Matter

@misc{dickerson1976chemistry1,
    author = "Dickerson, R. E. and Geis, I",
    title = "Chemistry, Matter, and the Universe",
    year = "1976",
    howpublished = "Menlo Park, Ca., W.A. Benjamin",
    note = "talkorigins\_source = {true}; raw\_reference = {Dickerson, R. E., and Geis, I., 1976, Chemistry, Matter, and the Universe: Menlo Park, Ca., W.A. Benjamin.}"
}

@book{openalexw322605492,
    author = "Dickerson, Richard E. and Geis, Irving",
    title = "Chemistry, matter, and the universe: An integrated approach to general chemistry",
    year = "1976",
    journal = "Medical Entomology and Zoology",
    url = "https://openalex.org/W322605492",
    openalex = "W322605492"
}

The standard model of hot big-bang cosmology requires initial conditions which are problematic in two ways: (1) The early universe is assumed to be highly homogeneous, in spite of the fact that separated regions were causally disconnected (horizon problem); and (2) the initial value of the Hubble constant must be fine tuned to extraordinary accuracy to produce a universe as flat (i.e., near critical mass density) as the one we see today (flatness problem). These problems would disappear if, in its early history, the universe supercooled to temperatures 28 or more orders of magnitude below the critical temperature for some phase transition. A huge expansion factor would then result from a period of exponential growth, and the entropy of the universe would be multiplied by a huge factor when the latent heat is released. Such a scenario is completely natural in the context of grand unified models of elementary-particle interactions. In such models, the supercooling is also relevant to the problem of monopole suppression. Unfortunately, the scenario seems to lead to some unacceptable consequences, so modifications must be sought.

@article{doi101103physrevd23347,
    author = "Guth, Alan H.",
    title = "Inflationary universe: A possible solution to the horizon and flatness problems",
    year = "1981",
    journal = "Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields",
    abstract = "The standard model of hot big-bang cosmology requires initial conditions which are problematic in two ways: (1) The early universe is assumed to be highly homogeneous, in spite of the fact that separated regions were causally disconnected (horizon problem); and (2) the initial value of the Hubble constant must be fine tuned to extraordinary accuracy to produce a universe as flat (i.e., near critical mass density) as the one we see today (flatness problem). These problems would disappear if, in its early history, the universe supercooled to temperatures 28 or more orders of magnitude below the critical temperature for some phase transition. A huge expansion factor would then result from a period of exponential growth, and the entropy of the universe would be multiplied by a huge factor when the latent heat is released. Such a scenario is completely natural in the context of grand unified models of elementary-particle interactions. In such models, the supercooling is also relevant to the problem of monopole suppression. Unfortunately, the scenario seems to lead to some unacceptable consequences, so modifications must be sought.",
    url = "https://doi.org/10.1103/physrevd.23.347",
    doi = "10.1103/physrevd.23.347",
    openalex = "W2134251287",
    references = "doi1010160003491675902110, doi1010160016003274900623, doi1010160550321374904866, doi1010880305447098029, doi101103physrevd152929, doi101103physrevd161762, doi101103physrevd71888, doi101103physrevd93320, doi101103physrevlett32438, doi101103revmodphys51591"
}

The quantum state of a spatially closed universe can be described by a wave function which is a functional on the geometries of compact three-manifolds and on the values of the matter fields on these manifolds. The wave function obeys the Wheeler-DeWitt second-order functional differential equation. We put forward a proposal for the wave function of the "ground state" or state of minimum excitation: the ground-state amplitude for a three-geometry is given by a path integral over all compact positive-definite four-geometries which have the three-geometry as a boundary. The requirement that the Hamiltonian be Hermitian then defines the boundary conditions for the Wheeler-DeWitt equation and the spectrum of possible excited states. To illustrate the above, we calculate the ground and excited states in a simple minisuperspace model in which the scale factor is the only gravitational degree of freedom, a conformally invariant scalar field is the only matter degree of freedom and $\ensuremath{\Lambda}>0$. The ground state corresponds to de Sitter space in the classical limit. There are excited states which represent universes which expand from zero volume, reach a maximum size, and then recollapse but which have a finite (though very small) probability of tunneling through a potential barrier to a de Sitter-type state of continual expansion. The path-integral approach allows us to handle situations in which the topology of the three-manifold changes. We estimate the probability that the ground state in our minisuperspace model contains more than one connected component of the spacelike surface.

@article{doi101103physrevd282960,
    author = "Hartle, James B. and Hawking, S. W.",
    title = "Wave function of the Universe",
    year = "1983",
    journal = "Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields",
    abstract = {The quantum state of a spatially closed universe can be described by a wave function which is a functional on the geometries of compact three-manifolds and on the values of the matter fields on these manifolds. The wave function obeys the Wheeler-DeWitt second-order functional differential equation. We put forward a proposal for the wave function of the "ground state" or state of minimum excitation: the ground-state amplitude for a three-geometry is given by a path integral over all compact positive-definite four-geometries which have the three-geometry as a boundary. The requirement that the Hamiltonian be Hermitian then defines the boundary conditions for the Wheeler-DeWitt equation and the spectrum of possible excited states. To illustrate the above, we calculate the ground and excited states in a simple minisuperspace model in which the scale factor is the only gravitational degree of freedom, a conformally invariant scalar field is the only matter degree of freedom and $\ensuremath{\Lambda}>0$. The ground state corresponds to de Sitter space in the classical limit. There are excited states which represent universes which expand from zero volume, reach a maximum size, and then recollapse but which have a finite (though very small) probability of tunneling through a potential barrier to a de Sitter-type state of continual expansion. The path-integral approach allows us to handle situations in which the topology of the three-manifold changes. We estimate the probability that the ground state in our minisuperspace model contains more than one connected component of the spacelike surface.},
    url = "https://doi.org/10.1103/physrevd.28.2960",
    doi = "10.1103/physrevd.28.2960",
    openalex = "W2147762346",
    references = "doi101007354012291524, doi101007bf01626516, doi1010160370269382908668, doi101016055032137890161x, doi101049sqj19660063, doi101103physrev1601113, doi101103physrevd152929, doi101103physrevd272848, doi101103physrevlett281082, doi101103revmodphys20367"
}

We construct semi-analytic models for galaxy formation within the framework of a hierarchical clustering scenario for structure formation in the Universe. We use the algorithm of Kauffmann & White to generate ensembles of merging histories for present-day dark matter haloes with a wide range of circular velocities. A galaxy is assumed to form from gas which cools and turns into stars at the centre of a halo until that halo merges with a more massive object. At this time the galaxy loses its source of new gas and becomes a non-dominant object within a larger group or cluster. Our methods thus enable us to ‘look inside’ present dark matter haloes and investigate the formation, evolution and merging of the galaxies that they contain. We begin by investigating the properties of haloes with Vc = 220 km s–1, and use the observed properties of our Milky Way system to tune the free parameters that regulate star formation, hydrodynamic feedback from supernovae and the transformation of discs into spheroids by mergers. We then show that the same parameters lead to good agreement between the properties of galaxies in a Vc = 1000 km s–1 halo and observational data on the Virgo cluster of galaxies. This model correctly reproduces the observed trends in the luminosity, colour, gas content and morphology of galaxies. Turning to an investigation of the properties of the galaxy population as a whole, we highlight a problem that arises when applying this model to a ‘standard’ cold dark matter universe. If the zero-point of the Tully–Fisher relation is set by the properties of our Milky Way system, we find that standard CDM predicts too many haloes and results in a B-band luminosity density of the Universe that is a factor of 2 too high. The only apparent solution to this problem is to assume that many haloes remain observationally undetectable. We also compute the gas mass–luminosity relation for galaxies, the variation in galaxy morphology as a function of luminosity, star formation histories according to environment, the field galaxy luminosity function, and predictions for faint galaxy counts in the B and K bands. We conclude that, although it would be premature to attempt a detailed quantitative fit to specific cosmological models, the qualitative agreement between the data and the general picture that we present is already very encouraging.

@article{doi101093mnras2641201,
    author = "Kauffmann, Guinevere and White, Simon D. M. and Guiderdoni, B.",
    title = "The formation and evolution of galaxies within merging dark matter haloes*",
    year = "1993",
    journal = "Monthly Notices of the Royal Astronomical Society",
    abstract = "We construct semi-analytic models for galaxy formation within the framework of a hierarchical clustering scenario for structure formation in the Universe. We use the algorithm of Kauffmann \& White to generate ensembles of merging histories for present-day dark matter haloes with a wide range of circular velocities. A galaxy is assumed to form from gas which cools and turns into stars at the centre of a halo until that halo merges with a more massive object. At this time the galaxy loses its source of new gas and becomes a non-dominant object within a larger group or cluster. Our methods thus enable us to ‘look inside’ present dark matter haloes and investigate the formation, evolution and merging of the galaxies that they contain. We begin by investigating the properties of haloes with Vc = 220 km s–1, and use the observed properties of our Milky Way system to tune the free parameters that regulate star formation, hydrodynamic feedback from supernovae and the transformation of discs into spheroids by mergers. We then show that the same parameters lead to good agreement between the properties of galaxies in a Vc = 1000 km s–1 halo and observational data on the Virgo cluster of galaxies. This model correctly reproduces the observed trends in the luminosity, colour, gas content and morphology of galaxies. Turning to an investigation of the properties of the galaxy population as a whole, we highlight a problem that arises when applying this model to a ‘standard’ cold dark matter universe. If the zero-point of the Tully–Fisher relation is set by the properties of our Milky Way system, we find that standard CDM predicts too many haloes and results in a B-band luminosity density of the Universe that is a factor of 2 too high. The only apparent solution to this problem is to assume that many haloes remain observationally undetectable. We also compute the gas mass–luminosity relation for galaxies, the variation in galaxy morphology as a function of luminosity, star formation histories according to environment, the field galaxy luminosity function, and predictions for faint galaxy counts in the B and K bands. We conclude that, although it would be premature to attempt a detailed quantitative fit to specific cosmological models, the qualitative agreement between the data and the general picture that we present is already very encouraging.",
    url = "https://doi.org/10.1093/mnras/264.1.201",
    doi = "10.1093/mnras/264.1.201",
    openalex = "W2043685494"
}

We consider chaotic inflation in the theories with the effective potentials which at large $\ensuremath{\varphi}$ behave either as ${\ensuremath{\varphi}}^{n}$ or as ${e}^{\ensuremath{\alpha}\ensuremath{\varphi}}$. In such theories inflationary domains containing a sufficiently large and homogeneous scalar field $\ensuremath{\varphi}$ permanently produce new inflationary domains of a similar type. This process may occur at densities considerably smaller than the Planck density. Self-reproduction of inflationary domains is responsible for the fundamental stationarity which is present in many inflationary models: properties of the parts of the Universe formed in the process of self-reproduction do not depend on the time when this process occurs. We call this property of the inflationary Universe local stationarity. In addition to it, there may exist either a stationary distribution of probability ${P}_{c}$ to find a given field $\ensuremath{\varphi}$ at a given time at a given point, or a stationary distribution of probability ${P}_{p}$ to find a given field $\ensuremath{\varphi}$ at a given time in a given physical volume. If any of these distributions is stationary, we will be speaking of a global stationarity of the inflationary Universe. In all realistic inflationary models which are known to us the probability distribution ${P}_{c}$ is not stationary. On the other hand, investigation of the probability distribution ${P}_{p}$ describing a self-reproducing inflationary universe shows that the center of this distribution moves towards greater and greater $\ensuremath{\varphi}$ with increasing time. It is argued, however, that the probability of inflation (and of the self-reproduction of inflationary domains) becomes strongly suppressed when the energy density of the scalar field approaches the Planck density. As a result, the probability distribution ${P}_{p}$ rapidly approaches a stationary regime, which we have found explicitly for the theories $\frac{\ensuremath{\lambda}}{4}{\ensuremath{\varphi}}^{4}$ and ${e}^{\ensuremath{\alpha}\ensuremath{\varphi}}$. In this regime the relative fraction of the physical volume of the Universe in a state with given properties (with given values of fields, with a given density of matter, etc.) does not depend on time, both at the stage of inflation and after it. Each of the two types of stationarity mentioned above constitutes a significant deviation of inflationary cosmology from the standard big bang paradigm. We compare our approach with other approaches to quantum cosmology, and illustrate some of the general conclusions mentioned above with the results of a computer simulation of stochastic processes in the inflationary Universe.

