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@article{baugh_primer_2006,
title = {A primer on hierarchical galaxy formation: the semi-analytical approach},
volume = {69},
issn = {0034-4885},
shorttitle = {A primer on hierarchical galaxy formation},
url = {http://stacks.iop.org/0034-4885/69/i=12/a=R02},
doi = {10.1088/0034-4885/69/12/R02},
abstract = {Recent observational and theoretical breakthroughs make this an exciting time to be working towards understanding the physics of galaxy formation. The goal of this review is to make the principles behind the hierarchical paradigm accessible to a wide audience by providing a pedagogical introduction to modern theories of galaxy formation. I outline the ingredients of the powerful approach called semi-analytical modelling and contrast this method with numerical simulations of the gas dynamics of baryons. Semi-analytical models have enjoyed many successes, but it is the observations which the models struggle to match which mark out areas where future progress is most likely to be made; these are also reviewed.},
language = {en},
number = {12},
urldate = {2017-01-18},
journal = {Reports on Progress in Physics},
author = {Baugh, C. M.},
year = {2006},
pages = {3101}
}
@article{coe_dark_2010,
title = {Dark {Matter} {Halo} {Mass} {Profiles}},
url = {http://arxiv.org/abs/1005.0411},
abstract = {I provide notes on the NFW, Einasto, Sersic, and other mass profiles which provide good fits to simulated dark matter halos (S3). I summarize various published c(M) relations: halo concentration as a function of mass (S1). The definition of the virial radius is discussed and relations are given to convert c\_vir, M\_vir, and r\_vir between various defined values of the halo overdensity (S2).},
urldate = {2017-01-12},
journal = {arXiv:1005.0411 [astro-ph]},
author = {Coe, Dan},
month = may,
year = {2010},
note = {arXiv: 1005.0411},
keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},
annote = {Comment: 14 pages, 20 figures, not submitted to any journal. Comments welcome at http://scirate.com/who.php?id=1005.xxxx\&what=comments (insert arXiv number at xxxx; free \& easy registration). If I failed to cite your work, please let me know.},
file = {arXiv\:1005.0411 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/5SPB6ZHD/Coe - 2010 - Dark Matter Halo Mass Profiles.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/5HZF5799/1005.html:text/html}
}
@article{ostriker_maximally_2011,
title = {Maximally {Star}-forming {Galactic} {Disks}. {I}. {Starburst} {Regulation} {Via} {Feedback}-driven {Turbulence}},
volume = {731},
issn = {0004-637X},
url = {http://stacks.iop.org/0004-637X/731/i=1/a=41},
doi = {10.1088/0004-637X/731/1/41},
abstract = {Star formation rates in the centers of disk galaxies often vastly exceed those at larger radii, whether measured by the surface density of star formation Σ SFR , by the star formation rate per unit gas mass, Σ SFR /Σ, or even by total output. In this paper, we investigate the idea that central starbursts are self-regulated systems in which the momentum flux injected to the interstellar medium (ISM) by star formation balances the gravitational force confining the ISM gas in the disk. For most starbursts, supernovae are the largest contributor to the momentum flux, and turbulence provides the main pressure support for the predominantly molecular ISM. If the momentum feedback per stellar mass formed is p * / m * 3000 km s –1 , the predicted star formation rate is Σ SFR 2π G Σ 2 m * / p * 0.1 M ☉ kpc –2 yr –1 (Σ/100 M ☉ pc –2 ) 2 in regions where gas dominates the vertical gravity. We compare this prediction with numerical simulations of vertically resolved disks that model star formation including feedback, finding good agreement for gas surface densities in the range Σ 10 2 -10 3 M ☉ pc –2 . We also compare to a compilation of star formation rates and gas contents from local and high-redshift galaxies (both mergers and normal galaxies), finding good agreement provided that the conversion factor X CO from integrated CO emission to H 2 surface density decreases modestly as Σ and Σ SFR increase. Star formation rates in dense, turbulent gas are also expected to depend on the gravitational free-fall time at the corresponding mean ISM density ρ 0 ; if the star formation efficiency per free-fall time is ε ff (ρ 0 ) 0.01, the turbulent velocity dispersion driven by feedback is expected to be v z = 0.4 ε ff (ρ 0 ) p * / m * 10 km s –1 , relatively independent of Σ or Σ SFR . Turbulence-regulated starbursts (controlled by kinetic momentum feedback) are part of the larger scheme of self-regulation; primarily atomic low-Σ outer disks may have star formation regulated by ultraviolet heating feedback, whereas regions at extremely high Σ may be regulated by feedback of stellar radiation that is reprocessed into trapped infrared.},
