@article{levitt1952the,
    author = "Levitt, I.M.",
    title = "The astronomical universe",
    year = "1952",
    journal = "Journal of the Franklin Institute",
    url = "https://doi.org/10.1016/0016-0032(52)90693-5",
    doi = "10.1016/0016-0032(52)90693-5",
    number = "6",
    openalex = "W2320479335",
    pages = "614",
    volume = "253"
}

@article{krogdahl1953the,
    author = "Krogdahl, Wasley S. and Riggs, Philip S.",
    title = "The Astronomical Universe",
    year = "1953",
    journal = "American Journal of Physics",
    url = "https://doi.org/10.1119/1.1933353",
    doi = "10.1119/1.1933353",
    number = "1",
    openalex = "W1997173335",
    pages = "69-69",
    volume = "21"
}

@article{doi101086148245,
    author = "Sandage, Allan",
    title = "The Existence of a Major New Constituent of the Universe: the Quasistellar Galaxies.",
    year = "1965",
    journal = "The Astrophysical Journal",
    abstract = {Photometric, number count, and spectrographic evidence is presented to show that most of the blue, starlike objects fainter than mpg = 16"' found in color surveys of high4atitude fields are extragalactic and represent an entirely new class of objects Members of the class called here quasi-stellar galaxies (QSG) resemble the quasi-stellar radio sources (QSS) in many optical properties, but they are radio-quiet. The QSG brighter than `npg = 19"' are 10 times more numerous per square degree than the QSS that are brighter than 9 flux units. The surface density of QSG is about 4 objects per square degree to `npg = 19"'. The evidence is developed in three parts: (1) Photoelectric photometry shows that a fundamental change occurs in the color distribution of high-latitude blue objects at about V = 14."'5. Brighter than this, the objects fall near the luminosity class V line of the U - B, B - V diagram. Fainter than this, 80 per cent of the objects lie in the peculiar region known to be occupied by the quasi-stellar radio sources. (2) The observed integral-count-curve, log N(m), for objects in the Haro-Luyten catalogue undergoes a profound change of slope between `npg = 12"' and `npg = 15"', steepening and reaching a constant slope for mpg fainter than 16"'. This magnitude interval is the same as that in which the color distribution changes, as discussed above. The slope fainter than 16"' is d log N(m)/dm = 0.383. It is shown that this is the expected value from the theory of cosmological number counts for uniformly distributed objects with large redshifts. (3) Spectra of five of the faint blue objects are similar to spectra of quasi-stellar radio sources Intense, sharp emission lines of forbidden [0 iii], [0 ii], and [Ne iii], together with very broad (35 A wide) lines of H, H, H, Ho, and [Ne v] are present in two of the five. Two broad emission lines are present in another at X 3473 and X 4279, identified as C lv (1550) and C iii (1909). The other two objects have featureless spectra with only a blue continuum showing. The redshifts (AX/ 0) for the three objects with lines are 0.0877, 0.1307, and 1.2410. The position of the objects in the redshift-apparentmagnitude diagram shows each of the three to be superluminous. The space density of the quasi-stellar galaxies is estimated to be about 5 X 10-00 QSG/cm3, which is to be compared with the space density of normal galaxies of about 1 X 10-70 galaxies/cm3. The ratio, per unit volume, of QSG to QSS is estimated to be 500, which gives a lifetime of the QSG phase as 5 X 108 years if the lifetime of the radio source is 108 years. The objects would seem to be of major importance in the solution of the cosmological problem. They can be found at great distances because of their high luminosity. QSG at B = 22"' are estimated to have a mean redshift of Ax/x0 5 for a model universe of qo = +1. At these redshifts, we are sampling the universe in depth to 0.63 of the distance to the horizon (for qo = + 1), and are looking back in time more than 0.9 of the way to the "creation event" in an evolutionary model. Study of the [m, z]- and log N(m)curves using the QSG should eventually provide a crucial test of various cosmological models. But even more important, comparative study of the quasi-stellar galaxies and the intimately connected quasistellar radio sources is expected to shed light on the evolutionary processes of the violent events that characterize the two classes.},
    url = "https://doi.org/10.1086/148245",
    doi = "10.1086/148245",
    openalex = "W1989052264"
}

