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 Star-forming regions in the intragroup medium of compact groups of galaxies

2009 ◽  
Vol 5 (S262) ◽  
pp. 440-441
Author(s):  
S. Torres-Flores ◽  
C. Mendes de Oliveira ◽  
D. F. de Mello ◽  
P. Amram ◽  
H. Plana ◽  
...  
Keyword(s):  
Star Formation ◽  
Dwarf Galaxy ◽  
Early Stage ◽  
Velocity Fields ◽  
Compact Groups ◽  
Advanced Stage ◽  
Groups Of Galaxies ◽  
Star Forming ◽  
Star Forming Regions ◽  
Fabry Perot

AbstractWe present the results of a multiwavelength campaign searching for young objects in the intragroup medium of seven compact groups of galaxies: HCG 2, 7, 22, 23, 92, 100 and NGC 92. We used Fabry-Perot velocity fields and rotation curves together with GALEX NUV and FUV images, optical R-band and HI maps to evaluate the stage of interaction of each group. We conclude that groups (i) HCG 7 and HCG 23 are in an early stage of interaction, (ii) HCG 2 and HCG 22 are mildly interacting, and (iii) HCG 92, HCG 100 and NGC 92 are in a late stage of evolution. Evolved groups have a population of young objects in their intragroup medium while no such population is found within the less evolved groups. We also report the discovery of a tidal dwarf galaxy candidate in the tail of NGC 92. These three groups, besides containing galaxies which have peculiar velocity fields, also show extended HI tails. Our results indicate that the advanced stage of evolution of a group together with the presence of intragroup HI clouds may lead to star formation in the intragroup medium.

scholarly journals Dissecting star formation in the “Atoms-for-Peace” galaxy

2018 ◽  
Vol 614 ◽  
pp. A130 ◽  
Author(s):  
K. George ◽  
P Joseph ◽  
P. Côté ◽  
S. K. Ghosh ◽  
J. B. Hutchings ◽  
...  
Keyword(s):  
Star Formation ◽  
Dwarf Galaxies ◽  
Initial Conditions ◽  
Dwarf Galaxy ◽  
Main Body ◽  
Star Forming ◽  
Uv Imaging ◽  
Star Forming Regions ◽  
The Galaxy ◽  
Tidal Tails

Context. The tidal tails of post-merger galaxies exhibit ongoing star formation far from their disks. The study of such systems can be useful for our understanding of gas condensation in diverse environments. Aims. The ongoing star formation in the tidal tails of post-merger galaxies can be directly studied from ultraviolet (UV) imaging observations. Methods. The post merger galaxy NGC7252 (“Atoms-for-Peace” galaxy) is observed with the Astrosat UV imaging telescope (UVIT) in broadband NUV and FUV filters to isolate the star-forming regions in the tidal tails and study the spatial variation in star formation rates. Results. Based on ultraviolet imaging observations, we discuss star-forming regions of ages <200 Myr in the tidal tails. We measure star formation rates in these regions and in the main body of the galaxy. The integrated star formation rate (SFR) of NGC7252 (i.e., that in the galaxy and tidal tails combined) without correcting for extinction is found to be 0.81 ± 0.01 M⊙ yr−1. We show that the integrated SFR can change by an order of magnitude if the extinction correction used in SFR derived from other proxies are taken into consideration. The star formation rates in the associated tidal dwarf galaxies (NGC7252E, SFR = 0.02 M⊙ yr−1 and NGC7252NW, SFR = 0.03 M⊙ yr−1) are typical of dwarf galaxies in the local Universe. The spatial resolution of the UV images reveals a gradient in star formation within the tidal dwarf galaxy. The star formation rates show a dependence on the distance from the centre of the galaxy. This can be due to the different initial conditions responsible for the triggering of star formation in the gas reservoir that was expelled during the recent merger in NGC7252.

scholarly journals Hα Kinematics of Tidal Tails in Interacting Systems: Projection Effects and Dark Matter in TDGs

2004 ◽  
Vol 217 ◽  
pp. 526-531
Author(s):  
Philippe Amram ◽  
Fréderic Bournaud ◽  
Pierre-Alain Duc
Keyword(s):  
Dark Matter ◽  
Dwarf Galaxies ◽  
Matter Content ◽  
Field Of View ◽  
Large Field ◽  
Ionized Gas ◽  
Tidal Tail ◽  
Fabry Perot ◽  
Interacting Systems ◽  
Tidal Tails

