RECORD
Star Formation Feedback and Metal Enrichment History Of The Intergalactic Medium
Cosmology and Nongalactic Astrophysics · Submitted 10 May 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that galactic superwind (GSW) feedback can transport metals to the IGM and that the properties of simulated metal absorbers match observations.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
Using hydrodynamic simulations we compute the metal enrichment history of the intergalactic medium (IGM). We show that galactic superwind (GSW) feedback can transport metals to the IGM and that the properties of simulated metal absorbers match observations. The distance of influence of GSW is typically limited to >0.5Mpc and within regions of overdensity >10. Most CIV and OVI absorbers are located within shocked regions of elevated temperature (T>2x10^4K), overdensity (>10), and metallicity ([-2.5,-0.5]). OVI absorbers have typically higher metallicity, lower density and higher temperature than CIV absorbers. For OVI absorbers collisional ionization dominates over the entire redshift range z=0-6, whereas for CIV absorbers the transition occurs at moderate redshift z~3 from collisionally dominated to photoionization dominated. We find that the observed column density distributions for CIV and OVI in the range log N cm^2=12-15 are reasonably reproduced by the simulations. The evolution of mass densities contained in CIV and OVI lines, Omega_CIV and Omega_OVI, is also in good agreement with observations, which shows a near constancy at low redshifts and an exponential drop beyond redshift z=3-4. For both CIV and OVI, most absorbers are transient and the amount of metals probed by CIV and OVI lines of column log N cm^2=12-15 is only ~2% of total metal density at any epoch. While gravitational shocks from large-scale structure formation dominate the energy budget (80-90%) for turning about 50% of IGM to the warm-hot intergalactic medium (WHIM) by z=0, GSW feedback shocks are energetically dominant over gravitational shocks at z > 1-2. Most of the so-called "missing metals" at z=2-3 are hidden in a warm-hot (T=10^{4.5-7}K) gaseous phase, heated up by GSW feedback shocks. Their mass distribution is broadly peaked at $\delta=1-10$ in the IGM, outside virialized halos.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Using hydrodynamic simulations we compute the metal enrichment history of the intergalactic medium (IGM). | method 0.60 | 0.96 | 0.04 | asserted 0.93 |
| s1 | We show that galactic superwind (GSW) feedback can transport metals to the IGM and that the properties of simulated metal absorbers match observations. | result 0.96 | 0.94 | 0.61 | asserted 1.00 |
| s2 | The distance of influence of GSW is typically limited to >0.5Mpc and within regions of overdensity >10. | result 1.00 | 0.86 | 0.09 | asserted 0.99 |
| s3 | Most CIV and OVI absorbers are located within shocked regions of elevated temperature (T>2x10^4K), overdensity (>10), and metallicity ([-2.5,-0.5]). | result 1.00 | 0.88 | 0.09 | asserted 1.00 |
| s4 | OVI absorbers have typically higher metallicity, lower density and higher temperature than CIV absorbers. | result 1.00 | 0.87 | 0.07 | asserted 1.00 |
| s5 | For OVI absorbers collisional ionization dominates over the entire redshift range z=0-6, whereas for CIV absorbers the transition occurs at moderate redshift z~3 from collisionally dominated to photoionization dominated. | result 0.99 | 0.88 | 0.09 | asserted 1.00 |
| s6 | We find that the observed column density distributions for CIV and OVI in the range log N cm^2=12-15 are reasonably reproduced by the simulations. | result 1.00 | 0.93 | 0.10 | asserted 0.85 |
| s7 | The evolution of mass densities contained in CIV and OVI lines, Omega_CIV and Omega_OVI, is also in good agreement with observations, which shows a near constancy at low redshifts and an exponential drop beyond redshift z=3-4. | result 1.00 | 0.91 | 0.13 | asserted 1.00 |
| s8 | For both CIV and OVI, most absorbers are transient and the amount of metals probed by CIV and OVI lines of column log N cm^2=12-15 is only ~2% of total metal density at any epoch. | result 0.99 | 0.96 | 0.12 | asserted 1.00 |
| s9 | While gravitational shocks from large-scale structure formation dominate the energy budget (80-90%) for turning about 50% of IGM to the warm-hot intergalactic medium (WHIM) by z=0, GSW feedback shocks are energetically dominant over gravitational shocks at z > 1-2. | result 0.97 | 0.86 | 0.15 | asserted 1.00 |
| s10 | Most of the so-called "missing metals" at z=2-3 are hidden in a warm-hot (T=10^{4.5-7}K) gaseous phase, heated up by GSW feedback shocks. | result 0.67 | 0.86 | 0.25 | asserted 1.00 |
| s11 | Their mass distribution is broadly peaked at $\delta=1-10$ in the IGM, outside virialized halos. | result 0.99 | 0.87 | 0.09 | asserted 1.00 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
Using hydrodynamic simulations we compute the metal enrichment history of the intergalactic medium (IGM). We show that galactic superwind (GSW) feedback can transport metals to the IGM and that the properties of simulated metal absorbers match observations. The distance of influence of GSW is typically limited to >0.5Mpc and within regions of overdensity >10. Most CIV and OVI absorbers are located within shocked regions of elevated temperature (T>2x10^4K), overdensity (>10), and metallicity ([-2.5,-0.5]). OVI absorbers have typically higher metallicity, lower density and higher temperature than CIV absorbers. For OVI absorbers collisional ionization dominates over the entire redshift range z=0-6, whereas for CIV absorbers the transition occurs at moderate redshift z~3 from collisionally dominated to photoionization dominated. We find that the observed column density distributions for CIV and OVI in the range log N cm^2=12-15 are reasonably reproduced by the simulations. The evolution of mass densities contained in CIV and OVI lines, Omega_CIV and Omega_OVI, is also in good agreement with observations, which shows a near constancy at low redshifts and an exponential drop beyond redshift z=3-4. For both CIV and OVI, most absorbers are transient and the amount of metals probed by CIV and OVI lines of column log N cm^2=12-15 is only ~2% of total metal density at any epoch. While gravitational shocks from large-scale structure formation dominate the energy budget (80-90%) for turning about 50% of IGM to the warm-hot intergalactic medium (WHIM) by z=0, GSW feedback shocks are energetically dominant over gravitational shocks at z > 1-2. Most of the so-called "missing metals" at z=2-3 are hidden in a warm-hot (T=10^{4.5-7}K) gaseous phase, heated up by GSW feedback shocks. Their mass distribution is broadly peaked at $\delta=1-10$ in the IGM, outside virialized halos.
Human review
References
How the literature uses it
5 arXiv papers cite this in 10 sentences
Papers citing it · 9 sentences without a confident label
Uses its data or values 1 paper
-
Both [ref] and [ref] find that the total amount of carbon in the IGM increases by a factor of $2.5$ to $3$ in this interval, while the fraction of carbon in the triply–ionized state only increases by a factor of $1.25$.
Delayed Enrichment by Unseen Galaxies: Explaining the Rapid Rise in IGM CIV Absorption from z = 6-5 · Existing Observations and Models · 0.92
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.