@misc{freske1980evidence4,
    author = "Freske, S",
    title = "Evidence supporting a great age for the universe",
    year = "1980",
    howpublished = "Creation/ Evolution, v. 1, p. 34-39",
    note = "talkorigins\_source = {true}; raw\_reference = {Freske, S., 1980, Evidence supporting a great age for the universe: Creation/ Evolution, v. 1, p. 34-39.}"
}

@misc{slusher1980age10,
    author = "Slusher, H. S",
    title = "Age of the cosmos",
    year = "1980",
    howpublished = "ICR Technical Monograph, v. 9; Institute for Creation Research, 76 pp",
    note = "talkorigins\_source = {true}; raw\_reference = {Slusher, H. S., 1980, Age of the cosmos: ICR Technical Monograph, v. 9; Institute for Creation Research, 76 pp.}"
}

@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"
}

@misc{setterfield1981the6,
    author = "Setterfield, B",
    title = "The velocity of light and the age of the universe",
    year = "1981",
    howpublished = "Ex Nihilo, v. 4, no. 1, p. 38-48",
    note = "talkorigins\_source = {true}; raw\_reference = {Setterfield, B., 1981, The velocity of light and the age of the universe: Ex Nihilo, v. 4, no. 1, p. 38-48.}"
}

@misc{vandenbergh1981size11,
    author = "Van den Bergh, S",
    title = "Size and age of the universe",
    year = "1981",
    howpublished = "Science, v. 213, p. 825- 830",
    note = "talkorigins\_source = {true}; raw\_reference = {Van den Bergh, S., 1981, Size and age of the universe: Science, v. 213, p. 825- 830.}"
}

@article{doi101086160554,
    author = "Scargle, J. D.",
    title = "Studies in astronomical time series analysis. II - Statistical aspects of spectral analysis of unevenly spaced data",
    year = "1982",
    journal = "The Astrophysical Journal",
    abstract = "Detection of a periodic signal hidden in noise is frequently a goal in astronomical data analysis. This paper does not introduce a new detection technique, but instead studies the reliability and efficiency of detection with the most commonly used technique, the periodogram, in the case where the observation times are unevenly spaced. This choice was made because, of the methods in current use, it appears to have the simplest statistical behavior. A modification of the classical definition of the periodogram is necessary in order to retain the simple statistical behavior of the evenly spaced case. With this modification, periodogram analysis and least-squares fitting of sine waves to the data are exactly equivalent. Certain difficulties with the use of the periodogram are less important than commonly believed in the case of detection of strictly periodic signals. In addition, the standard method for mitigating these difficulties (tapering) can be used just as well if the sampling is uneven. An analysis of the statistical significance of signal detections is presented, with examples",
    url = "https://doi.org/10.1086/160554",
    doi = "10.1086/160554",
    openalex = "W1986316936"
}

@misc{setterfield1982the7,
    author = "Setterfield, B",
    title = "The velocity of light and the age of the universe",
    year = "1982",
    howpublished = "Ex Nihilo, v. 1, no. 1 (International Edition), p. 53-93",
    note = "talkorigins\_source = {true}; raw\_reference = {Setterfield, B., 1982, The velocity of light and the age of the universe: Ex Nihilo, v. 1, no. 1 (International Edition), p. 53-93.}"
}

@misc{abell1983the1,
    author = "Abell, G. O",
    title = "The Ages of the Earth and the Universe, in Godfrey, L",
    year = "1983",
    note = "talkorigins\_source = {true}; raw\_reference = {Abell, G. O., 1983, The Ages of the Earth and the Universe, in Godfrey, L.}"
}

@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"
}

@misc{setterfield1983the8,
    author = "Setterfield, B",
    title = "The velocity of light and the age of the universe",
    year = "1983",
    howpublished = "Ex Nihilo, v. 1, no. 3 (International Edition), p. 41-46",
    note = "talkorigins\_source = {true}; raw\_reference = {Setterfield, B., 1983, The velocity of light and the age of the universe: Ex Nihilo, v. 1, no. 3 (International Edition), p. 41-46.}"
}

