Real galaxy mergers from galaxy pair catalogues

Pfister, Hugo; Dotti, Massimo; Laigle, Clothilde; Dubois, Yohan; Volonteri, Marta

doi:10.1093/mnras/staa227

Cited by 8 publications

(4 citation statements)

References 68 publications

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“…Therefore, galaxy mergers that will happen in the future will most likely be gas-rich mergers 2 . To investigate which Choir group has conditions for galaxy mergers, we use approximated conditions from Pfister et al (2020) for the galaxy pair mergers. Utilizing the Horizon-AGN simulation, Pfister et al (2020) formulated a threshold on the projected distance d th and redshift difference ∆z th below which galaxy pairs are likely to merge.…”

Section: Choirs In Context Of Hickson Compact Groups and Their Evolutionmentioning

confidence: 99%

Environmental processing of galaxies in H i-rich groups

Džudžar

Kilborn

Sweet

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present and explore the resolved atomic hydrogen (H i) content of 13 H i-rich and late-type dominated groups denoted ‘Choirs’. We quantify the H i content of the Choir galaxies with respect to the median of the H i-mass fraction (f$_{\rm {{\small H\,{I}}}}$) of their grandparent Hipass sample. We find that the H i mass fraction of the Choir galaxies is dispersed around the Hipass median in the range -1.4≤Δf$_{\rm {{\small H\,{I}}}}\rm {[dex]}\le$0.7, from H i-excess to H i-deficient galaxy regime. The H i-excess/H i-deficient galaxies contain more/less than 2.5 times their expected H i content with respect to the Hipass median. We show and discuss that the environmental processing in Choirs occurs via tidal stripping and galaxy mergers. Our analysis suggests that tidal stripping contributes to the loss of the H i, while galaxy mergers contribute to the enhancement of the H i. Exploring the mid-infrared properties of Choir galaxies we find possible environmental processing in only nine Choir galaxies, which indicates that environmental processing is more perceptible in the H i content than the mid-infrared properties. Moreover, we find that environmental processing occurs in Choir groups regardless of their global environment, whether they are in isolation or in proximity to the denser structures, such as cosmic web filaments. We explore possible scenarios of the Choirs evolution, taking into account their H i content, velocity dispersion, crossing time and their global environment. We conclude that the most likely evolution for the majority of Choir groups is that they will become more compact as their members undergo multiple H i-rich mergers.

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Section: Choirs In Context Of Hickson Compact Groups and Their Evolutionmentioning

confidence: 99%

Environmental processing of galaxies in H i-rich groups

Džudžar

Kilborn

Sweet

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Training would of course have to be done on small-scale simulations (noncosmological, galactic and nuclear scale). For example, a first application of such techniques to galaxy dynamics is the morphological identification of merging versus isolated galaxies (Goulding et al 2018;Nevin et al 2019;Snyder et al 2019;Pfister et al 2020), which is becoming increasingly common in these years. An emulator of the "small-scale dynamics" could be then be designed by integrating the sub-grid model computed via neural networks within a large-scale simulation, using a zoomin simulation as intermediate step, to encapsulate their trends and results, and implant them in simulations of large cosmological volumes.…”

Section: New Methodologies: Artificial Intelligence Integrated With S...mentioning

confidence: 99%

Astrophysics with the Laser Interferometer Space Antenna

et al. 2023

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The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe.

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“…Training would of course have to be done on small-scale simulations (non-cosmological, galactic and nuclear scale). For example, a first application of such techniques to galaxy dynamics is the morphological identification of merging versus isolated galaxies (Goulding et al, 2018;Nevin et al, 2019;Snyder et al, 2019;Pfister et al, 2020), which is becoming increasingly common in these years. An emulator of the "small-scale dynamics" could be then be designed by integrating the sub-grid model computed via neural networks within a large-scale simulation, using a zoom-in simulation as intermediate step, to encapsulate their trends and results, and implant them in simulations of large cosmological volumes.…”

Section: New Methodologies: Artificial Intelligence Integrated With S...mentioning

confidence: 99%

Astrophysics with the Laser Interferometer Space Antenna

Amaro-Seoane¹,

Andrews²,

Sedda³

et al. 2022

Preprint

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AM CVn binaries consist of a WD accreting from a hydrogen-deficient star (or WD) companion (Warner, 1995;Solheim, 2010). In their formation history (Fig. 1.6 and Section 1.3.1.1), AM CVns form after at least one CE phase of their progenitor system. The current RLO is initiated, due to orbital damping caused by GW radiation, at orbital periods of typically 5−20 min (depending on the nature and the temperature of the companion star), and the mass-transfer rate is determined

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Real galaxy mergers from galaxy pair catalogues

Cited by 8 publications

References 68 publications

Environmental processing of galaxies in H i-rich groups

Environmental processing of galaxies in H i-rich groups

Astrophysics with the Laser Interferometer Space Antenna

Astrophysics with the Laser Interferometer Space Antenna

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