scholarly journals Outflows in the Seyfert 2 galaxy NGC 5643 traced by the [S iii] emission

2018 ◽  
Vol 35 ◽  
Author(s):  
Rogemar A. Riffel ◽  
C. Hekatelyne ◽  
Izabel C. Freitas
Keyword(s):  
Emission Line ◽  
Flux Distribution ◽  
Major Axis ◽  
Position Angle ◽  
Stellar Kinematics ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Outflow Rate ◽  
Field Unit ◽  
East West

AbstractWe use Gemini Multi-Object Spectrograph integral Field Unit observations of the inner 285 × 400 pc2 region of the Seyfert 2 galaxy NGC 5643 to map the [S iii]λ9069 emission line flux distribution and kinematics, as well as the stellar kinematics, derived by fitting the Ca iiλλλ8498,8542,8662 triplet, at a spatial resolution of 45 pc. The stellar velocity field shows regular rotation, with a projected velocity of 100 km s−1 and kinematic major axis along a position angle of –36°. A ring of low stellar velocity dispersion values (∼70 km s−1), attributed to young/intermediate age stellar populations, is seen surrounding the nucleus with a radius of 50 pc. We found that the [S iii] flux distribution shows an elongated structure along the east–west direction and its kinematics is dominated by outflows within a bi-cone at an ionised gas outflow rate of 0.3 M⊙ yr−1. In addition, velocity slices across the [S iii]λ9069 emission line reveal a kinematic component attributed to rotation of gas in the plane of the galaxy.

scholarly journals Outflows, inflows, and young stars in the inner 200 pc of the Seyfert galaxy NGC 2110

2019 ◽  
Vol 487 (3) ◽  
pp. 3958-3970 ◽  
Author(s):  
Marlon R Diniz ◽  
Rogemar A Riffel ◽  
Thaisa Storchi-Bergmann ◽  
Rogério Riffel
Keyword(s):  
Emission Line ◽  
Stellar Population ◽  
Dust Emission ◽  
Seyfert Galaxy ◽  
Bolometric Luminosity ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Outflow Rate ◽  
Mass Outflow ◽  
Integral Field Spectrograph

ABSTRACT We present a 2D mapping of stellar population age components, emission-line fluxes, gas excitation, and kinematics within the inner ∼200 pc of the Seyfert 2 galaxy NGC 2110. We used the Gemini North Integral Field Spectrograph (NIFS) in the J and K bands at a spatial resolution of ∼22  pc. The unresolved nuclear continuum is originated in combined contributions of young stellar population (SP; age ≤ 100  Myr), a featureless AGN continuum and hot dust emission. The young-intermediate SP (100 < age ≤ 700 Myr) is distributed in a ring-shaped structure at ≈140  pc from the nucleus, which is roughly coincident with the lowest values of the stellar velocity dispersion. In the inner ≈115  pc the old SP (age > 2 Gyr) is dominant. The [Fe ii] $\lambda \, 1.2570\, \mu$m emission-line flux distribution is correlated with the radio emission and its kinematics comprise two components, one from gas rotating in the galaxy plane and another from gas in outflow within a bicone-oriented along north–south. These outflows seem to originate in the interaction of the radio jet with the ambient gas producing shocks that are the main excitation mechanism of the [Fe ii] emission. We estimate: (1) an ionized gas mass outflow rate of ∼0.5  M⊙ yr−1 at ∼70 pc from the nucleus; and (2) a kinetic power for the outflow of only 0.05 per cent of the AGN bolometric luminosity implying weak feedback effect on the galaxy.

scholarly journals Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20

2019 ◽  
Vol 489 (3) ◽  
pp. 4111-4124 ◽  
Author(s):  
Pamela Soto-Pinto ◽  
Neil M Nagar ◽  
Carolina Finlez ◽  
Venkatessh Ramakrishnan ◽  
Dania Muñoz-Vergara ◽  
...  
Keyword(s):  
Major Axis ◽  
Position Angle ◽  
Emission Lines ◽  
Opening Angle ◽  
Stellar Kinematics ◽  
Velocity Amplitude ◽  
Gas Kinematics ◽  
Dispersion Component ◽  
Radiative Power ◽  
Field Unit

