 / Published online: 18 December 2017 © The Author(s) 2017. This article is an open access publication Abstract We revisit the constraints on inflation models by current cosmological observations can be used to explore using the current cosmological observations involving the the nature of inflation. For example, the measurements of latest local measurement of the Hubble constant (H0 = CMB anisotropies have confirmed that inflation can provide 73.00 ± 1.75 km s −1 Mpc−1). We constrain the primordial a nearly scale-invariant primordial power spectrum [5–8]. power spectra of both scalar and tensor perturbations with the Although inflation took place at energy scale as high as observational data including the Planck 2015 CMB full data, 1016 GeV, where particle physics remains elusive, hundreds the BICEP2 and Keck Array CMB B-mode data, the BAO of different theoretical scenarios have been proposed. Thus data, and the direct measurement of H0. In order to relieve the selecting an actual version of inflation has become a major tension between the local determination of the Hubble con- issue in the current study. As mentioned above, the primor- stant and the other astrophysical observations, we consider dial perturbations can lead to the CMB anisotropies and LSS the additional parameter Neff in the cosmological model.
    [Show full text]
  • New Upper Limit on the Total Neutrino Mass from the 2 Degree Field Galaxy Redshift Survey
    Swinburne Research Bank http://researchbank.swinburne.edu.au Elgary, O., et al. (2002). New upper limit on the total neutrino mass from the 2 Degree Field Galaxy Redshift Survey. Originally published in Physical Review Letters, 89(6). Available from: http://dx.doi.org/10.1103/PhysRevLett.89.061301 Copyright © 2002 The American Physical Society. This is the author’s version of the work, posted here with the permission of the publisher for your personal use. No further distribution is permitted. You may also be able to access the published version from your library. The definitive version is available at http://publish.aps.org/. Swinburne University of Technology | CRICOS Provider 00111D | swinburne.edu.au A new upper limit on the total neutrino mass from the 2dF Galaxy Redshift Survey Ø. Elgarøy1, O. Lahav1, W. J. Percival2, J. A. Peacock2, D. S. Madgwick1, S. L. Bridle1, C. M. Baugh3, I. K. Baldry4, J. Bland-Hawthorn5, T. Bridges5, R. Cannon5, S. Cole3, M. Colless6, C. Collins7, W. Couch8, G. Dalton9, R. De Propris8, S. P. Driver10, G. P. Efstathiou1, R. S. Ellis11, C. S. Frenk3, K. Glazebrook5, C. Jackson6, I. Lewis9, S. Lumsden12, S. Maddox13, P. Norberg3, B. A. Peterson6, W. Sutherland2, K. Taylor11 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edingburgh EH9 3HJ, UK 3 Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK 4 Department of Physics & Astronomy, John Hopkins University, Baltimore, MD 21218-2686, USA 5 Anglo-Australian Observatory, P.
    [Show full text]
  • The 6Df Galaxy Survey: Z ≈ 0 Measurements of the Growth Rate and Σ 8
    Mon. Not. R. Astron. Soc. 423, 3430–3444 (2012) doi:10.1111/j.1365-2966.2012.21136.x The 6dF Galaxy Survey: z ≈ 0 measurements of the growth rate and σ 8 Florian Beutler,1 Chris Blake,2 Matthew Colless,3 D. Heath Jones,4 Lister Staveley-Smith,1,5 Gregory B. Poole,2 Lachlan Campbell,6 Quentin Parker,3,7 Will Saunders3 and Fred Watson3 1International Centre for Radio Astronomy Research (ICRAR), University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia 2Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia 3Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia 4School of Physics, Monash University, Clayton, VIC 3800, Australia 5ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia 6Western Kentucky University, Bowling Green, KY 42101, USA 7Department of Physics and Astronomy, Faculty of Sciences, Macquarie University, NSW 2109, Sydney, Australia Accepted 2012 April 19. Received 2012 March 16; in original form 2011 November 14 ABSTRACT We present a detailed analysis of redshift-space distortions in the two-point correlation function of the 6dF Galaxy Survey (6dFGS). The K-band selected subsample which we employ in this 2 study contains 81 971 galaxies distributed over 17 000 degree with an effective redshift zeff = 0.067. By modelling the 2D galaxy correlation function, ξ(rp, π), we measure the parameter = ± γ combination f (zeff)σ 8(zeff) 0.423 0.055, where f m(z) is the growth rate of cosmic −1 structure and σ 8 is the rms of matter fluctuations in 8 h Mpc spheres.
    [Show full text]
  • Neutrino Cosmology
    International Workshop on Astroparticle and High Energy Physics PROCEEDINGS Neutrino cosmology Julien Lesgourgues∗† LAPTH Annecy E-mail: [email protected] Abstract: I will briefly summarize the main effects of neutrinos in cosmology – in particular, on the Cosmic Microwave Background anisotropies and on the Large Scale Structure power spectrum. Then, I will present the constraints on neutrino parameters following from current experiments. 1. A powerful tool: cosmological perturbations The theory of cosmological perturbations has been developed mainly in the 70’s and 80’s, in order to explain the clustering of matter observed in the Large Scale Structure (LSS) of the Universe, and to predict the anisotropy distribution in the Cosmic Microwave Background (CMB). This theory has been confronted with observations with great success, and accounts perfectly for the most recent CMB data (the WMAP satellite, see Spergel et al. 2003 [1]) and LSS observations (the 2dF redshift survey, see Percival et al. 2003 [2]). LSS data gives a measurement of the two-point correlation function of matter pertur- bations in our Universe, which is related to the linear power spectrum predicted by the theory of cosmological perturbations on scales between 40 Mega-parsecs (smaller scales cor- respond to non-linear perturbations, because they were enhanced by gravitational collapse) and 600 Mega-parsecs (larger scales are difficult to observe because galaxies are too faint). On should keep in mind that the reconstruction of the power spectrum starting from a red- shift survey is complicated by many technical issues, like the correction of redshift–space distortions, and relies on strong assumptions concerning the light–to–mass biasing factor.
    [Show full text]
  • The Detection of the Imprint of Filaments on Cosmic Microwave Background Lensing
    LETTERS https://doi.org/10.1038/s41550-018-0426-z The detection of the imprint of filaments on cosmic microwave background lensing Siyu He 1,2,3*, Shadab Alam4,5, Simone Ferraro6,7, Yen-Chi Chen8 and Shirley Ho1,2,3,6 Galaxy redshift surveys, such as the 2-Degree-Field Survey where n is the angular position, Πf(,nz ) is the angular posi- 1 2 (2dF) , Sloan Digital Sky Survey (SDSS) , 6-Degree-Field Survey tion of the closest point to n on the nearest filament and ρf (,nz ) 3 4 (6dF) , Galaxy And Mass Assembly survey (GAMA) and VIMOS is the uncertainty of the filament at Πf(,nz ). Using the inten- Public Extragalactic Redshift Survey (VIPERS)5, have shown that sity map at each redshift bin, we construct the filament intensity the spatial distribution of matter forms a rich web, known as the overdensity map via cosmic web6. Most galaxy survey analyses measure the ampli- tude of galaxy clustering as a function of scale, ignoring informa- In(,zz)d −Ī In(,zz)dΩ d tion beyond a small number of summary statistics. Because the ∫∫n δf()n = , Ī = , (2) matter density field becomes highly non-Gaussian as structure Ī ∫ dΩn evolves under gravity, we expect other statistical descriptions of the field to provide us with additional information. One way to study the non-Gaussianity is to study filaments, which evolve where Ωn is the solid angle at n. non-linearly from the initial density fluctuations produced in the In this work, we use the CMB lensing convergence map (pub- primordial Universe.