@article{fackerell1984the2,
    author = "Fackerell, E",
    title = "The age of the astronomical universe",
    year = "1984",
    journal = "Ex Nihilo Technical Journal, v. 1, p. 87-94",
    note = "talkorigins\_source = {true}; raw\_reference = {Fackerell, E., 1984, The age of the astronomical universe: Ex Nihilo Technical Journal, v. 1, p. 87-94.}"
}

@inproceedings{gentry1984radioactive5,
    author = "Gentry, R. V",
    title = "Radioactive Halos in a Radiochronological and Cosmological Perspective, in Awbery, F. T., and Thwaites, W. M., eds., Evolutionists Confront Creationists",
    year = "1984",
    booktitle = "San Francisco, Ca., American Association for the Advancement of Science, v. 1, Part 3, p. 38-65; Proceedings of the 63rd Annual Meeting of the Pacific Division",
    note = "talkorigins\_source = {true}; raw\_reference = {Gentry, R. V., 1984, Radioactive Halos in a Radiochronological and Cosmological Perspective, in Awbery, F. T., and Thwaites, W. M., eds., Evolutionists Confront Creationists: San Francisco, Ca., American Association for the Advancement of Science, v. 1, Part 3, p. 38-65; Proceedings of the 63rd Annual Meeting of the Pacific Division.}"
}

@article{setterfield1984the9,
    author = "Setterfield, B",
    title = "The age of the astronomical universe--a reply",
    year = "1984",
    journal = "Ex Nihilo Technical Journal, v. 1, p. 95-104",
    note = "talkorigins\_source = {true}; raw\_reference = {Setterfield, B., 1984, The age of the astronomical universe--a reply: Ex Nihilo Technical Journal, v. 1, p. 95-104.}"
}

@article{doi101103revmodphys571,
    author = "Brandenberger, Robert",
    title = "Quantum field theory methods and inflationary universe models",
    year = "1985",
    journal = "Reviews of Modern Physics",
    abstract = "This paper reviews the theory of inflationary universe models, giving particular emphasis to the question of origin and growth of energy-density fluctuations in these new cosmologies. The first four sections constitute a pedagogical introduction to some of the important quantum field theory methods used in inflationary universe scenarios: calculation of the effective potential, finite-temperature quantum field theory, analysis of the decay of a metastable quantum state, and free field theory in curved space-time.",
    url = "https://doi.org/10.1103/revmodphys.57.1",
    doi = "10.1103/revmodphys.57.1",
    openalex = "W2002313202"
}

@article{doi101086184864,
    author = "Winget, D. E. and Hansen, C. and Liebert, James and van Horn, H. M. and Fontaine, G. and Nather, R. E. and Kepler, S. O. and Lamb, D. Q.",
    title = "An independent method for determining the age of the universe",
    year = "1987",
    journal = "The Astrophysical Journal",
    abstract = "The observed number of white dwarfs in a given volume of space increases monotonically with decreasing luminosity, as expected from cooling rate considerations. However, their number drops abruptly at a luminosity of log (L/L\_sun;) ≈ -4.5, due to the finite age of our Galaxy. Comparing this sudden drop in the observed luminosity distribution with the best theoretical evolutionary white dwarf models, the authors derive an age for the Galactic disk of 9.3±2.0 Gyr. To obtain the age of the universe, one must add the time between the big bang and the first appearance of stars in the Galactic disk. The authors choose a value (and stated error) that can include all of the currently reasonable models describing this early era. They estimate the age of the universe to be 10.3±2.2 Gyr.",
    url = "https://doi.org/10.1086/184864",
    doi = "10.1086/184864",
    openalex = "W1998520428"
}

@article{gott1987astronomical,
    author = "Gott, J. R. and Rees, M. J.",
    title = "Astronomical constraints on a string-dominated universe",
    year = "1987",
    journal = "Monthly Notices of the Royal Astronomical Society",
    url = "https://doi.org/10.1093/mnras/227.2.453",
    doi = "10.1093/mnras/227.2.453",
    number = "2",
    openalex = "W2058127636",
    pages = "453-459",
    volume = "227"
}

