 |
Figure 1:
Color-magnitude diagram for all identified CLLA stars.
Hipparcos parallaxes were used to determine MV and its
standard error. The full lines indicate the zero age main sequence
(ZAMS) and main sequences of the old open clusters M 67 and NGC
188. The dashed line is the ZAMS shifted upward by
mag, used to remove the contamination by subgiants and
giants. |
| Open with DEXTER | |
In the text
 |
Figure 2:
Hipparcos trigonometric parallaxes versus the photometric
parallaxes of CLLA, for 539 stars ( top-left) and for different
metallicity cuts : [Fe/H] <-1.6 ( top-right), [Fe/H] >-1( center-left), 
[Fe/H] 
( center-right), and for stars at large
distances,
 mas ( bottom-left). The full line is a linear
fit to the data. |
| Open with DEXTER | |
In the text
 |
Figure 3: Spatial distribution of the samples CLLA-TYC2+HIP a) to c) and CLLA-Tycho-2 d) to f), respectively. X points towards the Galactic center, Y in the direction of galactic rotation and Z towards the Galactic north pole. |
| Open with DEXTER | |
In the text
 |
Figure 4:
Space velocity components
 versus metallicity [Fe/H] of
the samples CLLA-TYC2+HIP a) to c) and CLLA-Tycho-2 d) to f),
respectively. |
| Open with DEXTER | |
In the text
 |
Figure 5:
Toomre diagram:
(U2+W2)1/2 versus
distributions of CLLA-TYC2+HIP and CLLA-Tycho 2 samples. The solid lines represent total velocities of
50, 100, 150 and 200 km s-1, respectively. |
| Open with DEXTER | |
In the text
 |
Figure 6:
Rotational velocity (
)
distributions of
sample CLLA-TYC2+HIP grouped according to their metallicities. The
velocities are reduced to the local standard of rest. |
| Open with DEXTER | |
In the text
 |
Figure 7: The same as Fig. 6, but for sample CLLA-Tycho 2. |
| Open with DEXTER | |
In the text