language = {en},
number = {1},
urldate = {2016-11-14},
journal = {The Astrophysical Journal},
author = {Ostriker, Eve C. and Shetty, Rahul},
year = {2011},
pages = {41},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/HZW88XKE/Ostriker and Shetty - 2011 - Maximally Star-forming Galactic Disks. I. Starburs.pdf:application/pdf}
}
@article{bower_breaking_2006,
title = {Breaking the hierarchy of galaxy formation},
volume = {370},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2006MNRAS.370..645B},
doi = {10.1111/j.1365-2966.2006.10519.x},
abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AGN) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the
volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z {\textasciitilde} 5 and a star
formation rate density which rises at least out to z {\textasciitilde} 2 in objects of all masses. Although observational data on these properties have been cited as evidence for `antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations.},
urldate = {2017-02-21},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.},
month = aug,
year = {2006},
keywords = {galaxies: evolution, galaxies: evolution: galaxies: formation: galaxies: luminosity function, galaxies: formation, galaxies: luminosity function},
pages = {645--655},
file = {NASA/ADS Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/JHBAXZGU/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation.pdf:application/pdf}
}
@article{white_galaxy_1991,
title = {Galaxy formation through hierarchical clustering},
volume = {379},
issn = {0004-637X},
url = {http://adsabs.harvard.edu/abs/1991ApJ...379...52W},
doi = {10.1086/170483},
abstract = {Analytic methods for studying the formation of galaxies by gas condensation within massive dark halos are presented. The present scheme applies to cosmogonies where structure grows through hierarchical clustering of a mixture of gas and dissipationless dark matter. The simplest models consistent with the current understanding of N-body work on dissipationless clustering, and that of numerical and analytic work on gas evolution and cooling are adopted. Standard models for the evolution of the stellar population are also employed, and new models for the way star formation heats and enriches the surrounding gas are constructed. Detailed results are presented for a cold dark matter universe with Omega = 1 and H(0) = 50 km/s/Mpc, but the present methods are applicable to other models. The present luminosity functions contain significantly more faint galaxies than are observed.},
urldate = {2016-10-18},
journal = {The Astrophysical Journal},
author = {White, Simon D. M. and Frenk, Carlos S.},
month = sep,
year = {1991},
keywords = {Analytic Functions, Brightness Distribution, Cosmology, Dark Matter, Galactic Clusters, Galactic Evolution, Galactic Structure, Halos, Numerical Analysis, seminal, Star Distribution, Star Formation},
pages = {52--79},
file = {NASA/ADS Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/KK2D75MM/White and Frenk - 1991 - Galaxy formation through hierarchical clustering.pdf:application/pdf}
}
@article{joung_dependence_2009,
title = {Dependence of {Interstellar} {Turbulent} {Pressure} on {Supernova} {Rate}},
volume = {704},
issn = {0004-637X},
url = {http://stacks.iop.org/0004-637X/704/i=1/a=137},
doi = {10.1088/0004-637X/704/1/137},
abstract = {Feedback from massive stars is one of the least understood aspects of galaxy formation. We perform a suite of vertically stratified local interstellar medium (ISM) models in which supernova (SN) rates and vertical gas column densities are systematically varied based on the Schmidt-Kennicutt law. Our simulations have a sufficiently high spatial resolution (1.95 pc) to follow the hydrodynamic interactions among multiple SNe that structure the interstellar medium. At a given SN rate, we find that the mean mass-weighted sound speed and velocity dispersion decrease as the inverse square root of gas density. The sum of thermal and turbulent pressures is