SIMULATION OF THE COSMIC EVOLUTION OF ATOMIC AND MOLECULAR HYDROGEN IN GALAXIES

By D. Obreschkow, Darren Croton, G. Lucia, S. Khochfar, Steve Rawlings. 2009

139 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/cb899285f4597e9dbeac98d8bb1fbe3e1f106fd5

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In Astronomy and Astrophysics

1. P. Hopkins
2. R. Dav'e
3. R. Somerville
4. L. Hernquist
5. Volker Springel
6. D. Narayanan
7. A. Dekel
8. T. Naab

In Statistical and Nonlinear Physics

1. R. Dav'e
2. R. Somerville
3. A. Benson
4. C. Baugh
5. Carlos S. Frenk
6. S. Oh
7. C. Lacey
8. G. Popping

Citations in the corpus

• Cold gas stripping in satellite galaxies: from pairs to clusters (2016, background): “…significantly and successful comparisons have been made between theory and observations for general gas properties using both semianalytic (e.g. Obreschkow et al. 2009; Power, Baugh & Lacey 2010; Lagos et al. 2014; Popping, Somerville & Trager 2014) and hydrodynamical simulations (e.g. Davé…”
• THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY (2010, methodology): “Comparison with Simulations Obreschkow et al. (2009) (hereafter O09) used the Millennium Simulation catalog, the De Lucia & Blaizot (2007) virtual catalog of galaxies, and a physicallymotivated prescription to assign realistic gas (HI, He and H2) masses at a range of redshifts.”
• Evolution of the atomic and molecular gas content of galaxies (2013, methodology): “Obreschkow et al. (2009b) estimate the CO luminosity (ranging from CO J=1-0 to CO J=10-9) of a galaxy from its gas temperature based on the SFR surface density or AGN bolometric luminosity under local thermodynamic equilibrium (i.e. a single gas phase).”
• A unified model for galactic discs: star formation, turbulence driving, and mass transport (2017, background): “…indicate regions of transport-driven versus feedback-driven turbulence; see the main text for details. this fraction on halo mass and redshift is highly complex and substantially uncertain (e.g. Obreschkow et al. 2009; Fu et al. 2010; Lagos et al. 2011; Krumholz & Dekel 2012; Forbes et al. 2014a).”
• Cool Gas in High-Redshift Galaxies (2013, methodology): “The molecular gas is affected in two ways by the CMB: First, the higher temperature of the CMB will lead to an increase of the line excitation, and thus the line luminosities (e.g., Obreschkow et al. 2009a, da Cunha et al. 2013).”
• Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “Nonetheless, SAMs and simulations can broadly reproduce H i mass functions and scaling relations (Davé et al. 2013, Duffy et al. 2012, Lagos et al. 2011a, Obreschkow et al. 2009, Popping et al. 2009, 2014b).”
• Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift (2017, methodology): “The evolution of the ISM mass density shown in Figure 14-Left is similar in magnitude to the theoretical predictions based on semi-analytic models by Obreschkow et al. (2009); Lagos et al. (2011); Sargent et al. (2013) (see Figure 12 in Carilli & Walter (2013)).”
• The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations (2013, background): “Obreschkow et al. (2009), Power et al. (2010), Cook et al. (2010) and Lagos et al. (2011) all present various independent SAMs that are broadly successful, though curiously they all tend to overpredict the observed HIMF by ∼ ×3 in the vicinity of MHI ∼ 10 8−9M⊙.”
• The CO-H2 Conversion Factor in Disc Galaxies and Mergers (2011, background): “Similarly, both semi-analytic models (Obreschkow et al. 2009; Obreschkow & Rawlings 2009), as well as full numerical solutions exist which model the effect of dissociating photons through models of galaxies (e.g. Pelupessyt al.”
• THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, background): “For the last step we have assumed that at high−z, MH2 ≫ MHI or equivalently that Mgas ≈ MH2 , as supported by both observational evidence (e.g., Daddi et al. 2010; Tacconi et al. 2010, Geach et al. 2011) and theoretical arguments (Blitz & Rosolowsky 2006; Bigiel et al. 2008, Obreschkow et al. 2009).”
• A COMPARISON OF METHODS FOR DETERMINING THE MOLECULAR CONTENT OF MODEL GALAXIES (2010, methodology): “Driven by these observations, analytic models (Blitz & Rosolowsky 2006; Krumholz et al. 2009c), semi-analytic models (Obreschkow & Rawlings 2009; Obreschkow et al. 2009; Fu et al. 2010; Dutton et al. 2010), and simulations (Pelupessy et al. 2006; Robertson & Kravtsov 2008; Pelupessy & Papadopoulos…”
• Molecular hydrogen abundances of galaxies in the EAGLE simulations (2015, methodology): “At z = 0, the H2 mass function has been measured by Keres et al. (2003) and Obreschkow et al. (2009a).”
• THE CLUSTERING CHARACTERISTICS OF H i-SELECTED GALAXIES FROM THE 40% ALFALFA SURVEY (2012, methodology): “Martin et al. (2010) took advantage of the Obreschkow et al. (2009) (hereafter O09) simulation, which assigned cold gas to galaxies from the De Lucia & Blaizot (2007) catalog of Millennium Simulation galaxies.”
• METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, background): “…rates of cosmological inflow of gas and stars (Section 2.1.1), Ṁ∗,form is the star formation rate (Section 2.1.2), R is the stellar return fraction, 2 Obreschkow et al. (2009) and Obreschkow & Rawlings (2009) also studied the H i to H2 transition in their semi-analytic models, but they included…”
• INTENSITY MAPPING WITH CARBON MONOXIDE EMISSION LINES AND THE REDSHIFTED 21 cm LINE (2011, methodology): “However, there is likely less dust in these high redshift star-forming regions than in their low redshift counterparts, and the dust helps shield CO from UV dissociating radiation (e.g. Obreschkow et al. 2009).”
• Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, methodology): “Recently, Obreschkow et al. (2009b) showed that by using a simple phenomenological model to calculate the luminosity of different CO transitions, which includes information about the ISM of galaxies, the CO(1 − 0) luminosity function of Fig.”
• Is there a "too big to fail" problem in the field? (2014, methodology): “Both the galactic VF and WF have been used extensively in the literature to testΛCDM on galactic scales (Obreschkow et al. 2009; Zavala et al. 2009; Zwaan et al. 2010; Papastergis et al. 2011; Trujillo-Gomez et al. 2011; Obreschkow et al. 2013; Schneider et al. 2014; Klypin et al. 2014).”