Several interacting systems exhibit at the tip of their long tidal tails massive condensations of atomic hydrogen, which may be the progenitors of Tidal Dwarf Galaxies. Because, quite often, these tails are observed edge-on, projection effects have been claimed to account for the large HI column densities measured there. Here we show that determining the velocity field all along the tidal features, one may disentangle projection effects along the line of view from real bound structures. Due to its large field of view, high spectral and 2D spatial resolutions, Fabry-Perot observations of the ionized gas are well adapted to detect a kinematical signature of either streaming motions along a bent tidal tail or of in-falling/rotating material associated with a forming TDG. Spectroscopic observations also allow to measure the dynamical masses of the TDGs that are already relaxed and check their dark matter content.

scholarly journals Azimuthal variations of oxygen abundance profiles in star-forming regions of disc galaxies in EAGLE simulations

2019 ◽  
Vol 491 (4) ◽  
pp. 4894-4901
Author(s):  
Martín Solar ◽  
Patricia B Tissera ◽  
Jose A Hernandez-Jimenez
Keyword(s):  
Stellar Populations ◽  
Chemical Abundances ◽  
Oxygen Abundance ◽  
Star Forming ◽  
Chemical Enrichment ◽  
Numerical Resolution ◽  
Star Forming Regions ◽  
Star Formation Activity ◽  
Large Dispersion ◽  
The Mean

ABSTRACT The exploration of the spatial distribution of chemical abundances in star-forming regions of galactic discs can help us to understand the complex interplay of physical processes that regulate the star formation activity and the chemical enrichment across a galaxy. We study the azimuthal variations of the normalized oxygen abundance profiles in the highest numerical resolution run of the Evolution and Assembly of GaLaxies and their Environments (EAGLE) Project at $z$ = 0. We use young stellar populations to trace the abundances of star-forming regions. Oxygen profiles are estimated along different line of sights from a centrally located observer. The mean azimuthal variation in the EAGLE discs are ∼0.12 ± 0.03 dex $R_{\rm eff}^{-1}$ for slopes and ∼0.12 ± 0.03 dex for the zero-points, in agreement with previous works. Metallicity gradients measured along random directions correlate with those determined by averaging over the whole discs, although with a large dispersion. We find a slight trend for higher azimuthal variations in the disc components of low star-forming and bulge-dominated galaxies. We also investigate the metallicity profiles of stellar populations with higher and lower levels of enrichment than the average metallicity profiles, and we find that high star-forming regions with high metallicity tend to have slightly shallower metallicity slopes compared with the overall metallicity gradient. The simulated azimuthal variations in the EAGLE discs are in agreement with observations, although the large variety of metallicity gradients would encourage further exploration of the metal mixing in numerical simulations.

scholarly journals Star formation enhancement characteristics in interacting galaxies

2014 ◽  
Vol 10 (S309) ◽  
pp. 354-354
Author(s):  
J. Zaragoza-Cardiel ◽  
J. E. Beckman ◽  
J. Font ◽  
A. Camps-Fariña ◽  
B. García-Lorenzo ◽  
...  
Keyword(s):  
Physical Properties ◽  
Hii Regions ◽  
Interacting Galaxies ◽  
Full Sample ◽  
Star Forming ◽  
Star Forming Regions ◽  
La Palma ◽  
Isolated Galaxies ◽  
Fabry Perot ◽  
William Herschel

AbstractWe have observed 12 interacting galaxies using the Fabry-Perot interferometer GHαFaS (Galaxy Hα Fabry-Perot system) on the 4.2m William Herschel Telescope (La Palma). We have extracted the physical properties (sizes, Hα luminosity and velocity dispersion) of 236 HII regions for the full sample of interacting galaxies. We have derived the physical properties of 664 HII regions for a sample of 28 isolated galaxies observed with the same instrument in order to compare both populations of HII regions, finding that there are brighter and denser star forming regions in the interacting galaxies compared with the isolated galaxies sample.

scholarly journals Clues on Arp 142: The spiral–elliptical merger

2019 ◽  
Vol 488 (1) ◽  
pp. 830-846
Author(s):  
Marcelo D Mora ◽  
Sergio Torres-Flores ◽  
Verónica Firpo ◽  
Jose A Hernandez-Jimenez ◽  
Fernanda Urrutia-Viscarra ◽  
...  
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Morphological Characteristics ◽  
Current Data ◽  
Ionization Mechanism ◽  
H Ii Regions ◽  
Data Set ◽  
Star Forming ◽  
Star Forming Regions ◽  
The Individual

