The Mass Distribution in the Nearby Universe

Costa, L. N. da; Freudling, W.; Wegner, Gary A.; Giovanelli, Riccardo; Haynes, Martha P.; Salzer, John J.

doi:10.1086/310223

Cited by 81 publications

(84 citation statements)

References 24 publications

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“…Using I-band TF peculiar velocities of clusters in PP, Han & Mould (1992, hereafter HM) claimed a motion of -400 km s −1 . In contrast, the recent TF field survey of Giovanelli et al (1996;da Costa et al 1996) indicates no net motion of PP.…”

Section: Introductionmentioning

confidence: 72%

Galaxy clusters in the Perseus-Pisces region -- II. The peculiar velocity field

Hudson

Lucey

Smith

et al. 1997

Monthly Notices of the Royal Astronomical Society

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We have measured the mean peculiar motions of 103 early-type galaxies in 7 clusters in the Perseus-Pisces (PP) ridge or PP background, and a further 249 such galaxies in 9 calibrating clusters from the literature, using the inverse Fundamental Plane relation. This relation is found to have a distance error of 20% per galaxy. None of the 6 clusters in the PP ridge has a significant motion with respect to the cosmic microwave background (CMB) frame, but the PP background cluster J8 shows marginal evidence of 'backside infall' into the PP supercluster. We find that the full 16 cluster sample has a mean CMB-frame bulk motion of 420±280 km s −1 towards l = 262 • , b = −25 • . This result is consistent both with no bulk motion in the CMB frame and with the ∼ 350 km s −1 bulk motion found by Courteau, Faber, Dressler and Willick. It is inconsistent at the 98% confidence level with the ∼ 700 km s −1 bulk flow found by Lauer & Postman. The PP ridge clusters are found to have a small and statistically insignificant mean radial motion with respect to the CMB frame: −60 ± 220 km s −1 . Our error analysis fully accounts for the uncertainties in the mean Hubble flow, as well as the errors due to the merging of different spectroscopic datasets. A comparison between our cluster peculiar velocities and the predicted peculiar velocities from the IRAS 1.2 Jy density field, smoothed on a 500 km s −1 scale, yields β I ≡ Ω 0.6 /b I = 0.95 ± 0.48, consistent with previous results. We find agreement between our peculiar motions and published Tully-Fisher results for the same clusters. The disagreement between the 11 clusters common to our sample and that of Lauer & Postman, based on brightest cluster galaxies (BCGs), is statistically significant at the > ∼ 99.7% confidence level indicating that the errors of one or both of these data sets are underestimated. When the BCG distances corrected for the X-ray luminosity of the host cluster are used, the disagreement is reduced to the ∼94% confidence level.

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Section: Introductionmentioning

confidence: 72%

Galaxy clusters in the Perseus-Pisces region -- II. The peculiar velocity field

Hudson

Lucey

Smith

et al. 1997

Monthly Notices of the Royal Astronomical Society

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“…This is particularly important for the SFI sample because the adopted redshift-dependent selection criteria imply that near each redshift limit, outflowing galaxies are preferentially excluded from the sample. As shown in Figure 3b, this effect becomes dominant at large distances, leading to a spurious systematic infall of galaxies at the outer edge of the survey volume (da Costa et al 1996). In earlier studies with the SFI data, the biases were estimated using the numerical Monte Carlo technique (Freudling et al 1995;da Costa et al 1996;Branchini et al 2001) or using the semianalytic approach (Freudling et al 1999).…”

Section: Bias Correctionmentioning

confidence: 98%

“…The galaxy peculiar velocities have been used to reconstruct the three-dimensional velocity field or the real-space matter density field of the local universe (e.g., da Costa et al 1996;Dekel et al 1999) and to estimate the amplitude of the mass fluctuation and/or ¼ 0:6 m /b parameter, where b is the linear bias factor. Among the many analysis methods that have been developed and applied to the observational data, one of the major developments has been the POTENT method (Bertschinger et al 1990;Dekel et al 1999), which reconstructs the smoothed three-dimensional peculiar velocity field from the observed radial velocity data.…”

