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fix: Update bibliography records
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Expand Up @@ -9,25 +9,6 @@ @book{abramowitz_handbook_1970
note = {OCLC: 18003605}
}

@article{abrarov_rapid_2013,
title = {A rapid and highly accurate approximation for the error function of complex argument},
volume = {1308},
url = {http://adsabs.harvard.edu/abs/2013arXiv1308.3399A},
abstract = {We present efficient approximation of the error function obtained by
Fourier expansion of the exponential function \${\textbackslash}exp [\{- \{(t - 2
{\textbackslash}sigma){\textasciicircum}2\}/4\}]\$. The error analysis reveals that it is highly accurate
and can generate numbers that match up to the last decimal digits with
reference values. Due to simple representation the proposed error
function approximation can be utilized in a rapid algorithm.},
urldate = {2014-09-04},
journal = {{ArXiv} e-prints},
author = {Abrarov, S. M. and Quine, B. M.},
month = aug,
year = {2013},
keywords = {Mathematics - Numerical Analysis},
pages = {3399}
}

@article{abel_modeling_1997,
title = {Modeling primordial gas in numerical cosmology},
volume = {2},
Expand Down Expand Up @@ -353,21 +334,6 @@ @article{baugh_can_2005
pages = {1191--1200}
}

@article{begelman_accreting_2014,
title = {Accreting {Black} {Holes}},
volume = {1410},
url = {http://adsabs.harvard.edu/abs/2014arXiv1410.8132B},
abstract = {I outline the theory of accretion onto black holes, and its application to observed phenomena such as X-ray binaries, active galactic nuclei, tidal disruption events, and gamma-ray bursts. The dynamics as well as radiative signatures of black hole accretion depend on interactions between the relatively simple black-hole spacetime and complex
radiation, plasma and magnetohydrodynamical processes in the surrounding gas. I will show how transient accretion processes could provide clues to these interactions. Larger global magnetohydrodynamic simulations as well as simulations incorporating plasma microphysics and full radiation hydrodynamics will be needed to unravel some of the current mysteries of black hole accretion.},
urldate = {2016-03-31},
journal = {ArXiv e-prints},
author = {Begelman, Mitchell C.},
month = oct,
year = {2014},
keywords = {Astrophysics - High Energy Astrophysical Phenomena},
pages = {arXiv:1410.8132}
}

@article{behroozi_comprehensive_2010,
title = {A Comprehensive Analysis of Uncertainties Affecting the Stellar Mass-Halo Mass Relation for 0 {\textless} z {\textless} 4},
volume = {717},
Expand Down Expand Up @@ -543,40 +509,6 @@ @article{benson_galaxy_2010-1
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@misc{benson_cold_2010,
title = {Cold Mode Accretion in Galaxy Formation},
url = {http://adsabs.harvard.edu/abs/2010arXiv1004.1162B},
abstract = {A generic expectation for gas accreted by high mass haloes is that it is
shock heated to the virial temperature of the halo. In low mass haloes,
or at high redshift, however, the gas cooling rate is sufficiently rapid
that an accretion shock is unlikely to form. Instead, gas can accrete
directly into the centre of the halo in a `cold mode' of accretion.
Although semi-analytic models have always made a clear distinction
between hydrostatic and rapid cooling they have not made a distinction
between whether or not an accretion shock forms. Starting from the
well-established Galform code, we investigate the effect of explicitly
accounting for cold mode accretion using the shock stability model of
Birnboim \& Dekel. When we modify the code so that there is no
effective feedback from galaxy formation, we find that cold mode
accretion is the dominant channel for feeding gas into the galaxies at
high redshifts. However, this does not translate into a significant
difference in the star formation history of the universe compared to the
previous code. When effective feedback is included in the model, we find
that the the cold mode is much less apparent because of the presence of
gas ejected from the galaxy. Thus the inclusion of the additional cold
mode physics makes little difference to basic results from earlier
semi-analytic models which used a simpler treatment of gas accretion.
For more sophisticated predictions of its consequences, we require a
better understanding of how the cold mode delivers angular momentum to
galaxies and how it interacts with outflows.},
journal = {{ArXiv} e-prints},
author = {Andrew J. Benson and Richard Bower},
month = apr,
year = {2010},
keywords = {Astrophysics - Cosmology and Extragalactic Astrophysics},
howpublished = {{http://adsabs.harvard.edu/abs/2010arXiv1004.1162B}}
},