@article{doi101103physrevd491783,
    author = "Linde, Andrei and Linde, Dmitri and Mezhlumian, Arthur",
    title = "From the big bang theory to the theory of a stationary universe",
    year = "1994",
    journal = "Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields",
    abstract = "We consider chaotic inflation in the theories with the effective potentials which at large $\ensuremath{\varphi}$ behave either as ${\ensuremath{\varphi}}^{n}$ or as ${e}^{\ensuremath{\alpha}\ensuremath{\varphi}}$. In such theories inflationary domains containing a sufficiently large and homogeneous scalar field $\ensuremath{\varphi}$ permanently produce new inflationary domains of a similar type. This process may occur at densities considerably smaller than the Planck density. Self-reproduction of inflationary domains is responsible for the fundamental stationarity which is present in many inflationary models: properties of the parts of the Universe formed in the process of self-reproduction do not depend on the time when this process occurs. We call this property of the inflationary Universe local stationarity. In addition to it, there may exist either a stationary distribution of probability ${P}\_{c}$ to find a given field $\ensuremath{\varphi}$ at a given time at a given point, or a stationary distribution of probability ${P}\_{p}$ to find a given field $\ensuremath{\varphi}$ at a given time in a given physical volume. If any of these distributions is stationary, we will be speaking of a global stationarity of the inflationary Universe. In all realistic inflationary models which are known to us the probability distribution ${P}\_{c}$ is not stationary. On the other hand, investigation of the probability distribution ${P}\_{p}$ describing a self-reproducing inflationary universe shows that the center of this distribution moves towards greater and greater $\ensuremath{\varphi}$ with increasing time. It is argued, however, that the probability of inflation (and of the self-reproduction of inflationary domains) becomes strongly suppressed when the energy density of the scalar field approaches the Planck density. As a result, the probability distribution ${P}\_{p}$ rapidly approaches a stationary regime, which we have found explicitly for the theories $\frac{\ensuremath{\lambda}}{4}{\ensuremath{\varphi}}^{4}$ and ${e}^{\ensuremath{\alpha}\ensuremath{\varphi}}$. In this regime the relative fraction of the physical volume of the Universe in a state with given properties (with given values of fields, with a given density of matter, etc.) does not depend on time, both at the stage of inflation and after it. Each of the two types of stationarity mentioned above constitutes a significant deviation of inflationary cosmology from the standard big bang paradigm. We compare our approach with other approaches to quantum cosmology, and illustrate some of the general conclusions mentioned above with the results of a computer simulation of stochastic processes in the inflationary Universe.",
    url = "https://doi.org/10.1103/physrevd.49.1783",
    doi = "10.1103/physrevd.49.1783",
    openalex = "W2148968450"
}

We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 z 0.62. The luminosity distances of these objects are determined by methods that employ relations between SN Ia luminosity and light curve shape. Combined with previous data from our High-z Supernova Search Team and recent results by Riess et al., this expanded set of 16 high-redshift M \ 1) methods. We estimate the dynamical age of the universe to be 14.2 ^1.7 Gyr including systematic uncertainties in the current Cepheid distance scale. We estimate the likely e ect of several sources of systematic error, including progenitor and metallicity evolution, extinction, sample selection bias, local perturbations in the expansion rate, gravitational lensing, and sample contamination. Presently, none of these e ects appear to reconcile the data with and) " \ 0 q 0 0.

@article{doi101086300499,
    author = "Riess, Adam G. and Filippenko, A. V. and Challis, P. and Clocchiatti, A. and Diercks, Alan H. and Garnavich, P. and Gilliland, Ron and Hogan, Craig J. and Jha, Saurabh W. and Kirshner, R. and Leibundgut, B. and Phillips, M. M. and Reiss, David J. and Schmidt, B. and Schommer, R. A. and Smith, R. Chris and Spyromilio, J. and Stubbs, C. W. and Suntzeff, N. B. and Tonry, J.",
    title = "Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant",
    year = "1998",
    journal = "The Astronomical Journal",
    abstract = {We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 z 0.62. The luminosity distances of these objects are determined by methods that employ relations between SN Ia luminosity and light curve shape. Combined with previous data from our High-z Supernova Search Team and recent results by Riess et al., this expanded set of 16 high-redshift M \ 1) methods. We estimate the dynamical age of the universe to be 14.2 ^1.7 Gyr including systematic uncertainties in the current Cepheid distance scale. We estimate the likely e ect of several sources of systematic error, including progenitor and metallicity evolution, extinction, sample selection bias, local perturbations in the expansion rate, gravitational lensing, and sample contamination. Presently, none of these e ects appear to reconcile the data with and) " \ 0 q 0 0.},
    url = "https://doi.org/10.1086/300499",
    doi = "10.1086/300499",
    openalex = "W2073832139"
}

We provide scaling relations and tting formulae for adiabatic cold dark matter cosmologies that account for all baryon e ects in the matter transfer function to better than 10% in the large-scale structure regime. They are based upon a physically well-motivated separation of the e ects of acoustic oscillations, Compton drag, velocity overshoot, baryon infall, adiabatic damping, Silk damping, and cold dark matter growth suppression. We also nd a simpler, more accurate, and better motivated form for the zero-baryon transfer function than previous works. These descriptions are employed to quantify the amplitude and location of baryonic features in linear theory. While baryonic oscillations are prominent if the baryon fraction the main e ect in more conventional cosmologies is a sharp

@article{doi101086305424,
    author = "Eisenstein, Daniel J. and Hu, Wayne",
    title = "Baryonic Features in the Matter Transfer Function",
    year = "1998",
    journal = "The Astrophysical Journal",
    abstract = "We provide scaling relations and tting formulae for adiabatic cold dark matter cosmologies that account for all baryon e ects in the matter transfer function to better than 10\% in the large-scale structure regime. They are based upon a physically well-motivated separation of the e ects of acoustic oscillations, Compton drag, velocity overshoot, baryon infall, adiabatic damping, Silk damping, and cold dark matter growth suppression. We also nd a simpler, more accurate, and better motivated form for the zero-baryon transfer function than previous works. These descriptions are employed to quantify the amplitude and location of baryonic features in linear theory. While baryonic oscillations are prominent if the baryon fraction the main e ect in more conventional cosmologies is a sharp",
    url = "https://doi.org/10.1086/305424",
    doi = "10.1086/305424",
    openalex = "W2169866137",
    references = "doi101007bf00653471"
}

The High-Z Supernova Search is an international collaboration to discover and monitor type Ia supernovae (SN Ia) at $z > 0.2$ with the aim of measuring cosmic deceleration and global curvature. Our collaboration has pursued a basic understanding of supernovae in the nearby Universe, discovering and observing a large sample of objects, and developing methods to measure accurate distances with SN Ia. This paper describes the extension of this program to $z \\geq 0.2$, outlining our search techniques and follow-up program. We have devised high-throughput filters which provide accurate two-color restframe $B$ and $V$ light curves of SN Ia, enabling us to produce precise, extinction-corrected luminosity distances in the range $0.25 < z < 0.55$. Sources of systematic error from K-corrections, extinction, selection effects, and evolution are investigated, and their effects estimated. We present photometric and spectral observations of SN 1995K, our program's first supernova, and use the data to obtain a precise measurement of the luminosity distance to the $z=0.479$ host galaxy. This object, when combined with a nearby sample of SN, yields an estimate for the matter density of the Universe of $\\Omega_M = -0.2^{+1.0}_{-0.8}$ if $\\Omega_\\Lambda = 0$. For a spatially flat universe composed of normal matter and a cosmological constant, we find $\\Omega_M = 0.4^{+0.5}_{-0.4}$, $\\Omega_\\Lambda = 0.6^{+0.4}_{-0.5}$. We demonstrate that with a sample of $\\sim 30$ objects, we should be able to determine relative luminosity distances over the range $0 < z< 0.5$ with sufficient precision to measure $\\Omega_M$ with an uncertainty of $\\pm 0.2$.

@article{doi101086306308,
    author = "Schmidt, B. and Suntzeff, N. B. and Phillips, M. M. and Schommer, R. A. and Clocchiatti, A. and Kirshner, R. and Garnavich, P. and Challis, P. and Leibundgut, B. and Spyromilio, J. and Riess, Adam G. and Filippenko, A. V. and Hamuy, M. and Smith, R. Chris and Hogan, Craig J. and Stubbs, C. W. and Diercks, Alan H. and Reiss, David J. and Gilliland, Ron and Tonry, J. and Maza, J. and Dressler, Alan and Walsh, J. R. and Ciardullo, Robin",
    title = "The High‐Z Supernova Search: Measuring Cosmic Deceleration and Global Curvature of the Universe Using Type Ia Supernovae",
    year = "1998",
    journal = "The Astrophysical Journal",
    abstract = "The High-Z Supernova Search is an international collaboration to discover and monitor type Ia supernovae (SN Ia) at $z > 0.2$ with the aim of measuring cosmic deceleration and global curvature. Our collaboration has pursued a basic understanding of supernovae in the nearby Universe, discovering and observing a large sample of objects, and developing methods to measure accurate distances with SN Ia. This paper describes the extension of this program to $z \\geq 0.2$, outlining our search techniques and follow-up program. We have devised high-throughput filters which provide accurate two-color restframe $B$ and $V$ light curves of SN Ia, enabling us to produce precise, extinction-corrected luminosity distances in the range $0.25 < z < 0.55$. Sources of systematic error from K-corrections, extinction, selection effects, and evolution are investigated, and their effects estimated. We present photometric and spectral observations of SN 1995K, our program's first supernova, and use the data to obtain a precise measurement of the luminosity distance to the $z=0.479$ host galaxy. This object, when combined with a nearby sample of SN, yields an estimate for the matter density of the Universe of $\\Omega\_M = -0.2^{+1.0}\_{-0.8}$ if $\\Omega\_\\Lambda = 0$. For a spatially flat universe composed of normal matter and a cosmological constant, we find $\\Omega\_M = 0.4^{+0.5}\_{-0.4}$, $\\Omega\_\\Lambda = 0.6^{+0.4}\_{-0.5}$. We demonstrate that with a sample of $\\sim 30$ objects, we should be able to determine relative luminosity distances over the range $0 < z< 0.5$ with sufficient precision to measure $\\Omega\_M$ with an uncertainty of $\\pm 0.2$.",
    url = "https://doi.org/10.1086/306308",
    doi = "10.1086/306308",
    openalex = "W2146293885",
    references = "doi101086147041, doi101112plmss242190, doi105860choice311499"
}

The chemistry of deuterium, as well as that of hydrogen and helium, in the postrecombination era of the expanding early universe is presented. A thorough survey of all potentially important gas-phase reactions involving the primordial elements produced in the Big Bang, with a particular emphasis on deuterium, is given. The reaction set, consisting of 144 processes, is used in a nonequilibrium chemistry model to follow the production of primordial molecules in the postrecombination era. It is found that significant deuterium fractionation occurs for HD+, HD, and H2D+, while the abundance of D+ is reduced compared to the proton abundance. Even with the enhanced fractionation of H2D+, its abundance is predicted to be too small to cause any interesting cosmological consequences, such as possible attenuation of spatial anisotropies in the cosmic background radiation held, detections of the epochs of reionization and reheating, or constraints on the primordial deuterium abundance. HD, being the second most abundant primordial molecule after H-2, may play a role in subsequent structure formation because of its cooling radiation.

