Quenching of satellite galaxies of Milky Way analogues: reconciling theory and observations

Font, Andreea S.; McCarthy, Ian G.; Belokurov, Vasily; Brown, S F; Stafford, Sam G.

doi:10.1093/mnras/stac183

Cited by 31 publications

(64 citation statements)

References 57 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using the ARTEMIS simulations, Font et al (2022) found a quiescent fraction similar to the LG and other simulations. They defined a galaxy as quiescent if its instantaneous specific star formation rate is zero at 𝑧 = 0, and they verified that this agrees with lookback time and time-averaged sSFR criteria.…”

Section: Comparison To Other Simulationssupporting

confidence: 74%

“…Our results on host mass effects generally agree with previous studies of simulations and observations that leverage larger samples of MW-mass hosts. Font et al (2022) found lower quiescent fractions of satellites (𝑀 * ≈ 10 6.5−9.5 M ) around less massive hosts in the ARTEMIS simulations (45 hosts with 8×10 11 < 𝑀 200m /M < 2 × 10 12 ). Carlsten et al (2022) also found a similar trend in observations where the overall quiescent fraction of satellites (𝑀 𝑉 < −9 mag, 𝑀 * 5 × 10 5 M ) increases with the luminosity of observed MW-like hosts (30 host galaxies with 𝑀 𝐾 𝑠 < −22.1 mag) in the Local Volume (𝐷 < 12 Mpc).…”

Section: Mw-mass Host Environmentmentioning

confidence: 72%

“…This difference in the quiescent fraction of satellites presents a unique tension, given that the host galaxies in SAGA are selected specifically to match the MW's stellar mass, and the number and radial distribution of satellites around SAGA hosts broadly agrees with LG satellites and zoom-in simulations of MW-mass galaxies (e.g., Samuel et al 2020;Font et al 2021). Furthermore, Font et al (2022) used the colors of satellites of MW-mass galaxies in the local Universe, which have been surveyed extensively (e.g., Karachentsev & Kudrya 2014;Müller et al 2015;Danieli et al 2017;Smercina et al 2018;Bennet et al 2019;Crnojević et al 2019;Müller et al 2019;Carlsten et al 2021Carlsten et al , 2022, to estimate their star-forming or quenched status and found broad agreement between the LG and the local Universe, extending the observational tension between the SAGA survey and and other MW-mass galaxies.…”

Section: Introductionmentioning

confidence: 94%

“…They defined a galaxy as quiescent if its instantaneous specific star formation rate is zero at 𝑧 = 0, and they verified that this agrees with lookback time and time-averaged sSFR criteria. However, Font et al (2022) also showed that by including a surface brightness limit (𝜇 𝑒,𝑟 ≈ 25 mag arcsec −2 ) in their comparisons to the SAGA survey, the ARTEMIS simulations can reproduce the quiescent fraction of satellites observed in SAGA. Therefore, they suggest that the reported tensions between simulations and SAGA exist because the simulations do not account for the potential implicit observational selection of higher surface brightness satellites in the SAGA survey.…”

Section: Comparison To Other Simulationsmentioning

confidence: 99%

“…The results of their observational analysis support the original SAGA quiescent fraction, but their simulation results are consistent with the LG, leading them to claim that there may be a physical difference in satellite evolution around SAGA hosts. Using the ARTEMIS simulations, Font et al (2022) showed that the inclusion of an observational selection function, or correction for the detectability of galaxies based on their surface brightness, has a significant effect on the measured quiescent fraction, which can account for differences between the LG and the SAGA survey. Moreover, the SAGA survey could also be including interlopers or non-satellites because of projection effects along the line of sight.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Extinguishing the FIRE: environmental quenching of satellite galaxies around Milky Way-mass hosts in simulations

Samuel,

Wetzel,

Santistevan

et al. 2022

Preprint

View full text Add to dashboard Cite

The star formation and gas content of satellite galaxies around the Milky Way (MW) and Andromeda (M31) are depleted relative to more isolated galaxies in the Local Group (LG) at fixed stellar mass. We explore the environmental regulation of gas content and quenching of star formation in 𝑧 = 0 galaxies at 𝑀 * = 10 5−10 M around 14 MW-mass hosts from the FIRE-2 simulations. Lower-mass satellites (𝑀 * 10 7 M ) are mostly quiescent and highermass satellites (𝑀 * 10 8 M ) are mostly star-forming, with intermediate-mass satellites (𝑀 * ≈ 10 7−8 M ) split roughly equally between quiescent and star-forming. Hosts with more gas in their circumgalactic medium have a higher quiescent fraction of massive satellites (𝑀 * = 10 8−9 M ). We find no significant dependence on isolated versus paired (LG-like) host environments, and the quiescent fractions of satellites around MW-mass and LMC-mass hosts from the FIRE-2 simulations are remarkably similar. Environmental effects that lead to quenching can also occur as preprocessing in low-mass groups prior to MW infall. Lower-mass satellites typically quenched before MW infall as central galaxies or rapidly during infall into a low-mass group or a MW-mass galaxy. Intermediate-to high-mass satellites usually require ≥ 1 − 2 pericentre passages (≈ 2.5 − 5 Gyr) within a MW-mass halo to quench. Most galaxies with 𝑀 * 10 6.5 M did not quench before falling into a host, indicating a possible upper mass limit for isolated quenching. The simulations are broadly consistent with the quiescent fractions of satellites observed in the LG and the SAGA survey, because the simulation average lies between them and the host-to-host scatter is large.