ABSTRACT We present two-dimensional ionized gas and stellar kinematics in the inner 1.4 × 1.9 kpc2 of the Seyfert 2 galaxy ESO 153-G20 obtained with the Gemini-South/Gemini multi-object spectrograph integral field unit (GMOS-IFU) at a spatial resolution of ~250 pc and spectral resolution of 36 km s−1. Strong [O iii], Hα, [N ii] and [S ii] emission lines are detected over the entire field of view. The stellar kinematics trace circular rotation with a projected velocity amplitude of ±96 km s−1, a kinematic major axis in position angle of 11°, and an average velocity dispersion of 123 km s−1. To analyse the gas kinematics, we used aperture spectra, position–velocity diagrams and single/double Gaussian fits to the emission lines. All lines show two clear kinematic components: a rotating component that follows the stellar kinematics, and a larger-dispersion component, close to the systemic velocity (from which most of the [O iii] emission comes), mainly detected to the south-west. We interpret this second component as gas outflowing at ∼400 km s−1 in a compact (300 pc) ionization cone with a half-opening angle ≤40°. The counter-cone is probably obscured behind a dust lane. We estimate a mass outflow rate of 1.1 M$\odot$ yr−1, 200 times larger than the estimated accretion rate on to the supermassive black hole, and a kinetic to radiative power ratio of 1.7 × 10−3. Bar-induced perturbations probably explain the remaining disturbances observed in the velocity field of the rotating gas component.

scholarly journals The Orientation of Galaxies in Superclusters

1988 ◽  
Vol 130 ◽  
pp. 239-241
Author(s):  
Piotr Flin
Keyword(s):  
Positive Result ◽  
Spatial Orientation ◽  
Axial Ratio ◽  
Major Axis ◽  
Position Angle ◽  
Main Plane ◽  
Local Supercluster ◽  
The Galaxy ◽  
Spatial Geometry

The alignment of galaxies with the main plane of supercluster can contribute to recovering information on the structure origin. The positive result of the preliminary search for galaxy alignment in the Local Supercluster /Flin and Godlowski 1986, hereafter FG/ have stimulated further studies. Following Jaaniste and Saar /1977/, the both parameters, the position angle of the galaxy major axis p and the axial ratio b/a of the galaxy image, were used for the better determination of the actual spatial orientation of the galaxy disc. This approach also permit to consider “face-on” objects, whose discounting leads to obvious incompleteness of the analysed data. Each galaxy has two possible orientations and both were taken into account during calculations. The analysis is perfomed by transforming position angle p and coordinates α, δ of galaxies expressed in the equatorial coordinates into coordinate system connected with each parent supercluster separately, which gives parameters P, l and b respectively. The main supercluster plane should be determined, which resticts the present study to the three superclusters with a known spatial geometry, i.e. LSC /Tully 1982/, Perseus and Coma/A1367 /Chincarini et al. 1983/.

scholarly journals Discovery of an edge-on galaxy with X-shaped bi-cone – SDSS J171359.00+333625.5

2019 ◽  
Vol 490 (3) ◽  
pp. 3830-3839 ◽  
Author(s):  
Min Bao ◽  
Yan-mei Chen ◽  
Qi-rong Yuan ◽  
Yong Shi ◽  
Dmitry Bizyaev ◽  
...  
Keyword(s):  
Velocity Dispersion ◽  
Rotation Velocity ◽  
Major Axis ◽  
Joint Effect ◽  
Galactic Winds ◽  
The Galaxy ◽  
Disc Rotation ◽  
Nearby Galaxies ◽  
Field Unit ◽  
Gas Accretion

