scholarly journals NEWLY DISCOVERED FOOTPRINTS OF GALAXY INTERACTION AROUND SEYFERT 2 GALAXY NGC 7743

2015 ◽  
Vol 30 (2) ◽  
pp. 463-464
Author(s):  
YONGJUNG KIM ◽  
MYUNGSHIN IM ◽  
CHANGSU CHOI ◽  
MINHEE HYUN ◽  
YONGMIN YOON ◽  
...  
Keyword(s):  
Galaxy Interaction

scholarly journals Luminous Infrared Galaxies in a Merging Sequence: ISO Observations

1999 ◽  
Vol 186 ◽  
pp. 282-282 ◽  
Author(s):  
C.-Y. Hwang ◽  
K.Y. Lo ◽  
Y. Gao ◽  
R.A. Gruendl ◽  
N.-Y. Lu
Keyword(s):  
High Spatial Resolution ◽  
Molecular Gas ◽  
Infrared Images ◽  
Infrared Galaxies ◽  
Space Observatory ◽  
Infrared Space Observatory ◽  
Mid Infrared ◽  
Luminous Infrared Galaxies ◽  
Physical Conditions ◽  
Galaxy Interaction

We report mid-infrared images of several luminous infrared galaxies (LIGs) taken with ISOCAM on the Infrared Space Observatory (ISO). These LIGs were chosen to represent different phases of a merger sequence of galaxy-galaxy interaction with special emphasis on early/intermediate stages of merging. The molecular gas distribution of these LIGs has also been mapped at high spatial resolution (see contribution by Gao et al., this volume). The goal is to do a synoptic study of the evolution of physical conditions in these LIGs along the merger sequence.

Kinematic asymmetry of galaxy pairs

2019 ◽  
Vol 14 (S353) ◽  
pp. 262-263
Author(s):  
Shuai Feng ◽  
Shi-Yin Shen ◽  
Fang-Ting Yuan
Keyword(s):  
Star Formation ◽  
Velocity Field ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Control Sample ◽  
Interacting Galaxies ◽  
Ionized Gas ◽  
Galaxy Interaction ◽  
The Galaxy

AbstractThe interaction between galaxies is believed to be the main origin of the peculiarities of galaxies. It can disturb not only the morphology but also the kinematics of galaxies. These disturbed and asymmetric features are the indicators of galaxy interaction. We study the velocity field of ionized gas in galaxy pairs based on MaNGA survey. Using the kinemetry package, we fit the velocity field and quantify the degree of kinematic asymmetry. We find that the fraction of high kinematic asymmetry is much higher for galaxy pairs with dp⩽30h−1kpc. Moreover, compared to a control sample of single galaxies, we find that the star formation rate is enhanced in paired galaxies with high kinematic asymmetry. For paired galaxies with low kinematic asymmetry, no significant SFR enhancement has been found. The galaxy pairs with high kinematic asymmetry are more likely to be real interacting galaxies rather than projected pairs.

scholarly journals Kinematics of Planetary Nebulae in M51's Tidal Tail

2003 ◽  
Vol 209 ◽  
pp. 633-634
Author(s):  
John J. Feldmeier ◽  
J. Christopher Mihos ◽  
Patrick R. Durrell ◽  
Robin Ciardullo ◽  
George H. Jacoby
Keyword(s):  
Surface Brightness ◽  
Numerical Models ◽  
Planetary Nebulae ◽  
Tidal Tail ◽  
Low Surface Brightness ◽  
Galaxy Interaction ◽  
Self Consistent ◽  
The Galaxy ◽  
Interacting Systems ◽  
Kinematic Properties

The galaxy pair NGC 5194/95 (M51) is one of the closest and best known interacting systems. Despite its notoriety, however, many of its features are not well studied. Extending westward from NGC 5195 is a low surface brightness tidal tail, which can only be seen in deep broadband exposures. Our previous [O III] λ5007 planetary nebulae (PN) survey of M51 recovered this tidal tail, and presented us with a opportunity to study the kinematics of a galaxy interaction in progress. We report the results of a spectroscopy survey of the PN, aimed at determining their kinematic properties. We then use these data to constrain new self-consistent numerical models of the system.

