1106.3335
Oscillons after inflation
Amin, Easther, Finkel, Flauger, Hertzberg
* what's a oscillon? --- looks like a large soliton of a scalar field.
Oscillons are massive, long-lived, localized excitations of a scalar field. Inflation is followed by self-resonance, leading to copious oscillon generation and a lengthy period of oscillon domination. They are characterized by an inflaton potential which has a quadratic minimum. Includes both string monodromy models and class of supergravity scenarios, and is in good agreement with concordance cosmology. Assume inflaton is weakly coupled to other fields, so the oscillons are not so quickly drained (or its formation is not completely prevented). Oscillon-dominated universe has a greatly enhanced primordial power spectrum on very small scales relative to the quadratic potential--leading to novel gravitational effects.
* monodromy?
* if true, doesn't it mean that we can observe the small scale enhanced power spectrum? Or does this get efficiently erased by the radiation-domiated era?
1106.3337
Modeling the color magnitude relation for galaxy clusters
Jiminiz, Cora, Castelli, Bassino
* I thought I already read this one yesterday.
Investigate CMR in cluster galaxies. On the bright end, slight departure from CMR, can be explained by the influence of minor mergers.
* probably should explain how the minor mergers do this, in the abstract.
1104.3156
Galaxy Evolution in cosmological simulations with outflows II: Metallicities and gas fractions
Dave, Finlator, Oppenheimer
* I've read this one too
Use hydro sims to investigate inflows, SF, and outflows govern the gas and metal content of galaxies. Mass-metallicity relation reflects how the outflow rate varies with stellar mass (M*). Gas content is set by competition between inflow (impacted by wind recycling and preventive feedback), and gas consumption within the ISM (governed by SF law). Stochastic variations in the inflow rate move galaxies off the equilibrium M*-Z and Z*-fgas relations, correlated to SFR, and scatater is set by the timescale to re-equilibrate. Evolution is slow for 0<z<3. Gas fraction at a given M* slowly decrease with time because inflow diminishes faster than consumption, while metallicities slowly increase as infalling gas becomes more enriched. Observations better match momentum-driven wind scalings rather than constant wind speeds, but all models have too low gas fractions at low mass, and too high metallicities at high M*. mass-metallicity relation with SFR and environment reproduced well--indicates these are consequence of equilibrium and not feedback.
* well, maybe I hadn't read it yet.
* What is preventive feedback?
1106.3256
The mass-loss return from evoloved stars to the LMC V. The GRAMS carbon-star model grid
Srinivasan, Sargent, Meixner
* wait, I'm pretty sure I've read this one
* yup, I have.... or maybe just the first half?
* monodromy?
* if true, doesn't it mean that we can observe the small scale enhanced power spectrum? Or does this get efficiently erased by the radiation-domiated era?
1106.3337
Modeling the color magnitude relation for galaxy clusters
Jiminiz, Cora, Castelli, Bassino
* I thought I already read this one yesterday.
Investigate CMR in cluster galaxies. On the bright end, slight departure from CMR, can be explained by the influence of minor mergers.
* probably should explain how the minor mergers do this, in the abstract.
1104.3156
Galaxy Evolution in cosmological simulations with outflows II: Metallicities and gas fractions
Dave, Finlator, Oppenheimer
* I've read this one too
Use hydro sims to investigate inflows, SF, and outflows govern the gas and metal content of galaxies. Mass-metallicity relation reflects how the outflow rate varies with stellar mass (M*). Gas content is set by competition between inflow (impacted by wind recycling and preventive feedback), and gas consumption within the ISM (governed by SF law). Stochastic variations in the inflow rate move galaxies off the equilibrium M*-Z and Z*-fgas relations, correlated to SFR, and scatater is set by the timescale to re-equilibrate. Evolution is slow for 0<z<3. Gas fraction at a given M* slowly decrease with time because inflow diminishes faster than consumption, while metallicities slowly increase as infalling gas becomes more enriched. Observations better match momentum-driven wind scalings rather than constant wind speeds, but all models have too low gas fractions at low mass, and too high metallicities at high M*. mass-metallicity relation with SFR and environment reproduced well--indicates these are consequence of equilibrium and not feedback.
* well, maybe I hadn't read it yet.
* What is preventive feedback?
1106.3256
The mass-loss return from evoloved stars to the LMC V. The GRAMS carbon-star model grid
Srinivasan, Sargent, Meixner
* wait, I'm pretty sure I've read this one
* yup, I have.... or maybe just the first half?
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