Galactic fountains and outflows in star-forming dwarf galaxies: interstellar medium expulsion and chemical enrichment

Melioli, C.; Brighenti, F.; D’Ercole, A.

doi:10.1093/mnras/stu2008

Cited by 21 publications

(15 citation statements)

References 76 publications

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“…These models were run either with higher or lower gas metallicity than the solar values 7 and with different SN distribution, considering both single and clustered SN explosions. We have found similar results between these tests, nearly independent of the metallicity (see, hoever, Melioli et al 2009Melioli et al , 2013Melioli et al , 2015 for a more detail study on the effects of metalicity in galactic and SB winds), which are also consistent with those presented above. Of course, the mass transfer rate from the disk to the halo is higher and, almost insensitive to the presence of the jet, reaches a maximum value of ∼ 170 M ⊙ yr −1 and a mean value of ∼ 90 M ⊙ yr −1 , resulting in a total mass exchange between the disk and the halo involving about 40% of the mass of the system.…”

Section: )supporting

confidence: 90%

Gas Outflows in Seyfert Galaxies: Effects of Star Formation Versus Agn Feedback

Melioli¹,

Pino²

2015

ApJ

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Large scale, weakly collimated outflows are very common in galaxies with large infrared luminosities. In complex systems in particular, where intense star formation (SF) coexists with an active galactic nucleus (AGN), it is not clear yet from observations whether the SF, the AGN, or both are driving these outflows. Accreting supermassive black holes (SMBHs) are expected to influence their host galaxies through kinetic and radiative feedback processes, but in a Seyfert galaxy where the energy emitted in the nuclear region is comparable to that of the body of the galaxy, it is possible that stellar activity is also playing a key role in these processes. In order to achieve a better understanding of the mechanisms driving the gas evolution specially at the nuclear regions of these galaxies, we have performed high-resolution three-dimensional hydrodynamical simulations with radiative cooling considering the feedback from both star formation regions including supernova (type I and II) explosions and an AGN jet emerging from the central region of the active spiral galaxy. We computed the gas mass lost by the system, separating the role of each of these injection energy sources on the galaxy evolution and found that at scales within one kiloparsec an outflow can be generally established considering intense nuclear star formation only. The jet alone is unable to drive a massive gas outflow, although it can sporadically drag and accelerate clumps of the underlying outflow to very high velocities.

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Section: )supporting

confidence: 90%

Gas Outflows in Seyfert Galaxies: Effects of Star Formation Versus Agn Feedback

Melioli¹,

Pino²

2015

ApJ

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“…Both the above-shown anisotropic metal outflows and turbulent distributions have been found by a wide range of hot halo observations involving mechanical AGN feedback (Section 2.3.3) and a diverse range of HD numerical studies and groups [207,[235][236][237][238][239][240]. We note that galactic SN-driven outflows, albeit weaker and difficult to spatially detect, can enhance the anisotropic enrichment, especially in low-mass halos (e.g., References [241,242]).…”

Section: High-resolution Hydrodynamical Simulations and Small-scale Astrophysicssupporting

confidence: 56%

The Metal Content of the Hot Atmospheres of Galaxy Groups

et al. 2021

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Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (107 K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA.

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“…Contrary to other proposed mechanisms such as galactic fountains, turbulence and accretion (cf. Tolstoy et al 2009;Melioli et al 2015, and references therein) this framework can explain the absence of significant metal abundance gradients throughout the dwarf galaxies, and represents our main current understanding of the ISM pollution.…”

Section: Potential Pollution By the Gc Windmentioning

confidence: 90%

Accretion of pristine gas and dilution during the formation of multiple-population globular clusters

D’Ercole

D’Antona

Vesperini

2016

Mon. Not. R. Astron. Soc.

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We study the interaction of the early spherical GC wind powered by Type II supernovae (SNe II) with the surrounding ambient medium consisting of the gaseous disk of a star forming galaxy at redshift z > ∼ 2. The bubble formed by the wind eventually breaks out of the disk, and most of the wind moves directly out of the galaxy and is definitively lost. The fraction of the wind moving nearly parallel to the galactic plane carves a hole in the disk which will contract after the end of the SN activity. During the interval of time between the end of the SN explosions and the "closure" of the hole, very O-poor stars (the Extreme population) can form out of the super-AGB (asymptotic giant branch) ejecta collected in the GC center. Once the hole contracts, the AGB ejecta mix with the pristine gas, allowing the formation of stars with an oxygen abundance intermediate between that of the very O-poor stars and that of the pristine gas. We show that this mechanism may explain why Extreme populations are present only in massive clusters, and can also produce a correlation between the spread in helium and the cluster mass.Finally, we also explore the possibility that our proposed mechanism can be extended to the case of multiple populations showing bimodality in the iron content, with the presence of two populations characterized by a small difference in [Fe/H]. Such a result can be obtained taking into account the contribution of delayed SN II.

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Galactic fountains and outflows in star-forming dwarf galaxies: interstellar medium expulsion and chemical enrichment

Cited by 21 publications

References 76 publications

Gas Outflows in Seyfert Galaxies: Effects of Star Formation Versus Agn Feedback

Gas Outflows in Seyfert Galaxies: Effects of Star Formation Versus Agn Feedback

The Metal Content of the Hot Atmospheres of Galaxy Groups

Accretion of pristine gas and dilution during the formation of multiple-population globular clusters

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