Section: Introductionmentioning

confidence: 99%

“…For completeness of the SFI sample, we exclude galaxies with diameters smaller than 1A7 on the second and the third redshift shells. A small fraction of galaxies with small line widths (log w < 2:25) have also been discarded because of the large fractional errors in the measurement of their widths and thus the large uncertainties in the peculiar velocity measurement (da Costa et al 1996). The total number of galaxies we use in our analysis is 661.…”

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confidence: 99%

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Untitled

2006

ApJ

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We have measured the cosmic momentum power spectrum from the peculiar velocities of galaxies in the SFI sample. The SFI catalog contains field spiral galaxies with radial peculiar velocities derived from the I-band TullyFisher relation. As a natural measure of the large-scale peculiar velocity field, we use the cosmic momentum field that is defined as the peculiar velocity field weighted by the local number of galaxies. We have shown that the momentum power spectrum can be derived from the density power spectrum for the constant linear biasing of galaxy formation, which makes it possible to estimate the S ¼ 0:6 m /b S parameter precisely, where m is the matter density parameter and b S is the bias factor for optical spiral galaxies. At each wavenumber k we estimate S (k) as the ratio of the measured to the derived momentum power over a wide range of scales (0:026 h À1 Mpc P k P 0:157 h À1 Mpc) that spans the linear to the quasi-linear regimes. The estimated S (k) have stable values around 0.5, which demonstrates the constancy of the S parameter at scales down to 40 h À1 Mpc. , which is lower than the high-amplitude power spectra found from the previous maximum likelihood analyses of peculiar velocity samples such as Mark III, SFI, and ENEAR. Subject headingg s: cosmology: theory -large-scale structure of universe

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“…Further descriptive information and access to data are available at the Mark III Web site.4 3.4. SFI The sample contains radial velocities of D1300 SbcÈSc galaxies, with inclination north of d \ [45¡ and Z45¡ galactic latitude (da Costa et al 1996(da Costa et al , 1998 ; o b o Z 10¡ Haynes et al 1999aHaynes et al , 1999b. The data are distributed within an approximately spherical region of radius x max D 7000 km s~1.…”

Section: Numerical Resolutionmentioning

confidence: 99%

Overconstrained Dynamics in Galaxy Redshift Surveys

Susperregi

2001

ApJ

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The least-action principle (LAP) method is used on four galaxy redshift surveys to measure the density parameter and the matter and galaxy-galaxy power spectra. The data sets are PSCz, ORS, Mark III, ) m and SFI. The LAP method is applied on the surveys simultaneously, resulting in an overconstrained dynamical system that describes the cosmic overdensities and velocity Ñows. The system is solved by relaxing the constraint that each survey imposes upon the cosmic Ðelds. A least-squares optimization of the errors that arise in the process yields the cosmic Ðelds and the value of that is the best Ðt to the ) m ensemble of data sets. The analysis has been carried out with a high-resolution Gaussian smoothing of 500 km s~1 and over a spherical selected volume of radius 9000 km s~1. We have assigned a weight to each survey, depending on their density of sampling, and this parameter determines their relative inÑu-ence in limiting the domain of the overall solution. The inÑuence of each survey on the Ðnal value of ) m , the cosmographical features of the cosmic Ðelds, and the power spectra largely depends on the distribution function of the errors in the relaxation of the constraints. We Ðnd that PSCz and Mark III are closer to the Ðnal solution than ORS and SFI. The likelihood analysis yields to 1 p ) m \ 0.37^0.01 level. PSCz and SFI are the closest to this value, whereas ORS and Mark III predict a somewhat lowerThe model of bias employed is a scale-dependent one, and we retain up to 42 bias coefficients in ) m .b rl the spherical harmonics formalism. The predicted power spectra are estimated in the range of wavenumbers h Mpc~1, and we compare these results with measurements recently reported in the 0.02 [ k [ 0.49 literature.

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The Mass Distribution in the Nearby Universe

Cited by 81 publications

References 24 publications

Galaxy clusters in the Perseus-Pisces region -- II. The peculiar velocity field

Galaxy clusters in the Perseus-Pisces region -- II. The peculiar velocity field

Untitled

Overconstrained Dynamics in Galaxy Redshift Surveys

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