Revisiting the innermost kinematics of M31 galaxy with the OMM Fabry-Perot interferometer

2019 ◽  
Vol 14 (S353) ◽  
pp. 130-133
Author(s):  
Sié Zacharie Kam ◽  
Claude Carignan ◽  
Michel Marcelin ◽  
Philippe Amram ◽  
Jean Koulidiati
Keyword(s):  
Rotation Curve ◽  
Narrow Band ◽  
Optical Emission ◽  
Emission Lines ◽  
Interference Filters ◽  
Andromeda Galaxy ◽  
Fabry Perot ◽  
The Galaxy ◽  
Data Points ◽  
Made In

AbstractWe present observations on optical emission lines acquired with the scanning Fabry-Perot interferometer of the observatoire du Mont Mégantic, of the Andromeda galaxy (M31). A 765 order Fabry-Perot were used with a fast readout EM-CCD. From data obtained, kinematic maps and data points for the rotation curve of the innermost part of the galaxy are derived. Several dozen of regions have been scanned with the Fabry-Perot interferometer and narrow band interference filters. The central 10’x10’ were scanned with five different filters. Observations have been made in order to get better Hα data for kinematics purposes.

scholarly journals The Wisconsin Hα Mapper (WHAM): A Brief Review of Performance Characteristics and Early Scientific Results

1998 ◽  
Vol 15 (1) ◽  
pp. 14-18 ◽  
Author(s):  
R. J. Reynolds ◽  
S. L. Tufte ◽  
L. M. Haffner ◽  
K. Jaehnig ◽  
J. W. Percival
Keyword(s):  
High Velocity ◽  
Optical Emission ◽  
Emission Lines ◽  
Spectral Window ◽  
Sky Surveys ◽  
Early Results ◽  
Fabry Perot ◽  
The Galaxy ◽  
High Velocity Clouds ◽  
Scientific Results

Abstract. The Wisconsin Hα Mapper (WHAM) is a recently completed facility for the detection and study of faint optical emission lines from diffuse ionised gas in the disk and halo of the Galaxy. WHAM consists of a 15 cm diameter Fabry–Perot spectrometer coupled to a 0·6 m ‘telescope’, which provide a 1° diameter beam on the sky and produce a 12 km s−1 resolution spectrum within a 200 km s−1 spectral window. This facility is now located at Kitt Peak in Arizona and operated remotely from Madison, Wisconsin, 2400 km distant. Early results include a velocity-resolved Hα map of a 70° × 100° region of the sky near the Galactic anticentre, the first detections of Hα emission from the M I and A high velocity clouds, and the first detections of [O I] λ6300 and other faint ‘diagnostic’ lines from the warm ionised medium. Through the summer of 1998, WHAM will be devoted almost exclusively to a survey of the northern sky, which will provide maps of the distribution and kinematics of the diffuse HII through the optical Hα line in a manner that is analogous to earlier sky surveys of the HI made through the 21 cm line.

scholarly journals The rotation curve, mass, light, and velocity distribution of M31

1970 ◽  
Vol 38 ◽  
pp. 51-60
Author(s):  
J. Einasto ◽  
U. Rümmel
Keyword(s):  
Spectroscopic Data ◽  
Total Mass ◽  
Rotation Curve ◽  
Mass Density ◽  
Major Axis ◽  
Deviation Angle ◽  
Andromeda Galaxy ◽  
The Galaxy ◽  
M 31 ◽  
Central Concentration

A model for the Andromeda galaxy, M 31, has been derived from the available radio, photometric, and spectroscopic data. The model consists of four components – the nucleus, the bulge, the disc, and the flat component.For all components the following functions have been found: the mass density; the mass-to-light ratio; the velocity dispersions in three perpendicular directions (for the plane of symmetry and the axis of the galaxy); the deviation angle of the major axis of the velocity ellipsoid from the plane of symmetry; the centroid velocity (for the plane of symmetry).Our model differs in two points from the models obtained by other authors: the central concentration of mass is higher (in the nucleus the mass-to-light ratio is about 170), and the total mass of the galaxy (200 × 109 solar masses) is smaller. The differences can be explained by different rotation curves adopted, and by attributing more weight to photometric and spectroscopic data in the case of our model.

scholarly journals Longslit spectroscopy of the peculiar Seyfert 2 galaxy HRG 10103

2010 ◽  
Vol 6 ◽  
pp. 11-16
Author(s):  
Paulo C.R. Poppe ◽  
Vera A.F. Martin ◽  
Max Faúndez-Abans ◽  
Mariângela De Oliveira-Abans ◽  
Iranderly F. De Fernandes
Keyword(s):  
Spectroscopic Data ◽  
Rotation Curve ◽  
Abundance Ratio ◽  
Emission Lines ◽  
Physical Parameters ◽  
Narrow Line ◽  
Optical Range ◽  
Peculiar Galaxy ◽  
The Galaxy ◽  
The Continuum

