DEEP FABRY-PEROT Hα OBSERVATIONS OF NGC 7793: A VERY EXTENDED Hα DISK AND A TRULY DECLINING ROTATION CURVE

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.

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HI and Hα Mapping of M31 & M33

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311022599 ◽

2010 ◽

Vol 6 (S277) ◽

pp. 116-120

Author(s):

Z. S. Kam ◽

C. Carignan ◽

L. Chemin ◽

O. Hernandez ◽

M. de Denus-Baillargeon ◽

...

Keyword(s):

High Resolution ◽

Rotation Curve ◽

Local Group ◽

Low Resolution ◽

Rotation Curves ◽

Fabry Perot ◽

Central Regions ◽

Kinematical Parameters ◽

Kinematical Data

RésuméWe performed a deep Hi and Hα mapping of M31 and M33 in order to get accurate kinematical data of those two galaxies and also to make a comparison between the Hi and Hα kinematics. The Hi data were obtained with the DRAO interferometer and the Hα data with the Fabry-Perot system of the Observatoire du mont Mégantic using an EMCCD as a detector. These data will give us the best possible datasets to derive accurate rotation curves and mass models for those two Local Group spirals and provide some new data for the Hii regions studies of these galaxies. While the Hi observations are of low resolution (~1 arcmin), the high resolution of the Hα data (~1 arcsec) should allow us to get much more details in the central regions, allowing at the same time a much better determination of the kinematical parameters. Hence, the inner part of the rotation curve, so inportant to constraint properly the mass models, will be determined more accurately.

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Hα kinematics of nearby galaxies using Fabry-Perot and IFU data

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316009443 ◽

2016 ◽

Vol 11 (S321) ◽

pp. 275-275

Author(s):

Santiago Erroz-Ferrer ◽

Keyword(s):

Spectral Resolution ◽

Total Mass ◽

Rotation Curve ◽

Spiral Galaxies ◽

Rotation Curves ◽

Large Sample ◽

Mass Distributions ◽

Fabry Perot ◽

Nearby Galaxies

AbstractI present here analysis of the shapes of the rotation curves of a large sample of nearby spiral galaxies with high angular and spectral resolution Hα (Fabry-Perot GHαFaS) kinematics, and the resulting constraints on their total mass distributions. In particular I discuss how their rotation curve shapes relate to key galaxy properties. Finally I present related results from the MUSE Atlas of Disks (MAD) program, which is dissecting the nearby disk population with IFU spectroscopy at ~100pc resolution.

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Dark Matter Distribution in Nearby Galaxies

Symposium - International Astronomical Union ◽

10.1017/s0074180900183548 ◽

2004 ◽

Vol 220 ◽

pp. 327-328

Author(s):

Olivia Garrido ◽

Philippe Amram ◽

Claude Carignan ◽

Sébastien Blais-Ouellette ◽

Michel Marcelin ◽

...

Keyword(s):

Dark Matter ◽

High Resolution ◽

Mass Distribution ◽

Rotation Curve ◽

Velocity Fields ◽

Constant Density ◽

Matter Distribution ◽

Fabry Perot ◽

Nearby Galaxies ◽

Dark Matter Distribution

We present results obtained from a study of the mass distribution of 24 galaxies observed using Fabry-Pérot techniques, as part of the GHASP survey (see Russeil et al., this meeting). For each galaxy, we combined high resolution Hα rotation curves derived from 2-D velocity fields, with low resolution HI data, in order to determine accurately the inner slope of the rotation curve which strongly constrains the distribution of matter. Our work suggests the existence of a constant density core in the center of the dark halos.