@article{doi101086306473,
    author = "Stancil, P. C. and Lepp, S. and Dalgarno, A.",
    title = "The Deuterium Chemistry of the Early Universe",
    year = "1998",
    journal = "The Astrophysical Journal",
    abstract = "The chemistry of deuterium, as well as that of hydrogen and helium, in the postrecombination era of the expanding early universe is presented. A thorough survey of all potentially important gas-phase reactions involving the primordial elements produced in the Big Bang, with a particular emphasis on deuterium, is given. The reaction set, consisting of 144 processes, is used in a nonequilibrium chemistry model to follow the production of primordial molecules in the postrecombination era. It is found that significant deuterium fractionation occurs for HD+, HD, and H2D+, while the abundance of D+ is reduced compared to the proton abundance. Even with the enhanced fractionation of H2D+, its abundance is predicted to be too small to cause any interesting cosmological consequences, such as possible attenuation of spatial anisotropies in the cosmic background radiation held, detections of the epochs of reionization and reheating, or constraints on the primordial deuterium abundance. HD, being the second most abundant primordial molecule after H-2, may play a role in subsequent structure formation because of its cooling radiation.",
    url = "https://doi.org/10.1086/306473",
    doi = "10.1086/306473",
    openalex = "W1982817066"
}

The bulk of recent cosmological research has focused on the adiabatic cold dark matter model and its simple extensions. Here we present an accurate tting formula that describes the matter transfer functions of all common variants, including mixed dark matter models. The result is a function of wavenumber, time, and six cosmological parameters: the massive neutrino density, number of neutrino species degenerate in mass, baryon density, Hubble constant, cosmological constant, and spatial curvature. We show how observational constraints|e.g. the shape of the power spectrum, the abundance of clusters and damped Ly systems, and the properties of the Ly forest|can be extended to a wide range of cosmologies, including variations in the neutrino and baryon fractions in both high-density and low-density universes. Subject headings: cosmology: theory {dark matter {large-scale structure of the universe 1.

@article{doi101086306640,
    author = "Eisenstein, Daniel J. and Hu, Wayne",
    title = "Power Spectra for Cold Dark Matter and Its Variants",
    year = "1999",
    journal = "The Astrophysical Journal",
    abstract = "The bulk of recent cosmological research has focused on the adiabatic cold dark matter model and its simple extensions. Here we present an accurate tting formula that describes the matter transfer functions of all common variants, including mixed dark matter models. The result is a function of wavenumber, time, and six cosmological parameters: the massive neutrino density, number of neutrino species degenerate in mass, baryon density, Hubble constant, cosmological constant, and spatial curvature. We show how observational constraints|e.g. the shape of the power spectrum, the abundance of clusters and damped Ly systems, and the properties of the Ly forest|can be extended to a wide range of cosmologies, including variations in the neutrino and baryon fractions in both high-density and low-density universes. Subject headings: cosmology: theory (dark matter (large-scale structure of the universe 1.",
    url = "https://doi.org/10.1086/306640",
    doi = "10.1086/306640",
    openalex = "W2134287871"
}

We use numerical simulations to examine the substructure within galactic and cluster mass halos that form within a hierarchical universe. Clusters are easily reproduced with a steep mass spectrum of thousands of substructure clumps that closely matches observations. However, the survival of dark matter substructure also occurs on galactic scales, leading to the remarkable result that galaxy halos appear as scaled versions of galaxy clusters. The model predicts that the virialised extent of the Milky Way's halo should contain about 500 satellites with circular velocities larger than Draco and Ursa-Minor i.e. bound masses > 10^8Mo and tidally limited sizes > kpc. The substructure clumps are on orbits that take a large fraction of them through the stellar disk leading to significant resonant and impulsive heating. Their abundance and singular density profiles has important implications for the existence of old thin disks, cold stellar streams, gravitational lensing and indirect/direct detection experiments.

@article{doi101086312287,
    author = "Moore, Ben and Ghigna, Sebastiano and Governato, Fabio and Lake, George and Quinn, Thomas and Stadel, Joachim and Tozzi, P.",
    title = "Dark Matter Substructure within Galactic Halos",
    year = "1999",
    journal = "The Astrophysical Journal",
    abstract = "We use numerical simulations to examine the substructure within galactic and cluster mass halos that form within a hierarchical universe. Clusters are easily reproduced with a steep mass spectrum of thousands of substructure clumps that closely matches observations. However, the survival of dark matter substructure also occurs on galactic scales, leading to the remarkable result that galaxy halos appear as scaled versions of galaxy clusters. The model predicts that the virialised extent of the Milky Way's halo should contain about 500 satellites with circular velocities larger than Draco and Ursa-Minor i.e. bound masses > 10^8Mo and tidally limited sizes > kpc. The substructure clumps are on orbits that take a large fraction of them through the stellar disk leading to significant resonant and impulsive heating. Their abundance and singular density profiles has important implications for the existence of old thin disks, cold stellar streams, gravitational lensing and indirect/direct detection experiments.",
    url = "https://doi.org/10.1086/312287",
    doi = "10.1086/312287",
    openalex = "W2010581546"
}

Most of the information about the environment of the early Universe comes to us from radiation emitted from atoms and molecules. An understanding of the relevant atomic and molecular processes is needed to correctly interpret this radiation. Atomic and molecular process also control the evolution of the early Universe. In this paper, we review the atomic and molecular processes that are important in the early Universe.

@article{doi101088095340753510201,
    author = "Lepp, S. and Stancil, P. C. and Dalgarno, A.",
    title = "Atomic and molecular processes in the early Universe",
    year = "2002",
    journal = "Journal of Physics B Atomic Molecular and Optical Physics",
    abstract = "Most of the information about the environment of the early Universe comes to us from radiation emitted from atoms and molecules. An understanding of the relevant atomic and molecular processes is needed to correctly interpret this radiation. Atomic and molecular process also control the evolution of the early Universe. In this paper, we review the atomic and molecular processes that are important in the early Universe.",
    url = "https://doi.org/10.1088/0953-4075/35/10/201",
    doi = "10.1088/0953-4075/35/10/201",
    openalex = "W2170019704"
}

We consider the scenario emerging from the dynamics of a generalized Born-Infeld theory. The equation of state describing this system is given in terms of the energy density $\ensuremath{\rho}$ and pressure p by the relationship $p=\ensuremath{-}A/{\ensuremath{\rho}}^{\ensuremath{\alpha}},$ where A is a positive constant and $0<\ensuremath{\alpha}<~1.$ We discuss the conditions under which homogeneity arises and show that this equation of state describes the evolution of a universe evolving from a phase dominated by nonrelativistic matter to a phase dominated by a cosmological constant via an intermediate period where the effective equation of state is given by $p=\ensuremath{\alpha}\ensuremath{\rho}.$

@article{doi101103physrevd66043507,
    author = "Bento, M. C. and Bertolami, Orfeu and Sen, Anjan A.",
    title = "Generalized Chaplygin gas, accelerated expansion, and dark-energy-matter unification",
    year = "2002",
    journal = "Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields",
    abstract = "We consider the scenario emerging from the dynamics of a generalized Born-Infeld theory. The equation of state describing this system is given in terms of the energy density $\ensuremath{\rho}$ and pressure p by the relationship $p=\ensuremath{-}A/{\ensuremath{\rho}}^{\ensuremath{\alpha}},$ where A is a positive constant and $0<\ensuremath{\alpha}<\textasciitilde 1.$ We discuss the conditions under which homogeneity arises and show that this equation of state describes the evolution of a universe evolving from a phase dominated by nonrelativistic matter to a phase dominated by a cosmological constant via an intermediate period where the effective equation of state is given by $p=\ensuremath{\alpha}\ensuremath{\rho}.$",
    url = "https://doi.org/10.1103/physrevd.66.043507",
    doi = "10.1103/physrevd.66.043507",
    openalex = "W2108313227",
    references = "doi105860choice311499"
}

We describe results from a fully self-consistent three-dimensional hydrodynamical simulation of the formation of one of the first stars in the Universe. In current models of structure formation, dark matter initially dominates, and pregalactic objects form because of gravitational instability from small initial density perturbations. As they assemble via hierarchical merging, primordial gas cools through ro-vibrational lines of hydrogen molecules and sinks to the center of the dark matter potential well. The high-redshift analog of a molecular cloud is formed. As the dense, central parts of the cold gas cloud become self-gravitating, a dense core of approximately 100 M (where M is the mass of the Sun) undergoes rapid contraction. At particle number densities greater than 10(9) per cubic centimeter, a 1 M protostellar core becomes fully molecular as a result of three-body H2 formation. Contrary to analytical expectations, this process does not lead to renewed fragmentation and only one star is formed. The calculation is stopped when optical depth effects become important, leaving the final mass of the fully formed star somewhat uncertain. At this stage the protostar is accreting material very rapidly (approximately 10(-2) M year-1). Radiative feedback from the star will not only halt its growth but also inhibit the formation of other stars in the same pregalactic object (at least until the first star ends its life, presumably as a supernova). We conclude that at most one massive (M 1 M) metal-free star forms per pregalactic halo, consistent with recent abundance measurements of metal-poor galactic halo stars.