show abstract

Section: Comparison To Other Simulationssupporting

confidence: 74%

Section: Mw-mass Host Environmentmentioning

confidence: 72%

Section: Introductionmentioning

confidence: 94%

Section: Comparison To Other Simulationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Extinguishing the FIRE: environmental quenching of satellite galaxies around Milky Way-mass hosts in simulations

Samuel,

Wetzel,

Santistevan

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

Once in a blue stream

Martínez-Delgado,

Roca-Fàbrega,

Gil de Paz

et al. 2024

A&A

View full text Add to dashboard Cite

Aims. In this work we study the striking case of a narrow blue stream with a possible globular cluster-like progenitor around the NGC 7241 galaxy and its foreground dwarf companion. We want to figure out if the stream was generated by tidal interaction with NGC 7241 or if it first interacted with the foreground dwarf companion and later both fell together toward NGC 7241. Methods. We used four sets of observations, including a follow-up spectroscopic study of this stream based on data taken with the MEGARA instrument at the 10.4 m Gran Telescopio Canarias using the integral field spectroscopy mode, the Mount Lemmon 0.80 m telescope, the Telescopio Nazionale Galileo, the DESI Imaging Legacy surveys, and GALEX archival data. We also used high-resolution zoomed-in cosmological simulations. Results. Our data suggest that the compact object we detected in the stream is a foreground Milky Way halo star. Near this compact object we detect emission lines overlapping a less compact, bluer, and fainter blob of the stream that is clearly visible in both ultraviolet and optical deep images. From its heliocentric systemic radial velocity derived from the [O III]λ5007 Å lines (Vsyst = 1548.58 ± 1.80 km s−1) and new UV and optical broadband photometry, we conclude that this overdensity could be the actual core of the stream, with an absolute magnitude of Mg ∼ −10 and a g − r = 0.08 ± 0.11, consistent with a remnant of a low-mass dwarf satellite undergoing a current episode of star formation. From the width of the stream and assuming a circular orbit, we calculate that the progenitor mass can be typical of a dwarf galaxy, but it could also be substantially lower if the stream is on a very radial orbit or if it was created by tidal interaction with the companion dwarf instead of with NGC 7241. These estimates also suggest that this is one of the lowest mass streams detected to date beyond the Local Group. Finally, we find that blue stellar streams containing star formation regions are commonly predicted by high-resolution cosmological simulations of galaxies lighter than the Milky Way. This scenario is consistent with the processes explaining the bursty star formation history of some dwarf satellites, which are followed by a gas depletion and a fast quenching once they enter within the virial radius of their host galaxies for the first time. Thus, it is likely that the stream’s progenitor is undergoing a star formation burst comparable to those that have shaped the star formation history of several Local Group dwarfs in the last few gigayears.

show abstract

A search for stellar tidal streams around Milky Way analogues from the SAGA sample

Miro-Carretero

Martínez–Delgado

Farràs-Aloy

et al. 2023

A&A

View full text Add to dashboard Cite

Context. Stellar tidal streams are the result of tidal interactions between a central galaxy and lower mass systems such as satellite galaxies or globular clusters. For the Local Group, many diffuse substructures have been identified and their link to the galaxy evolution has been traced. However, it cannot simply be assumed that the Milky Way or M31 are representative of their galaxy class. Thus, a larger sample of analogue galaxies beyond the Local Group is required to bolster a broader generalisation of the underlying theory. Aims. We want to detect and photometrically characterise stellar streams around Milky Way (MW-) analogues in the local Universe in order to extend the observational evidence of interactions between this class of host galaxies and their satellites. This information will be applicable in a more general context around future studies on galaxy formation and evolution processes. Methods. In the present work, we identified and analysed stellar tidal streams around MW-analogue galaxies from the SAGA sample, using deep images of the DESI Legacy Imaging Surveys. For this sample, we obtained a range of r-band surface brightness limit between 27.8 and 29 mag arcsec −2 . We measured the surface brightness and colours of the detected streams using GNU Astronomy Utilities software. Results. We identified 16 new stellar tidal streams around MW-analogue galaxies at distances between 25 and 40 Mpc. In applying a statistical analysis to our findings for the SAGA II galaxy sample, we obtained a frequency of 12.2% ± 2.4% for these stellar streams. We measured the surface brightness and colours of the detected streams and carried out a comparison to the dwarf satellite galaxies population around galaxies belonging to the same SAGA sample. We show that the mean colour of the streams is 0.20 mag redder than that of the SAGA satellites; in addition, the streams are, on average, 0.057 ± 0.021 mag redder that their progenitor (for cases where a likely progenitor could be identified). Conclusions. The frequency of streams detected around MW-analogues in the Local Universe is in agreement with previous studies. The difference in colour between detected streams and satellites within the SAGA host galaxy sample could be explained by a combination of both selection biases in the SAGA study and physical processes.

show abstract

Quenching of satellite galaxies of Milky Way analogues: reconciling theory and observations

Cited by 31 publications

References 57 publications

Extinguishing the FIRE: environmental quenching of satellite galaxies around Milky Way-mass hosts in simulations

Extinguishing the FIRE: environmental quenching of satellite galaxies around Milky Way-mass hosts in simulations

Once in a blue stream

A search for stellar tidal streams around Milky Way analogues from the SAGA sample

Contact Info

Product

Resources

About