A southern sky survey of the peculiar velocities of 1355 spiral galaxies

Mathewson, D. S.; Ford, V. L.; Buchhorn, Markus

doi:10.1086/191700

Cited by 406 publications

(600 citation statements)

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“…For this section, we use data presented by Persic & Salucci (1995): they re-analyze 967 Hα velocity rotation curves originally observed by Mathewson et al (1992), and publish the offset between the kinematical center (which symmetrize the rotation curve) and the optical center. We divide these galaxies into a screened and unscreened sample using the methodology presented in Section 2, leading to 25 (690) unscreened galaxies and 858 (193) screened galaxies for fR0 = 2 × 10 −7 (fR0 = 10 −6 ).…”

Section: Offset Between Optical Center and Hα Kinematical Centermentioning

confidence: 99%

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Vikram

Cabré

Jain

et al. 2013

J. Cosmol. Astropart. Phys.

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This paper is the third in a series on tests of gravity using observations of stars and nearby dwarf galaxies. We carry out four distinct tests using published data on the kinematics and morphology of dwarf galaxies, motivated by the theoretical work of Hui et al. (2009) andJain &Vanderplas (2011). In a wide class of gravity theories a scalar field couples to matter and provides an attractive fifth force. Due to their different self-gravity, stars and gas may respond differently to the scalar force leading to several observable deviations from standard gravity. HI gas, red giant stars and main sequence stars can be displaced relative to each other, and the stellar disk can display warps or asymmetric rotation curves aligned with external potential gradients. To distinguish the effects of modified gravity from standard astrophysical phenomena, we use a control sample of galaxies that are expected to be screened from the fifth force. In all cases we find no significant deviation from the null hypothesis of general relativity. The limits obtained from dwarf galaxies are not yet competitive with the limits from cepheids obtained in our first paper, but can be improved to probe regions of parameter space that are inaccessible using other tests. We discuss how our methodology can be applied to new radio and optical observations of nearby galaxies.

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Section: Offset Between Optical Center and Hα Kinematical Centermentioning

confidence: 99%

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Vikram

Cabré

Jain

et al. 2013

J. Cosmol. Astropart. Phys.

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“…by Centaurus or the GA, or whether it is due to more distant sources. For example, the claim by Mathewson, Ford and Buchhorn (1992) that 'backside infall' is not observed behind the Great Attractor, argues for coherent streaming motions generated at very large distances.…”

Section: Introductionmentioning

confidence: 99%

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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“…The lower value of 8 is the major factor in reducing the spread. However lower values of 8 than the ones shown in the gure are not allowed by the abundance of { 7 { clusters of galaxies (Mathewson et al 1992) as long as its scatter is ignored.…”

Section: Methods and Resultsmentioning

confidence: 86%

“…By now, various catalogs have been compiled with an interest in calibrating and applying this relation. Di erences in observational technique, such as bandpass, the method for observing the rotational velocity, and sample selection, a ect the power-law slope and degree of scatter in the relation, with I band observations providing the tightest t and 2:7 (Mathewson et al 1992). In the largest samples the scatter in the relation is around 0.4 mag over two decades in luminosity (Mathewson & Ford 1994;Willick et al 1995a,b,c), while in other samples, scatter as low as 0.1 mag has been reported (Bernstein et al 1994).…”

Section: Introductionmentioning

confidence: 99%