@misc{ferris1988coming3,
    author = "Ferris, T",
    title = "Coming of Age in the Milky Way",
    year = "1988",
    howpublished = "New York, William Morrow",
    note = "talkorigins\_source = {true}; raw\_reference = {Ferris, T., 1988, Coming of Age in the Milky Way: New York, William Morrow.}"
}

@book{openalexw3007754162,
    author = "Kolb, Edward W. and Turner, Michael S.",
    title = "The Early Universe",
    year = "1990",
    abstract = "* Editors Foreword * The Universe Observed * Robertson-Walker Metric * Standard Cosmology * Big-Bang Nucleosynthesis * Thermodynamics in the Expanding Universe * Baryogenesis * Phase Transitions * Inflation * Structure Formation * Axions * Toward the Planck Epoch * Finale",
    openalex = "W3007754162"
}

@book{openalexw1681076102,
    author = "Padmanabhan, Τ.",
    title = "Structure formation in the universe",
    year = "1993",
    booktitle = "CERN Document Server (European Organization for Nuclear Research)",
    abstract = "Preface Part I. The Smooth Universe: 1. Introducing the Universe 2. The Friedmann model 3. Thermal history of the Universe Part II. The Clumpy Universe: 4. Growth of linear perturbations 5. Statistical properties of the density fluctuations 6. The microwave background radiation 7. The linear theory: velocity fields 8. The non-linear evolution 9. The non-linear theory: high redshift objects Part III. Towards a More Complete Picture: 10. The origin of initial perturbations 11. Dark matter 12. Epilogue Appendices Notes and references Index.",
    openalex = "W1681076102"
}

@article{doi101086311074,
    author = "Spergel, David N. and Pen, Ue‐Li",
    title = "Cosmology in a String-Dominated Universe",
    year = "1997",
    journal = "The Astrophysical Journal",
    abstract = "The string-dominated universe locally resembles an open universe, and fits dynamical measures of power spectra, cluster abundances, redshift distortions, lensing constraints, luminosity and angular diameter distance relations and microwave background observations. We show examples of networks which might give rise to recent string-domination without requiring any fine-tuned parameters. We discuss how future observations can distinguish this model from other cosmologies. 1.",
    url = "https://doi.org/10.1086/311074",
    doi = "10.1086/311074",
    openalex = "W2103991091",
    references = "doi1010160370157380900915, doi1010631881088, doi101086177793, doi101086304265, doi1010880305447098029, doi101103revmodphys51591, doi101201b16971, doi105860choice311499, gott1987astronomical, openalexw1800127362, openalexw3007754162"
}

@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"
}

@article{doi101086319535,
    author = "Fontaine, G. and Brassard, P. and Bergeron, P.",
    title = "The Potential of White Dwarf Cosmochronology",
    year = "2001",
    journal = "Publications of the Astronomical Society of the Pacific",
    abstract = {In the light of recent significant progress on both the observational and theoretical fronts, we review the status of white dwarf stars as cosmochronometers. These objects represent the end products of stellar evolution for the vast majority of stars and, as such, can be used to constrain the ages of various populations of evolved stars in the Galaxy. For example, the oldest white dwarfs in the solar neighborhood (the remnants of the very first generation of intermediate‐mass stars in the Galactic disk) are still visible and can be used, in conjunction with cooling theory, to estimate the age of the disk. More recent observations suggest the tantalizing possibility that a population of very old white dwarfs inhabits the Galactic halo. Such a population may contribute significantly to baryonic "dark" matter in the Milky Way and may be used to obtain an independent estimate of the age of the halo. In addition, white dwarf cosmochronology is likely to play a very significant role in the coming era of giant 8–10 m telescopes when faint white dwarf populations should be routinely discovered and studied in open and globular clusters.},
    url = "https://doi.org/10.1086/319535",
    doi = "10.1086/319535",
    openalex = "W2175046768",
    references = "doi101086133661, doi101086146614, doi101086177381, doi101086184864, doi101086191659, doi101086192204, doi101086192264, doi101086320356, doi101146annurevaa13090175000441, doi1015159781400879175"
}

