Streaming motions of galaxy clusters within 12 000 km s−1– V. The peculiar velocity field

By M. Hudson, Russell J. Smith, J. Lucey, E. Branchini. 2004

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We analyse in detail the peculiar velocity field traced by 56 clusters within 120 h −1 Mpc in the ‘Streaming Motions of Abell Clusters’ (SMAC) sample. The bulk flow of the SMAC sample is 687 ± 203 km s −1 , toward l = 260 ◦ ± 13 ◦ , b = 0 ◦ ± 11 ◦ . We discuss possible systematic errors and show that no systematic effect is larger than half of the random error. The flow does not drop off significantly with depth, which suggests that it is generated by structures on large scales. In particular, a Great Attractor as originally proposed by Lynden-Bell et al. cannot be responsible for the SMAC bulk flow. The SMAC data suggest infall into an attractor at the location of the Shapley Concentration, but the detection is marginal (at the 90 per cent confidence level). We find that distant attractors in addition to the Shapley Concentration are required to explain the SMAC bulk flow. A comparison with peculiar velocities predicted from the IRAS Point Source Catalogue redshift (PSCz) survey shows good agreement with a best-fitting value of β I = � 0.6 m /bI = 0.39 ± 0.17. However, the PSCz density field is not sufficient to account for all of the SMAC bulk motion. We also detect, at the 98 per cent confidence level, a residual bulk flow of 372 ± 127 km s −1 toward l = 273 ◦ , b = 6 ◦ which must be generated by sources not included in the PSCz catalogue, that is, either beyond 200 h −1 Mpc, in the zone of avoidance or in superclusters undersampled by IRAS. Finally, we compare the SMAC bulk flow with other recent measurements. We argue that, at depths ranging from 60 to 120 h −1 Mpc, flows of order 600 km s −1 are excluded by multiple data sets. However, convergence to the cosmic microwave background frame by a depth of 60 h −1 Mpc is also excluded by multiple data sets. We suggest that a bulk flow of 225 km s −1 toward l = 300 ◦ , b = 10 ◦ at depths greater than 60 h −1 Mpc is consistent with all peculiar velocity surveys, when allowance is made for sparse

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/78b9385e3a0509014bc3f80e17a44e26a8d6fda3

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In Astronomy and Astrophysics

1. A. Riess
2. Volker Springel
3. R. Kirshner
4. P. Hopkins
5. S. Jha
6. L. Hernquist
7. Simon D. M. White
8. H. Hoekstra

Citations in the corpus

• (An)isotropy of the Hubble diagram: comparing hemispheres (2007, background): “…consistent with the fits of the asymmetric sets A and D. Putting together all the evidence on the local flow direction in the Universe, mainly based on the analysis of galaxy clusters, Hudson et al. (2004) suggest a bulk flow of 225 km/s toward (l, b) = (300◦, 10◦) at depth greater than 60h−1 Mpc.”
• Cosmic flows in the nearby universe from Type Ia supernovae (2011, background): “As discussed in detail in Hudson et al. (2004), these structures could be missing from the PSCz because they are (i) outside the survey volume (ii) in the zone of avoidance or (iii) present but under-represented.”
• The Hubble Constant from Infrared Surface Brightness Fluctuation Distances (2021, background): “This results in a mean total velocity error of 250 km s−1, typical of many peculiar velocity surveys involving early-type galaxies in groups (e.g., Zaroubi et al. 2001; Hudson et al. 2004).”
• Consistently large cosmic flows on scales of 100 h−1 Mpc: a challenge for the standard ΛCDM cosmology (2008, methodology): “There are independent reasons to question the LP results: Hudson et al. (2004) compared, cluster by cluster, the distance to the BCG derived by LP to that derived from the FP for other cluster members, and found that in a few cases, these distances differed significantly, in the sense that the LP…”
• Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2 (2006, methodology): “Using TullyFisher distances to galaxy clusters, Giovanelli et al. (1999) find H ¼ 1:0% 2:2% at 7000 km s 1, while Hudson et al. (2004) derive H ¼ 2:3% 1:9% via fundamental plane cluster distances, both consistent with no void.”
• Cosmic ray feedback in hydrodynamical simulations of galaxy formation (2006, background): “…fluctuations (e.g. Spergel et al., 2003), galaxy clustering (e.g. Tegmark et al., 2004; Cole et al., 2005), cos- mic flows in the present universe (e.g. Willick et al., 1997; Hudson et al., 2004), or the observational data on distant supernovae (Riess et al., 1998; Perlmutter et al., 1999).”
• Evidence for anisotropy of cosmic acceleration (2018, methodology): “With respect to the 372±127 km s−1 bulk flow of the model (Hudson et al. 2004) from which the redshifts of the local SNe Ia have been corrected, only 108 are in the upper hemisphere while 632 are in the lower hemisphere.”
• Cosmic flows on 100 h−1 Mpc scales: standardized minimum variance bulk flow, shear and octupole moments (2009, methodology): “As in Paper I, we have removed outliers by using the predictions of the IRAS-PSCz (Point Source Catalogue Survey z=redshift) density field (for more details see Paper I; Hudson et al. 2004; Neill et al. 2007).”
• The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, methodology): “Past analyses, like S14 and B14, use the velocity field in Hudson et al. (2004), which is derived using the galaxy density field from the IRAS PSCz redshift survey (Branchini et al. 1999).”
• Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Over the years the bulk flows has been estimated from the measured peculiar velocities of a large variety of objects ranging from galaxies [528, 529, 408, 345, 363, 1038] clusters of galaxies [730, 226, 618] and SN Ia [1013].”
• SUPERNOVA CONSTRAINTS AND SYSTEMATIC UNCERTAINTIES FROM THE FIRST THREE YEARS OF THE SUPERNOVA LEGACY SURVEY (2011, methodology): “The peculiar velocity model used in this analysis (Hudson et al. 2004) is based on the galaxy density field in the nearby universe (z < 0.06) and accounts for infall into nearby superclusters (e.g. Virgo, Hydra-Centaurus and Perseus-Pisces) as well as a large-scale bulk flow.”
• Kinematics of the Local Universe. XIII. 21-cm line measurements of 452 galaxies with the Nançay radiotelescope, JHK Tully-Fisher relation, and preliminary maps of the peculiar velocity field (2006, background): “The direction and amplitude of this bulk motion are close to the one of the putative Great Attractor (Lynden-Bell et al 1988, Hudson et al 2004, Radburn-Smith 2006) and cannot be associated to any structure in particular.”