We present the rst optical longslit spectroscopy for the galaxy HRG 10103, an Sa(r) type peculiar galaxy seen face-on with an asymmetrical elliptical structure. The main goal of this work is to provide the spectral classication of the current object using the `traditional' diagnostic diagrams. However, we also present a diagnostic involving the known emission line ratio R23, usually used to estimate the O/H abundance ratio. The idea is to make a better distinction between the narrow-line AGNs and the H II galaxies. The spectra were obtained in two observatories (OPD-LNA/MCT and Gemini-South) and includes some of the most important emission lines for ionization diagnostic. Based on the observed spectra, HRG 10103 is a Seyfert 2 galaxy with typical line-ratios values in the optical range. We have estimated nuclear redshift of z = 0.039. The resulting reddening values as a function of distance from the nucleus are presented too. The errors in the  fluxes were mostly caused by uncertainties in the placement of the continuum level. The rotation curve is typical of spiral disks, rising shallowly and  attening at an observed amplitude of about 200 km s^(-1). Some other physical parameters have been derived whenever possible. The spectroscopic data reduction was carried out using the GEMINI.GMOS package as well as the standard IRAF procedures.

scholarly journals Kinematics of Supernova Remnants in the Galaxy and LMC

1983 ◽  
Vol 101 ◽  
pp. 295-298
Author(s):  
Peter Shull
Keyword(s):  
Supernova Remnants ◽  
Spectral Feature ◽  
Optical Emission ◽  
Emission Lines ◽  
Cygnus Loop ◽  
Interstellar Media ◽  
The Galaxy ◽  
Very High

The optical emission lines of six SNRs have been observed at very high angular and kinematic resolutions. Kinematic ion temperatures were derived, and evidence was found in shocked regions for Maxwellian microturbulence on scales ≤ 0.01 pc, and for non-Maxwellian macroturbulence on scales > 0.1 pc. The widths of shocked regions in the Cygnus Loop and the existence of three types of spectral feature in the LMC remnants are discussed in terms of SNR evolution in cloudy interstellar media.

scholarly journals CO in NGC 5055

1987 ◽  
Vol 115 ◽  
pp. 659-660
Author(s):  
L.E.B. Johansson ◽  
R. S. Booth
Keyword(s):  
Velocity Field ◽  
Radial Distribution ◽  
Rotation Curve ◽  
A Priori ◽  
Optical Emission ◽  
Major Axis ◽  
Rotation Curves ◽  
Fitting Procedure ◽  
The Galaxy ◽  
Co Emission

The flocculent spiral galaxy NGC 5055 has been mapped along the major axis in the 12CO (J = 1-0) line using the Onsala 20-m telescope (HPBW = 33″). Figure 1, which gives the spatial velocity diagram of CO emission on the major axis with observed Hα velocities (Kruit and Bosma, 1978) superimposed, seems to imply higher velocities of the regions responsible for the optical emission. Taking into account the cruder spatial resolution of the CO observations, this effect is expected in a region where the rotation curve rises rapidly provided that the CO emission increases toward the centre. Figure 2 shows the rotation velocities for the eastern and western parts of the galaxy separately, as observed in Hα and CO. For CO we only give the portion of the rotation curve which is accurately determined, i.e. where it is relatively flat. The CO velocities in this region agree closely with those observed in HI (Bosma, 1978). These data suggest a difference of 10-20 km s−1 between the Hα and CO velocities at a distance of ∼ 60″ from the centre. The radial distribution of the CO emission, also indicated in Fig. 2, is defined by an iterative fitting procedure to the observed line profiles (see Scoville et al. 1983). This procedure requests an a priori knowledge of the velocity field, here assumed to be defined by the Hα data inside a radius of 60″. However, the shapes of the observed spectra and “best fit” model profiles differ significantly in some cases, again indicating that the Hα velocities do not apply to the molecular gas. The derived radial distribution of the CO emission is dependent on the assumed velocity field; however, the gross characteristics are retained for more feasible rotation curves (i.e. rotation curves giving better fits to the observed profiles).

