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Measuring the cosmic bulk flow with 6dFGSv

Published online by Cambridge University Press:  12 October 2016

Christina Magoulas ,
Christopher Springob ,
Matthew Colless ,
Jeremy Mould ,
John Lucey ,
Pirin Erdoğdu  and
D. Heath Jones
Christina Magoulas
Affiliation:
Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, RSA, email: [email protected] Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia
Christopher Springob
Affiliation:
Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia ICRAR, The University of Western Australia, Crawley, WA 6009, Australia ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)
Matthew Colless
Affiliation:
RSAA, The Australian National University, Canberra, ACT 2611, Australia
Jeremy Mould
Affiliation:
ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) CAS, Swinburne University, Hawthorn, VIC 3122, Australia
John Lucey
Affiliation:
Department of Physics, University of Durham, Durham, DH1 3LE, UK
Pirin Erdoğdu
Affiliation:
Australian College of Kuwait, PO Box 1411, Safat 13015, Kuwait
D. Heath Jones
Affiliation:
School of Physics, Monash University, Clayton, VIC 3800, Australia.
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Abstract

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While recent years have seen rapid growth in the number of galaxy peculiar velocity measurements, disagreements remain about the extent to which the peculiar velocity field - a tracer of the large-scale distribution of mass - agrees with both ΛCDM expectations and with velocity field models derived from redshift surveys. The 6dF Galaxy Survey includes peculiar velocities for nearly 9 000 early-type galaxies (6dFGSv), making it the largest and most homogeneous galaxy peculiar velocity sample to date. We have used the 6dFGS velocity field to determine the amplitude and scale of large-scale cosmic flows in the local universe and test standard cosmological models. We also compare the galaxy density and peculiar velocity fields to establish the distribution of dark and luminous matter and better constrain key cosmological parameters such as the redshift-space distortion parameter.

Keywords

galaxies: distances and redshiftscosmology: observations - distance scale - large-scale structure of universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 336 - 339
Copyright
Copyright © International Astronomical Union 2016 

References

Bilicki, M., Chodorowski, M., Jarrett, T., & Mamon, G. A. 2011, ApJ, 741, 31 CrossRefGoogle Scholar
Branchini, E. et al. 1999, MNRAS, 308, 1 Google Scholar
Campbell, L. et al. 2014, MNRAS, 443, 1231 Google Scholar
Colin, J., Mohayaee, R., Sarkar, S., & Shafieloo, A. 2011, MNRAS, 414, 264 CrossRefGoogle Scholar
Dai, D.-C., Kinney, W. H., & Stojkovic, D. 2011, JCAP, 4, 15 Google Scholar
Davis, M. et al. 2011, MNRAS, 413, 2906 CrossRefGoogle Scholar
Erdoğdu, P. et al. 2006, MNRAS, 373, 45 Google Scholar
Jones, D. H. et al. 2009, MNRAS, 399, 683 Google Scholar
Kogut, A. et al. 1993, ApJ, 419, 1 Google Scholar
Magoulas, C. et al. 2012, MNRAS, 427, 245 Google Scholar
Nusser, A. & Davis, M. 2011, ApJ, 736, 93 Google Scholar
Nusser, A. et al. 2001, MNRAS, 320, 3 Google Scholar
Pike, R. W. & Hudson, M. J. 2005, ApJ, 635, 11 Google Scholar
The Planck Collaboration 2013, ArXiv e-prints, 1303.5090Google Scholar
Radburn-Smith, D. J., Lucey, J. R., & Hudson, M. J. 2004, MNRAS, 355, 4 CrossRefGoogle Scholar
Springob, C. M. et al. 2014, MNRAS, 445, 3 Google Scholar
Turnbull, S. J. et al. 2012, MNRAS, 420, 447 CrossRefGoogle Scholar
Watkins, R., Feldman, H. A., & Hudson, M. J. 2009, MNRAS, 392, 743 CrossRefGoogle Scholar