    [Show full text]
  • The Zcosmos Redshift Survey
    Reports from Observers The zCOSMOS Redshift Survey Simon Lilly (ETH, Zürich, Switzerland) that have been developed, using almost are the product of the gravitational growth and the zCOSMOS team* all of the most powerful observing facil- of initially tiny density fluctuations in the ities in the world. This next step is called distribution of dark matter in the Universe COSMOS and the ESO VLT will make a – fluctuations which likely arise from quan- The last ten years have seen the open- major enabling contribution to this pro- tum processes in the earliest moments ing up of dramatic new vistas of the fur- gramme through the zCOSMOS survey of the Big Bang, τ ~10–35 s. These densi- thest reaches of space and time – an being carried out with the VIMOS spec- ty fluctuations eventually collapse to make exploration in which the VLT has played trograph. gravitationally-bound dark matter struc- a major role. However, the work so far tures within which the baryonic material has been exploratory, and sampled only cools, concentrating at the bottom of the small and possibly unrepresentative vol- It is well known that the finite speed gravitational potential wells where it forms umes of the distant Universe. The next of light enables us to observe very distant the visible components of galaxies. step is to bring to bear on a single large objects as they were when the Universe area of sky the full range of techniques as a whole was much younger, and there- In many respects, the Λ-CDM paradigm by to directly observe the evolving prop- is strikingly successful, especially in de- erties of the galaxy population over cos- scribing large-scale structure.
    [Show full text]
  • Measuring Neutrino Masses with a Future Galaxy Survey
    Prepared for submission to JCAP Measuring neutrino masses with a future galaxy survey Jan Hamanna Steen Hannestada Yvonne Y.Y. Wongb aDepartment of Physics and Astronomy University of Aarhus, DK-8000 Aarhus C, Denmark bInstitut f¨ur Theoretische Teilchenphysik und Kosmologie RWTH Aachen, D-52056 Aachen, Germany E-mail: [email protected], [email protected], [email protected] Abstract. We perform a detailed forecast on how well a Euclid-like photometric galaxy and cosmic shear survey will be able to constrain the absolute neutrino mass scale. Adopting conservative assumptions about the survey specifications and assuming complete ignorance of the galaxy bias, we estimate that the minimum mass sum of mν ≃ 0.06 eV in the normal hierarchy can be detected at 1.5σ to 2.5σ significance, depending on the model complexity, P using a combination of galaxy and cosmic shear power spectrum measurements in conjunction with CMB temperature and polarisation observations from Planck. With better knowledge of the galaxy bias, the significance of the detection could potentially reach 5.4σ. Interestingly, neither Planck+shear nor Planck+galaxy alone can achieve this level of sensitivity; it is the combined effect of galaxy and cosmic shear power spectrum measurements that breaks the persistent degeneracies between the neutrino mass, the physical matter density, and the Hubble parameter. Notwithstanding this remarkable sensitivity to mν, Euclid-like shear and galaxy data will not be sensitive to the exact mass spectrum of the neutrino sector; no P significant bias (< 1σ) in the parameter estimation is induced by fitting inaccurate models of the neutrino mass splittings to the mock data, nor does the goodness-of-fit of these models arXiv:1209.1043v2 [astro-ph.CO] 7 Nov 2012 2 suffer any significant degradation relative to the true one (∆χeff < 1).
    [Show full text]
  • The Amplitudes of Fluctuations in The
    Mon. Not. R. Astron. Soc. 333, 961–968 (2002) The 2dF Galaxy Redshift Survey: the amplitudes of fluctuations in the 2dFGRS and the CMB, and implications for galaxy biasing Ofer Lahav,1P Sarah L. Bridle,1 Will J. Percival,2 John A. Peacock,2 George Efstathiou,1 Carlton M. Baugh,3 Joss Bland-Hawthorn,4 Terry Bridges,4 Russell Cannon,4 Shaun Cole,3 Matthew Colless,5 Chris Collins,6 Warrick Couch,7 Gavin Dalton,8 Roberto De Propris,7 Simon P. Driver,9 Richard S. Ellis,10 Carlos S. Frenk,3 Karl Glazebrook,11 Carole Jackson,5 Ian Lewis,8 Stuart Lumsden,12 Steve Maddox,13 Darren S. Madgwick,1 Stephen Moody,1 Peder Norberg,3 Bruce A. Peterson,5 Will Sutherland2 and Keith Taylor10 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA 2Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ 3Department of Physics, University of Durham, South Road, Durham DH1 3LE 4Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia 5Research School of Astronomy and Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia 6Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD 7Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia 8Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH 9School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY6 9SS 10Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 11Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218-2686, USA 12Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT 13School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD Accepted 2002 March 6.