Very Narrow Band Interference Filters

1967 ◽  
Vol 1 (2) ◽  
pp. 66-66 ◽  
Author(s):  
J. V. Ramsay
Keyword(s):  
Narrow Band ◽  
Raw Materials ◽  
Solar Physics ◽  
The Other ◽  
Interference Filters ◽  
Limited Availability ◽  
Fabry Perot ◽  
Alternative Type

In solar physics a need exists for filters which have very narrow passbands, ~0.01 nm or less. While Lyot-Öhman birefringent filters have been used particularly for investigations at the Hα line, the limited availability of the raw materials, especially calcite, have usually restricted these filters to passbands of ~ 0.025 nm or more. A possible alternative type of filter consists of a number of Fabry-Perot interferometers mounted one behind the other.

scholarly journals 3.15. Narrow-band imaging of the nuclear region of the Seyfert galaxy NGC1068

1998 ◽  
Vol 184 ◽  
pp. 119-120
Author(s):  
T. Ishigaki ◽  
H. Ohtani ◽  
T. Hayashi ◽  
S. Ozaki ◽  
T. Hattori ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
Narrow Band ◽  
Narrow Band Imaging ◽  
Seyfert Galaxy ◽  
Tunable Filter ◽  
Nuclear Region ◽  
Fabry Perot ◽  
Imaging Observation ◽  
Made In

A narrow-band imaging observation of the Seyfert galaxy NGC1068 was made in the Fabry-Perot mode of the Kyoto 3D Spectrograph attached to the 188cm telescope of the Okayama Astrophysical Observatory. We observed at wavelengths of Hα, [S ii]λ6716, [S ii]λ6731 and adjacent continua of the respective lines with a “tunable filter”, i.e. a gap-scanning etalon with a spectral resolution of 20 Å.

scholarly journals Observations of Comet Kohoutek (1973f) with a Ground-Based Fabry-Perot Spectrometer

1976 ◽  
Vol 25 (Part1) ◽  
pp. 214-219
Author(s):  
D. Huppler ◽  
R. J. Reynolds ◽  
F.L. Roesler ◽  
F Scherb ◽  
J. Trauger
Keyword(s):  
Relative Velocity ◽  
Optical Emission ◽  
Emission Lines ◽  
Resolving Power ◽  
Line Profiles ◽  
National Observatory ◽  
Fabry Perot ◽  
Airglow Emissions ◽  
Effective Temperatures ◽  
Gas Cloud

Between 1973 December 1 and 1974 February 2, optical emission lines from the gas cloud surrounding comet Kohoutek were observed using a double Fabry-Perot etalon spectrometer at Kitt Peak National Observatory. The spectrometer had a resolving power of 40,000, corresponding to a velocity resolution of about 7.5 km sec-1. With this resolution it was possible to use the cometearth relative velocity to resolve faint cometary Hα λ6563, [01] λ6300 and other emission lines from geocoronal and airglow emissions and to study the cometary line profiles in order to obtain information about the composition, effective temperatures, outflow velocities, and production rates of atoms and ions in the cometary envelope.

scholarly journals Gas and Stellar Kinematics in the Disk and Bar of Mrk 573

1996 ◽  
Vol 157 ◽  
pp. 218-220 ◽  
Author(s):  
V. L. Afanasiev ◽  
A. N. Burenkov ◽  
A. I. Shapovalova ◽  
V. V. Vlasyuk
Keyword(s):  
Velocity Field ◽  
Complex Structure ◽  
Seyfert Galaxy ◽  
Helical Structure ◽  
Emission Lines ◽  
Stellar Kinematics ◽  
Gas Distribution ◽  
Fabry Perot ◽  
The Galaxy ◽  
Galaxy Center

AbstractResults of 3D-spectroscopy for the nearby Seyfert galaxy Mrk 573 obtained at the 6-m telescope with the scanning Fabry-Perot interferometer and the Multi-Pupil Field Spectrograph (MPFS) are presented. Emission lines images of the galaxy center demonstrate a complex structure of ENLR, coinciding with the radio data. An analysis of the velocity field shows that some gas structures do not lie in the plane of the galaxy. An explanation of the observed velocity field and gas distribution by radiation of a helical structure located inside an ionization cone is proposed.

scholarly journals A 2μm narrow-band survey for emission-line stars in the inner Galaxy

1999 ◽  
Vol 193 ◽  
pp. 472-473
Author(s):  
Robert D. Blum ◽  
Augusto Damineli
Keyword(s):  
Emission Line ◽  
Near Infrared ◽  
Narrow Band ◽  
Emission Lines ◽  
Evolved Stars ◽  
The Galaxy ◽  
Band Survey

We have begun a search for emission-line stars toward the inner Galaxy using narrow-band photometry centered on the emission lines of He I 2.06μm, C IV 2.08μm, H I Brγ 2.166μm and He II 2.189μm. The census of Wolf-Rayet and other emission-line stars in the Galaxy is incomplete, owing to the large extinction at optical and shorter wavelengths toward the inner Galaxy. However, these massive, evolved stars are bright and can be detected at large distances in the near infrared.

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