Bursting and quenching in satellite galaxies

Koutsouridou, Ioanna; Cattaneo, Andrea

doi:10.1093/mnras/stz2916

Cited by 11 publications

(12 citation statements)

References 123 publications

(189 reference statements)

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“…Here, Eq. (19) is incorporared into the GalICS 2.0 SAM (Cattaneo et al 2017;Koutsouridou & Cattaneo 2019). Hence, the values of f d used to compute B/T are those predicted by our SAM.…”

Section: Application To Samsmentioning

confidence: 99%

“…Besides the model for major mergers, the only other differences with the version of GalICS 2.0 described in Koutsouridou & Cattaneo (2019) are the model for disc instabilities and a detail in the calculation of disc sizes. Disc radii are important because compact discs are less stable (Sect.…”

Section: B/tmentioning

confidence: 99%

“…The effect is small for central galaxies, but it can be significant for satellites and is particularly strong in the central regions of groups and clusters, where the halo finder 6 may incorrectly assign to the host system particles that in reality belong to a subhalo. Koutsouridou & Cattaneo (2019) showed that this numerical effect causes the discs of satellite galaxies to shrink at pericentric passages. Discs regain their previous sizes after moving away from their orbital pericentres, but the temporary contraction affects their stability and drives the formation of 6 GalICS 2.0 uses a halo finder that is called HaloMaker (Tweed et al 2009) and is based on AdaptaHOP (Aubert et al 2004).…”

Section: B/tmentioning

confidence: 99%

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Bulge formation through disc instability

Devergne

Cattaneo

Bournaud

et al. 2020

A&A

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We use simulations to study the growth of a pseudobulge in an isolated thin exponential stellar disc embedded in a static spherical halo. We observe a transition from later to earlier morphological types and an increase in bar prominence for higher disc-to-halo mass ratios, for lower disc-to-halo size ratios, and for lower halo concentrations. We compute bulge-to-total stellar mass ratios B/T by fitting a two-component Sérsic-exponential surface-density distribution. The final B/T is strongly related to the disc’s fractional contribution fd to the total gravitational acceleration at the optical radius. The formula B/T = 0.5 fd1.8 fits the simulations to an accuracy of 30%, is consistent with observational measurements of B/T and fd as a function of luminosity, and reproduces the observed relation between B/T and stellar mass when incorporated into the GALICS 2.0 semi-analytic model of galaxy formation.

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“…Here, Eq. (19) is incorporared into the GalICS 2.0 SAM (Cattaneo et al 2017;Koutsouridou & Cattaneo 2019). Hence, the values of f d used to compute B/T are those predicted by our SAM.…”

Section: Application To Samsmentioning

confidence: 99%

Section: B/tmentioning

confidence: 99%

Section: B/tmentioning

confidence: 99%

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Bulge formation through disc instability

Devergne

Cattaneo

Bournaud

et al. 2020

A&A

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“…Peng et al (2015) highlight a key aspect of strangulation: the process happens slowly, with star formation using up the remaining gas, resulting in more metal rich galaxies. Koutsouridou & Cattaneo (2019) use differing timescales and metallicities to untangle the effects of strangulation, ram pressure stripping and tides on star formation in dwarf galaxies. Weak impacts from ram pressure stripping and tides will stop the infall of gas but not remove the gas already present in the galaxy, so star formation will continue (but decline), resulting in increasingly metal rich populations.…”

Section: The Evolution Of Dwarfsmentioning

confidence: 99%

Solo dwarfs IV: comparing and contrasting satellite and isolated dwarf galaxies in the Local Group

Higgs

McConnachie

2021

Monthly Notices of the Royal Astronomical Society

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We compare and contrast the stellar structures of isolated Local Group dwarf galaxies, as traced by their oldest stellar populations, with the satellite dwarf galaxies of the Milky Way and M 31. All Local Group dwarfs with Mv ≤ −6 and μo < 26.5 mags arcsec−2 are considered, taking advantage of measurements from surveys that use similar observations and analysis techniques. For the isolated dwarfs, we use the results from Solitary Local (Solo) Dwarf Galaxy Survey. We begin by confirming that the structural and dynamical properties of the two satellite populations are not obviously statistically different from each other, but we note that there many more satellites around M 31 than around the Milky Way down to equivalent magnitude and surface brightness limits. We find that dwarfs in close proximity to a massive galaxy generally show more scatter in their Kormendy relations than those in isolation. Specifically, isolated Local Group dwarf galaxies show a tighter trend of half-light radius versus magnitude than the satellite populations, and similar effects are also seen for related parameters. There appears to be a transition in the structural and dynamical properties of the dwarf galaxy population around ∼400 kpc from the Milky Way and M 31, such that the smallest, faintest, most circular dwarf galaxies are found closer than this separation. We discuss the impact of selection effects on our analysis, and we argue that our results point to the significance of tidal interactions on the population of systems within approximately 400 kpc from the MW and M 31.

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“…However, this scenario does not apply to all dwarf-central galaxy interactions. From the theory of galaxy formation and evolution we expect that changes on the mass of the central galaxy modify the efficiency that the gas ram pressure stripping process has on removing gas from the incoming satellites (Koutsouridou & Cattaneo 2019). This probably happened to the Milky Way -Andromeda galactic systems when transiting from a low-mass system with no warm-hot corona to the current situation with a well defined warm-hot CGM.…”

Section: The Origin Of Blue Streams: Insights From Theory Simulations...mentioning

confidence: 99%

Once in a blue stream: Detection of recent star formation in the NGC 7241 stellar stream with MEGARA

Martínez–Delgado¹,

Roca-Fàbrega²,

Paz³

et al. 2021

Preprint

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The census of stellar tidal streams around nearby massive galaxies has significantly grown from recent deep imaging of the low-surface brightness sky. In this work we study the striking case of a blue narrow stream with a possible globular clusterlike progenitor around the Milky Way-size galaxy NGC 7241 and its foreground dwarf companion. We present 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. Although our data suggest that this compact object in the stream is actually a foreground Milky Way halo star, we detect emission lines overlapping a less compact, bluer and fainter blob of the stream that is clearly visible in both ultra-violet and optical deep images. From its heliocentric systemic radial velocity derived from the [O ]𝜆5007Å lines (𝑉 syst = 1548.58±1.80 km s −1 ) and new UV and optical broad-band photometry, we conclude that this over-density 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 is between 6.4 × 10 6 M − 2.7 × 10 7 M , which is typical of a dwarf galaxy, but its mass could be substantially lower if the stream is on a very radial orbit. These estimates also suggest that this is one of the lowest mass streams detected so far beyond the Local Group. 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 suffering a star-formation burst comparable to those that have shaped the star-formation history of several Local Group dwarfs in the last few Gigayears.

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Bursting and quenching in satellite galaxies

Cited by 11 publications

References 123 publications

Bulge formation through disc instability

Bulge formation through disc instability

Solo dwarfs IV: comparing and contrasting satellite and isolated dwarf galaxies in the Local Group

Once in a blue stream: Detection of recent star formation in the NGC 7241 stellar stream with MEGARA

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