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Formation of Isolated Dwarf Galaxies with Feedback
Astrophysics of Galaxies · Submitted 10 Feb 2009
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that a combination of feedback and the cosmic UV background results in the formation of galaxies with properties similar to the Local Group dwarf spheroidals, and that their effect is strongly moderated by the depth of the gravitational potential.
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We present results of high resolution hydrodynamical simulations of the formation and evolution of dwarf galaxies. Our simulations start from cosmological initial conditions at high redshift. They include metal-dependent cooling, star formation, feedback from type II and type Ia supernovae and UV background radiation, with physical recipes identical to those applied in a previous study of Milky Way type galaxies. We find that a combination of feedback and the cosmic UV background results in the formation of galaxies with properties similar to the Local Group dwarf spheroidals, and that their effect is strongly moderated by the depth of the gravitational potential. Taking this into account, our models naturally reproduce the observed luminosities and metallicities. The final objects have halo masses between 2.3x10^8 and 1.1x10^9 solar masses, mean velocity dispersions between 6.5 and 9.7 kms-1, stellar masses ranging from 5x10^5 to 1.2x10^7 solar masses, median metallicities between [Fe/H] = -1.8 and -1.1, and half-light radii of the order of 200 to 300 pc, all comparable with Local Group dwarf spheroidals. Our simulations also indicate that the dwarf spheroidal galaxies observed today lie near a halo mass threshold around 10^9 solar masses, in agreement with stellar kinematic data, where supernova feedback not only suffices to completely expel the interstellar medium and leave the residual gas-free, but where the combination of feedback, UV radiation and self-shielding establishes a dichotomy of age distributions similar to that observed in the Milky Way and M31 satellites.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present results of high resolution hydrodynamical simulations of the formation and evolution of dwarf galaxies. | contribution 0.96 | 0.95 | 0.02 | asserted 0.91 |
| s1 | Our simulations start from cosmological initial conditions at high redshift. | method 1.00 | 0.83 | 0.01 | asserted 1.00 |
| s2 | They include metal-dependent cooling, star formation, feedback from type II and type Ia supernovae and UV background radiation, with physical recipes identical to those applied in a previous study of Milky Way type galaxies. | method 1.00 | 0.62 | 0.02 | asserted 0.99 |
| s3 | We find that a combination of feedback and the cosmic UV background results in the formation of galaxies with properties similar to the Local Group dwarf spheroidals, and that their effect is strongly moderated by the depth of the gravitational potential. | result 0.99 | 0.97 | 0.80 | asserted 1.00 |
| s4 | Taking this into account, our models naturally reproduce the observed luminosities and metallicities. | result 0.90 | 0.92 | 0.13 | asserted 1.00 |
| s5 | The final objects have halo masses between 2.3x10^8 and 1.1x10^9 solar masses, mean velocity dispersions between 6.5 and 9.7 kms-1, stellar masses ranging from 5x10^5 to 1.2x10^7 solar masses, median metallicities between [Fe/H] = -1.8 and -1.1, and half-light radii of the order of 200 to 300 pc, all comparable with Local Group dwarf spheroidals. | result 1.00 | 0.96 | 0.16 | asserted 1.00 |
| s6 | Our simulations also indicate that the dwarf spheroidal galaxies observed today lie near a halo mass threshold around 10^9 solar masses, in agreement with stellar kinematic data, where supernova feedback not only suffices to completely expel the interstellar medium and leave the residual gas-free, but where the combination of feedback, UV radiation and self-shielding establishes a dichotomy of age distributions similar to that observed in the Milky Way and M31 satellites. | result 0.85 | 0.92 | 0.31 | hedged possibility 0.90 |
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Original abstract
We present results of high resolution hydrodynamical simulations of the formation and evolution of dwarf galaxies. Our simulations start from cosmological initial conditions at high redshift. They include metal-dependent cooling, star formation, feedback from type II and type Ia supernovae and UV background radiation, with physical recipes identical to those applied in a previous study of Milky Way type galaxies. We find that a combination of feedback and the cosmic UV background results in the formation of galaxies with properties similar to the Local Group dwarf spheroidals, and that their effect is strongly moderated by the depth of the gravitational potential. Taking this into account, our models naturally reproduce the observed luminosities and metallicities. The final objects have halo masses between 2.3x10^8 and 1.1x10^9 solar masses, mean velocity dispersions between 6.5 and 9.7 kms-1, stellar masses ranging from 5x10^5 to 1.2x10^7 solar masses, median metallicities between [Fe/H] = -1.8 and -1.1, and half-light radii of the order of 200 to 300 pc, all comparable with Local Group dwarf spheroidals. Our simulations also indicate that the dwarf spheroidal galaxies observed today lie near a halo mass threshold around 10^9 solar masses, in agreement with stellar kinematic data, where supernova feedback not only suffices to completely expel the interstellar medium and leave the residual gas-free, but where the combination of feedback, UV radiation and self-shielding establishes a dichotomy of age distributions similar to that observed in the Milky Way and M31 satellites.
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5 arXiv papers cite this in 5 sentences
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Cites as support 1 paper
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Under the assumption, supported by observations [ref] , that at least some of the local Group dwarf spheroidals have evolved in isolation, these results suggest that supernova feedback is the key factor in determining their stellar evolution.
Life at the Periphery of the Local Group: the kinematics of the Tucana Dwarf Galaxy · The Importance of Feedback · 0.99
Cites as background 1 paper
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Examples of earlier numerical studies of the formation of dwarf galaxies include simulations by [ref] , [ref] , [ref] and [ref] .
A k-generalized statistical mechanics approach to income analysis · Introduction · 1.00
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