Isolated Galaxies versus Interacting Pairs with MaNGA

Argudo-Fernández, M.; Yuan, Fang-Ting; Shen, Shiyin; Yin, Jian-Tao; Chang, Ruixiang; Feng, Shuai

doi:10.3390/galaxies3040156

Cited by 5 publications

(3 citation statements)

References 16 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These masses are based on a homogeneous catalog of g and r band photometry described by Simard et al (2011) and extended with bulge+disk and Sérsic profile photometric decompositions in the SDSS u, i, and z bands. We also define a field sample, comprising 5997 galaxies, which is a result of stacking three catalogs available in the literature (Khim et al 2015;Bradford et al 2015;Fernández et al 2015) in the SDSS DR7, DR8 & DR10 fields, respectively, and removing repeated objects and those belonging to galaxy clusters catalogs of Yang et al (2007) and Tempel et al (2017).…”

Section: Additional Informationmentioning

confidence: 99%

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Morell

Ribeiro

Carvalho

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We analyze the dependence of galaxy evolution on cluster dynamical state and galaxy luminosities for a sample of 146 galaxy clusters from the Yang SDSS catalog. Clusters were split according to their velocity distribution in Gaussians (G) and Non-Gaussians (NG), and further divided by luminosity regime. We performed a classification in the Age-SSFR plane providing three classes: star-forming (SF), passive (PAS), and intermediate (GV -green valley). We show that galaxies evolve in the same way in G and NG systems, but also suggest that their formation histories leads to different mixtures of galactic types and infall patterns. Separating the GV into star-forming and passive components, we find more bright galaxies in the passive mode of NG than in G systems. We also find more intermediate faint galaxies in the star-forming component of NG than in G systems. Our results suggest the GV as the stage where the transition from types Sab and Scd to S0 must be taking place, but the conversion between morphological types is independent of the dynamical stage of the clusters. Analyzing the velocity dispersion profiles, we find that objects recently infalling in clusters have a different composition between G and NG systems. While all galaxy types infall onto G systems, Sab and Scd dominate the infall onto NG systems. Finally, we find that faint Scd in the outskirts of NG systems present higher asymmetries relative to the mean asymmetry of field galaxies, suggesting environmental effects acting on these objects.

show abstract

Section: Additional Informationmentioning

confidence: 99%

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Morell

Ribeiro

Carvalho

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…We only use these values in Figure 2. While these group masses span all three mass subsamples, the group environments may have different absorption characteristics due to interaction effects (Alonso et al 2012;Fernández et al 2015;Pointon et al 2017) so we consider these to be a separate sample.…”

Section: Absorber Kinematicsmentioning

confidence: 99%

Kinematics of the O vi Circumgalactic Medium: Halo Mass Dependence and Outflow Signatures

Nielsen

Kacprzak

et al. 2019

ApJ

View full text Add to dashboard Cite

We probe the high-ionization circumgalactic medium by examining absorber kinematics, absorber-galaxy kinematics, and average absorption profiles of 31 O VI absorbers from the "Multiphase Galaxy Halos" Survey as a function of halo mass, redshift, inclination, and azimuthal angle. The galaxies are isolated at 0.12 < z gal < 0.66 and are probed by a background quasar within D ≈ 200 kpc. Each absorber-galaxy pair has Hubble Space Telescope images and COS quasar spectra, and most galaxy redshifts have been accurately measured from Keck/ESI spectra. Using the pixel-velocity two-point correlation function (TPCF) method, we find that O VI absorber kinematics have a strong halo mass dependence. Absorbers hosted by ∼ L * galaxies have the largest velocity dispersions, which we interpret to be that the halo virial temperature closely matches the temperature at which the collisionally ionized O VI fraction peaks. Lower mass galaxies and group environments have smaller velocity dispersions. Total column densities follow the same behavior, consistent with theoretical findings. After normalizing out the observed mass dependence, we studied absorber-galaxy kinematics with a modified TPCF and found non-virialized motions due to outflowing gas. Edge-on minor axis gas has large optical depths concentrated near the galaxy systemic velocity as expected for bipolar outflows, while faceon minor axis gas has a smoothly decreasing optical depth distribution out to large normalized absorbergalaxy velocities, suggestive of decelerating outflowing gas. Accreting gas signatures are not observed due to "kinematic blurring" in which multiple line-of-sight structures are observed. These results indicate that galaxy mass dominates O VI properties over baryon cycle processes.

show abstract

“…In the last few years, a number of specific interacting/merging systems in the local universe have been observed with such techniques at optical wavelengths (e.g., Wild et al 2014;Fernández et al 2015;Cortijo-Ferrero et al 2017a,c,b). Cortijo-Ferrero et al (2017c) have also characterized the star cluster properties in an early-stage merger.…”

Section: Introductionmentioning

confidence: 99%

GASP. VIII. Capturing the Birth of a Tidal Dwarf Galaxy in a Merging System at z ∼ 0.05

Vulcani

Moretti

Poggianti

et al. 2017

ApJ

View full text Add to dashboard Cite

Within the GAs Stripping Phenomena in galaxies with MUSE (GASP) sample, we identified an ongoing 1:1 merger between two galaxies and the consequent formation of a tidal dwarf galaxy (TDG). The system is observed at z = 0.05043 and is part of a poor group. Exploiting the exquisite quality of the MUSE/VLT data, we present the spatially resolved kinematics and physical properties of gas and stars of this object and describe its evolutionary history. An old (luminosity weighted age ∼ 2 × 10 9 yr), gas poor, early-type-like galaxy is merging with a younger (luminosity weighted age ∼ 2.5 × 10 8 yr), gas rich, late-type galaxy . The system has a quite strong metallicity gradient, indicative of an early-stage phase. Comparing the spatial extension of the star formation at different epochs, we date the beginning of the merger between 2 × 10 7 yr < t < 5.7 × 10 8 yr ago. The gas kinematic pattern reflects that of the late-type object and is distorted in correspondence to the location of the impact . The stellar kinematic instead is more chaotic, as expected for mergers. The gas redistribution in the system induces high levels of star formation between the two components, where we indeed detect the birth of the TDG. This stellar structure has a mass of ∼ 6 × 10 9 M , a radius of ∼ 2 kpc and, even though it has already accreted large quantities of gas and stars, it is still located within the disk of the progenitor, is characterized by a high velocity dispersion, indicating that it is still forming, is dusty and has high levels of star formation (SFR∼ 0.3M yr −1 ). This TDG is originated in an early-stage merger, while these structures usually form in more evolved systems.

show abstract

Isolated Galaxies versus Interacting Pairs with MaNGA

Cited by 5 publications

References 16 publications

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Kinematics of the O vi Circumgalactic Medium: Halo Mass Dependence and Outflow Signatures

GASP. VIII. Capturing the Birth of a Tidal Dwarf Galaxy in a Merging System at z ∼ 0.05

Contact Info

Product

Resources

About