Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f01.ps}\end{figure}$ Figure 1: Aitoff projection of the observed sample in J2000 equatorial coordinates, histogram of radial velocities V₂₀ and HI fluxes (see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{6187f02.ps}\end{figure}$ Figure 2: Top: comparison of some of our HI-line width at the 20% level with some independent measurements from Springob et al. (2005). Middle: distribution of signal-to-noise ratio (S/N) as a function of the 20% level line width W₂₀. Bottom: rms noise $\sigma$ in mJy (outside the 21-cm line) versus integration time. The curve shows the line $\sigma =20/\sqrt {T_{\rm int}}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{6187f03.ps}\end{figure}$ Figure 3: Projection of the major axis D₂₅ on the East-West direction.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=9cm,clip]{6187f05.ps}\end{figure}$ Figure 5: Sky distribution of KLUN galaxies used in the current analysis.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6187f06.ps}\end{figure}$ Figure 6: TF residuals ( $Y_{\rm n}$ against the normalised distance modulus ( $X_{\rm n}$ ). The "unbiased plateau'' is the region at $X_{\rm n}<-1$ , where the binned average of the residuals, the balls with error bars, are close to the zero line. The curve going through the balls is the analytical correction formula described by Eq. (8) in Sect. 4.1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f07.ps}\end{figure}$ Figure 7: The evolution of peculiar velocities with respect to the number of iterative loop. Here are the two first galaxies in our sample and an exceptionally "bad'' case (pgc 17978) that was rejected from the final analysis.
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In the text

$\begin{figure} \par\includegraphics[width=16.28cm,clip]{6187f08.ps}\end{figure}$ Figure 8: The true peculiar velocities (on y axis) vs. the velocities obtained with a smoothing method for the GIF consortium simulated data. The upper left corner of each panel gives the essential information about the plot; TS stands for the tensorial smoothing, using nine parameters, the bulk velocity B, and the tensor L; BK is the three parameter bulk smoothing (only B), and SC means scalar smoothing, using a simple Gaussian smoothing window. $r_{\rm s}$ is the smoothing radius, either a distance-dependent value, e.g. 0.15 d or a fixed value, e.g. 10 Mpc h^-1. The rms difference between the smoothed and the true velocity field, $\delta v_{\rm rms}$ , is given in km s^-1. N is the number of points, the simulated galaxies, in each figure. The upper left figure shows the smoothing giving the smallest $\delta v_{\rm rms}$ . In each figure the galaxies in densest regions were excluded, as well as the objects at the low Galactic latitudes. The two panels in the upper right corner show how these points give substantially more divergent values. The "Dense regions'' and " $\vert b\vert<15^\circ$ '' maps were obtained with the TS $r_{\rm s}=0.15 d$ smoothing. V₄ and V₈ correspond to the volume weighted method, using the volume defined by the fourth and the eight closest galaxies, respectively. The volume weighting is claimed to reduce the sampling gradient bias, but in this test they fail to produce a better estimate of the true velocity field than the non-weighted method.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{6187f09.ps}\end{figure}$ Figure 9: Tully-Fisher relations in J, H, and K bands for unbiased plateau galaxies. See Table 4 for the parameters of the relations.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f10.ps}\end{figure}$ Figure 10: Comparison of MarkIII and KLUN distances expressed in km s^-1. The colours represent the different Mark III samples (Willick et al. 1997): HMCL is black, W91CL red, W91PP green, CF blue, MAT turquoise, and A82 purple.