Abstract Nearby merging pairs are unique laboratories in which one can study the gravitational effects on the individual interacting components. In this manuscript, we report the characterization of selected H ii regions along the peculiar galaxy NGC 2936, member of the galaxy pair Arp 142, an E+S interaction, known as ‘The Penguin’. Using Gemini South spectroscopy, we have derived a high enhancement of the global star formation rate (SFR) = 35.9 M⊙ yr−1 probably stimulated by the interaction. Star-forming regions on this galaxy display oxygen abundances that are consistent with solar metallicities. The current data set does not allow us to conclude any clear scenario for NGC 2936. Diagnostic diagrams suggest that the central region of NGC 2936 is ionized by active galactic nucleus (AGN) activity and the eastern tidal plume in NGC 2936 is experiencing a burst of star formation, which may be triggered by the gas compression due to the interaction event with its elliptical companion galaxy: NGC 2937. The ionization mechanism of these sources is consistent with shock models of low velocities of 200–300 km s −1. The isophotal analysis shows tidal features on NGC 2937: at inner radii non-concentric (or off-centring) isophotes, and at large radii, a faint excess of the surface brightness profile with respect to de Vaucouleurs law. By comparing the radial velocity profiles and morphological characteristics of Arp 142 with a library of numerical simulations, we conclude that the current stage of the system would be about 50 ± 25 Myr after the first pericentre passage.

scholarly journals Gravity Binding and Pressure Bounding of Hii regions and Molecular Clouds in Interacting Galaxies

2015 ◽  
Vol 11 (S315) ◽  
Author(s):  
J. Zaragoza-Cardiel ◽  
J. Beckman ◽  
J. Font ◽  
A. Camps-Fariña ◽  
B. Garcìa-Lorenzo ◽  
...  
Keyword(s):  
Physical Properties ◽  
Molecular Clouds ◽  
Velocity Dispersion ◽  
Hii Regions ◽  
Interacting Galaxies ◽  
Star Forming ◽  
Star Forming Regions ◽  
La Palma ◽  
Fabry Perot ◽  
William Herschel

AbstractWe have observed 3 pairs of interacting galaxies (the Antennae, Arp 236, and NGC 1614) using the Fabry-Perot interferometer GHαFaS (Galaxy Hα Fabry-Perot system) on the 4.2m William Herschel Telescope (WHT) at the Observatorio del Roque de los Muchachos, La Palma. We have extracted the physical properties (sizes, Hα luminosity and velocity dispersion) of Hii regions. We have combined also these observations with ALMA archival observations of these interacting galaxies, finding that there is a set of brighter and denser star forming regions. We have been able to compare these properties with those of two SMGs at redshift ~ 2.

scholarly journals Kinematic properties of superbubbles in the Antennae, M83 and Arp 270

2014 ◽  
Vol 10 (S309) ◽  
pp. 304-304
Author(s):  
A. Camps-Fariña ◽  
J. Beckman ◽  
J. Zaragoza-Cardiel ◽  
J. Font ◽  
K. Fathi ◽  
...  
Keyword(s):  
Large Scale ◽  
Interacting Galaxies ◽  
Dynamical Study ◽  
Star Forming ◽  
Fabry Perot ◽  
Galaxy Interaction ◽  
Scale Expansion ◽  
Kinematic Properties

AbstractSuperbubbles and large scale expansion in galaxies are important indicators of activity in galaxies: they are formed in starbursts and around active nuclei. Superbubbles can be used to give information about the star-forming region which produced them. We present in-depth results of our study of kinematically detected superbubbles using a method based on Fabry-Perot spectroscopy, which allows us to map regions of expansion across the entire disk of a galaxy. Three objects have been selected for this poster based on the interest of the results they show: two interacting galaxies, the Antennae and Arp270, at different stages of galaxy interaction, and the more isolated galaxy M83. We present the kinematic expansion maps, as well as a census of detected superbubbles and a dynamical study of their properties.

scholarly journals Star-forming regions and the metallicity gradients in the tidal tails: the case of NGC 92★

2013 ◽  
Vol 438 (2) ◽  
pp. 1894-1908 ◽  
Author(s):  
S. Torres-Flores ◽  
S. Scarano ◽  
C. Mendes de Oliveira ◽  
D. F. de Mello ◽  
P. Amram ◽  
...  
Keyword(s):  
Star Forming ◽  
Star Forming Regions ◽  
Tidal Tails
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