Frequency of Tidal Features Correlates with Age and Internal Structure of Early-type Galaxies

Yoon, Yongmin; Lim, Gu

doi:10.3847/1538-4357/abc621

Cited by 17 publications

(32 citation statements)

References 80 publications

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“…The detection limit of coadded images of Stripe 82 is ∼ 2 mag deeper than single-epoch images of SDSS (Jiang et al 2014). Therefore, faint tidal features of ETGs that are difficult to detect in the SDSS singleepoch images can be discovered in the coadded images of Stripe 82 (Kaviraj 2010;Schawinski et al 2010;Hong et al 2015;Yoon & Lim 2020).…”

Section: Selection Of Etg Samples With Fine Qualities In Stripe 82mentioning

confidence: 96%

“…To detect tidal features, we performed visual inspection, as in Yoon & Lim (2020), on deep coadded images of the Stripe 82 from Jiang et al (2014). Among the five bands of SDSS, we used r-band coadded images of which the surface brightness limit (1σ of the background noise over a 1 × 1 region) is ∼ 27 mag arcsec −2 and the 5σ detection limit of the aperture magnitude is 24.6.…”

Section: Detection Of Tidal Featuresmentioning

confidence: 99%

“…Among the five bands of SDSS, we used r-band coadded images of which the surface brightness limit (1σ of the background noise over a 1 × 1 region) is ∼ 27 mag arcsec −2 and the 5σ detection limit of the aperture magnitude is 24.6. We note that many studies still prefer visual inspection rather than quantitative methods (Schawinski et al 2010;Kaviraj et al 2011;Atkinson et al 2013;Hong et al 2015;Yoon & Lim 2020) as it can be difficult to detect faint irregular tidal features (or distinguish them from contaminations due to nearby sources) with the automatic and quantitative determination (Kartaltepe et al 2010;Miskolczi et al 2011;Atkinson et al 2013). We examined each image to find tidal features such as tidal tails, shell structures, streams, and diffuse fans (see Figures 1 and 2), adjusting the scale of pixel values.…”

Section: Detection Of Tidal Featuresmentioning

confidence: 99%

“…However, mergers between galaxies leave tidal features around the remnants that are detectable in deep images (Toomre & Toomre 1972;Quinn 1984;Barnes 1988;Hernquist & Spergel 1992;Feldmann et al 2008). Therefore, tidal features such as tidal tails, streams, and shells are considered the most direct observational ev-idence for recent mergers, through which it is possible to investigate the influence of mergers on photometric (Schweizer & Seitzer 1992;Tal et al 2009;Schawinski et al 2010;Kaviraj et al 2011;Hong et al 2015;Yoon & Lim 2020) and kinematic (Krajnović et al 2011;Duc et al 2015;Oh et al 2016) properties of ETGs. For instance, Hong et al (2015) suggested that luminous AGNs in ETGs are related to galaxy mergers based on the discovery that almost half of luminous AGN hosts have tidal features.…”

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confidence: 99%

“…For instance, Hong et al (2015) suggested that luminous AGNs in ETGs are related to galaxy mergers based on the discovery that almost half of luminous AGN hosts have tidal features. Yoon & Lim (2020) discovered direct evidence that compact young ETGs especially with blue cores and ETGs with dust lanes are involved in recent mergers, by investigating how the fraction of ETGs having tidal features depends on the age and internal structure of ETGs.…”

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confidence: 99%

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Evidence for Impact of Galaxy Mergers on Stellar Kinematics of Early-type Galaxies

Yoon,

Park,

Chung

et al. 2021

Preprint

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We provide observational evidence that galaxy mergers significantly affect stellar kinematics of earlytype galaxies (ETGs) such as specific stellar angular momentum within the half-light radius (λ Re ) and kinematic misalignment (ψ mis ), using MaNGA integral field unit spectroscopic data that are in the Stripe 82 region of the Sloan Digital Sky Survey. In this study, tidal features around ETGs, which are detected in deep coadded images, are used as direct evidence for mergers that occurred recently. In the case of ETGs that do not have dust lanes, λ Re is lower in ETGs with tidal features than in those without tidal features (median λ Re : 0.21 versus 0.39) in all stellar mass and Sérsic index ranges except the most massive bin, so that the fraction of ETGs with tidal features in slow rotators is more than twice as large as that in fast rotators (42% versus 18%). Moreover, ETGs with tidal features have larger ψ mis than those without tidal features (mean ψ mis : 28 • versus 15 • ). By contrast, ETGs with dust lanes are fast rotators, and ETGs with both dust lanes and tidal features have the highest λ Re (median λ Re : 0.59) among all ETG categories. In addition, ETGs with dust lanes have small ψ mis regardless of the existence of tidal features (ψ mis < 7.5 • ). Our results can be explained if mergers with different gas fractions generate merger remnants that have different kinematic properties.

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Section: Selection Of Etg Samples With Fine Qualities In Stripe 82mentioning

confidence: 96%

Section: Detection Of Tidal Featuresmentioning

confidence: 99%

Section: Detection Of Tidal Featuresmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Evidence for Impact of Galaxy Mergers on Stellar Kinematics of Early-type Galaxies

Yoon,

Park,

Chung

et al. 2021

Preprint

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emerge: constraining merging probabilities and time-scales of close galaxy pairs

O'Leary

Moster

Krämer

2021

Monthly Notices of the Royal Astronomical Society

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Theoretical models are vital for exploring the galaxy merger process, which plays a crucial role in the evolution of galaxies. Recent advances in modelling have placed tight constraints on the buildup of stellar material in galaxies across cosmic time. Despite these successes, extracting the merger rates from observable data remains a challenge. Differences in modelling techniques, combined with limited observational data, drive conflicting conclusions on the merging timescales of close pairs. We employ an empirical model for galaxy formation that links galaxy properties to the growth of simulated dark matter haloes, along with mock lightcone galaxy catalogues, to probe the dependencies of pair merging probabilities and merging timescales. In this work, we demonstrate that the pair merging probabilities are best described by a logistic function and that mean merging timescales can be well approximated by a linear relation in the projected separation and line of sight velocity difference in observed pairs. Together, our fitting formulae can accurately predict merger rates from galaxy pairs to at least z ∼ 4 under a wide variety of pair selection criteria. Additionally, we show that some commonly used pair selection criteria may not represent a suitable sample of galaxies to reproduce underlying merger rates. Finally, we conclude from our analysis that observation timescales are primarily driven by dynamics and are not strongly impacted by the star formation properties of the component galaxies.

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Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images

Martin

Bazkiaei

Spavone

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially of millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilising automated techniques and human visual classification in conjunction with realistic mock images produced using the NewHorizon cosmological simulation, we investigate the nature, frequency and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-year depth of the Legacy Survey of Space and Time (30 − 31 mag arcsec−2), falling to 60 per cent assuming a shallower final depth of 29.5 mag arcsec−2. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M⋆ ∼ 1011.5 M⊙). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterisation of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimised, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z < 0.2).

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Frequency of Tidal Features Correlates with Age and Internal Structure of Early-type Galaxies

Cited by 17 publications

References 80 publications

Evidence for Impact of Galaxy Mergers on Stellar Kinematics of Early-type Galaxies

Evidence for Impact of Galaxy Mergers on Stellar Kinematics of Early-type Galaxies

emerge: constraining merging probabilities and time-scales of close galaxy pairs

Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images

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