Velocity fields in late-type galaxies from H-alpha Fabry-Perot interferometry. I - Instrumentation and data reduction

1980 ◽  
Vol 242 ◽  
pp. 18 ◽  
Author(s):  
G. de Vaucouleurs ◽  
W. D. Pence
Keyword(s):  
Data Reduction ◽  
Velocity Fields ◽  
Late Type ◽  
Fabry Perot

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 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).

scholarly journals Reduction of 3D Spectral Data, Obtained with the 6-meter Telescope

1995 ◽  
Vol 149 ◽  
pp. 308-310
Author(s):  
V. V. Vlasiouk
Keyword(s):  
Spectral Data ◽  
Spectral Methods ◽  
Data Reduction ◽  
Simultaneous Detection ◽  
Personal Computers ◽  
Specialized Software ◽  
Fabry Perot ◽  
Extended Sources ◽  
Integral Field Spectrograph ◽  
Integral Field

Development of 3D spectral methods on the 6-meter telescope prompted the necessity of creating specialized software for data reduction, adapted to personal computers IBM AT/386/486 class. We had to concentrate our efforts on preparing the software for bidimensional spectral data produced by Multi-Pupil Integral Field Spectrograph of the 6-meter telescope (MPFS) and analog of panoramic spectrophotometer with spectral channeling, using scanning Fabry-Perot interferometer (PYTHEAS-6).MPFS - analog of spectrograph TIGER (Courtes et al., 1988), developed for the 6-meter telescope, provides bidimensional spectroscopy of extended sources, allowing the simultaneous detection of 99 individual spectra, produced by a lens raster from 9 by 11 microlenses. The main features of this instrument are described in (Afanasiev et al, 1994).

scholarly journals Star-forming regions in the intragroup medium of compact groups of galaxies

2009 ◽  
Vol 5 (S262) ◽  
pp. 440-441
Author(s):  
S. Torres-Flores ◽  
C. Mendes de Oliveira ◽  
D. F. de Mello ◽  
P. Amram ◽  
H. Plana ◽  
...  
Keyword(s):  
Star Formation ◽  
Dwarf Galaxy ◽  
Early Stage ◽  
Velocity Fields ◽  
Compact Groups ◽  
Advanced Stage ◽  
Groups Of Galaxies ◽  
Star Forming ◽  
Star Forming Regions ◽  
Fabry Perot

AbstractWe present the results of a multiwavelength campaign searching for young objects in the intragroup medium of seven compact groups of galaxies: HCG 2, 7, 22, 23, 92, 100 and NGC 92. We used Fabry-Perot velocity fields and rotation curves together with GALEX NUV and FUV images, optical R-band and HI maps to evaluate the stage of interaction of each group. We conclude that groups (i) HCG 7 and HCG 23 are in an early stage of interaction, (ii) HCG 2 and HCG 22 are mildly interacting, and (iii) HCG 92, HCG 100 and NGC 92 are in a late stage of evolution. Evolved groups have a population of young objects in their intragroup medium while no such population is found within the less evolved groups. We also report the discovery of a tidal dwarf galaxy candidate in the tail of NGC 92. These three groups, besides containing galaxies which have peculiar velocity fields, also show extended HI tails. Our results indicate that the advanced stage of evolution of a group together with the presence of intragroup HI clouds may lead to star formation in the intragroup medium.

Adaptive optics pipeline data reduction: application to spectroimaging with Fabry-Perot

1997 ◽  
Author(s):  
Nicolas Devillard ◽  
Christian Drouet D'Aubigny ◽  
Patrice Corporon
Keyword(s):  
Adaptive Optics ◽  
Data Reduction ◽  
Fabry Perot

scholarly journals A guide to TAURUS-2 Fabry-Perot data reduction

2000 ◽  
Vol 315 (2) ◽  
pp. 248-262 ◽  
Author(s):  
S. Gordon ◽  
B. Koribalski ◽  
S. Houghton ◽  
K. Jones
Keyword(s):  
Data Reduction ◽  
Fabry Perot

scholarly journals Spectroscopic Variability in Late-Type Dwarfs Using High S:N Spectra

1988 ◽  
Vol 132 ◽  
pp. 287-289
Author(s):  
B. H. Foing ◽  
J. E. Beckman ◽  
G. Vladilo
Keyword(s):  
High Resolution ◽  
Surface Activity ◽  
Resonance Line ◽  
Velocity Fields ◽  
Doppler Imaging ◽  
Late Type ◽  
3 Dimensional ◽  
Spectral Signatures ◽  
Activity Cycles

Monitoring of active late-type dwarfs, spectroscopically with high resolution (λ/Δλ ∼ 105) and high S:N (>300) round their activity cycles, principally in the Call H resonance line, offers techniques to explore (a) plage filling factors (b) 3-dimensional chromospheric velocity fields (c) maps of surface activity via “Doppler Imaging”. In this paper we deal with the use of spectral signatures to derive plage cover.

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