@article{doi101126science1063991,
    author = "Abel, Tom and Bryan, Greg L. and Norman, Michael L.",
    title = "The Formation of the First Star in the Universe",
    year = "2002",
    journal = "Science",
    abstract = "We describe results from a fully self-consistent three-dimensional hydrodynamical simulation of the formation of one of the first stars in the Universe. In current models of structure formation, dark matter initially dominates, and pregalactic objects form because of gravitational instability from small initial density perturbations. As they assemble via hierarchical merging, primordial gas cools through ro-vibrational lines of hydrogen molecules and sinks to the center of the dark matter potential well. The high-redshift analog of a molecular cloud is formed. As the dense, central parts of the cold gas cloud become self-gravitating, a dense core of approximately 100 M (where M is the mass of the Sun) undergoes rapid contraction. At particle number densities greater than 10(9) per cubic centimeter, a 1 M protostellar core becomes fully molecular as a result of three-body H2 formation. Contrary to analytical expectations, this process does not lead to renewed fragmentation and only one star is formed. The calculation is stopped when optical depth effects become important, leaving the final mass of the fully formed star somewhat uncertain. At this stage the protostar is accreting material very rapidly (approximately 10(-2) M year-1). Radiative feedback from the star will not only halt its growth but also inhibit the formation of other stars in the same pregalactic object (at least until the first star ends its life, presumably as a supernova). We conclude that at most one massive (M 1 M) metal-free star forms per pregalactic halo, consistent with recent abundance measurements of metal-poor galactic halo stars.",
    url = "https://doi.org/10.1126/science.1063991",
    doi = "10.1126/science.1063991",
    openalex = "W2040912209",
    references = "doi1010160021999184901426, doi101086148317, doi101086177793, doi101086191681, doi101086303434, doi101086306832, doi101086310975, doi101093mnras1163351, doi101146annurevaa30090192002551, openalexw3106449272"
}

We study the formation of the first generation of stars in the standard cold dark matter model, using a very high-resolution hydordynamic simulations. Our simulation achieves a dynamic range of 10^{10} in length scale. With accurate treatment of atomic and molecular physics, it allows us to study the chemo-thermal evolution of primordial gas clouds to densities up to n = 10^{16}/cc without assuming any a priori equation of state; a six orders of magnitudes improvement over previous three-dimensional calculations. All the relevant atomic and molecular cooling and heating processes, including cooling by collision-induced continuum emission, are implemented. For calculating optically thick H2 cooling at high densities, we use the Sobolev method. To examine possible gas fragmentation owing to thermal instability, we compute explicitly the growth rate of isobaric perturbations. We show that the cloud core does not fragment in either the low-density or high-density regimes. We also show that the core remains stable against gravitational deformation and fragmentation. We obtain an accurate gas mass accretion rate within a 10 Msun innermost region around the protostar. The protostar is accreting the surrounding hot gas at a rate of 0.001-0.01 Msun/yr. From these findings we conclude that primordial stars formed in early minihalos are massive. We carry out proto-stellar evolution calculations using the obtained accretion rate. The resulting mass of the first star is M_ZAMS = 60-100 Msun, with the exact mass dependent on the actual accretion rate.

@article{doi101086507978,
    author = "Yoshida, Naoki and Omukai, Kazuyuki and Hernquist, Lars and Abel, Tom",
    title = "Formation of Primordial Stars in a ΛCDM Universe",
    year = "2006",
    journal = "The Astrophysical Journal",
    abstract = "We study the formation of the first generation of stars in the standard cold dark matter model, using a very high-resolution hydordynamic simulations. Our simulation achieves a dynamic range of 10^{10} in length scale. With accurate treatment of atomic and molecular physics, it allows us to study the chemo-thermal evolution of primordial gas clouds to densities up to n = 10^{16}/cc without assuming any a priori equation of state; a six orders of magnitudes improvement over previous three-dimensional calculations. All the relevant atomic and molecular cooling and heating processes, including cooling by collision-induced continuum emission, are implemented. For calculating optically thick H2 cooling at high densities, we use the Sobolev method. To examine possible gas fragmentation owing to thermal instability, we compute explicitly the growth rate of isobaric perturbations. We show that the cloud core does not fragment in either the low-density or high-density regimes. We also show that the core remains stable against gravitational deformation and fragmentation. We obtain an accurate gas mass accretion rate within a 10 Msun innermost region around the protostar. The protostar is accreting the surrounding hot gas at a rate of 0.001-0.01 Msun/yr. From these findings we conclude that primordial stars formed in early minihalos are massive. We carry out proto-stellar evolution calculations using the obtained accretion rate. The resulting mass of the first star is M\_ZAMS = 60-100 Msun, with the exact mass dependent on the actual accretion rate.",
    url = "https://doi.org/10.1086/507978",
    doi = "10.1086/507978",
    openalex = "W2023968025"
}

A universe without weak interactions is constructed that undergoes big-bang nucleosynthesis, matter domination, structure formation, and star formation. The stars in this universe are able to burn for billions of years, synthesize elements up to iron, and undergo supernova explosions, dispersing heavy elements into the interstellar medium. These definitive claims are supported by a detailed analysis where this hypothetical ``weakless universe'' is matched to our Universe by simultaneously adjusting standard model and cosmological parameters. For instance, chemistry and nuclear physics are essentially unchanged. The apparent habitability of the weakless universe suggests that the anthropic principle does not determine the scale of electroweak breaking, or even require that it be smaller than the Planck scale, so long as technically natural parameters may be suitably adjusted. Whether the multiparameter adjustment is realized or probable is dependent on the ultraviolet completion, such as the string landscape. Considering a similar analysis for the cosmological constant, however, we argue that no adjustments of other parameters are able to allow the cosmological constant to raise up even remotely close to the Planck scale while obtaining macroscopic structure. The fine-tuning problems associated with the electroweak breaking scale and the cosmological constant therefore appear to be qualitatively different from the perspective of obtaining a habitable universe.

@article{doi101103physrevd74035006,
    author = "Harnik, Roni and Kribs, Graham D. and Pérez, Gilad",
    title = "A universe without weak interactions",
    year = "2006",
    journal = "Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D, Particles, fields, gravitation, and cosmology",
    abstract = "A universe without weak interactions is constructed that undergoes big-bang nucleosynthesis, matter domination, structure formation, and star formation. The stars in this universe are able to burn for billions of years, synthesize elements up to iron, and undergo supernova explosions, dispersing heavy elements into the interstellar medium. These definitive claims are supported by a detailed analysis where this hypothetical ``weakless universe'' is matched to our Universe by simultaneously adjusting standard model and cosmological parameters. For instance, chemistry and nuclear physics are essentially unchanged. The apparent habitability of the weakless universe suggests that the anthropic principle does not determine the scale of electroweak breaking, or even require that it be smaller than the Planck scale, so long as technically natural parameters may be suitably adjusted. Whether the multiparameter adjustment is realized or probable is dependent on the ultraviolet completion, such as the string landscape. Considering a similar analysis for the cosmological constant, however, we argue that no adjustments of other parameters are able to allow the cosmological constant to raise up even remotely close to the Planck scale while obtaining macroscopic structure. The fine-tuning problems associated with the electroweak breaking scale and the cosmological constant therefore appear to be qualitatively different from the perspective of obtaining a habitable universe.",
    url = "https://doi.org/10.1103/physrevd.74.035006",
    doi = "10.1103/physrevd.74.035006",
    openalex = "W2094809047",
    references = "doi101017cbo9780511524370, doi10106312808637, doi10106312820190, doi101086305002, doi10108800319112382028, doi10108811266708200006006, doi10108811266708200305046, doi101103physrevd68046005, doi101103physrevlett592607, doi101103revmodphys73719"
}

Ten years ago, the discovery that the expansion of the universe is accelerating put in place the last major building block of the present cosmological model, in which the universe is composed of 4% baryons, 20% dark matter, and 76% dark energy. At the same time, it posed one of the most profound mysteries in all of science, with deep connections to both astrophysics and particle physics. Cosmic acceleration could arise from the repulsive gravity of dark energy—for example, the quantum energy of the vacuum—or it may signal that general relativity (GR) breaks down on cosmological scales and must be replaced. We review the present observational evidence for cosmic acceleration and what it has revealed about dark energy, discuss the various theoretical ideas that have been proposed to explain acceleration, and describe the key observational probes that will shed light on this enigma in the coming years.

@article{doi101146annurevastro46060407145243,
    author = "Frieman, J. and Turner, Michael S. and Huterer, Dragan",
    title = "Dark Energy and the Accelerating Universe",
    year = "2008",
    journal = "Annual Review of Astronomy and Astrophysics",
    abstract = "Ten years ago, the discovery that the expansion of the universe is accelerating put in place the last major building block of the present cosmological model, in which the universe is composed of 4\% baryons, 20\% dark matter, and 76\% dark energy. At the same time, it posed one of the most profound mysteries in all of science, with deep connections to both astrophysics and particle physics. Cosmic acceleration could arise from the repulsive gravity of dark energy—for example, the quantum energy of the vacuum—or it may signal that general relativity (GR) breaks down on cosmological scales and must be replaced. We review the present observational evidence for cosmic acceleration and what it has revealed about dark energy, discuss the various theoretical ideas that have been proposed to explain acceleration, and describe the key observational probes that will shed light on this enigma in the coming years.",
    url = "https://doi.org/10.1146/annurev.astro.46.060407.145243",
    doi = "10.1146/annurev.astro.46.060407.145243",
    openalex = "W2102197207",
    references = "doi101073pnas153168, doi10108811266708200006006, doi101093mnras1085372, doi101103physrevd68023509, doi101103physrevlett592607, doi105860choice311499, openalexw3098371892"
}

List of Contributors. Foreword. Preface. Acknowledgements. 1.0. Introduction (Kevin R. Henke). Abstract. 1.1 Arsenic Origin, Chemistry, and Use. 1.2 Arsenic Environmental Impacts. 1.3 Arsenic Toxicity. 1.4 Arsenic Treatment and Remediation. 1.5 References. 2.0. Arsenic Chemistry (Kevin R. Henke and Aaron Hutchison). Abstract. 2.1 Introduction. 2.2 Atomic Structure and Isotopes of Arsenic. 2.3 Arsenic Valence State and Bonding. 2.4 Chemistry of Arsenic Solids. 2.5 Introduction to Arsenic Oxidation and Reduction. 2.6 Introduction to Arsenic Methylation and Demethylation. 2.7 Arsenic in water. 2.8 Chemistry of Gaseous Arsenic Emissions. 2.9 References. 3.0. Arsenic in Natural Environments (Kevin R. Henke). Abstract. 3.1 Introduction. 3.2 Nucleosynthesis: The Origin of Arsenic. 3.3 Arsenic in the Universe as a Whole. 3.4 Arsenic Chemistry of the Solar System. 3.5 Arsenic in the Bulk Earth, Crusts, and Interior. 3.6 Arsenic in Hydrothermal and Geothermal Fluids and their Deposits. 3.7 Oxidation of Arsenic-Bearing Sulfides in Geologic Materials and Mining Wastes. 3.8 Interactions between Arsenic and Natural Organic Matter (NOM). 3.9 Sorption and Coprecipitation of Arsenic with Iron and Other (Oxy)(hydr)oxides. 3.10 Arsenate (As(V)) Precipitation. 3.11 Reductive Dissolution of Iron and Manganese (Oxy)(hydr)oxides. 3.12 Arsenic and Sulfide at < 50oC. 3.13 Arsenic and its Chemistry in Mined Materials. 3.14 Marine Waters and Sediments. 3.15 Estuaries. 3.16 Rivers and Other Streams. 3.17 Lakes. 3.18 Wetlands. 3.19 Groundwater. 3.20 Glacial Ice and Related Sediments. 3.21 Arsenic in Air and Wind-blown Sediments. 3.22 Petroleum. 3.23 Soils. 3.24 Sedimentary Rocks. 3.25 Metamorphic Rocks. 3.26 References. 4.0. Toxicology and Epidemiology of Arsenic and its Compounds (Michael F. Hughes, David J. Thomas, and Elaina M. Kenyon). Abstract. 4.1 Introduction. 4.2 Physical and Chemical Properties of Arsenic. 4.3 Exposure to Arsenic. 4.4 Arsenic Disposition and Biotransformation in Mammals. 4.5 Systemic Clearance of Arsenic and Binding to Blood Components. 4.6 Tissue Distribution. 4.7 Placental Transfer and Distribution in the Fetus. 4.8 Arsenic Biotransformation. 4.9 Arsenic Excretion. 4.10 Effects of Arsenic Exposure. 4.11. Cardiovascular. 4.12. Endocrine. 4.13 Hepatic. 4.14 Neurological. 4.15 Skin. 4.16 Developmental. 4.17 Other Organ Systems. 4.18 Cancer. 4.19 Animal Models for Arsenic-induced Cancer. 4.20 Mechanism of Action. 4.21 Regulation of Arsenic. 4.22 References. 5.0. Arsenic in Human History and Modern Societies (Kevin R. Henke and David A. Atwood). Abstract. 5.1 Introduction. 5.2. Early Recognition and Uses of Arsenic by Humans. 5.3 Alchemy, Development of Methods to Recover Elemental Arsenic, and the Synthesis of Arsenic Compounds. 5.4 Applications with Arsenic. 5.5 Increasing Health, Safety, and Environmental Concerns. 5.6 Arsenic in Crime. 5.7 Poisoning Controversies: Napoleon Bonaparte. 5.8 Arsenic in Prospecting, Mining, and Markets. 5.9 Arsenic in Coal and Oil Shale Utilization and their Byproducts. 5.10 References. 6.0. Major Occurrences of Elevated Arsenic in Groundwater and Other Natural Waters (Abhijit Mukherjee, Alan E. Fryar, and Bethany M. O'Shea). Abstract. 6.1 Introduction. 6.2 Arsenic Speciation and Mobility in Natural Waters. 6.3 Immobilization of Arsenic in Hydrologic Systems. 6.4 Mobilization of Arsenic in Water. 6.5 Natural Occurrences of Elevated Arsenic around the World. 6.6 References. 7.0. Waste Treatment and Remediation Technologies for Arsenic (Kevin R. Henke). Abstract. 7.1 Introduction. 7.2 Treatment Technologies for Arsenic in Water. 7.3 Treatment Technologies for Arsenic in Solids. 7.4 Treatment Technologies for Arsenic in Gases. 7.5 References. Appendices. A: Common Physical and Chemical Constants and Conversions for Units of Measure. B: Glossary of Terms. B.1 Introduction. B.2 Glossary. C: Arsenic Thermodynamic Data. C.1 Introduction. C.2 Modeling Applications with Thermodynamic Data. C.3 Thermodynamic Data. D: Locations of Significant Arsenic Contamination. E: Regulation of Arsenic: A Brief Survey and Bibliography. E.1 Introduction. E.2 Regulation of Arsenic in Water. E.3 Regulation of Arsenic in Solid and Liquid Wastes. E.4 Sediment and Soil Guidelines and Standards for Arsenic. E.5 Regulation of Arsenic in Food and Drugs. E.6 Regulation of Arsenic in Air. E.7 Other References. Subject Index.