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Hα KINEMATICS OF THE ISOLATED INTERACTING GALAXY PAIR KPG 486 (NGC 6090)

Revista Mexicana de Astronomía y Astrofísica ◽

10.22201/ia.01851101p.2020.56.01.09 ◽

2020 ◽

Vol 56 (1) ◽

pp. 71-83

Author(s):

M. M. Sardaneta ◽

M. Rosado ◽

M. Sánchez-Cruces

Keyword(s):

Velocity Field ◽

Emission Line ◽

Kinematic Analysis ◽

Rotation Curve ◽

Dynamic Behaviour ◽

Hydrogen Gas ◽

Kinematic Parameters ◽

Optical Images ◽

Fabry Perot ◽

Hα Emission

In optical images, the barely studied isolated interacting galaxy pair KPG 486 (NGC 6090) displays similar features to the Antennae (NGC 4038/39) galaxy pair. To compare the distribution of ionized hydrogen gas, morphology and kinematic and dynamic behaviour of both galaxy pairs, we present observations in the Hα emission line of NGC 6090 acquired with the scanning Fabry-Perot interferometer, PUMA. For each galaxy in NGC 6090 we obtained several kinematic parameters, its velocity field and its rotation curve. We also analysed some of the perturbations induced by their encounter. We verified the consistency of our results by comparing them with kinematic results from the literature. The comparison of our results on NGC 6090 with those obtained in a previous similar kinematic analysis of the Antennae highlighted great differences between these galaxy pairs.

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KPG 390: A pair of trailing spirals.

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311017534 ◽

2010 ◽

Vol 6 (S271) ◽

pp. 127-134

Author(s):

P. Repetto ◽

M. Rosado ◽

R. Gabbasov ◽

I. Fuentes-Carrera

Keyword(s):

Dark Matter ◽

Surface Brightness ◽

Rotation Curve ◽

Velocity Fields ◽

Minor Axis ◽

The Other ◽

Kinematic Parameters ◽

First Case ◽

Fabry Perot ◽

Different Types

AbstractIn this study we present scanning Fabry-Perot Hα observations of the isolated interacting galaxy pair NGC 5278/79. We derived velocity fields, various kinematic parameters and rotation curves for both galaxies. These kinematical results together with the fact that dust lanes have been detected in both galaxies, as well as the analysis of surface brightness profiles along the minor axis, allowed us to determine univocally that both components of the interacting pair are trailing spirals. We have also estimated the mass of NGC 5278 fitting its rotation curve with a disk-halo component. We have tested three different types of halo (pseudo-isothermal, Hernquist and Navarro Frenk White) and we have obtained that the rotation curve can be fitted either with a pseudo-isothermal, an Hernquist halo or a Navarro Frenk White halo component, although in the first case the amount of dark matter required is about ten times smaller than for the other two halo distributions.

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2D kinematics of the edge-on spiral galaxy ESO 379-006

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313004894 ◽

2012 ◽

Vol 8 (S295) ◽

pp. 234-235

Author(s):

M. Rosado ◽

R. F. Gabbasov ◽

P. Repetto ◽

I. Fuentes-Carrera ◽

P. Amram ◽

...

Keyword(s):

Velocity Field ◽

Radial Velocity ◽

Rotation Curve ◽

Minor Axis ◽

Ionized Gas ◽

Diffuse Ionized Gas ◽

Fabry Perot ◽

The Galaxy ◽

Rotation Motion

AbstractWe present a kinematical study of the marginally edge-on galaxy ESO 379-006. With Fabry-Perot spectroscopy at Hα we obtain velocity maps, the radial velocity field, and position-velocity diagrams parallel to the major and to the minor axis of the galaxy. We build the rotation curve of the galaxy and discuss the role of projection effects. The twisting of isovelocities in the radial velocity field of the disk of ESO 379-006 as well as a kinematical asymmetry found in the position-velocity diagrams parallel to the minor axis suggest the existence of non-circular motions that can be modeled by including a radial inflow besides the rotation motion. Extraplanar Diffuse Ionized gas was detected in this galaxy both from the images and from its kinematics. It is possible that the diffuse gas is lagging in rotation.

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