Probing the Evolution of the Galaxy Interaction/Merger Rate Using Collisional Ring Galaxies

2004 ◽  
Vol 612 (2) ◽  
pp. 679-689 ◽  
Author(s):  
Russell J. Lavery ◽  
Anthony Remijan ◽  
Vassilis Charmandaris ◽  
Richard D. Hayes ◽  
Amy A. Ring
Keyword(s):  
Galaxy Interaction ◽  
The Galaxy ◽  
Ring Galaxies ◽  
Merger Rate

scholarly journals Evidence of galaxy interaction in the narrow-line Seyfert 1 galaxy IRAS 17020+4544 seen by NOEMA

2020 ◽  
Vol 501 (1) ◽  
pp. 219-228
Author(s):  
Q Salomé ◽  
A L Longinotti ◽  
Y Krongold ◽  
C Feruglio ◽  
V Chavushyan ◽  
...  
Keyword(s):  
Gas Content ◽  
Host Galaxy ◽  
Molecular Gas ◽  
Narrow Line ◽  
Nuclear Region ◽  
X Ray ◽  
Molecular Outflow ◽  
Galaxy Interaction ◽  
Massive Outflow ◽  
First Time

ABSTRACT The narrow-line Seyfert 1 galaxy IRAS 17020+4544 is one of the few sources where both an X-ray ultrafast outflow and a molecular outflow were observed to be consistent with energy conservation. However, IRAS 17020+4544 is less massive and has a much more modest active galactic nucleus (AGN) luminosity than the other examples. Using recent CO(1–0) observations with the NOrthern Extended Millimeter Array, we characterized the molecular gas content of the host galaxy for the first time. We found that the molecular gas is distributed into an apparent central disc of 1.1 × 109 M⊙, and a northern extension located up to 8 kpc from the centre with a molecular gas mass $M_{\mathrm{ H}_2}\sim 10^8\, \mathrm{ M}_\odot$. The molecular gas mass and the CO dynamics in the northern extension reveal that IRAS 17020+4544 is not a standard spiral galaxy, instead it is interacting with a dwarf object corresponding to the northern extension. This interaction possibly triggers the high accretion rate on to the supermassive black hole. Within the main galaxy, which hosts the AGN, a simple analytical model predicts that the molecular gas may lie in a ring, with less molecular gas in the nuclear region. Such distribution may be the result of the AGN activity that removes or photodissociates the molecular gas in the nuclear region (AGN feedback). Finally, we have detected a molecular outflow of mass $M_{\mathrm{ H}_2}=(0.7\!-\!1.2)\times 10^7\, \mathrm{ M}_\odot$ in projection at the location of the northern galaxy, with a similar velocity to that of the massive outflow reported in previous millimetre data obtained by the Large Millimeter Telescope.

scholarly journals Numerical Simulations of Star Formation Bursts Induced by the Galaxy-Galaxy Interaction

1987 ◽  
Vol 115 ◽  
pp. 650-653
Author(s):  
Masafumi Noguchi ◽  
Shiro Ishibashi
Keyword(s):  
Star Formation ◽  
Kinetic Energy ◽  
Supernova Explosion ◽  
Particle Model ◽  
Disk Galaxies ◽  
Triggering Mechanism ◽  
Cloud Particle ◽  
Test Particles ◽  
Galaxy Interaction ◽  
The Galaxy

The galaxy-galaxy interaction has been proposed as a possible triggering mechanism of the star formation bursts in some galaxies (e.g. Larson and Tinsley 1978). To investigate the nature of star formation bursts triggered by interaction we have numerically simulated close encounters between disk galaxies, taking the star formation process into account (see Noguchi and Ishibashi 1986 for details). We used the cloud-particle model, in which gas clouds move as test particles in the gravitational field of the galaxies. When two clouds collide with each other, an OB-star is formed. The cloud system loses its kinetic energy by inelastic cloud-cloud collisions. The supernova explosion which follows the formation of an OB-star provides kinetic energy to the nearby clouds.

scholarly journals A radio-jet-galaxy interaction in 3C 441

1998 ◽  
Vol 298 (4) ◽  
pp. 966-976 ◽  
Author(s):  
M. Lacy ◽  
S. Rawlings ◽  
K. M. Blundell ◽  
S. E. Ridgway
Keyword(s):  
Galaxy Interaction

scholarly journals IRAS 03158+4227 - a ULIRG in a Widely Separated Pair of Galaxies