@book{openalexw1868970315,
    author = "Henke, Kevin R.",
    title = "Arsenic: Environmental Chemistry, Health Threats and Waste Treatment",
    year = "2009",
    abstract = "List of Contributors. Foreword. Preface. Acknowledgements. 1.0. Introduction (Kevin R. Henke). Abstract. 1.1 Arsenic Origin, Chemistry, and Use. 1.2 Arsenic Environmental Impacts. 1.3 Arsenic Toxicity. 1.4 Arsenic Treatment and Remediation. 1.5 References. 2.0. Arsenic Chemistry (Kevin R. Henke and Aaron Hutchison). Abstract. 2.1 Introduction. 2.2 Atomic Structure and Isotopes of Arsenic. 2.3 Arsenic Valence State and Bonding. 2.4 Chemistry of Arsenic Solids. 2.5 Introduction to Arsenic Oxidation and Reduction. 2.6 Introduction to Arsenic Methylation and Demethylation. 2.7 Arsenic in water. 2.8 Chemistry of Gaseous Arsenic Emissions. 2.9 References. 3.0. Arsenic in Natural Environments (Kevin R. Henke). Abstract. 3.1 Introduction. 3.2 Nucleosynthesis: The Origin of Arsenic. 3.3 Arsenic in the Universe as a Whole. 3.4 Arsenic Chemistry of the Solar System. 3.5 Arsenic in the Bulk Earth, Crusts, and Interior. 3.6 Arsenic in Hydrothermal and Geothermal Fluids and their Deposits. 3.7 Oxidation of Arsenic-Bearing Sulfides in Geologic Materials and Mining Wastes. 3.8 Interactions between Arsenic and Natural Organic Matter (NOM). 3.9 Sorption and Coprecipitation of Arsenic with Iron and Other (Oxy)(hydr)oxides. 3.10 Arsenate (As(V)) Precipitation. 3.11 Reductive Dissolution of Iron and Manganese (Oxy)(hydr)oxides. 3.12 Arsenic and Sulfide at < 50oC. 3.13 Arsenic and its Chemistry in Mined Materials. 3.14 Marine Waters and Sediments. 3.15 Estuaries. 3.16 Rivers and Other Streams. 3.17 Lakes. 3.18 Wetlands. 3.19 Groundwater. 3.20 Glacial Ice and Related Sediments. 3.21 Arsenic in Air and Wind-blown Sediments. 3.22 Petroleum. 3.23 Soils. 3.24 Sedimentary Rocks. 3.25 Metamorphic Rocks. 3.26 References. 4.0. Toxicology and Epidemiology of Arsenic and its Compounds (Michael F. Hughes, David J. Thomas, and Elaina M. Kenyon). Abstract. 4.1 Introduction. 4.2 Physical and Chemical Properties of Arsenic. 4.3 Exposure to Arsenic. 4.4 Arsenic Disposition and Biotransformation in Mammals. 4.5 Systemic Clearance of Arsenic and Binding to Blood Components. 4.6 Tissue Distribution. 4.7 Placental Transfer and Distribution in the Fetus. 4.8 Arsenic Biotransformation. 4.9 Arsenic Excretion. 4.10 Effects of Arsenic Exposure. 4.11. Cardiovascular. 4.12. Endocrine. 4.13 Hepatic. 4.14 Neurological. 4.15 Skin. 4.16 Developmental. 4.17 Other Organ Systems. 4.18 Cancer. 4.19 Animal Models for Arsenic-induced Cancer. 4.20 Mechanism of Action. 4.21 Regulation of Arsenic. 4.22 References. 5.0. Arsenic in Human History and Modern Societies (Kevin R. Henke and David A. Atwood). Abstract. 5.1 Introduction. 5.2. Early Recognition and Uses of Arsenic by Humans. 5.3 Alchemy, Development of Methods to Recover Elemental Arsenic, and the Synthesis of Arsenic Compounds. 5.4 Applications with Arsenic. 5.5 Increasing Health, Safety, and Environmental Concerns. 5.6 Arsenic in Crime. 5.7 Poisoning Controversies: Napoleon Bonaparte. 5.8 Arsenic in Prospecting, Mining, and Markets. 5.9 Arsenic in Coal and Oil Shale Utilization and their Byproducts. 5.10 References. 6.0. Major Occurrences of Elevated Arsenic in Groundwater and Other Natural Waters (Abhijit Mukherjee, Alan E. Fryar, and Bethany M. O'Shea). Abstract. 6.1 Introduction. 6.2 Arsenic Speciation and Mobility in Natural Waters. 6.3 Immobilization of Arsenic in Hydrologic Systems. 6.4 Mobilization of Arsenic in Water. 6.5 Natural Occurrences of Elevated Arsenic around the World. 6.6 References. 7.0. Waste Treatment and Remediation Technologies for Arsenic (Kevin R. Henke). Abstract. 7.1 Introduction. 7.2 Treatment Technologies for Arsenic in Water. 7.3 Treatment Technologies for Arsenic in Solids. 7.4 Treatment Technologies for Arsenic in Gases. 7.5 References. Appendices. A: Common Physical and Chemical Constants and Conversions for Units of Measure. B: Glossary of Terms. B.1 Introduction. B.2 Glossary. C: Arsenic Thermodynamic Data. C.1 Introduction. C.2 Modeling Applications with Thermodynamic Data. C.3 Thermodynamic Data. D: Locations of Significant Arsenic Contamination. E: Regulation of Arsenic: A Brief Survey and Bibliography. E.1 Introduction. E.2 Regulation of Arsenic in Water. E.3 Regulation of Arsenic in Solid and Liquid Wastes. E.4 Sediment and Soil Guidelines and Standards for Arsenic. E.5 Regulation of Arsenic in Food and Drugs. E.6 Regulation of Arsenic in Air. E.7 Other References. Subject Index.",
    url = "https://openalex.org/W1868970315",
    openalex = "W1868970315"
}

Environmental context. On a global scale, soils store more carbon than plants or the atmosphere. The cycling of this vast reservoir of reduced carbon is closely tied to variations in environmental conditions, but robust predictions of climate–carbon cycle feedbacks are hampered by a lack of mechanistic knowledge regarding the sensitivity of organic matter decomposition to rising temperatures. This text provides a critical discussion of the practice to conceptualise parts of soil organic matter as intrinsically resistant to decomposition or ‘recalcitrant’. Abstract. The understanding that some natural organic molecules can resist microbial decomposition because of certain molecular properties forms the basis of the biogeochemical paradigm of ‘intrinsic recalcitrance’. In this concept paper I argue that recalcitrance is an indeterminate abstraction whose semantic vagueness encumbers research on terrestrial carbon cycling. Consequently, it appears to be advantageous to view the perceived ‘inherent resistance’ to decomposition of some forms of organic matter not as a material property, but as a logistical problem constrained by (i) microbial ecology; (ii) enzyme kinetics; (iii) environmental drivers; and (iv) matrix protection. A consequence of this view would be that the frequently observed temperature sensitivity of the decomposition of organic matter must result from factors other than intrinsic molecular recalcitrance.

@article{doi101071en10006,
    author = "Kleber, Markus",
    title = "What is recalcitrant soil organic matter?",
    year = "2010",
    journal = "Environmental Chemistry",
    abstract = "Environmental context. On a global scale, soils store more carbon than plants or the atmosphere. The cycling of this vast reservoir of reduced carbon is closely tied to variations in environmental conditions, but robust predictions of climate–carbon cycle feedbacks are hampered by a lack of mechanistic knowledge regarding the sensitivity of organic matter decomposition to rising temperatures. This text provides a critical discussion of the practice to conceptualise parts of soil organic matter as intrinsically resistant to decomposition or ‘recalcitrant’. Abstract. The understanding that some natural organic molecules can resist microbial decomposition because of certain molecular properties forms the basis of the biogeochemical paradigm of ‘intrinsic recalcitrance’. In this concept paper I argue that recalcitrance is an indeterminate abstraction whose semantic vagueness encumbers research on terrestrial carbon cycling. Consequently, it appears to be advantageous to view the perceived ‘inherent resistance’ to decomposition of some forms of organic matter not as a material property, but as a logistical problem constrained by (i) microbial ecology; (ii) enzyme kinetics; (iii) environmental drivers; and (iv) matrix protection. A consequence of this view would be that the frequently observed temperature sensitivity of the decomposition of organic matter must result from factors other than intrinsic molecular recalcitrance.",
    url = "https://doi.org/10.1071/en10006",
    doi = "10.1071/en10006",
    openalex = "W2128817158",
    references = "openalexw322605492"
}

We present a robust method to constrain average galaxy star formation rates, star formation histories, and the intracluster light as a function of halo mass. Our results are consistent with observed galaxy stellar mass functions, specific star formation rates, and cosmic star formation rates from z=0 to z=8. We consider the effects of a wide range of uncertainties on our results, including those affecting stellar masses, star formation rates, and the halo mass function at the heart of our analysis. As they are relevant to our method, we also present new calibrations of the dark matter halo mass function, halo mass accretion histories, and halo-subhalo merger rates out to z=8. We also provide new compilations of cosmic and specific star formation rates; more recent measurements are now consistent with the buildup of the cosmic stellar mass density at all redshifts. Implications of our work include: halos near 10^12 Msun are the most efficient at forming stars at all redshifts, the baryon conversion efficiency of massive halos drops markedly after z ~ 2.5 (consistent with theories of cold-mode accretion), the ICL for massive galaxies is expected to be significant out to at least z ~ 1-1.5, and dwarf galaxies at low redshifts have higher stellar mass to halo mass ratios than previous expectations and form later than in most theoretical models. Finally, we provide new fitting formulae for star formation histories that are more accurate than the standard declining tau model. Our approach places a wide variety of observations relating to the star formation history of galaxies into a self-consistent framework based on the modern understanding of structure formation in LCDM. Constraints on the stellar mass-halo mass relationship and star formation rates are available for download at http://www.peterbehroozi.com/data.html.