ABSTRACT Using the integral field unit (IFU) data from Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, we study the kinematics of gas and stellar components in an edge-on Seyfert 2 galaxy, SDSS J171359.00+333625.5, with X-shaped bi-conical outflows. The gas and stars therein are found to be counter-rotating, indicating that the collision between the inner and external gas might be an effective way to dissipate the angular momentum, which leads to remarkable gas accretion into the galaxy centre. Large [O iii]λ5007 equivalent width and AGN-like line ratio in the large bi-conical region suggest that the gas is ionized by the central AGN. The gas velocity in the bi-cone region shows that ionized gas is receding relative to the galaxy centre, which could be the joint effect of inflows, outflows, and disc rotation. We are probably witnessing the case where a great amount of gas in the disc is being efficiently accreted into the central black hole, and the AGN-driven galactic winds are blown out along the bi-cone. The kinematics of oxygen, including rotation velocity and velocity dispersion, is different from other elements, like hydrogen, nitrogen, and sulphur. The rotation velocity estimated from oxygen is slower than from other elements. The velocity dispersion of other elements follows galactic gravitational potential, while the velocity dispersion of oxygen stays roughly constant along the galactic major-axis. The further advanced observations, e.g. of cold gas or with an IFU of higher spatial resolution, are required to better understand this object.

scholarly journals A Possible Evolutionary Scenario for NGC 7217

1996 ◽  
Vol 171 ◽  
pp. 339-339 ◽  
Author(s):  
E. Athanassoula ◽  
A. Bosma ◽  
B. Guivarch ◽  
L. Verdes-Montenegro
Keyword(s):  
Spiral Galaxy ◽  
Major Axis ◽  
Position Angle ◽  
Minor Axis ◽  
Outer Ring ◽  
Stellar Kinematics ◽  
Evolutionary Scenario ◽  
Nuclear Ring ◽  
Oval Distortion

NGC 7217 is an ordinary spiral galaxy with three rings whose size ratios are such that they can be associated with resonances, as for barred spirals. From 21-cm HI line data and BVRI CCD-images of this galaxy we find (cf. Verdes-Montenegro et al. 1995) : 1) a nuclear ring strong in Hα, 2) an inner ring seen clearly in a B - I colour map, and 3) an outer ring, with blue colours and strong HI-emission. After deprojection the disk has a mean ellipticity of 0.04 ± 0.01, while the position angle of the deprojected galaxy changes suddenly at 65″ radius, where the minor axis becomes major axis. Thus a very mild oval distortion could exist, with the outer ring perpendicular to the oval. Merrifield and Kuijken (1994) find from the stellar kinematics that about 20 – 30 % of the stars are in retrograde orbits.

scholarly journals The Fornax Deep Survey with the VST

2019 ◽  
Vol 623 ◽  
pp. A1 ◽  
Author(s):  
E. Iodice ◽  
M. Spavone ◽  
M. Capaccioli ◽  
R. F. Peletier ◽  
G. van de Ven ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Surface Brightness ◽  
Major Axis ◽  
Position Angle ◽  
Early Type ◽  
Semi Major Axis ◽  
Cluster Galaxies ◽  
The Galaxy ◽  
Deep Survey ◽  
Fornax Cluster

