Arp 70: an interacting galaxy with extreme outflows

2020 ◽  
Vol 493 (1) ◽  
pp. 1434-1446
Author(s):  
A Camps-Fariña ◽  
J E Beckman ◽  
J Font ◽  
I del Moral-Castro ◽  
S F Sanchez ◽  
...  
Keyword(s):  
Emission Line ◽  
The Other ◽  
Spectral Signature ◽  
Main Peak ◽  
Physical Parameters ◽  
Line Profiles ◽  
Public Repository ◽  
Line Region ◽  
Fabry Perot ◽  
H Ii Region

ABSTRACT We analysed a Fabry–Pérot (FP) cube of the interacting pair of galaxies Arp 70, which was obtained from the CeSAM public repository of FP data. On the larger galaxy Arp 70b, we detected the spectral signature of two different outflows, one located in the centre and the other associated with a giant H ii region in the arm region. The central outflow is especially prominent, with the flux of the secondary peaks in the emission-line profiles due to the outflowing gas being similar to that of the main peak. We used an archive fibre spectrum from SDSS to confirm this detection in H α as well as in the [N ii] line and, in addition, to perform diagnostics on the nature of the ionization. The emission at the centre is consistent with a low-ionization nuclear emission-line region and a weak active galactic nucleus. Using the spatial distribution of the profiles in the FP cube, we estimated the shape of the outflow which is consistent with two cones of expanding material, one approaching and the other receding from us, and used this to estimate the physical parameters of the outflow, finding energies of order 1057 erg and masses of order 108 M⊙. On the giant H ii region, we found a very large expanding superbubble with a diameter of ∼5 kpc. The bubble has an energy of order 1054 erg and a mass of about 4 × 107 M⊙. We discuss the possible origins for both of these features and whether they could be associated with the interaction between the galaxies.

scholarly journals The Kinematics of Quasar Broad Emission Line Regions Using a Disk-Wind Model

2017 ◽  
Vol 34 ◽  
Author(s):  
Suk Yee Yong ◽  
Rachel L. Webster ◽  
Anthea L. King ◽  
Nicholas F. Bate ◽  
Matthew J. O’Dowd ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Inclination Angle ◽  
Opening Angle ◽  
Line Profiles ◽  
Wind Model ◽  
Disk Wind ◽  
Reverberation Mapping ◽  
Broad Emission ◽  
Line Region

AbstractThe structure and kinematics of the broad line region in quasars are still unknown. One popular model is the disk-wind model that offers a geometric unification of a quasar based on the viewing angle. We construct a simple kinematical disk-wind model with a narrow outflowing wind angle. The model is combined with radiative transfer in the Sobolev, or high velocity, limit. We examine how angle of viewing affects the observed characteristics of the emission line. The line profiles were found to exhibit distinct properties depending on the orientation, wind opening angle, and region of the wind where the emission arises.At low inclination angle (close to face-on), we find that the shape of the emission line is asymmetric, narrow, and significantly blueshifted. As the inclination angle increases (close to edge-on), the line profile becomes more symmetric, broader, and less blueshifted. Additionally, lines that arise close to the base of the disk wind, near the accretion disk, tend to be broad and symmetric. Single-peaked line profiles are recovered for the intermediate and equatorial wind. The model is also able to reproduce a faster response in either the red or blue sides of the line profile, consistent with reverberation mapping studies.

scholarly journals The Nature and Origin of Structure in Broad Emission Line Profiles

1997 ◽  
Vol 159 ◽  
pp. 193-194 ◽  
Author(s):  
C. Martin Gaskell ◽  
Stephanie A. Snedden
Keyword(s):  
Emission Line ◽  
The Other ◽  
Central Component ◽  
Balmer Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Broad Emission Line

AbstractWe postulate that all structure in broad lines can be explained by a central component (at the systemic redshift) and the addition of two ‘displaced components’, one blueshifted and the other redshifted. We have been able to successfully classify all Balmer-line profiles on this basis. 3C 390.3-type objects are merely examples where the shifts of the displaced components are unusually large. We believe that the displaced peaks are less prominent in the UV lines because the higher ionization lines are broader.

scholarly journals Emission-line profiles and kinematics of the narrow-line region in Seyfert and radio galaxies

1981 ◽  
Vol 247 ◽  
pp. 403 ◽  
Author(s):  
T. M. Heckman ◽  
H. R. Butcher ◽  
G. K. Miley ◽  
W. J. M. van Breugel
Keyword(s):  
Emission Line ◽  
Radio Galaxies ◽  
Narrow Line ◽  
Line Profiles ◽  
Line Region ◽  
Narrow Line Region

scholarly journals The broad line emission from the AGN 3C 390.3: complex broad-line region and perturbation in accretion disk

2012 ◽  
Vol 8 (S290) ◽  
pp. 205-206
Author(s):  
Ilić Dragana ◽  
Luka Č. Popović ◽  
Alla I. Shapovalova ◽  
Alexander N. Burenkov ◽  
Vahram H. Chavushyan ◽  
...  
Keyword(s):  
Emission Line ◽  
Accretion Disk ◽  
Radio Galaxy ◽  
Dominant Role ◽  
Line Emission ◽  
Broad Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Line Region ◽  
Present Part