@article{doi1010880004637x770157,
    author = "Behroozi, Peter and Wechsler, Risa H. and Conroy, Charlie",
    title = "THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0-8",
    year = "2013",
    journal = "The Astrophysical Journal",
    abstract = "We present a robust method to constrain average galaxy star formation rates, star formation histories, and the intracluster light as a function of halo mass. Our results are consistent with observed galaxy stellar mass functions, specific star formation rates, and cosmic star formation rates from z=0 to z=8. We consider the effects of a wide range of uncertainties on our results, including those affecting stellar masses, star formation rates, and the halo mass function at the heart of our analysis. As they are relevant to our method, we also present new calibrations of the dark matter halo mass function, halo mass accretion histories, and halo-subhalo merger rates out to z=8. We also provide new compilations of cosmic and specific star formation rates; more recent measurements are now consistent with the buildup of the cosmic stellar mass density at all redshifts. Implications of our work include: halos near 10^12 Msun are the most efficient at forming stars at all redshifts, the baryon conversion efficiency of massive halos drops markedly after z \textasciitilde\ 2.5 (consistent with theories of cold-mode accretion), the ICL for massive galaxies is expected to be significant out to at least z \textasciitilde\ 1-1.5, and dwarf galaxies at low redshifts have higher stellar mass to halo mass ratios than previous expectations and form later than in most theoretical models. Finally, we provide new fitting formulae for star formation histories that are more accurate than the standard declining tau model. Our approach places a wide variety of observations relating to the star formation history of galaxies into a self-consistent framework based on the modern understanding of structure formation in LCDM. Constraints on the stellar mass-halo mass relationship and star formation rates are available for download at http://www.peterbehroozi.com/data.html.",
    url = "https://doi.org/10.1088/0004-637x/770/1/57",
    doi = "10.1088/0004-637x/770/1/57",
    openalex = "W2074259895",
    references = "doi10108800670049192218"
}

Within the precise cosmological framework provided by the Λ-cold dark matter model and standard Big Bang nucleosynthesis, the chemical evolution of the pregalactic gas can now be followed with accuracy limited only by the uncertainties on the reaction rates. Starting during the recombination era, the formation of the first molecules and molecular ions containing hydrogen, deuterium, helium, and lithium was severely hindered by the low density of the expanding Universe, the intensity of the cosmic radiation field, and the absence of solid catalyzers. Molecular hydrogen and deuterated hydrogen, the most abundant species formed in the gas phase prior to structure formation, played a fundamental role in the cooling of the gas clouds that gave birth to the first stellar generation, contributing to determine the scale of fragmentation. Primordial molecules also interacted with the photons of the cosmic background via resonant scattering, absorption, and emission. In this review, we examine the current status of the chemistry of the early Universe and discuss the most relevant reactions for which uncertainties still exist from theory or laboratory experiments. The prospects for detecting spectral distortions or spatial anisotropies due to the first atoms and molecules are also addressed.

@article{doi101146annurevastro082812141029,
    author = "Galli, Daniele and Palla, F.",
    title = "The Dawn of Chemistry",
    year = "2013",
    journal = "Annual Review of Astronomy and Astrophysics",
    abstract = "Within the precise cosmological framework provided by the Λ-cold dark matter model and standard Big Bang nucleosynthesis, the chemical evolution of the pregalactic gas can now be followed with accuracy limited only by the uncertainties on the reaction rates. Starting during the recombination era, the formation of the first molecules and molecular ions containing hydrogen, deuterium, helium, and lithium was severely hindered by the low density of the expanding Universe, the intensity of the cosmic radiation field, and the absence of solid catalyzers. Molecular hydrogen and deuterated hydrogen, the most abundant species formed in the gas phase prior to structure formation, played a fundamental role in the cooling of the gas clouds that gave birth to the first stellar generation, contributing to determine the scale of fragmentation. Primordial molecules also interacted with the photons of the cosmic background via resonant scattering, absorption, and emission. In this review, we examine the current status of the chemistry of the early Universe and discuss the most relevant reactions for which uncertainties still exist from theory or laboratory experiments. The prospects for detecting spectral distortions or spatial anisotropies due to the first atoms and molecules are also addressed.",
    url = "https://doi.org/10.1146/annurev-astro-082812-141029",
    doi = "10.1146/annurev-astro-082812-141029",
    openalex = "W2119813984",
    references = "doi101007bf00653471, doi101086186504, doi101086303434, doi101086323947, doi101086377226, doi1010880004637x7072916, doi10108800344885758086901, doi10108800670049192218, doi101126science1063991, doi105860choice311499"
}

Abstract In chemistry textbooks, the p K value of water in the solvent water at 25 °C is sometimes given as 14.0, sometimes as 15.7. This is confusing. The particular chemical reaction considered is the one in which water as Brønsted  Lowry acid reacts with water as Brønsted  Lowry base in water as solvent to yield equal concentrations of hydrated oxonium and hydroxide ions, H 3 O + (aq) and HO − (aq), respectively. This reaction is also known as the ‘self‐ionization’ of water for which the equilibrium constant is abbreviated as K w with its known value of 10 −14.0 at 25 °C, i.e., p K w (25 °C)=14.0. Identical values for p K and p K w at a fixed temperature appear reasonable, since K and K w refer to one and the same reaction. Therefore, reasons for the apparent disagreement between the ‘thermodynamically correct’ p K a value for water (14.0 at 25 °C) and the value reported in most organic chemistry textbooks (15.7) should be discussed when teaching acidbase chemistry. There are good arguments for introducing, from the very beginning, the concepts of activity and thermodynamic standard states when teaching quantitative aspects of chemical equilibria. This also explains in a straightforward way why all thermodynamic equilibrium constants, including K w, are dimensionless, and why p K (25 °C)=0.

@article{doi101002hlca201300321,
    author = "Meister, Erich C. and Willeke, Martin and Angst, Werner and Togni, Antonio and Walde, Peter",
    title = "Confusing Quantitative Descriptions of Brønsted Lowry AcidBase Equilibria in Chemistry Textbooks – A Critical Review and Clarifications for Chemical Educators",
    year = "2014",
    journal = "Helvetica Chimica Acta",
    abstract = "Abstract In chemistry textbooks, the p K value of water in the solvent water at 25 °C is sometimes given as 14.0, sometimes as 15.7. This is confusing. The particular chemical reaction considered is the one in which water as Brønsted  Lowry acid reacts with water as Brønsted  Lowry base in water as solvent to yield equal concentrations of hydrated oxonium and hydroxide ions, H 3 O + (aq) and HO − (aq), respectively. This reaction is also known as the ‘self‐ionization’ of water for which the equilibrium constant is abbreviated as K w with its known value of 10 −14.0 at 25 °C, i.e., p K w (25 °C)=14.0. Identical values for p K and p K w at a fixed temperature appear reasonable, since K and K w refer to one and the same reaction. Therefore, reasons for the apparent disagreement between the ‘thermodynamically correct’ p K a value for water (14.0 at 25 °C) and the value reported in most organic chemistry textbooks (15.7) should be discussed when teaching acidbase chemistry. There are good arguments for introducing, from the very beginning, the concepts of activity and thermodynamic standard states when teaching quantitative aspects of chemical equilibria. This also explains in a straightforward way why all thermodynamic equilibrium constants, including K w, are dimensionless, and why p K (25 °C)=0.",
    url = "https://doi.org/10.1002/hlca.201300321",
    doi = "10.1002/hlca.201300321",
    openalex = "W2081675302",
    references = "openalexw322605492"
}

Proudly serving the scientific community for over a century, this 95th edition of the CRC Handbook of Chemistry and Physics is an update of a classic reference, mirroring the growth and direction of science. This venerable work continues to be the most accessed and respected scientific reference in the world. An authoritative resource consisting of

@book{doi101201b17118,
    author = "Haynes, W.M.",
    title = "CRC Handbook of Chemistry and Physics",
    year = "2014",
    abstract = "Proudly serving the scientific community for over a century, this 95th edition of the CRC Handbook of Chemistry and Physics is an update of a classic reference, mirroring the growth and direction of science. This venerable work continues to be the most accessed and respected scientific reference in the world. An authoritative resource consisting of",
    url = "https://doi.org/10.1201/b17118",
    doi = "10.1201/b17118",
    openalex = "W2132905138"
}

We present a semi-analytic, physically motivated model for dark matter halo concentration as a function of halo mass and redshift. The semi-analytic model combines an analytic model for the halo mass accretion history (MAH), based on extended Press–Schechter (EPS) theory, with an empirical relation between concentration and formation time obtained through fits to the results of numerical simulations. Because the semi-analytic model is based on EPS theory, it can be applied to wide ranges in mass, redshift and cosmology. The resulting concentration–mass (c–M) relations are found to agree with the simulations, and because the model applies only to relaxed haloes, they do not exhibit the upturn at high masses or high redshifts found by some recent works. We predict a change of slope in the z ∼ 0 c–M relation at a mass-scale of 1011 M⊙. We find that this is due to the change in the functional form of the halo MAH, which goes from being dominated by an exponential (for high-mass haloes) to a power law (for low-mass haloes). During the latter phase, the core radius remains approximately constant, and the concentration grows due to the drop of the background density. We also analyse how the c–M relation predicted by this work affects the power produced by dark matter annihilation, finding that at z = 0 the power is two orders of magnitude lower than that obtained from extrapolating best-fitting c–M relations. We provide fits to the c–M relations as well as numerical routines to compute concentrations and MAHs.

@article{doi101093mnrasstv1363,
    author = "Correa, Camila A. and Wyithe, J. Stuart B. and Schaye, Joop and Duffy, Alan R.",
    title = "The accretion history of dark matter haloes – III. A physical model for the concentration–mass relation",
    year = "2015",
    journal = "Monthly Notices of the Royal Astronomical Society",
    abstract = "We present a semi-analytic, physically motivated model for dark matter halo concentration as a function of halo mass and redshift. The semi-analytic model combines an analytic model for the halo mass accretion history (MAH), based on extended Press–Schechter (EPS) theory, with an empirical relation between concentration and formation time obtained through fits to the results of numerical simulations. Because the semi-analytic model is based on EPS theory, it can be applied to wide ranges in mass, redshift and cosmology. The resulting concentration–mass (c–M) relations are found to agree with the simulations, and because the model applies only to relaxed haloes, they do not exhibit the upturn at high masses or high redshifts found by some recent works. We predict a change of slope in the z ∼ 0 c–M relation at a mass-scale of 1011 M⊙. We find that this is due to the change in the functional form of the halo MAH, which goes from being dominated by an exponential (for high-mass haloes) to a power law (for low-mass haloes). During the latter phase, the core radius remains approximately constant, and the concentration grows due to the drop of the background density. We also analyse how the c–M relation predicted by this work affects the power produced by dark matter annihilation, finding that at z = 0 the power is two orders of magnitude lower than that obtained from extrapolating best-fitting c–M relations. We provide fits to the c–M relations as well as numerical routines to compute concentrations and MAHs.",
    url = "https://doi.org/10.1093/mnras/stv1363",
    doi = "10.1093/mnras/stv1363",
    openalex = "W1895726190",
    references = "doi10108800344885758086901"
}

Over the last forty years, scientists have uncovered evidence that if the Universe had been forged with even slightly different properties, life as we know it - and life as we can imagine it - would be impossible. Join us on a journey through how we understand the Universe, from its most basic particles and forces, to planets, stars and galaxies, and back through cosmic history to the birth of the cosmos. Conflicting notions about our place in the Universe are defined, defended and critiqued from scientific, philosophical and religious viewpoints. The authors' engaging and witty style addresses what fine-tuning might mean for the future of physics and the search for the ultimate laws of nature. Tackling difficult questions and providing thought-provoking answers, this volumes challenges us to consider our place in the cosmos, regardless of our initial convictions.