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6187f11.ps}\end{figure}$ Figure 11: Radial peculiar velocity field in the supergalactic plane. Blue colors are regions with negative peculiar velocities (infalling), red colors refer to positive ones (outfalling). The shade of the colour corresponds to the amplitude of the motion, and is saturated at 1000 km s^-1. The regions where the threshold requirement of at least two velocity measurements is not satisfied are set white. Black dots are all galaxies with a known redshift in Hyperleda. Green marks show positions of some well known structures - here Virgo, Ursa Major, Norma, Pisces, N533, and Zwicky33. The coordinates are in "real space'', i.e. redshift distances corrected for the smoothed peculiar velocity field, in units of km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6187f12.ps}\end{figure}$ Figure 12: The peculiar velocity maps, as in Fig. 11, projected on four discs of different orientations with respect to the supergalactic plane (SGZ = 0). a) Is rotated by 10 $^\circ$ around the SGX axis. It illustrates the features well around two large rosary structures: the Great Wall starting from Coma and extending counterclockwise up to the Centaurus region, and another starting from the Perseus-Pisces complex, going down through N533 and beyond. Both front and backside infall are visible along the structures. b) Is rotated by -30 $^\circ$ around SGZ from the SGY = 0 plane, and shows the large infall motions towards the two opposite regions, one in Perseus-Pisces and the other in the Great Attractor or Centaurus area. c) Rotated 50 $^\circ$ around SGY from the SGX = 0 plane, shows the infall patterns towards Pegasus, Hydra, and Coma. d) Which is almost perpendicular to the supergalactic plane, rotated -30 $^\circ$ around SGY from the SGX = 0 plane shows an example of some very detailed structures of the velocity field.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{6187f13.ps}\end{figure}$ Figure 13: Upper panel shows the amplitude of the observed bulk motion within a growing sphere of radius $R_{\rm max}$ , and the corresponding $\Lambda$ CDM expected curve for a flat cosmological model using: n=1, $\Omega _{\rm b} = 0.04$ , h = 0.57, and $\Omega _{\rm m}$ = 0.22 $\pm$ 0.02. The bottom panel shows the direction of the bulk flow in galactic coordinates and its evolution with $R_{\rm max}=10$ -60 h^-1 Mpc. The main published results as listed in Table 6 are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f01.ps}\end{figure}$	Figure 1: Aitoff projection of the observed sample in J2000 equatorial coordinates, histogram of radial velocities V₂₀ and HI fluxes (see Table 2).
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$\begin{figure} \par\includegraphics[width=8.45cm,clip]{6187f02.ps}\end{figure}$	Figure 2: Top: comparison of some of our HI-line width at the 20% level with some independent measurements from Springob et al. (2005). Middle: distribution of signal-to-noise ratio (S/N) as a function of the 20% level line width W₂₀. Bottom: rms noise $\sigma$ in mJy (outside the 21-cm line) versus integration time. The curve shows the line $\sigma =20/\sqrt {T_{\rm int}}$ .
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$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{6187f03.ps}\end{figure}$	Figure 3: Projection of the major axis D₂₅ on the East-West direction.
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$\begin{figure} \par\includegraphics[angle=270,width=9cm,clip]{6187f05.ps}\end{figure}$	Figure 5: Sky distribution of KLUN galaxies used in the current analysis.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{6187f06.ps}\end{figure}$	Figure 6: TF residuals ( $Y_{\rm n}$ against the normalised distance modulus ( $X_{\rm n}$ ). The "unbiased plateau'' is the region at $X_{\rm n}<-1$ , where the binned average of the residuals, the balls with error bars, are close to the zero line. The curve going through the balls is the analytical correction formula described by Eq. (8) in Sect. 4.1.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f07.ps}\end{figure}$	Figure 7: The evolution of peculiar velocities with respect to the number of iterative loop. Here are the two first galaxies in our sample and an exceptionally "bad'' case (pgc 17978) that was rejected from the final analysis.
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$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{6187f09.ps}\end{figure}$	Figure 9: Tully-Fisher relations in J, H, and K bands for unbiased plateau galaxies. See Table 4 for the parameters of the relations.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6187f10.ps}\end{figure}$	Figure 10: Comparison of MarkIII and KLUN distances expressed in km s^-1. The colours represent the different Mark III samples (Willick et al. 1997): HMCL is black, W91CL red, W91PP green, CF blue, MAT turquoise, and A82 purple.
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