On systematic errors in distance estimates of the Virgo cluster and the intrinsic scatter in the Tully-Fisher relation

1989 ◽  
Vol 343 ◽  
pp. 18 ◽  
Author(s):  
David Burstein ◽  
Somak Raychaudhury
Keyword(s):  
Systematic Errors ◽  
Virgo Cluster ◽  
Fisher Relation ◽  
Intrinsic Scatter

The Tully-Fisher Relation in Coma and Virgo Cluster S0 Galaxies

2003 ◽  
Vol 126 (6) ◽  
pp. 2622-2634 ◽  
Author(s):  
J. L. Hinz ◽  
G. H. Rieke ◽  
N. Caldwell
Keyword(s):  
Virgo Cluster ◽  
Fisher Relation ◽  
S0 Galaxies

scholarly journals The stochastic enrichment of Population II stars

2020 ◽  
Vol 500 (4) ◽  
pp. 5214-5228
Author(s):  
Louise Welsh ◽  
Ryan Cooke ◽  
Michele Fumagalli
Keyword(s):  
First Generation ◽  
Milky Way ◽  
Systematic Errors ◽  
Chemical Abundances ◽  
Chemical Enrichment ◽  
Halo Stars ◽  
Chemical Products ◽  
Population Iii Stars ◽  
Intrinsic Scatter ◽  
Population Iii

ABSTRACT We investigate the intrinsic scatter in the chemical abundances of a sample of metal-poor ([Fe/H] < −2.5) Milky Way halo stars. We draw our sample from four historic surveys and focus our attention on the stellar Mg, Ca, Ni, and Fe abundances. Using these elements, we investigate the chemical enrichment of these metal-poor stars using a model of stochastic chemical enrichment. Assuming that these stars have been enriched by the first generation of massive metal-free stars, we consider the mass distribution of the enriching population alongside the stellar mixing and explosion energy of their supernovae. For our choice of stellar yields, our model suggests that the most metal-poor stars were enriched, on average, by $\hat{N}_{\star }=5^{+13}_{-3}~(1\sigma)$ Population III stars. This is comparable to the number of enriching stars inferred for the most metal-poor DLAs. Our analysis therefore suggests that some of the lowest mass structures at z ∼ 3 contain the chemical products from < 13(2σ) Population III enriched minihaloes. The inferred IMF is consistent with that of a Salpeter distribution and there is a preference towards ejecta from minimally mixed hypernovae. However, the estimated enrichment model is sensitive to small changes in the stellar sample. An offset of ∼ 0.1 dex in the [Mg/Ca] abundance is shown to be sensitive to the inferred number of enriching stars. We suggest that this method has the potential to constrain the multiplicity of the first generation of stars, but this will require: (1) a stellar sample whose systematic errors are well understood; and, (2) documented uncertainties associated with nucleosynthetic yields.

scholarly journals Corrections for Velocity Dispersion in the Tully-Fisher Relation

1983 ◽  
Vol 6 ◽  
pp. 283-285
Author(s):  
L. Bottinelli ◽  
L. Gouguenheim ◽  
G. Paturel ◽  
G. de Vaucouleurs
Keyword(s):  
Line Width ◽  
Velocity Dispersion ◽  
Rotational Velocity ◽  
Systematic Errors ◽  
Fisher Relation

The 21-cm line width is a good indication of the maximum rotational velocity in a galaxy. However, the turbulent motions affect the observed line width and must be corrected. Not taking them into account introduces both accidental and systematic errors.A first example of this effect is the dependence of the slope a of the Tully-Fisher relation:on the level at which the line width ΔVobs. is measured. In their 1977 paper, Tully and Fisher find the following values:A second example is the departure from linearity in the H-band Tully-Fisher relation obtained by Aaronson et al. (1982) (their figure 2): the narrow lines are more strongly affected by these turbulent motions.

scholarly journals Study of the Virgo Cluster Using the B ‐Band Tully‐Fisher Relation

1997 ◽  
Vol 108 (2) ◽  
pp. 417-448 ◽  
Author(s):  
Naoki Yasuda ◽  
Masataka Fukugita ◽  
Sadanori Okamura
Keyword(s):  
Virgo Cluster ◽  
Fisher Relation

scholarly journals Tully-Fisher Relations from an HI-Selected Sample

2004 ◽  
Vol 220 ◽  
pp. 411-412
Author(s):  
Martin J. Meyer ◽  
Martin A. Zwaan ◽  
Rachel L. Webster ◽  
Stephen E. Schneider
Keyword(s):  
Distance Measure ◽  
Sky Survey ◽  
Fisher Relation ◽  
Intrinsic Scatter

The Tully-Fisher relation is of interest because of its use as a secondary distance measure and the constraints it places on the physics of rotationally supported galaxies. We use data from the HI Parkes All-Sky Survey Catalogue to study and apply the Tully-Fisher relation on a sample of galaxies selected on their HI properties. the issues of third parameter dependencies and intrinsic scatter of the Tully-Fisher relation are investigated.

scholarly journals Large Peculiar Velocities in the Hydra Centaurus Supercluster

1988 ◽  
Vol 130 ◽  
pp. 185-189
Author(s):  
M. Aaronson ◽  
G.D. Bothun ◽  
K.G. Budge ◽  
J.A. Dawe ◽  
R.J. Dickens ◽  
...  
Keyword(s):  
Velocity Field ◽  
Data Collection ◽  
Large Scale ◽  
Galactic Plane ◽  
Systematic Errors ◽  
Preliminary Results ◽  
Peculiar Velocities ◽  
Upper Limit ◽  
Fisher Relation

Six clusters forming part of the Hydra-Cen Supercluster and its extension on the opposite side of the galactic plane are under study at 21 cm with the Parkes radiotelescope. The infrared Tully-Fisher relation is used to determine the relative distances of the clusters. These clusters exhibit significant and generally positive peculiar velocities ranging from essentially zero for the Hydra cluster to as much as 1000 km/sec for the Pavo and Centaurus clusters. An upper limit of 500 km/sec was previously found in the study of clusters accessible from Arecibo. Data collection is not yet complete, however, and is further subject to unstudied systematic errors due to present reliance on photographic galaxy diameters. Nevertheless, these preliminary results support the notion of a large scale (and presumably gravitationally) disturbed velocity field in the second and third quadrants of the supergalactic plane.

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