@book{doi1010179781316661413,
    author = "Lewis, Geraint F. and Barnes, Luke A. and Schmidt, B.",
    title = "A Fortunate Universe: Life in a Finely Tuned Cosmos",
    year = "2016",
    abstract = "Over the last forty years, scientists have uncovered evidence that if the Universe had been forged with even slightly different properties, life as we know it - and life as we can imagine it - would be impossible. Join us on a journey through how we understand the Universe, from its most basic particles and forces, to planets, stars and galaxies, and back through cosmic history to the birth of the cosmos. Conflicting notions about our place in the Universe are defined, defended and critiqued from scientific, philosophical and religious viewpoints. The authors' engaging and witty style addresses what fine-tuning might mean for the future of physics and the search for the ultimate laws of nature. Tackling difficult questions and providing thought-provoking answers, this volumes challenges us to consider our place in the cosmos, regardless of our initial convictions.",
    url = "https://doi.org/10.1017/9781316661413",
    doi = "10.1017/9781316661413",
    openalex = "W2530318121",
    references = "doi1010079783030112981, doi1010160167278984902458, doi101017cbo9780511498978, doi101017cbo9780511790423, doi10106312820190, doi10108816741137389090001, doi101088167411374010100001, doi101103physrevd74035006, doi101103revmodphys851491, doi105860choice342091, doi107551mitpress110680010001, openalexw1587819869, openalexw1648570772"
}

Visualisation of molecules in the field of chemistry has been important for understanding their structure, whether simple or complicated. Initially, this was done by hand, but latterly software has come to the aid of researchers and the vast majority of chemistry visualisation is now computer-generated. As well as aiding understanding, many molecules, especially if complex in nature, can take on an artistic quality when visualised, using artificial colour for example. Often these are used for creative reasons on the front of chemistry journals, for example, and sometimes as an inspiration for more pure art forms. This paper introduces molecular graphics in the context of creative computing. It also provides a history of the development of visualisation in chemistry, especially more recently with the use of software and the increasing use on journal covers. A brief survey of some of the software involved is included. Finally, some conclusions are drawn with respect to the creative directions being taken now and possible directions in the future.

@article{doi101504ijcrc2016076058,
    author = "Bowen, Jonathan P. and Bowen, Alice M. and Harrison, Karl N.",
    title = "Creative visualisation in chemistry",
    year = "2016",
    journal = "International Journal of Creative Computing",
    abstract = "Visualisation of molecules in the field of chemistry has been important for understanding their structure, whether simple or complicated. Initially, this was done by hand, but latterly software has come to the aid of researchers and the vast majority of chemistry visualisation is now computer-generated. As well as aiding understanding, many molecules, especially if complex in nature, can take on an artistic quality when visualised, using artificial colour for example. Often these are used for creative reasons on the front of chemistry journals, for example, and sometimes as an inspiration for more pure art forms. This paper introduces molecular graphics in the context of creative computing. It also provides a history of the development of visualisation in chemistry, especially more recently with the use of software and the increasing use on journal covers. A brief survey of some of the software involved is included. Finally, some conclusions are drawn with respect to the creative directions being taken now and possible directions in the future.",
    url = "https://doi.org/10.1504/ijcrc.2016.076058",
    doi = "10.1504/ijcrc.2016.076058",
    openalex = "W2338004479",
    references = "openalexw322605492"
}

Cosmic background (CB) radiation, encompassing the sum of emission from all sources outside our own Milky Way galaxy across the entire electromagnetic spectrum, is a fundamental phenomenon in observational cosmology. Many experiments have been conceived to measure it (or its constituents) since the extragalactic Universe was first discovered; in addition to estimating the bulk (cosmic monopole) spectrum, directional variations have also been detected over a wide range of wavelengths. Here we gather the most recent of these measurements and discuss the current status of our understanding of the CB from radio to γ-ray energies. Using available data in the literature, we piece together the sky-averaged intensity spectrum and discuss the emission processes responsible for what is observed. We examine the effect of perturbations to the continuum spectrum from atomic and molecular line processes and comment on the detectability of these signals. We also discuss how one could, in principle, obtain a complete census of the CB by measuring the full spectrum of each spherical harmonic expansion coefficient. This set of spectra of multipole moments effectively encodes the entire statistical history of nuclear, atomic, and molecular processes in the Universe.

@article{doi1011770003702818767133,
    author = "Hill, Ryley and Masui, Kiyoshi W. and Scott, D.",
    title = "The Spectrum of the Universe",
    year = "2018",
    journal = "Applied Spectroscopy",
    abstract = "Cosmic background (CB) radiation, encompassing the sum of emission from all sources outside our own Milky Way galaxy across the entire electromagnetic spectrum, is a fundamental phenomenon in observational cosmology. Many experiments have been conceived to measure it (or its constituents) since the extragalactic Universe was first discovered; in addition to estimating the bulk (cosmic monopole) spectrum, directional variations have also been detected over a wide range of wavelengths. Here we gather the most recent of these measurements and discuss the current status of our understanding of the CB from radio to γ-ray energies. Using available data in the literature, we piece together the sky-averaged intensity spectrum and discuss the emission processes responsible for what is observed. We examine the effect of perturbations to the continuum spectrum from atomic and molecular line processes and comment on the detectability of these signals. We also discuss how one could, in principle, obtain a complete census of the CB by measuring the full spectrum of each spherical harmonic expansion coefficient. This set of spectra of multipole moments effectively encodes the entire statistical history of nuclear, atomic, and molecular processes in the Universe.",
    url = "https://doi.org/10.1177/0003702818767133",
    doi = "10.1177/0003702818767133",
    openalex = "W2786867706",
    references = "doi101146annurevastro082812141029"
}

Abstract In recent years, the discovery of massive quasars at $z\sim7$ has provided a striking challenge to our understanding of the origin and growth of supermassive black holes in the early Universe. Mounting observational and theoretical evidence indicates the viability of massive seeds, formed by the collapse of supermassive stars, as a progenitor model for such early, massive accreting black holes. Although considerable progress has been made in our theoretical understanding, many questions remain regarding how (and how often) such objects may form, how they live and die, and how next generation observatories may yield new insight into the origin of these primordial titans. This review focusses on our present understanding of this remarkable formation scenario, based on the discussions held at the Monash Prato Centre from November 20 to 24, 2017, during the workshop ‘ Titans of the Early Universe: The Origin of the First Supermassive Black Holes ’.

@article{doi101017pasa201914,
    author = "Woods, Tyrone E. and Agarwal, Bhaskar and Bromm, Volker and Bunker, Andrew J. and Chen, Ke-Jung and Chon, Sunmyon and Ferrara, Andrea and Glover, Simon C. O. and Haemmerlé, L. and Haiman, Zoltán and Hartwig, Tilman and Heger, Alexander and Hirano, Shingo and Hosokawa, Takashi and Inayoshi, Kohei and Klessen, Ralf S. and Kobayashi, Chiaki and Koliopanos, F. and Latif, Muhammad and Li, Yuexing and Mayer, Lucio and Mezcua, Mar and Natarajan, Priyamvada and Pacucci, Fabio and Rees, M. J. and Regan, John A. and Sakurai, Yuya and Salvadori, Stefania and Schneider, Raffaella and Surace, Marco and Tanaka, Takamitsu and Whalen, Daniel J. and Yoshida, Naoki",
    title = "Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes",
    year = "2019",
    journal = "Publications of the Astronomical Society of Australia",
    abstract = "Abstract In recent years, the discovery of massive quasars at $z\sim7$ has provided a striking challenge to our understanding of the origin and growth of supermassive black holes in the early Universe. Mounting observational and theoretical evidence indicates the viability of massive seeds, formed by the collapse of supermassive stars, as a progenitor model for such early, massive accreting black holes. Although considerable progress has been made in our theoretical understanding, many questions remain regarding how (and how often) such objects may form, how they live and die, and how next generation observatories may yield new insight into the origin of these primordial titans. This review focusses on our present understanding of this remarkable formation scenario, based on the discussions held at the Monash Prato Centre from November 20 to 24, 2017, during the workshop ‘ Titans of the Early Universe: The Origin of the First Supermassive Black Holes ’.",
    url = "https://doi.org/10.1017/pasa.2019.14",
    doi = "10.1017/pasa.2019.14",
    openalex = "W2899338238",
    references = "doi101093mnrasstv044"
}

ABSTRACT The Southern Photometric Local Universe Survey (S-PLUS) is imaging ∼9300 deg2 of the celestial sphere in 12 optical bands using a dedicated 0.8 m robotic telescope, the T80-South, at the Cerro Tololo Inter-american Observatory, Chile. The telescope is equipped with a 9.2k × 9.2k e2v detector with 10 $\rm {\mu m}$ pixels, resulting in a field of view of 2 deg2 with a plate scale of 0.55 arcsec pixel−1. The survey consists of four main subfields, which include two non-contiguous fields at high Galactic latitudes (|b| &gt; 30°, 8000 deg2) and two areas of the Galactic Disc and Bulge (for an additional 1300 deg2). S-PLUS uses the Javalambre 12-band magnitude system, which includes the 5 ugriz broad-band filters and 7 narrow-band filters centred on prominent stellar spectral features: the Balmer jump/[OII], Ca H + K, H δ, G band, Mg b triplet, H α, and the Ca triplet. S-PLUS delivers accurate photometric redshifts (δz/(1 + z) = 0.02 or better) for galaxies with r &lt; 19.7 AB mag and z &lt; 0.4, thus producing a 3D map of the local Universe over a volume of more than $1\, (\mathrm{Gpc}/h)^3$. The final S-PLUS catalogue will also enable the study of star formation and stellar populations in and around the Milky Way and nearby galaxies, as well as searches for quasars, variable sources, and low-metallicity stars. In this paper we introduce the main characteristics of the survey, illustrated with science verification data highlighting the unique capabilities of S-PLUS. We also present the first public data release of ∼336 deg2 of the Stripe 82 area, in 12 bands, to a limiting magnitude of r = 21, available at datalab.noao.edu/splus.

