Статья

The 2dF Galaxy Redshift Survey: the bias of galaxies and the density of the Universe

Licia VerdeDepartment of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854‐8019, USAAlan HeavensInstitute for Astronomy University of Edinburgh Royal Observatory, Blackford Hill Edinburgh EH9 3HJWill J. PercivalInstitute for Astronomy University of Edinburgh Royal Observatory, Blackford Hill Edinburgh EH9 3HJS. MatarreseDipartimento di Fisica “G. Galilei,” Università di Padova, and INFN, Sezione di Padova, via Marzolo 8, I-35131, Padova, ItalyC. M. BaughDepartment of Physics, University of Durham, South Road, Durham DH1 3LEJoss Bland‐HawthornAnglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaTerry BridgesAnglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaRussell CannonAnglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaShaun ColeDepartment of Physics, University of Durham, South Road, Durham DH1 3LEMatthew CollessResearch School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia,Chris CollinsAstrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Birkenhead L14 1LDW. J. CouchDepartment of Astrophysics; University of New South Wales; Sydney; NSW; 2052; AustraliaGavin DaltonDepartment of Physics, university of Oxford, Keble Road, Oxford OX1 3RHRoberto De ProprisDepartment of Astrophysics; University of New South Wales; Sydney; NSW; 2052; AustraliaSimon P. DriverSchool of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY6 9SSG. EfstathiouInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA,Richard S. EllisDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USACarlos S. FrenkDepartment of Physics, University of Durham, South Road, Durham DH1 3LEKarl GlazebrookDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218‐2686, USA,Carole JacksonResearch School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia,O. LahavInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA,Ian LewisDepartment of Physics, university of Oxford, Keble Road, Oxford OX1 3RHS. L. LumsdenDepartment of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT,S. MaddoxSchool of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD,Darren S. MadgwickInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA,P. NorbergDepartment of Physics, University of Durham, South Road, Durham DH1 3LEJ. A. PeacockInstitute for Astronomy University of Edinburgh Royal Observatory, Blackford Hill Edinburgh EH9 3HJB. A. PetersonResearch School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia,William J. SutherlandInstitute for Astronomy University of Edinburgh Royal Observatory, Blackford Hill Edinburgh EH9 3HJKeith TaylorAnglo‐Australian Observatory, PO Box 296, Epping, NSW 2121, Australia

2002en

ABI

Аннотация

We compute the bispectrum of the 2dF Galaxy Redshift Survey (2dFGRS) and use it to measure the bias parameter of the galaxies. This parameter quantifies the strength of clustering of the galaxies relative to the mass in the Universe. By analysing 80 × 106 triangle configurations in the wavenumber range 0.1 < k < 0.5 h Mpc-1 (i.e. on scales roughly between 5 and 30 h-1 Mpc) we find that the linear bias parameter is consistent with unity: b1 = 1.04 ± 0.11, and the quadratic (non-linear) bias is consistent with zero: b2 = -0.054 ± 0.08. Thus, at least on large scales, optically selected galaxies do indeed trace the underlying mass distribution. The bias parameter can be combined with the 2dFGRS measurement of the redshift distortion parameter β ≃ Ω0.6m/b1, to yield Ωm = 0.27 ± 0.06 for the matter density of the Universe, a result that is determined entirely from this survey, independent of other data sets. Our measurement of the matter density of the Universe should be interpreted as Ωm at the effective redshift of the survey (z = 0.17).

Перевод пока недоступен

Идентификаторы

DOI: 10.1046/j.1365-8711.2002.05620.x

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar