scholarly journals The HI in the Large Barred Spiral NGC 1365

1996 ◽  
Vol 157 ◽  
pp. 168-171 ◽  
Author(s):  
S. Jörsäter ◽  
G. A. van Moorsel
Keyword(s):  
High Resolution ◽  
Velocity Field ◽  
Spiral Galaxy ◽  
Rotation Curve ◽  
Spiral Arms ◽  
Barred Spiral Galaxy ◽  
Inner Parts ◽  
Ngc 1365

AbstractWe have made high resolution HI observations using the VLA1 of the barred spiral galaxy NGC 1365. This galaxy contains 15.2 × 109M⊙ of HI. The velocity field is strongly affected by the bar only in the inner parts. NGC 1365 has a warp and it has 4 well developed spiral arms and 2 rudimentary ones. NGC 1365 has an unusually dropping rotation curve.

scholarly journals The Circumnuclear Region in NGC 4321

1995 ◽  
Vol 10 ◽  
pp. 539-542
Author(s):  
J.H. Knapen ◽  
J.E. Beckman ◽  
I. Shlosman ◽  
C.H. Heller ◽  
R.F. Peletier ◽  
...  
Keyword(s):  
High Resolution ◽  
Spiral Galaxy ◽  
Resonance Interaction ◽  
Dynamical Model ◽  
High Resolution Imaging ◽  
Spiral Arms ◽  
Near Ir ◽  
Resolution Imaging ◽  
Barred Spiral Galaxy

AbstractWe present results from a recent study of the inner 1 kpc zone of the weakly barred spiral galaxy NGC 4321 (M100), which reveals a circumnuclear starburst, organized in a pair of tightly-wound spiral arms. Combining high-resolution imaging in the optical and near-IR with a detailed dynamical model, we show that the morphology of this region can be explained by a resonance interaction between the disk and the stellar bar and its effects on the gas.

scholarly journals Optical long slit velocities and a combined optical and H i  velocity field for the barred spiral galaxy NGC 1365

1996 ◽  
Vol 120 (3) ◽  
pp. 403-414 ◽  
Author(s):  
P. O. Lindblad ◽  
M. Hjelm ◽  
J. Högbom ◽  
S. Jörsäter ◽  
P. A.B. Lindblad ◽  
...  
Keyword(s):  
Velocity Field ◽  
Spiral Galaxy ◽  
Barred Spiral Galaxy ◽  
Ngc 1365

scholarly journals Hydrodynamical Simulations of the Barred Spiral Galaxy NGC 1365

1996 ◽  
Vol 157 ◽  
pp. 413-415
Author(s):  
P. A. B. Lindblad ◽  
P. O. Lindblad ◽  
E. Athanassoula
Keyword(s):  
Gravitational Field ◽  
Gas Dynamics ◽  
Rotation Curve ◽  
Barred Galaxies ◽  
Mosaic Image ◽  
Dynamical Parameters ◽  
Pattern Speed ◽  
Barred Spiral Galaxy ◽  
Hydrodynamical Simulations ◽  
Ngc 1365

Several authors have explored the field of gas dynamics in barred systems. One of the aims of these investigations was to compare the model gaseous response, due to some assumed underlying stellar gravitational field, with observed gas density distribution and kinematics of barred galaxies. The gas is known to respond in a highly non-linear way, and therefore should give clues to dynamical parameters like the mass distribution, positions and existence of principal resonances and thereby the pattern speed.High resolution HI data now exist for NGC 1365 (Jörsäter & van Moorsel 1995), and the kinematical HI data have been combined with optical long slit measurements to obtain the velocity field (Lindblad et al. 1995) used for extracting the rotation curve, representing the axisymmetric forces in NGC 1365, and for comparisons with models. A mosaic image of NGC 1365 in the J-band was used to compute the perturbing potential used in the models.

The velocity field of the barred spiral galaxy NGC 5383

1978 ◽  
Vol 219 ◽  
pp. 31 ◽  
Author(s):  
C. J. Peterson ◽  
N. Thonnard ◽  
V. C. Rubin ◽  
W. K., Jr. Ford
Keyword(s):  
Velocity Field ◽  
Spiral Galaxy ◽  
Barred Spiral Galaxy

scholarly journals HI Study of the NGC 6744 System

1999 ◽  
Vol 16 (1) ◽  
pp. 84-88 ◽  
Author(s):  
Stuart D. Ryder ◽  
Wilfred Walsh ◽  
David Malin
Keyword(s):  
Velocity Field ◽  
Spiral Galaxy ◽  
Neutral Hydrogen ◽  
Optical Disk ◽  
Mass Model ◽  
Spiral Arms ◽  
Preliminary Results ◽  
Heliocentric Velocity ◽  
Compact Array

AbstractWe present the preliminary results of our 5-configuration, 20-pointing mosaic with the Australia Telescope Compact Array of the neutral hydrogen in the nearby spiral galaxy NGC 6744. The bulk of the HI resides in a ‘ring’ underlying the outer optical disk, with 2 HI spiral arms extending further out to almost 1·5 optical radii. The velocity field is fairly regular, apart from evidence for streaming motions along the HI arms, and the influence of the companion IB(s)m galaxy NGC 6744A. We associate a cloud of HI at a heliocentric velocity of 846 km s−1 with another companion object, ESO 104–g44. Our attempts to construct a mass model for NGC 6744 suffer from poor resolution in the inner disk, and the uncertainty in the total HI flux of NGC 6744. We anticipate that HIPASS observations will be crucial in resolving the latter issue.

scholarly journals Zoom-in cosmological hydrodynamical simulation of a star-forming barred, spiral galaxy at redshift z = 2

2019 ◽  
Vol 488 (4) ◽  
pp. 4674-4689 ◽  
Author(s):  
Fiorenzo Vincenzo ◽  
Chiaki Kobayashi ◽  
Tiantian Yuan
Keyword(s):  
Star Formation ◽  
Angular Velocity ◽  
Spiral Galaxy ◽  
Stellar Populations ◽  
Spiral Arms ◽  
Star Forming ◽  
Thin Disc ◽  
The Galaxy ◽  
Barred Spiral Galaxy ◽  
Zoom In

ABSTRACTWe present gas and stellar kinematics of a high-resolution zoom-in cosmological chemodynamical simulation, which fortuitously captures the formation and evolution of a star-forming barred spiral galaxy, from redshift z ∼ 3 to z ∼ 2 at the peak of the cosmic star formation rate. The galaxy disc grows by accreting gas and substructures from the environment. The spiral pattern becomes fully organized when the gas settles from a thick (with vertical dispersion σv > 50 km s−1) to a thin (σv ∼ 25 km s−1) disc component in less than 1 Gyr. Our simulated disc galaxy also has a central X-shaped bar, the seed of which formed by the assembly of dense gas-rich clumps by z ∼ 3. The star formation activity in the galaxy mainly happens in the bulge and in several clumps along the spiral arms at all redshifts, with the clumps increasing in number and size as the simulation approaches z = 2. We find that stellar populations with decreasing age are concentrated towards lower galactic latitudes, being more supported by rotation, and having also lower velocity dispersion; furthermore, the stellar populations on the thin disc are the youngest and have the highest average metallicities. The pattern of the spiral arms rotates like a solid body with a constant angular velocity as a function of radius, which is much lower than the angular velocity of the stars and gas on the thin disc; moreover, the angular velocity of the spiral arms steadily increases as a function of time, always keeping its radial profile constant. The origin of our spiral arms is also discussed.

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