    [Show full text]
  • UC Berkeley UC Berkeley Previously Published Works
    UC Berkeley UC Berkeley Previously Published Works Title The DESI Experiment Part I: Science,Targeting, and Survey Design Permalink https://escholarship.org/uc/item/2nz5q3bt Authors Collaboration, DESI Aghamousa, Amir Aguilar, Jessica et al. Publication Date 2016-10-31 Peer reviewed eScholarship.org Powered by the California Digital Library University of California The DESI Experiment Part I: Science,Targeting, and Survey Design DESI Collaboration: Amir Aghamousa73, Jessica Aguilar76, Steve Ahlen85, Shadab Alam41;59, Lori E. Allen81, Carlos Allende Prieto64, James Annis52, Stephen Bailey76, Christophe Balland88, Otger Ballester57, Charles Baltay84, Lucas Beaufore45, Chris Bebek76, Timothy C. Beers39, Eric F. Bell28, Jos Luis Bernal66, Robert Besuner89, Florian Beutler62, Chris Blake15, Hannes Bleuler50, Michael Blomqvist2, Robert Blum81, Adam S. Bolton35;81, Cesar Briceno18, David Brooks33, Joel R. Brownstein35, Elizabeth Buckley-Geer52, Angela Burden9, Etienne Burtin12, Nicolas G. Busca7, Robert N. Cahn76, Yan-Chuan Cai59, Laia Cardiel-Sas57, Raymond G. Carlberg23, Pierre-Henri Carton12, Ricard Casas56, Francisco J. Castander56, Jorge L. Cervantes-Cota11, Todd M. Claybaugh76, Madeline Close14, Carl T. Coker26, Shaun Cole60, Johan Comparat67, Andrew P. Cooper60, M.-C. Cousinou4, Martin Crocce56, Jean-Gabriel Cuby2, Daniel P. Cunningham1, Tamara M. Davis86, Kyle S. Dawson35, Axel de la Macorra68, Juan De Vicente19, Timoth´eeDelubac74, Mark Derwent26, Arjun Dey81, Govinda Dhungana44, Zhejie Ding31, Peter Doel33, Yutong T. Duan85, Anne Ealet4, Jerry Edelstein89, Sarah Eftekharzadeh32, Daniel J. Eisenstein53, Ann Elliott45, St´ephanieEscoffier4, Matthew Evatt81, Parker Fagrelius76, Xiaohui Fan90, Kevin Fanning48, Arya Farahi40, Jay Farihi33, Ginevra Favole51;67, Yu Feng47, Enrique Fernandez57, Joseph R. Findlay32, Douglas P. Finkbeiner53, Michael J. Fitzpatrick81, Brenna Flaugher52, Samuel Flender8, Andreu Font-Ribera76, Jaime E.
    [Show full text]
  • Measuring H0 from the 6Df Galaxy Survey and Future Low-Redshift Surveys
    Advancing the Physics of Cosmic Distances Proceedings IAU Symposium No. 289, 2012 c 2012 International Astronomical Union Richard de Grijs & Giuseppe Bono, eds. DOI: 00.0000/X000000000000000X Measuring H0 from the 6dF Galaxy Survey and future low-redshift surveys Matthew Colless,1 Florian Beutler,2;3 and Chris Blake4 1Australian Astronomical Observatory, P. O. Box 915, North Ryde, NSW 1670, Australia email: [email protected] 2International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Perth, WA 6009, Australia 3Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA email: [email protected] 4Centre for Astrophysics & Supercomputing, Swinburne University of Technology, P. O. Box 218, Hawthorn, VIC 3122, Australia email: [email protected] Abstract. Baryon acoustic oscillations (BAO) at low redshift provide a precise and largely model-independent way to measure the Hubble constant, H0. The 6dF Galaxy Survey measure- −1 −1 ment of the BAO scale gives a value of H0 = 67 ± 3:2 km s Mpc , achieving a 1σ precision of 5%. With improved analysis techniques, the planned wallaby (Hi) and taipan (optical) redshift surveys are predicted to measure H0 to 1{3% precision. Keywords. cosmology: observations, surveys, distance scale, large-scale structure of universe 1. Introduction Baryon acoustic oscillations (BAO) produced by the interaction of photons and baryons in the early universe provide an absolute standard rod that is calibrated by observations of the cosmic microwave background (CMB). The BAO scale is determined by well- understood linear physics and depends only on the physical densities of dark matter and baryons.
