The PARADIGM project II : The lifetimes and quenching of satellites in Milky Way-mass haloes
(2025) In Monthly Notices of the Royal Astronomical Society 544(3). p.2811-2834- Abstract
The abundance and star formation histories of satellites of Milky Way (MW)-like galaxies are linked to their hosts' assembly histories. To explore this connection, we use the PARADIGM suite of zoom-in hydrodynamical simulations of MW-mass haloes, evolving the same initial conditions spanning various halo assembly histories with the VINTERGATAN and IllustrisTNG models. Our VINTERGATAN simulations overpredict the number of satellites compared to observations (and to IllustrisTNG) due to a higher at fixed. Despite this difference, the two models show good qualitative agreement for both satellite disruption fractions and time-scales, and quenching. The number of satellites rises rapidly until and then remains nearly constant. The fraction... (More)
The abundance and star formation histories of satellites of Milky Way (MW)-like galaxies are linked to their hosts' assembly histories. To explore this connection, we use the PARADIGM suite of zoom-in hydrodynamical simulations of MW-mass haloes, evolving the same initial conditions spanning various halo assembly histories with the VINTERGATAN and IllustrisTNG models. Our VINTERGATAN simulations overpredict the number of satellites compared to observations (and to IllustrisTNG) due to a higher at fixed. Despite this difference, the two models show good qualitative agreement for both satellite disruption fractions and time-scales, and quenching. The number of satellites rises rapidly until and then remains nearly constant. The fraction of satellites from each epoch that are disrupted by decreases steadily from nearly 100 per cent to 0 per cent during z>0.1$]]>. These fractions are higher for VINTERGATAN than IllustrisTNG, except for massive satellites (10^{7}{\rm M}_{\odot }$]]>) at 0.5$]]>. This difference is largely due to varying distributions of pericentric distance, orbital period, and number of orbits, in turn determined by which sub(haloes) are populated with galaxies by the two models. The time between accretion and disruption also remains approximately constant over z>0.3$]]> at Gyr. For surviving satellites at, both models recover the observed trend of 10^{7}{\rm M}_{\odot }$]]> satellites quenching more recently (<![CDATA[$ Gyr ago) and within of the host, while lower mass satellites quench earlier and often outside the host. Our results provide constraints on satellite accretion, quenching, and disruption time-scales while highlighting the convergent trends from two very different galaxy formation models.
(Less)
- author
- Joshi, Gandhali D. ; Pontzen, Andrew ; Agertz, Oscar LU ; Read, Justin and Rey, Martin P. LU
- organization
- publishing date
- 2025-12-01
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- galaxies: abundances, galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: interactions
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 544
- issue
- 3
- pages
- 24 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:105022622046
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/staf1871
- language
- English
- LU publication?
- yes
- additional info
- Publisher Copyright: © 2025 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.
- id
- 5ddd92cd-e181-4400-83ca-5e28411daf15
- date added to LUP
- 2026-01-16 14:05:37
- date last changed
- 2026-01-16 14:06:16
@article{5ddd92cd-e181-4400-83ca-5e28411daf15,
abstract = {{<p>The abundance and star formation histories of satellites of Milky Way (MW)-like galaxies are linked to their hosts' assembly histories. To explore this connection, we use the PARADIGM suite of zoom-in hydrodynamical simulations of MW-mass haloes, evolving the same initial conditions spanning various halo assembly histories with the VINTERGATAN and IllustrisTNG models. Our VINTERGATAN simulations overpredict the number of satellites compared to observations (and to IllustrisTNG) due to a higher at fixed. Despite this difference, the two models show good qualitative agreement for both satellite disruption fractions and time-scales, and quenching. The number of satellites rises rapidly until and then remains nearly constant. The fraction of satellites from each epoch that are disrupted by decreases steadily from nearly 100 per cent to 0 per cent during z>0.1$]]>. These fractions are higher for VINTERGATAN than IllustrisTNG, except for massive satellites (10^{7}{\rm M}_{\odot }$]]>) at 0.5$]]>. This difference is largely due to varying distributions of pericentric distance, orbital period, and number of orbits, in turn determined by which sub(haloes) are populated with galaxies by the two models. The time between accretion and disruption also remains approximately constant over z>0.3$]]> at Gyr. For surviving satellites at, both models recover the observed trend of 10^{7}{\rm M}_{\odot }$]]> satellites quenching more recently (<![CDATA[$ Gyr ago) and within of the host, while lower mass satellites quench earlier and often outside the host. Our results provide constraints on satellite accretion, quenching, and disruption time-scales while highlighting the convergent trends from two very different galaxy formation models.</p>}},
author = {{Joshi, Gandhali D. and Pontzen, Andrew and Agertz, Oscar and Read, Justin and Rey, Martin P.}},
issn = {{0035-8711}},
keywords = {{galaxies: abundances; galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: interactions}},
language = {{eng}},
month = {{12}},
number = {{3}},
pages = {{2811--2834}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{The PARADIGM project II : The lifetimes and quenching of satellites in Milky Way-mass haloes}},
url = {{http://dx.doi.org/10.1093/mnras/staf1871}},
doi = {{10.1093/mnras/staf1871}},
volume = {{544}},
year = {{2025}},
}