@article{benson_comparison_2001,
title = {A comparison of semi-analytic and smoothed particle hydrodynamics galaxy formation},
volume = {320},
Expand Down Expand Up @@ -2284,23 +2216,6 @@ @article{dutton_cold_2014
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{dijkstra_saas-fee_2017,
author = {{Dijkstra}, Mark},
title = "{Saas-Fee Lecture Notes: Physics of Lyman Alpha Radiative Transfer}",
journal = {arXiv e-prints},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
year = 2017,
month = apr,
eid = {arXiv:1704.03416},
pages = {arXiv:1704.03416},
doi = {10.48550/arXiv.1704.03416},
archivePrefix = {arXiv},
eprint = {1704.03416},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017arXiv170403416D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{edgar_review_2004,
title = {A review of {Bondi-Hoyle-Lyttleton} accretion},
volume = {48},
Expand Down Expand Up @@ -3426,23 +3341,6 @@ @article{hoffman_dynamics_2007
pages = {957--976}
}

@article{hogan_warm_1999,
author = {{Hogan}, Craig J.},
title = "{Warm Dark Matter: Clues to Primordial Phase Density from the Structure of Galaxy Halos}",
journal = {arXiv e-prints},
keywords = {Astrophysics},
year = 1999,
month = dec,
eid = {astro-ph/9912549},
pages = {astro-ph/9912549},
doi = {10.48550/arXiv.astro-ph/9912549},
archivePrefix = {arXiv},
eprint = {astro-ph/9912549},
primaryClass = {astro-ph},
adsurl = {https://ui.adsabs.harvard.edu/abs/1999astro.ph.12549H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{hogg_k_2002,
title = {The K correction},
url = {http://arxiv.org/abs/astro-ph/0210394},
Expand Down Expand Up @@ -5398,28 +5296,6 @@ @article{moustakas_primus:_2013
file = {NASA/ADS Full Text PDF:/home/abenson/.mozilla/firefox/f54gqgdx.default/zotero/storage/8BQF56IF/Moustakas et al. - 2013 - PRIMUS Constraints on Star Formation Quenching an.pdf:application/pdf}
}

@misc{munoz-cuartas_redshift_2011,
title = {The Redshift Evolution of {LCDM} Halo Parameters},
url = {http://adsabs.harvard.edu/abs/2011arXiv1102.2186M},
abstract = {We study the mass and redshift dependence of the concentration parameter
in Nbody simulations spanning masses from \$10{\textasciicircum}{10} {{\textbackslash}hMsun\$} to \$10{\textasciicircum}{15}
{{\textbackslash}hMsun\$} and redshifts from 0 to 2. We present a series of fitting
formulas that accurately describe the time evolution of the
concentration-mass relation since z=2. Using arguments based on the
spherical collapse model we study the behaviour of the scale length of
the density profile during the assembly history of haloes, obtaining
physical insights on the origin of the observed time evolution of the
concentration mass relation. We present preliminary results of the
implementation of this model in the prediction of the values of the
concentration parameter for different masses and redshifts.},
journal = {{ArXiv} e-prints},
author = {J. C. {Muñoz-Cuartas} and Andrea Macci`o and Stefan Gottlöber and Aaron Dutton},
month = feb,
year = {2011},
keywords = {Astrophysics - Cosmology and Extragalactic Astrophysics},
howpublished = {{http://adsabs.harvard.edu/abs/2011arXiv1102.2186M}}
}

@article{murgia_non-cold_2017,
title = {"{Non}-cold" dark matter at small scales: a general approach},
volume = {11},
Expand Down Expand Up @@ -5890,23 +5766,6 @@ @article{patej_simple_2015
file = {NASA/ADS Full Text PDF:/home/abenson/.mozilla/firefox/f54gqgdx.default/zotero/storage/H5RVH63V/Patej and Loeb - 2015 - A Simple Physical Model for the Gas Distribution i.pdf:application/pdf}
}

@misc{peimbert_primordial_2008,
title = {The Primordial Helium Abundance},
url = {http://adsabs.harvard.edu/abs/2008arXiv0811.2980P},
abstract = {I present a brief review on the determination of the primordial helium
abundance by unit mass, Yp. I discuss the importance of the primordial
helium abundance in: (a) cosmology, (b) testing the standard big bang
nucleosynthesis, (c) studying the physical conditions in H {II} regions,
(d) providing the initial conditions for stellar evolution models, and
(e) testing the galactic chemical evolution models.},
journal = {{ArXiv} e-prints},
author = {Manuel Peimbert},
month = nov,
year = {2008},
keywords = {Astrophysics},
howpublished = {{http://adsabs.harvard.edu/abs/2008arXiv0811.2980P}}
},

@article{peacock_non-linear_1996,
title = {Non-linear evolution of cosmological power spectra},
volume = {280},
Expand Down

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