AbstractFrom 13-years of the spectral optical monitoring of a well-known broad-line radio galaxy 3C 390.3 we concluded that the geometry of the broad emission-line region is complex, while still the main part of the emission is coming from the accretion disk. Here we present part of the analysis of the broad Hα and Hβ emission lines, which are showing highly variable double-peaked profiles during the monitoring period (1995-2007), with the aim to probe the accretion disk properties. The disk-like geometry plays a dominant role, but the variability of Hα and Hβ line profiles and intensities shows a presence of an additional emission-line region, that has a different nature for different periods, e.g. in one period the observed variation can be well modeled if one assumes changes in position and size of the emitting disk along the accretion disk.

scholarly journals Hα Survey of the Large Magellanic Cloud

1995 ◽  
Vol 149 ◽  
pp. 155-159 ◽  
Author(s):  
A. Laval ◽  
E. le Coarer ◽  
Y.P. Georgelin ◽  
M. Marcelin ◽  
P. Amram ◽  
...  
Keyword(s):  
Kinetic Energy ◽  
Emission Line ◽  
Large Magellanic Cloud ◽  
Central Core ◽  
Evolutionary Stage ◽  
Line Profiles ◽  
Fabry Perot ◽  
Hα Emission ◽  
Spherical Expansion ◽  
The One

AbstractThe LMC is being surveyed in the Hα emission line with a scanning Fabry-Perot interferometer, attached to the 36 cm telescope of the Observatoire de Marseille. The present results concern the kinematical mapping of bright nebulae; it shows that the kinetic energy involved in the gas motion is closely related to the evolutionary stage of the embedded stars. In particular, in the 30 Dor nebula, a few one-peaked line profiles remain at the boundaries of the shells, among the numerous split areas. The 50-100 pc shells exhibit a relatively usual spherical expansion, with velocities in the same range at the boundaries. On the contrary, the 10-20 pc shells of the central core show different velocities of the one-peak sides of the shells.

scholarly journals Spectral variability of the 3C 390.3 nucleus for more than 20 years – II.  Variability of the broad emission-line profiles and He ii λ4686 Å emission-line fluxes

2020 ◽  
Vol 495 (1) ◽  
pp. 971-980
Author(s):  
S G Sergeev
Keyword(s):  
Emission Line ◽  
Emission Region ◽  
Line Profiles ◽  
Broad Emission ◽  
Line Region ◽  
Balmer Lines ◽  
Optical Continuum ◽  
Broad Emission Line ◽  
Disc Configuration ◽  
Factor C

ABSTRACT Results of the analysis of the variability of the H β and H α broad emission-line profiles and the He ii λ4686 Å emission-line fluxes in the 3C 390.3 nucleus during 1992–2014 are present. The observed velocity-dependent lag for the Balmer lines is similar to that expected from the Keplerian disc configuration, although there are some differences. Probably, a radial infall motion can be present in the broad-line region of 3C 390.3 in addition to the Keplerian rotation. The lag of the broad He ii line is 26 ± 8 d, significantly less than that of the Balmer lines, so the He ii emission region is much smaller in size. In terms of the power-law relationship between line and optical continuum fluxes with slowly varying scale factor c(t): $F_{\rm line}\propto c(t)\, F_{\rm cont}^a$, the power a is 1.03 for the broad He ii line, while according to Paper I, the power is equal to 0.77 and 0.54 for the broad H β and H α lines, respectively. It means that the variability amplitude is the largest in the He ii, less in H β, and more less in H α. However, the Balmer lines contain a long-term trend that is not seen in the helium line. The narrow He ii line is variable with the amplitude (max-to-min ratio) Rmax ≈ 3, which is much greater than the variability amplitudes of both the narrow Balmer lines and the narrow [O iii] λ5007 Å line.

Infrared Spectroscopy of NGC 4151:Infrared Space ObservatoryObservations and Narrow Emission Line Region Line Profiles

1999 ◽  
Vol 512 (1) ◽  
pp. 197-203 ◽  
Author(s):  
E. Sturm ◽  
T. Alexander ◽  
D. Lutz ◽  
A. Sternberg ◽  
H. Netzer ◽  
...  
Keyword(s):  
Infrared Spectroscopy ◽  
Emission Line ◽  
Line Profiles ◽  
Ngc 4151 ◽  
Line Region ◽  
Narrow Emission ◽  
Region Line

scholarly journals Complex broad emission line profiles of AGN – Geometry of the broad line region

2009 ◽  
Vol 53 (7-10) ◽  
pp. 121-127 ◽  
Author(s):  
E. Bon ◽  
N. Gavrilović ◽  
G. La Mura ◽  
L.Č. Popović
Keyword(s):  
Emission Line ◽  
Broad Line ◽  
Line Profiles ◽  
Broad Line Region ◽  
Broad Emission ◽  
Line Region ◽  
Broad Emission Line

scholarly journals Substructures in the Narrow-Line Region of AGN

1989 ◽  
Vol 134 ◽  
pp. 312-313
Author(s):  
Sylvain Veilleux
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Seyfert Galaxies ◽  
Narrow Line ◽  
Line Profiles ◽  
Preliminary Results ◽  
Line Region ◽  
Narrow Line Region ◽  
Narrow Emission ◽  
Resolution Study

The preliminary results of a high-resolution study of narrow emission-line profiles in bright Seyfert galaxies are reported. Profile substructures such as secondary peaks and shoulders are observed in nearly all the objects. The results of profile comparisons in Mrk 359, Mrk 533, and Mrk 1066 are briefly discussed.

Sign in / Sign up

Export Citation Format

Share Document