Velocity fields in late-type galaxies from H-alpha Fabry-Perot interferometry. III - The spiral galaxy NGC 6503

1982 ◽  
Vol 49 ◽  
pp. 515 ◽  
Author(s):  
G. de Vaucouleurs ◽  
A. Caulet
Keyword(s):  
Spiral Galaxy ◽  
Velocity Fields ◽  
Late Type ◽  
Fabry Perot

scholarly journals Spectroscopy of H II regions in the late-type spiral galaxy NGC 6946

2013 ◽  
Vol 68 (1) ◽  
pp. 40-52 ◽  
Author(s):  
A. S. Gusev ◽  
F. H. Sakhibov ◽  
S. N. Dodonov
Keyword(s):  
Spiral Galaxy ◽  
H Ii Regions ◽  
Late Type ◽  
Ngc 6946

Ca II Emission from Late-type Stars

1983 ◽  
Vol 5 (2) ◽  
pp. 152-157 ◽  
Author(s):  
L. E. Cram
Keyword(s):  
Line Profile ◽  
Strong Correlation ◽  
Velocity Fields ◽  
Line Profiles ◽  
Late Type ◽  
Wide Range ◽  
Cool Stars ◽  
Visual Magnitude ◽  
The Absolute ◽  
Emission Core

Two recent observational surveys of the Ca II resonance lines (Zarro and Rodgers 1983; Linsky et al. 1979) illustrate the great diversity of line profile shapes found in the spectra of cool stars. This diversity reflects a corresponding wide range in the underlying chromospheric properties of the stars. There are, however, three well-marked systematic trends in the shapes of Ca II line profiles which presumably reflect systematic trends in chromospheric properties. One of these, the Wilson-Bappu effect (Wilson and Bappu 1957), describes the strong correlation betweeen the width of the emission core (see Figure 1) and the absolute visual magnitude of the star. Despite much work, it is still not clear whether this is due primarily to systematic changes of velocity fields (e.g. Hoyle and Wilson 1958) or optical depths (e.g. Jefferies and Thomas 1959) in stellar chromospheres.

scholarly journals An exceptional population of late-type WC stars in the metal-rich spiral galaxy M 83

2004 ◽  
Vol 419 (2) ◽  
pp. L17-L20 ◽  
Author(s):  
P. A. Crowther ◽  
L. J. Hadfield ◽  
H. Schild ◽  
W. Schmutz
Keyword(s):  
Spiral Galaxy ◽  
Late Type

scholarly journals The imprint of arms and bars on rotation curves: in-plane and off-plane

2020 ◽  
Vol 496 (2) ◽  
pp. 1845-1856
Author(s):  
Luis A Martinez-Medina ◽  
Barbara Pichardo ◽  
Antonio Peimbert
Keyword(s):  
Spiral Galaxy ◽  
Pitch Angle ◽  
Local Minima ◽  
Late Type ◽  
Rotation Curves ◽  
Spiral Arms ◽  
Stellar Disc ◽  
Secular Evolution ◽  
Galaxy Model ◽  
Characteristic Features

ABSTRACT Within rotation curves (RCs) is encoded the kinematical state of the stellar disc as well as information about the dynamical mechanisms driving the secular evolution of galaxies. To explain the characteristic features of RCs which arise by the influence of spiral patterns and bar, we study the kinematics of the stellar disc in a set of spiral galaxy models specifically tailored for this purpose. We find that, for our models, the induced non-circular motions are more prominent for spirals with larger pitch angle, the ones typical in late-type galaxies. Moreover, inside corotation, stars rotate slower along the spiral arms than along the interarm, which translates into a local minima or maxima in the RC, respectively. We also see, from off-plane RC, that the rotation is faster for stars that at observed closer to the plane, and diminishes as one looks farther off plane; this trend is more noticeable in our Sa galaxy model than our Sc galaxy model. Additionally, in a previous work we found that the diagonal ridges in the Vϕ–R plane, revealed through the GaiaDR2, have a resonant origin due to the spiral arms and bar and that these ridges project themselves as wiggles in the RC; here, we further notice that the development of these ridges, and the development of high orbital eccentricities in the stellar disc are the same. Hence, we conclude that, the following explanations of bumps and wiggles in RCs are equivalent: they are manifestations of diagonal ridges in the Vϕ–R plane, or of the rearrangement of the orbital eccentricities in the stellar disc.

scholarly journals DYNAMICAL CONSTRAINTS ON THE MASSES OF THE NUCLEAR STAR CLUSTER AND BLACK HOLE IN THE LATE-TYPE SPIRAL GALAXY NGC 3621

2008 ◽  
Vol 690 (1) ◽  
pp. 1031-1044 ◽  
Author(s):  
Aaron J. Barth ◽  
Louis E. Strigari ◽  
Misty C. Bentz ◽  
Jenny E. Greene ◽  
Luis C. Ho
Keyword(s):  
Black Hole ◽  
Spiral Galaxy ◽  
Star Cluster ◽  
Late Type ◽  
Dynamical Constraints ◽  
The Masses

scholarly journals Mass Determination in the Late-Type Spiral NGC 5457

2004 ◽  
Vol 220 ◽  
pp. 321-322
Author(s):  
Ivânio Puerari ◽  
Margarita Valdez-Gutiérrez ◽  
Margarita Rosado
Keyword(s):  
Dark Matter ◽  
Hii Regions ◽  
Matter Content ◽  
Gas Content ◽  
Dynamical Analysis ◽  
Mass Determination ◽  
Late Type ◽  
Ionized Gas ◽  
Fabry Perot ◽  
Insight Into

We have performed a kinematical and dynamical analysis of the ionized gas content of the late–type spiral NGC 5457 (M101) by means of scanning Fabry–Perot interferometry. the purpose of this study is to gain insight into the dark matter content in this galaxy. A sample of 263 HII regions were catalogued. We calculated radial velocity and velocity dispersions. From the dynamics of the ionized gas we were able to infer a mass of 9.8 × 1010 M⊙ inside a radius of 4'8 (or 10 kpc).

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