    [Show full text]
  • First Results from the 2Df Galaxy Redshift Survey
    First results from the 2dF Galaxy Redshift Survey By Matthew Colless† Mount Stromlo and Siding Spring Observatories, The Australian National University, Private Bag, Weston Creek Post Office, Canberra, ACT 2611, Australia The 2dF Galaxy Redshift Survey is a major new initiative to map a representative volume of the universe. The survey makes use of the 2dF multi-fibre spectrograph at the Anglo-Australian Telescope to measure redshifts for over 250 000 galaxies brighter than bJ =19.5 and a further 10 000 galaxies brighter than R = 21. The main goals of the survey are to characterize the large-scale structure of the universe and quantify the properties of the galaxy population at low redshifts. This paper describes the design of the survey and presents some preliminary results from the first 8000 galaxy redshifts to be measured. Keywords: redshift surveys; large-scale structure; galaxy evolution; observational cosmology 1. The goals of the survey Cosmology is undergoing a fin-de-millennium flowering brought on by the hothouse of recent technological progress. Cosmography, one of the roots of cosmology, is thriving too: maps of the distribution of luminous objects are covering larger volumes, reaching higher redshifts and encompassing a wider variety of sources than ever before. New ways of interpreting these observations are yielding a richer and more detailed picture of the structure and evolution of the universe, and of the underlying cosmology. The 2dF Galaxy Redshift Survey at the Anglo-Australian Telescope (AAT) aims to map the optically luminous galaxies over a statistically representative volume of the universe in order to characterize, as fully as possible, the large-scale structure of the galaxy distribution and the interplay between this structure and the properties of the galaxies themselves.
    [Show full text]
  • The 6Df Galaxy Survey Is a Very Effective Means of Determining the True Mass Distribution in the Local Universe
    **TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The 6dF Galaxy Survey Ken-ichi Wakamatsu Faculty of Engineering, Gifu University, Gifu 501-1192, Japan Matthew Colless Mount Stromlo & Siding Spring Observatories, ACT 2611, Australia Tom Jarrett IPAC, Caltech, MS 100-22, Pasadena, CA 91125, USA Quentin Parker Macquarie University, Sydney 2109, Australia William Saunders Anglo-Australian Observatory, Epping NSW 2121, Australia Fred Watson Anglo-Australian Observatory, Coonabarabran NSW 2357, Australia Abstract. The 6dF Galaxy Survey (6dFGS) 1 is a spectroscopic sur- vey of the entire southern sky with |b| > 10◦, based on the 2MASS near infrared galaxy catalog. It is conducted with the 6dF multi-fiber spec- trograph attached to the 1.2-m UK Schmidt Telescope. The survey will produce redshifts for some 170,000 galaxies, and peculiar velocities for about 15,000 and is expected to be complete by June 2005. arXiv:astro-ph/0306104v1 5 Jun 2003 1. Introduction In order to reveal large-scale structures at intermediate and large distances, ex- tensive galaxy redshift surveys have been carried out, e.g. the 2dFGRS and SDSS, and the Hubble- and Subaru-deep field surveys. There is now an ur- gent need to study the large-scale structure of the Local Universe that can be compared with the above deeper surveys. However to do this required hemi- 1Member of Science Advisory Group: M. Colless (Chair; ANU, Australia), J. Huchra (CfA, USA), T. Jarrett (IPAC, USA), O. Lahav (Cambridge, UK), J. Lucey (Dahram, UK), G. Mamon (IAP, France), Q. Parker (Maquarie Univ. Australia), D. Proust (Meudon, France), E.
    [Show full text]