The I band Tully-Fisher relation for cluster galaxies: data presentation.

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

doi:10.1086/118233

Cited by 256 publications

(426 citation statements)

References 29 publications

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“…Our mean PP radial motion result is in apparent conflict with the TF results of Willick (1990Willick ( , 1991 and HM which had found a ∼ −400 km s −1 peculiar velocity of the PP ridge, but our results are in better agreement with the recent TF data of Giovanelli et al (1996Giovanelli et al ( ,1997a. Comparison of elliptical and spiral samples, is far from straightforward, however, due to the complex nature of the peculiar velocity field and the different regions probed by different surveys.…”

Section: Discussioncontrasting

confidence: 86%

“…Our measured cluster peculiar velocities are compared with FP, TF and BCG results from the literature, for clusters in common. Literature sources are JFK96, HM data rederived by Willick et al (1997a), Giovanelli et al (1997b) (SCI), LP and HE. To the distance errors we have added in quadrature the error in the mean redshift, using the number of galaxies in the cluster and the cluster velocity dispersions derived in our work.…”

Section: Individual Cluster Distances and Peculiar Velocitiesmentioning

confidence: 99%

See 1 more Smart Citation

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: Discussioncontrasting

confidence: 86%

Section: Individual Cluster Distances and Peculiar Velocitiesmentioning

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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“…The luminosities of their galaxies have been corrected for absorption as if observed face-on. Unfortunately this correction does not take into account the demonstrated dependence of such a correction on total luminosity of a galaxy (Giovanelli et al 1997;Tully et al 1998). In practice Palunas & Williams make a correction more or less as if all their galaxies belong to the most luminous category.…”

Section: The Mass-to-light Ratiomentioning

confidence: 99%

Dark and luminous matter in the NGC 3992 group of galaxies

Bottema¹,

Verheijen²

2002

A&A

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Abstract. Detailed neutral hydrogen observations have been obtained of the large barred spiral galaxy NGC 3992 and its three small companion galaxies, UGC 6923, UGC 6940, and UGC 6969. For the main galaxy, the H i distribution is regular with a low level radial extension outside the stellar disc. However, at exactly the region of the bar, there is a pronounced central H i hole in the gas distribution. Likely gas has been transported inwards by the bar and because of the emptyness of the hole no large accretion events can have happened in recent galactic times. The gas kinematics is very regular and it is demonstrated that the influence of the bar potential on the velocity field is negligible. A precise and extended rotation curve has been derived showing some distinct features which can be explained by the non-exponential radial light distribution of NGC 3992. The decomposition of the rotation curve gives a slight preference for a sub maximal disc, though a range of disc contributions, up to a maximum disc situation fits nearly equally well. For such a maximum disc contribution, which might be expected in order to generate and maintain the bar, the required mass-to-light ratio is large but not exceptional.

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“…McGaugh et al 2000;Bell & de Jong 2001;Gurovich et al 2004;McGaugh 2005;Pfenniger & Revaz 2005;Begum et al 2008;Trachternach et al 2009;Stark et al 2009;Gurovich et al 2010;Zaritsky et al 2014), extension of the Tully-Fisher relation (hereafter TF, e.g. Tully & Fisher 1977;Pierce & Tully 1988;Teerikorpi 1995;Giovanelli et al 1997b;Courteau & Rix 1999;Tully & Pierce 2000;Giovanelli et al 1997a;Karachentsev et al 2002;Bedregal et al 2006;Noordermeer & Verheijen 2007;Springob et al 2007;Williams et al 2010;Tully & Courtois 2012;Mocz et al 2012;Rawle et al 2013;Torres-Flores et al 2013;Sorce et al 2013Sorce et al , 2014b to the low luminosity galaxies, is often used to constrain and test galaxy formation and evolution models, with various computational methods, in the ΛCDM scenario as well as in alternative theories (e.g. Steinmetz & Navarro 1999;Mo et al 1998;McGaugh & de Blok 1998;Eisenstein & Loeb 1995;van den Bosch 2000;Mayer & Moore 2004;Gnedin et al 2007;Governato et al 2007;Avila-Reese et al 2008;McGaugh 2012;…”

Section: Introductionmentioning

confidence: 99%

The baryonic Tully–Fisher relation cares about the galaxy sample

Sorce¹,

Guo²

2016

Mon. Not. R. Astron. Soc.

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The Baryonic Tully-Fisher relation (BTFR) is a clear manifestation of the underlying physics of galaxy formation. As such, it is used to constrain and test galaxy formation and evolution models. Of particular interest, apart from the slope of the relation, is its intrinsic scatter. In this paper, we use the eagle simulation to study the dependence of the BTFR on the size of the simulated galaxy sample. The huge number of datapoint available in the simulation is indeed not available with current observations. Observational studies that computed the BTFR used various (small) size samples with the only obligation to have galaxies spanning over a large range of masses and rotation rates. Accordingly, to compare observational and theoretical results, we build a large number of various size datasets using the same criterion and derive the BTFR for all of them. Unmistakably, their is an effect of the number of galaxies used to derive the relation. The smaller the number, the larger the standard deviation around the average slope and intrinsic scatter of a given size sample of galaxies. This observation allows us to alleviate the tensions between observational measurements and ΛCDM predictions. Namely, the size of the observational samples adds up to the complexity in comparing observed and simulated relations to discredit or confirm ΛCDM. Similarly, samples, even large, that do not reflect the galaxy distribution give on average biased results. Large size samples reproducing the underlying distribution of galaxies constitute a supplementary necessity to compare efficiently observations and simulations.

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The I band Tully-Fisher relation for cluster galaxies: data presentation.

Cited by 256 publications

References 29 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

Dark and luminous matter in the NGC 3992 group of galaxies

The baryonic Tully–Fisher relation cares about the galaxy sample

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