@article{doi101111j13652966200407881x,
    author = "Brinchmann, J. and Charlot, S. and White, Simon D. M. and Tremonti, Christy and Kauffmann, Guinevere and Heckman, Timothy M. and Brinkmann, J.",
    title = "The physical properties of star-forming galaxies in the low-redshift Universe",
    year = "2004",
    journal = "Monthly Notices of the Royal Astronomical Society",
    abstract = "Abstract We present a comprehensive study of the physical properties of ∼ 105 galaxies with measurable star formation in the Sloan Digital Sky Survey (SDSS). By comparing physical information extracted from the emission lines with continuum properties, we build up a picture of the nature of star-forming galaxies at z \< 0.2. We develop a method for aperture correction using resolved imaging and show that our method takes out essentially all aperture bias in the star formation rate (SFR) estimates, allowing an accurate estimate of the total SFRs in galaxies. We determine the SFR density to be 1.915+0.02−0.01 (random)+0.14−0.42 (systematic) h7010−2 M⊙ yr−1 Mpc−3 at z= 0.1 (for a Kroupa initial mass function) and we study the distribution of star formation as a function of various physical parameters. The majority of the star formation in the low-redshift Universe takes place in moderately massive galaxies (1010–1011 M⊙), typically in high surface brightness disc galaxies. Roughly 15 per cent of all star formation takes place in galaxies that show some sign of an active nucleus. About 20 per cent occurs in starburst galaxies. By focusing on the SFR per unit mass we show that the present to past average SFR, the Scalo b-parameter, is almost constant over almost three orders of magnitude in mass, declining only at M* \> 1010 M⊙. The volume averaged b parameter is 0.408+0.005−0.002 (random)+0.029−0.090 (systematic)h−170. We use this value to constrain the star formation history of the Universe. For the concordance cosmology the present-day Universe is forming stars at at least 1/3 of its past average rate. For an exponentially declining cosmic star formation history this corresponds to a time-scale of 7+0.7−1.5 Gyr. In agreement with other work we find a correlation between b and morphological type, as well as a tight correlation between the 4000-Å break (D4000) and b. We discuss how D4000 can be used to estimate b parameters for high-redshift galaxies.",
    url = "https://doi.org/10.1111/j.1365-2966.2004.07881.x",
    doi = "10.1111/j.1365-2966.2004.07881.x",
    openalex = "W2166365370",
    references = "doi101086145971, doi1023071269179, doi1023073556160"
}

@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"
}

@incollection{crossref2009radioactive,
    title = "Radioactive cosmochronology",
    year = "2009",
    booktitle = "Nucleosynthesis and Chemical Evolution of Galaxies",
    url = "https://doi.org/10.1017/cbo9780511812170.012",
    doi = "10.1017/cbo9780511812170.012",
    openalex = "W1014328234",
    pages = "327-344"
}

@article{crossref2009the,
    title = "The Birds and the Dinosaurs",
    year = "2009",
    journal = "Science",
    url = "https://doi.org/10.1126/science.324\_565d",
    doi = "10.1126/science.324\_565d",
    number = "5927",
    pages = "565-565",
    volume = "324"
}

@book{doi101017cbo9780511735288,
    author = "Hearnshaw, J. B.",
    title = "Astronomical Spectrographs and their History",
    year = "2009",
    booktitle = "Cambridge University Press eBooks",
    abstract = "Astronomical spectrographs analyse light emitted by the Sun, stars, galaxies and other objects in the Universe, and have been used in astronomy since the early nineteenth century. This book provides a comprehensive account of spectrographs from an historical perspective, from their theory and development over the last two hundred years, to the recent advances of the early twenty-first century. The author combines the theoretical principles behind astronomical spectrograph design with their historical development. Spectrographs of all types are considered, with prism, grating or grism dispersing elements. Included are Cassegrain, coudé, prime focus, échelle, fibre-fed, ultraviolet, nebular, objective prism, multi-object instruments and those which are ground-based, on rockets and balloons or in space. The book contains several tables listing the most significant instruments, around 900 references, and over 150 images, making it an indispensable reference for professional astronomers, graduate students, advanced amateur astronomers, and historians of science.",
    url = "https://doi.org/10.1017/cbo9780511735288",
    doi = "10.1017/cbo9780511735288",
    openalex = "W1665688180"
}