Context. This paper is based on the multi-band (ugri) Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We study bright early-type galaxies (mB ≤ 15 mag) in the 9 square degrees around the core of the Fornax cluster, which covers the virial radius (Rvir  ∼ 0.7 Mpc). Aims. The main goal of the present work is to provide an analysis of the light distribution for all galaxies out to unprecedented limits (in radius and surface brightness) and to release the main products resulting from this analysis in all FDS bands. We give an initial comprehensive view of the galaxy structure and evolution as a function of the cluster environment. Methods. From the isophote fit, we derived the azimuthally averaged surface brightness profiles, the position angle, and ellipticity profiles as a function of the semi-major axis. In each band, we derived the total magnitudes, effective radii, integrated colours, and stellar mass-to-light ratios. Results. The long integration times, the arcsec-level angular resolution of OmegaCam at VST, and the large covered area of FDS allow us to map the light and colour distributions out to large galactocentric distances (up to about 10−15 Re) and surface brightness levels beyond μr = 27 mag arcsec−2 (μB ≥ 28 mag arcsec−2). Therefore, the new FDS data allow us to explore in great detail the morphology and structure of cluster galaxies out to the region of the stellar halo. The analysis presented in this paper allows us to study how the structure of galaxies and the stellar population content vary with the distance from the cluster centre. In addition to the intra-cluster features detected in previous FDS works, we found a new faint filament between FCC 143 and FCC 147, suggesting an ongoing interaction. Conclusions. The observations suggest that the Fornax cluster is not completely relaxed inside the virial radius. The bulk of the gravitational interactions between galaxies happens in the W-NW core region of the cluster, where most of the bright early-type galaxies are located and where the intra-cluster baryons (diffuse light and globular clusters) are found. We suggest that the W-NW sub-clump of galaxies results from an infalling group onto the cluster, which has modified the structure of the galaxy outskirts (making asymmetric stellar halos) and has produced the intra-cluster baryons (ICL and GCs), concentrated in this region of the cluster.

scholarly journals MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

2019 ◽  
Vol 490 (3) ◽  
pp. 4368-4381 ◽  
Author(s):  
Ilane Schroetter ◽  
Nicolas F Bouché ◽  
Johannes Zabl ◽  
Thierry Contini ◽  
Martin Wendt ◽  
...  
Keyword(s):  
Gas Flow ◽  
Formation Rate ◽  
Azimuthal Angle ◽  
Major Axis ◽  
Geometrical Model ◽  
Mass Rate ◽  
The Galaxy ◽  
Field Unit ◽  
Halo Gas ◽  
Stellar Masses

ABSTRACT We present results from our on-going MusE GAs FLOw and Wind (MEGAFLOW) survey, which consists of 22 quasar lines of sight, each observed with the integral field unit MUSE and the UVES spectrograph at the ESO Very Large Telescopes (VLT). The goals of this survey are to study the properties of the circumgalactic medium around z ∼ 1 star-forming galaxies. The absorption-line selected survey consists of 79 strong Mg ii absorbers (with rest-frame equivalent width ≳0.3 Å) and, currently, 86 associated galaxies within 100 projected kpc of the quasar with stellar masses (M⋆) from 109 to 1011 M⊙. We find that the cool halo gas traced by Mg ii is not isotropically distributed around these galaxies from the strong bi-modal distribution in the azimuthal angle of the apparent location of the quasar with respect to the galaxy major axis. This supports a scenario in which outflows are bi-conical in nature and co-exist with a co-planar gaseous structure extending at least up to 60–80 kpc. Assuming that absorbers near the minor axis probe outflows, the current MEGAFLOW sample allowed us to select 26 galaxy–quasar pairs suitable for studying winds. From this sample, using a simple geometrical model, we find that the outflow velocity only exceeds the escape velocity when M⋆ ≲ 4 × 109 M⊙, implying the cool material is likely to fall back except in the smallest haloes. Finally, we find that the mass loading factor η, the ratio between the ejected mass rate and the star formation rate, appears to be roughly constant with respect to the galaxy mass.

scholarly journals Morphology, Stellar Kinematics and Dynamics of Barred Galaxies

1983 ◽  
Vol 100 ◽  
pp. 193-196
Author(s):  
John Kormendy
Keyword(s):  
Velocity Dispersion ◽  
Rotation Velocity ◽  
Stellar Kinematics ◽  
Barred Galaxies ◽  
Circular Velocity ◽  
Local Ratio ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Random Motions ◽  
Velocity Dispersions

