125 research outputs found
Multifrequency Method for Mapping Active Galactic Nuclei with Allowance for the Frequency-Dependent Image Shift
We consider the problem of multifrequency VLBA image synthesis and
spectral-index mapping for active galactic nuclei related to the necessity of
taking into account the frequency-dependent image shift. We describe our
generalized multifrequency synthesis algorithm with a spectral correction based
on the maximum entropy method. The results of our processing of multifrequency
VLBI data for the radio sources J2202+4216, J0336+3218, and J1419+5423 are
presented.Comment: 12 pages, 2 tables, 6 figure
Peculiarities of Open Star Clusters with High Vertical Velocities from the Region of the Sco-Cen OB Association
We have studied the kinematics of a unique sample of young open star clusters
(OSCs) with high vertical velocities, km s. The
characteristics of these clusters were taken from the catalogue by Hunt and
Reffert (2023), where their mean proper motions, line-of-sight velocities, and
distances were calculated using Gaia DR3 data. These OSCs are located within
0.6 kpc of the Sun and form two clumps: one in the region of the Sco-Cen OB
association and the other one in the region of the Per OB3-Per OB2
associations. The OSC group of 47 members in the region of the Sco-Cen
association is shown to expand along the axis, km s kpc. This group also has a positive rotation
around the axis with an angular velocity of km s
kpc and a negative rotation around the axis with an angular velocity
of km s kpc. Based on the velocities of 27 OSCs from
the region of the Per OB3-Per OB2 associations, we have found no gradients
differing significantly from zero. We have studied the kinematics of more than
1700 stars selected by Luhman (2022) as probable members of the Sco-Cen OB
association. These stars are shown to have no high vertical velocities. The
expansion coefficient of the stellar system in the plane has been found
from all stars to be km s kpc. Based on stars
from the three UCL, LCC, and V1062 Sco groups with a mean age 20 Myr, for
the first time we have found a volume expansion coefficient of the stellar
system differing significantly from zero, km s
kpc.Comment: 13 pages, 7 figures, 0 table
Determination of the Spiral Pattern Speed in the Milky Way from Young Open Star Clusters
We have estimated the spiral pattern speed in the Galaxy from a
large sample of young open star clusters (OSCs). For this purpose, we have used
2494 OSCs younger than 50 Myr. Their mean proper motions, line-of-sight
velocities, and distances were calculated by Hunt and Reffert (2023) based on
data from the Gaia~DR3 catalogue. Three methods have been applied to estimate
. They all are based on the linear Lin-Shu spiral density wave
theory. We have obtained an estimate of ~km s
kpc by the first method, which is most reliable in our view, using the
velocity perturbations and found through a spectral analysis
of the radial, , and residual rotation, velocities.
Using the second method, we have found the velocity perturbations and
by solving the basic kinematic equations together with the Galactic
rotation parameters and obtained an estimate of ~km
s kpc. We have found ~km s
kpc by the third method based on an analysis of the position angles of
OSCs at their birth time .Comment: 15 pages, 5 figures, 1 table. arXiv admin note: text overlap with
arXiv:2203.12902, arXiv:1903.09313, arXiv:2207.0341
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