@article{doi105860choice491435,
    title = "Astronomical spectroscopy: an introduction to the atomic and molecular physics of astronomical spectra",
    year = "2011",
    journal = "Choice Reviews Online",
    abstract = "Why Record Spectra of Astronomical Objects? The Nature of Spectra Atomic Hydrogen Complex Atoms Helium Spectra Alkali Atoms Spectra of Nebulae X-Ray Spectra Molecular Structure Molecular Spectra",
    url = "https://doi.org/10.5860/choice.49-1435",
    doi = "10.5860/choice.49-1435",
    openalex = "W1635040702"
}

@article{blouin2020toward,
    author = "Blouin, Simon and Daligault, Jérôme and Saumon, Didier and Bédard, Antoine and Brassard, Pierre",
    title = "Toward precision cosmochronology",
    year = "2020",
    journal = "Astronomy \& Astrophysics",
    abstract = "The continuous cooling of a white dwarf is punctuated by events that affect its cooling rate. The most significant of these events is the crystallization of its core, a phase transition that occurs once the C/O interior has cooled down below a critical temperature. This transition releases latent heat, as well as gravitational energy due to the redistribution of the C and O ions during solidification, thereby slowing down the evolution of the white dwarf. The unambiguous observational signature of core crystallization–a pile-up of objects in the cooling sequence–was recently reported. However, existing evolution models struggle to quantitatively reproduce this signature, casting doubt on their accuracy when used to measure the ages of stellar populations. The timing and amount of the energy released during crystallization depend on the exact form of the C/O phase diagram. Using the advanced Gibbs–Duhem integration method and state-of-the-art Monte Carlo simulations of the solid and liquid phases, we obtained a very accurate version of this phase diagram that allows a precise modeling of the phase transition. Despite this improvement, the magnitude of the crystallization pile-up remains underestimated by current evolution models. We conclude that latent heat release and O sedimentation alone are not sufficient to explain the observations, and that other unaccounted physical mechanisms, possibly 22 Ne phase separation, play an important role.",
    url = "https://doi.org/10.1051/0004-6361/202038879",
    doi = "10.1051/0004-6361/202038879",
    openalex = "W4288080073",
    pages = "L11",
    volume = "640",
    references = "doi101007s0015901000331, doi101046j13658711200003426x, doi1010631465023, doi101086133661, doi101086145971, doi101086184864, doi101086319535, doi101086516819, doi1010880004637x7302128, doi101093mnrassty3016"
}

@article{doi10384715384357ad3df7,
    author = "Monjo, Robert",
    title = "What if the Universe Expands Linearly? A Local General Relativity to Solve the “Zero Active Mass” Problem",
    year = "2024",
    journal = "The Astrophysical Journal",
    abstract = "Abstract Modern cosmology presents important challenges such as the Hubble Tension, El Gordo’s collision, or the impossible galaxies (z > 10). Slight modifications to the standard model propose new parameters (e.g., the early and dynamical dark energy). On the other hand, alternatives such as the coasting universes (e.g., the hyperconical model and the spatially flat R h = ct universe) are statistically compatible with most of the observational tests, but still present theoretical problems in matching the observed matter contents since they predict a “zero active gravitational mass.” To solve these open issues, we suggest that general relativity might be not valid at cosmic scales, but it would be valid at local scales. This proposal is addressed from two main features of the embedding hyperconical model: (1) the background metric would be independent of the matter content, and (2) the observed cosmic acceleration would be fictitious and because of a distorted stereographic projection of coordinates that produce an apparent radial inhomogeneity from homogeneous manifolds. Finally, to support the discussion, standard observational tests were updated here, showing that the hyperconical model is adequately fitted to Type Ia supernovae, quasars, galaxy clusters, baryon acoustic oscillations, and cosmic chronometer data sets.",
    url = "https://doi.org/10.3847/1538-4357/ad3df7",
    doi = "10.3847/1538-4357/ad3df7",
    openalex = "W4397023665",
    references = "doi10108802649381145016"
}