A brief review is given of the morphology of barred galaxies, following Kormendy (1981, 1982). The features illustrated include bulges, bars, disks, lenses, and inner and outer rings.Most of the paper is devoted to a detailed discussion of the absorption-line velocity field of the prototypical SBO galaxy NGC 936. The stars in the bar region show systematic non-circular streaming motions, with average orbits which are elongated parallel to the bar. Beyond the end of the bar, the data are consistent with circular orbits. The bar region also shows large random motions: the velocity dispersion at one-half of the radius of the bar is 1/2–2/3 as large as the maximum circular velocity. The observed kinematics are qualitatively and quantitatively similar to the behavior of n-body models by Miller and Smith (1979) and by Hohl and Zang (1979). The galaxy and the models show similar radial dependences of simple dimensionless parameters that characterize the dynamics. These include the local ratio of rotation velocity to velocity dispersion, which measures the relative importance of the ordered and random motions discussed above. Also similar are the residual streaming motions (relative to the circular velocity) in a frame of reference rotating with the bar. Circulation is in the same direction as rotation in all galaxies studied to date. Thus, except for the fact that NGC 936 has a slightly larger velocity dispersion, both n-body models are good first-order approximations to bars. Thus bars are different from elliptical galaxies, which in general are also triaxial, but which rotate slowly. This study of NGC 936 will be published in Kormendy (1983).A brief discussion is given of the kinematics of lens components. In both barred and unbarred galaxies, the velocity dispersions in the inner parts of lenses are large. The ratio of rotational to random kinetic energy is ∼ 1/2 at 1/3–1/2 of the radius of the lens. This ratio then decreases to small values at the rim of the lens. Thus at least some kinds of disk components have large stellar velocity dispersions, even in unbarred galaxies.

Unveiling the nuclear region of NGC 6868: Mapping the stellar population and ionized gas

2019 ◽  
Vol 15 (S359) ◽  
pp. 418-420
Author(s):  
João P. V. Benedetti ◽  
Rogério Riffel ◽  
Tiago V. Ricci ◽  
João E. Steiner ◽  
Rogemar A. Riffel ◽  
...  
Keyword(s):  
Stellar Population ◽  
Star Formation History ◽  
Nuclear Region ◽  
Stellar Kinematics ◽  
Ionized Gas ◽  
Formation History ◽  
The Galaxy ◽  
History Of ◽  
Field Unit ◽  
New Generation

AbstractWe mapped the stellar population and emission gas properties in the nuclear region of NGC 6868 using datacubes extracted with Gemini Multi-Object Spectrograph (GMOS) in the Integral Field Unit (IFU) mode. To obtain the star-formation history of this galaxy we used the starlight code together with the new generation of MILES simple stellar population models. The stellar population dominating (95% in light fraction) the central region of NGC 6868 is old and metal rich (~10 Gyr, 2.2 Z⊙). We also derived the kinematics and emission line fluxes of ionized gas with the IFSCube package. A rotation disk is clearly detected in the nuclear region of the galaxy and no broad components were detected. Also, there is a region where the emission lines disappear almost completely, probably due to diffuse ionized gas component. Channel maps, diagnostic diagrams and stellar kinematics are still under analysis.

scholarly journals Detailed Surface Photometry of the Dust-Lane Elliptical NGC 6702

1987 ◽  
Vol 127 ◽  
pp. 407-408
Author(s):  
E. Davoust ◽  
M. Capaccioli ◽  
G. Lelièvre ◽  
J.-L. Nieto
Keyword(s):  
High Resolution ◽  
Major Axis ◽  
Position Angle ◽  
Morphological Type ◽  
Surface Photometry ◽  
Photometric Study ◽  
Axis Ratio ◽  
Dust Lane ◽  
Detailed Surface ◽  
The Galaxy

We present preliminary results of a detailed photometric study of NGC 6702, from high resolution photographs taken at the Cassegrain focus of the Canada-France-Hawaii (CFH) telescope. The luminosity distribution of the galaxy follows an r1/4 law (re* = 11.6″, μe* = 22.17). The axis ratio is 0.75 (corresponding to the morphological type E3) and the position angle of the major axis is 60 and fairly constant. Fig. 1 is an image in intensity of the galaxy, from a 30mn exposure in B. The galaxy is crossed by a dust lane, reported first by Capaccioli et al. (1984).

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