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    "info": {
        "author": "A3COSMOS Team",
        "author_email": "dzliu@mpe.mpg.de",
        "bugtrack_url": null,
        "classifiers": [
            "Development Status :: 4 - Beta",
            "Development Status :: 5 - Production/Stable",
            "Intended Audience :: Developers",
            "License :: OSI Approved :: ISC License (ISCL)",
            "Operating System :: OS Independent",
            "Programming Language :: Python",
            "Programming Language :: Python :: 2",
            "Programming Language :: Python :: 2.7",
            "Programming Language :: Python :: 3",
            "Programming Language :: Python :: 3.4",
            "Programming Language :: Python :: 3.5",
            "Programming Language :: Python :: 3.6",
            "Programming Language :: Python :: 3.7",
            "Programming Language :: Python :: 3.8",
            "Programming Language :: Python :: 3.9",
            "Programming Language :: Python :: Implementation",
            "Topic :: Scientific/Engineering :: Astronomy"
        ],
        "description": "######################\na3cosmos-gas-evolution\n######################\n\n***********************************************************************************\nA Python Package for Galaxy Cold Molecular Gas Mass and Depletion Time Calculation.\n***********************************************************************************\n\n\n\n\nA simple introduction:\n======================\n\nThis Python package provides functions to calculate a galaxy's cold molecular gas mass to stellar mass ratio (gas fraction), cold molecular gas depletion time and galaxy main-sequence star formation rate. \n\nThe motivation is that the evolution of star-forming galaxies' star formation rate (SFR) and cold molecular gas reservoir have now been reasonably well measured out to very high redshift (z~6), from present time up to as early as one giga-year after the Big Bang (Madau & Dickinson 2014; Genzel et al. 2015; Scoville et al. 2016, 2017; Tacconi et al. 2018; Liu et al. 2018, 2019). \nThese studies have found that the majority of galaxies have a steady and parametrizable evolution in their stellar mass growth, SFR, and molecular gas mass (or molecular gas to total baryon fraction, i.e., gas fraction). \nThese evolution functions have provided crucial constraints to cosmological simulations of dark matter halo evolution and the semi-analytic modeling of the simulated galaxy evolution in the dark matter halo (e.g., Popping et al. 2014ab, 2016, 2017, 2019ab). \nHowever, currently there are many parametrizations (or we say \"equations\") in the literature and each has its own limitation which is not very well aware by the generic users. \nTherefore, we provide this Python package which contains as many galaxy gas, dust, star formation and stellar mass evolution equations as possible for easier comparison and study. \n\n\n\n\nA simple usage:\n===============\n\nTo get cold molecular gas density evolution curve, e.g., Fig. 15 of `D. Liu et al. (2019b) <https://arxiv.org/abs/1910.12883>`__\n\n.. code-block:: python\n\n    import a3cosmos_gas_evolution\n    a3cosmos_gas_evolution.help()\n    z, rho_mol_gas = a3cosmos_gas_evolution.get_cosmic_mol_gas_density_A3COSMOS() # return rho_mol_gas in solar mass per cubic mega parsec.\n    z, rho_mol_gas = a3cosmos_gas_evolution.get_cosmic_mol_gas_density_Tacconi2018() # return rho_mol_gas in solar mass per cubic mega parsec.\n    z, rho_mol_gas = a3cosmos_gas_evolution.get_cosmic_mol_gas_density_Scoville2017() # return rho_mol_gas in solar mass per cubic mega parsec.\n    a3cosmos_gas_evolution.plot_cosmic_mol_gas_density() # or plot it with matplotlib\n\n\n\nTo compute gas fraction, i.e., ``M_molgas / (M_molgas + M_star)``\n\n.. code-block:: python\n\n    import a3cosmos_gas_evolution\n    a3cosmos_gas_evolution.help()\n    a3cosmos_gas_evolution.calc_gas_fraction_A3COSMOS(z = 3.0, lgMstar = 10.5, DeltaMS = 0.5) # or we can input cosmic_age = 2.178 instead of z = 3.0\n    a3cosmos_gas_evolution.calc_gas_fraction_Tacconi2018(z = 3.0, lgMstar = 10.5, DeltaMS = 0.5)\n    a3cosmos_gas_evolution.calc_gas_fraction_Scoville2017(z = 3.0, lgMstar = 10.5, DeltaMS = 0.5)\n\n\n\nTo compute gas depletion time, i.e., ``M_molgas / SFR``\n\n.. code-block:: python\n\n    import a3cosmos_gas_evolution\n    a3cosmos_gas_evolution.help()\n    a3cosmos_gas_evolution.calc_gas_depletion_time_A3COSMOS(z = 3.0, lgMstar = 10.5, DeltaMS = 0.0)\n    a3cosmos_gas_evolution.calc_gas_depletion_time_Tacconi2018(z = 3.0, lgMstar = 10.5, DeltaMS = 0.0)\n    a3cosmos_gas_evolution.calc_gas_depletion_time_Scoville2017(z = 3.0, lgMstar = 10.5, DeltaMS = 0.0)\n\n\n\nTo compute galaxy main-sequence star formation rate, i.e., ``SFR_MS``\n\n.. code-block:: python\n\n    import a3cosmos_gas_evolution\n    a3cosmos_gas_evolution.help()\n    a3cosmos_gas_evolution.calc_SFR_MS_Speagle2014(z = 3.0, lgMstar = 10.5)\n\n\n\n\nAcknowledgement:\n================\nPlease cite `Liu et al. (2019b) <https://arxiv.org/abs/1910.12883>`__ \nand/or \n`https://ascl.net/1910.003 <https://ascl.net/1910.003>`__\nif you would like to use this package for your research. Thank you. \n\n\n\n\n\n\n\n\n",
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        "keywords": "a3cosmos galaxy molecular gas dust star formation SFR evolution equation parametrization",
        "license": "BSD License",
        "maintainer": "A3COSMOS Team",
        "maintainer_email": "dzliu@mpe.mpg.de",
        "name": "a3cosmos-gas-evolution",
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