@article{doi101093mnrasstz1985,
    author = "de Oliveira, C. Mendes and Ribeiro, T. and Schoenell, W. and Kanaan, A. and Overzier, Roderik and Molino, A. and Sampedro, L. and Coelho, P. and Barbosa, C. E. and Cortesi, A. and Costa-Duarte, M. V. and Herpich, F. R. and Hernández-Jiménez, J. A. and Placco, Vinicius M. and Xavier, Henrique S. and Abramo, L. Raul and Saito, R. K. and Chies-Santos, Ana L. and Ederoclite, A. and de Oliveira, R. Lopes and Gonçalves, D. R. and Akras, S. and Almeida, L. A. and Almeida-Fernandes, F. and Beers, Timothy C. and Bonatto, C. and Bonoli, Silvia and Cypriano, E. S. and Vinicius-Lima, E and de Souza, Rafael S. and de Souza, G Fabiano and Ferrari, Fabrício and Gonçalves, Thiago S. and Gonzalez, Anthony H. and Gutiérrez-Soto, L. A. and Hartmann, Eduardo A. and Jaffé, Yara L. and Kerber, L. O. and Lima-Dias, Círia and Lopes, P. A. A. and Menéndez‐Delmestre, Karín and Nakazono, L. and de Novais, Patricia Martins and Ortega-Minakata, R. A. and Pereira, Eduardo and Perottoni, Hélio D. and Queiroz, C. and Reis, Ribamar R. R. and Santos, W. A. and Santos-Silva, T. and Santucci, Rafael M. and Barbosa, C. L. and Siffert, Beatriz B. and Sodré, L. and Torres-Flores, S. and Westera, P. and Whitten, Devin D. and Alcaniz, J. S. and Alonso-García, J. and Alencar, S. H. P. and Álvarez-Candal, A. and Amram, P. and Azanha, Luiz and Barbá, R. H. and Bernardinelli, Pedro H. and Fernandes, M. Borges and Branco, Vinicius and Brito-Silva, D. and Buzzo, Maria Luísa and Caffer, J and Campillay, A. and Cano, Z. and Carvano, J. M. and Castejon, M and Fernandes, R. Cid and Dantas, M. L. L. and Daflon, S. and Damke, G. and de la Reza, R. and de Melo de Azevedo, L J and Paula, D F De and Diem, Keith G. and Donnerstein, Richard L. and Dors, O. L. and Dupke, Renato A. and Eikenberry, S. S. and Escudero, Carlos and Faifer, F. R. and Farías, Humberto and Fernandes, B. and Fernandes, R. Cid and Fontes, Shauanda Stefhanny Leal Gadêlha and Galarza, Andrés and Hirata, Nina S. T. and Katena, L and Gregorio‐Hetem, J. and Hernández-Fernández, J. D. and Izzo, L. and Arancibia, M. Jaque and Jatenco‐Pereira, V.",
    title = "The Southern Photometric Local Universe Survey (S-PLUS): improved SEDs, morphologies, and redshifts with 12 optical filters",
    year = "2019",
    journal = "Monthly Notices of the Royal Astronomical Society",
    abstract = "ABSTRACT The Southern Photometric Local Universe Survey (S-PLUS) is imaging ∼9300 deg2 of the celestial sphere in 12 optical bands using a dedicated 0.8 m robotic telescope, the T80-South, at the Cerro Tololo Inter-american Observatory, Chile. The telescope is equipped with a 9.2k × 9.2k e2v detector with 10 $\rm {\mu m}$ pixels, resulting in a field of view of 2 deg2 with a plate scale of 0.55 arcsec pixel−1. The survey consists of four main subfields, which include two non-contiguous fields at high Galactic latitudes (|b| \> 30°, 8000 deg2) and two areas of the Galactic Disc and Bulge (for an additional 1300 deg2). S-PLUS uses the Javalambre 12-band magnitude system, which includes the 5 ugriz broad-band filters and 7 narrow-band filters centred on prominent stellar spectral features: the Balmer jump/[OII], Ca H + K, H δ, G band, Mg b triplet, H α, and the Ca triplet. S-PLUS delivers accurate photometric redshifts (δz/(1 + z) = 0.02 or better) for galaxies with r \< 19.7 AB mag and z \< 0.4, thus producing a 3D map of the local Universe over a volume of more than $1\, (\mathrm{Gpc}/h)^3$. The final S-PLUS catalogue will also enable the study of star formation and stellar populations in and around the Milky Way and nearby galaxies, as well as searches for quasars, variable sources, and low-metallicity stars. In this paper we introduce the main characteristics of the survey, illustrated with science verification data highlighting the unique capabilities of S-PLUS. We also present the first public data release of ∼336 deg2 of the Stripe 82 area, in 12 bands, to a limiting magnitude of r = 21, available at datalab.noao.edu/splus.",
    url = "https://doi.org/10.1093/mnras/stz1985",
    doi = "10.1093/mnras/stz1985",
    openalex = "W2954822162",
    references = "doi101146annurevastro082214122423"
}

Axions are some of the best motivated particles beyond the Standard Model. We show how the attractive self-interactions of dark matter (DM) axions over a broad range of masses, from ${10}^{\ensuremath{-}22}\text{}\text{}\mathrm{eV}$ to ${10}^{7}\text{}\text{}\mathrm{GeV}$, can lead to nongravitational growth of density fluctuations and the formation of bound objects. This structure formation enhancement is driven by parametric resonance when the initial field misalignment is large, and it affects axion density perturbations on length scales of order the Hubble horizon when the axion field starts oscillating, deep inside the radiation-dominated era. This effect can turn an otherwise nearly scale-invariant spectrum of adiabatic perturbations into one that has a spike at the aforementioned scales, producing objects ranging from dense DM halos to scalar-field configurations such as solitons and oscillons. We call this class of cosmological scenarios for axion DM production ``the large-misalignment mechanism.'' We explore observational consequences of this mechanism for axions with masses up to 10 eV. For axions heavier than ${10}^{\ensuremath{-}5}\text{}\text{}\mathrm{eV}$, the compact axion halos are numerous enough to significantly impact Earth-bound direct detection experiments, yielding intermittent but coherent signals with repetition rates exceeding one per decade and crossing times less than a day. These episodic increases in the axion density and kinematic coherence suggest new approaches for axion DM searches, including for the QCD axion. Dense structures made up of axions from ${10}^{\ensuremath{-}22}\text{}\text{}\mathrm{eV}$ to ${10}^{\ensuremath{-}5}\text{}\text{}\mathrm{eV}$ are detectable through gravitational lensing searches, and their gravitational interactions can also perturb baryonic structures and alter star formation. At very high misalignment amplitudes, the axion field can undergo self-interaction-induced implosions long before matter-radiation equality, producing potentially-detectable low-frequency stochastic gravitational waves.

@article{doi101103physrevd101083014,
    author = "Arvanitaki, Asimina and Dimopoulos, Savas and Galanis, M.D. and Lehner, Luis and Thompson, Jedidiah O. and Tilburg, Ken Van",
    title = "Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter",
    year = "2020",
    journal = "Physical review. D/Physical review. D.",
    abstract = "Axions are some of the best motivated particles beyond the Standard Model. We show how the attractive self-interactions of dark matter (DM) axions over a broad range of masses, from ${10}^{\ensuremath{-}22}\text{}\text{}\mathrm{eV}$ to ${10}^{7}\text{}\text{}\mathrm{GeV}$, can lead to nongravitational growth of density fluctuations and the formation of bound objects. This structure formation enhancement is driven by parametric resonance when the initial field misalignment is large, and it affects axion density perturbations on length scales of order the Hubble horizon when the axion field starts oscillating, deep inside the radiation-dominated era. This effect can turn an otherwise nearly scale-invariant spectrum of adiabatic perturbations into one that has a spike at the aforementioned scales, producing objects ranging from dense DM halos to scalar-field configurations such as solitons and oscillons. We call this class of cosmological scenarios for axion DM production ``the large-misalignment mechanism.'' We explore observational consequences of this mechanism for axions with masses up to 10 eV. For axions heavier than ${10}^{\ensuremath{-}5}\text{}\text{}\mathrm{eV}$, the compact axion halos are numerous enough to significantly impact Earth-bound direct detection experiments, yielding intermittent but coherent signals with repetition rates exceeding one per decade and crossing times less than a day. These episodic increases in the axion density and kinematic coherence suggest new approaches for axion DM searches, including for the QCD axion. Dense structures made up of axions from ${10}^{\ensuremath{-}22}\text{}\text{}\mathrm{eV}$ to ${10}^{\ensuremath{-}5}\text{}\text{}\mathrm{eV}$ are detectable through gravitational lensing searches, and their gravitational interactions can also perturb baryonic structures and alter star formation. At very high misalignment amplitudes, the axion field can undergo self-interaction-induced implosions long before matter-radiation equality, producing potentially-detectable low-frequency stochastic gravitational waves.",
    url = "https://doi.org/10.1103/physrevd.101.083014",
    doi = "10.1103/physrevd.101.083014",
    openalex = "W2975597507",
    references = "doi101088003448857611112901"
}

Abstract Western thought has been dominated by the dichotomy of traditional religion and secular atheism. But do we have to choose between these options? Philip Goff argues that it is time to move on from both God and atheism. Through an exploration of contemporary cosmology, as well as cutting-edge philosophical research on the nature of consciousness, Goff argues for cosmic purpose: the idea that the universe is directed towards certain goals, such as the emergence of intelligent life. However, in contrast to religious thinkers, Goff argues that the Omni-God (defined as all-knowing, all-powerful, and perfectly good) is a bad explanation of cosmic purpose. Instead, we explore a range of alternative possibilities for accounting for cosmic purpose. Perhaps our universe was created by an evil or morally indifferent designer, or a designer with limited abilities. Perhaps we live in a computer simulation. Maybe cosmic purpose is rooted not in a conscious mind but in natural tendencies towards the good, or laws of nature with purposes built into them. Or maybe the universe is itself a conscious mind which directs itself towards certain goals. Goff scrutinises these options with analytic rigour, laying the groundwork for a new paradigm of philosophical enquiry into the middle ground between God and atheism. The final chapter outlines a way of living in hope that cosmic purpose is still unfolding, involving political engagement and a non-literalist interpretation of traditional religion.

@book{doi101093oso97801988837600010001,
    author = "Goff, Philip",
    title = "Why? The Purpose of the Universe",
    year = "2023",
    abstract = "Abstract Western thought has been dominated by the dichotomy of traditional religion and secular atheism. But do we have to choose between these options? Philip Goff argues that it is time to move on from both God and atheism. Through an exploration of contemporary cosmology, as well as cutting-edge philosophical research on the nature of consciousness, Goff argues for cosmic purpose: the idea that the universe is directed towards certain goals, such as the emergence of intelligent life. However, in contrast to religious thinkers, Goff argues that the Omni-God (defined as all-knowing, all-powerful, and perfectly good) is a bad explanation of cosmic purpose. Instead, we explore a range of alternative possibilities for accounting for cosmic purpose. Perhaps our universe was created by an evil or morally indifferent designer, or a designer with limited abilities. Perhaps we live in a computer simulation. Maybe cosmic purpose is rooted not in a conscious mind but in natural tendencies towards the good, or laws of nature with purposes built into them. Or maybe the universe is itself a conscious mind which directs itself towards certain goals. Goff scrutinises these options with analytic rigour, laying the groundwork for a new paradigm of philosophical enquiry into the middle ground between God and atheism. The final chapter outlines a way of living in hope that cosmic purpose is still unfolding, involving political engagement and a non-literalist interpretation of traditional religion.",
    url = "https://doi.org/10.1093/oso/9780198883760.001.0001",
    doi = "10.1093/oso/9780198883760.001.0001",
    openalex = "W4387137342",
    references = "doi1010179781316661413, doi101093oso97801906770150010001"
}