Large-scale collective motion of RFGC galaxies

Abstract

We processed the data about radial velocities and HI linewidths for 1678 flat edge-on spirals from the Revised Flat Galaxy Catalogue. We obtained the parameters of the multipole components of large-scale velocity field of collective non-Hubble galaxy motion as well as the parameters of the generalized Tully-Fisher relationship in the "HI line width -linear diameter" version. All the calculations were performed independently in the framework of three models, where the multipole decomposition of the galaxy velocity field was limited to a dipole, quadrupole and octopole terms respectively. We showed that both the quadrupole and the octopole components are statistically significant.On the basis of the compiled list of peculiar velocities of 1623 galaxies we obtained the estimations of cosmological parameters Ω m and σ 8 . This estimation is obtained in both graphical form and as a constraint of the value S 8 = (Ω m /0.3) 0.35 σ 8 = 0.91 ± 0.05.

Declining rotation curves of galaxies as a test of gravitational theory

“…The galaxy NGC 4244 (Willick et al 1997;Parnovsky & Parnowski 2010) is the most effective source near to NGC 4736 (Sofue 1991;Becker, White, & Helfand 1995;Dale et al 2007;Radburn-Smith et al 2011) with a distance of 4.12 Mpc from us. With a luminosity of LV = 2.82 × 10 9 L⊙ and distance of 0.98…”

The distribution of interstellar dust in CALIFA edge-on galaxies via oligochromatic radiative transfer fitting

“…In the optical SDSS images, it is a regular galaxy without evidence for perturbations. We assumed a distance of 54.2 Mpc ( the average of Tully-Fisher based distances (Theureau et al 2007;Springob et al 2009;Parnovsky & Parnowski 2010)). The FitSKIRT model reproduces the images quite accurately.…”

Yet another sample of RFGC galaxies

“…This is demonstrated in Figure 1 where the boundaries of 1σ, 2σ and 3σ confidence areas of the apices of the dipolar component are shown for 3 different samples using the D-model with R max = 100h −1 Mpc. The new sample is shown with black lines, the sample introduced in the articles (Parnovsky & Parnowski 2009, 2010a) is shown with light green lines, and the sample introduced by Parnovsky & Tugay (2004) is shown with sky blue lines. The Figure 1 is a Mollweide projection of a part of the celestial sphere.…”

“…In our previous articles (Parnovsky et al 2001;Parnovsky & Tugay 2004;Parnovsky & Parnowski 2010a we described the models of the collective motion we used. Here we will only give two models given there.…”