2002 ◽  
Vol 184 ◽  
pp. 215-216
Author(s):  
Helmut Meusinger ◽  
Bringfried Stecklum ◽  
Jens Brunzendorf
Keyword(s):  
High Resolution ◽  
Optical Spectroscopy ◽  
Early Phase ◽  
Optical Images ◽  
Galaxy Interaction

AbstractWe present new deep optical images, optical spectroscopy, and high-resolution NIR images of IRAS 03158+4227, one of the most luminous ULIRGs from the IRAS 2 Jy sample. The data are best explained either by a multiple merger or by the assumption of a ULIRG triggered in an early phase of galaxy interaction.

Revealing the effects of galaxy interaction in the main galaxies of the southern group Arp 314

2020 ◽  
Vol 494 (2) ◽  
pp. 2785-2797
Author(s):  
S Torres-Flores ◽  
P Amram ◽  
D Olave-Rojas ◽  
N Muñoz-Elgueta ◽  
C Mendes de Oliveira ◽  
...  
Keyword(s):  
Gas Flows ◽  
Low Oxygen ◽  
Data Set ◽  
Oxygen Abundance ◽  
Star Forming ◽  
Star Forming Regions ◽  
Fabry Perot ◽  
Galaxy Interaction ◽  
Interacting Systems ◽  
Tidal Tails

ABSTRACT We present new Gemini imaging and spectroscopic data of the system Arp 314, which consists of a triplet of interacting galaxies. This new imagery exhibits tidal tails and stellar bridges between the galaxies' members and confirms the past interactions. Using this data set, we have analysed the physical properties of 22 star-forming regions located in the main disc of these galaxies, as well as in the intergalactic medium. All these regions have emission lines typical of young ages and a couple of them display very high Hα luminosities (LHα ∼ 1040 erg s−1). Using the star-forming regions located in Arp 314-1, we derive its gas-phase oxygen-abundance distribution, which suggests a flatter behaviour than the distribution shown by non-interacting systems. This is in agreement with results obtained for other interacting systems and simulations. The presence of gas flows, as indicated by its complex kinematics, could explain this finding. Most of the star formation in Arp 314-2 is located in a central starburst, where double Hα profiles can be identified, as shown by archival Fabry–Perot data. Additionally, we found that the irregular galaxy Arp 314-3 has a low oxygen abundance. Considering its luminosity, this object has a primordial origin, and it was not formed during the interaction event that this system has experienced.

scholarly journals FIR Infrared Emission as Indicator of Interaction in Hickson Compact Groups

2000 ◽  
Vol 174 ◽  
pp. 205-208
Author(s):  
P. Merluzzi ◽  
A. A. Shaker ◽  
G. Longo
Keyword(s):  
Infrared Emission ◽  
Spatial Density ◽  
Compact Groups ◽  
Low Velocity ◽  
Merging Galaxies ◽  
Groups Of Galaxies ◽  
Data Resolution ◽  
Galaxy Interaction ◽  
Hickson Compact Groups ◽  
Very High

Due to their very high spatial density and relatively low velocity dispersion, Hickson’s compact groups of galaxies (hereafter HCGs, Hickson et al. 1989a, H89a) are ideal test grounds where to study the physics of galaxy interaction.Tidal shocks induced by galaxy interaction are expected to trigger rapid bursts of star formation in the circumnuclear region of galaxies. The increases in density and temperature caused locally by such shocks produce an enhancement in both the total FIR luminosity and in the ratio between the FIR fluxes at 60 and 100 μm. These enhancements have been actually observed in the circumnuclear regions of both interacting and ”putative” merging galaxies and should therefore be found also in all galactic environments where the frequency of interaction is higher than in the field. However, while interactions are more frequent among HCGs members than in the field (e.g. Hickson 1994, Shaker et al. 1999), there are conflicting arguments on whether HCGs present or do not present a FIR excess. As stressed by many authors, the critical point is the IRAS data resolution which prevents to map the spatial distribution of the FIR emission. We investigate the FIR properties of a selected sample of HCGs by sing the new high spatial resolution data from Allam et al. 1996 (A96). In particular, we address the problem whether or not there is any FIR enhancement in the compact groups and the reasons of that. This is a short presentation of the analysis performed and of the results obtained (Merluzzi et al. 1999).

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