nearly constant in the midplane, so the effective equation of state is isobaric. In contrast, across our four models having SN rates that range from 1 to 512 times the Galactic SN rate, the mass-weighted velocity dispersion remains in the range 4-6 km s –1 . Hence, gas averaged over 100 pc regions follows P \#\#IMG\#\# [http://ej.iop.org/icons/Entities/vprop.gif] vprop ρ α with α \#\#IMG\#\# [http://ej.iop.org/icons/Entities/ap.gif] ≈ 1, indicating that the effective equation of state on this scale is close to isothermal. Simulated H I emission lines have widths of 10-18 km s –1 , comparable to observed values. In our highest SN rate model, superbubble blow-outs occur, and the turbulent pressure on large scales is \#\#IMG\#\# [http://ej.iop.org/icons/Entities/gsim.gif] gsim 4 times higher than the thermal pressure. We find a tight correlation between the thermal and turbulent pressures averaged over 100 pc regions in the midplane of each model, as well as across the four ISM models. We construct a subgrid model for turbulent pressure based on analytic arguments and explicitly calibrate it against our stratified ISM simulations. The subgrid model provides a simple yet physically motivated way to include SN feedback in cosmological simulations.},
language = {en},
number = {1},
urldate = {2016-10-28},
journal = {The Astrophysical Journal},
author = {Joung, M. Ryan and Low, Mordecai-Mark Mac and Bryan, Greg L.},
year = {2009},
pages = {137},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/AGBC8QC2/Joung et al. - 2009 - Dependence of Interstellar Turbulent Pressure on S.pdf:application/pdf}
}
@article{ferriere_interstellar_2001,
title = {The {Interstellar} {Environment} of our {Galaxy}},
volume = {73},
issn = {0034-6861, 1539-0756},
url = {http://arxiv.org/abs/astro-ph/0106359},
doi = {10.1103/RevModPhys.73.1031},
abstract = {We review the current knowledge and understanding of the interstellar medium of our galaxy. We first present each of the three basic constituents - ordinary matter, cosmic rays, and magnetic fields - of the interstellar medium, laying emphasis on their physical and chemical properties inferred from a broad range of observations. We then position the different interstellar constituents, both with respect to each other and with respect to stars, within the general galactic ecosystem.},
number = {4},
urldate = {2017-01-03},
journal = {Reviews of Modern Physics},
author = {Ferriere, Katia M.},
month = dec,
year = {2001},
note = {arXiv: astro-ph/0106359},
keywords = {Astrophysics},
pages = {1031--1066},
annote = {Comment: 39 pages, 12 figures (including 3 figures in 2 parts)},
file = {arXiv\:astro-ph/0106359 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/PADKQQAA/Ferriere - 2001 - The Interstellar Environment of our Galaxy.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/CA235JI3/0106359.html:text/html}
}
@article{porcel_radial_1997,
title = {The radial scale length of the {Milky} {Way}},
url = {http://arxiv.org/abs/astro-ph/9710197},
abstract = {The radial scale length of the exponential component of the disc of the Milky Way has been determined in the near infrared. We have used the TMGS (Two Micron Galactic Survey) database which contains positions and K-magnitudes of about 700.000 stars distributed in serveral regions along the galactic plane. From those we have selected areas more than \$5{\textasciicircum}{\textbackslash}circ\$ off the plane to minimize the effect of extinction and the contributions of the young disc; and with longitudes ranging from \$30{\textasciicircum}{\textbackslash}circ\$ to \$70{\textasciicircum}{\textbackslash}circ\$, to avoid contaminations from the central bulge, the bar and the molecular ring, in the inner end, and from the local arm, the warp and the truncation of the disc, in the outer end. We observed stars with magnitude \$ 9 {\textbackslash}leq m\_K {\textbackslash}leq 10 \$. The use of the NIR K-band also reduces the effect of extinction. In the observation region, m\_K=9.5 mag stars are K2-K5 III stars, with an absolute magnitude that is nearly constant, which also greatly simplifies the problem. We have obtained the value \$2.1 {\textbackslash}pm 0.3 kpc\$ for the radial scale length, which is a typical value when compared with external galaxies of similar types.},
urldate = {2017-03-04},
journal = {arXiv:astro-ph/9710197},
author = {Porcel, C. and Garzon, F. and Jimenez-Vicente, J. and Battaner, E.},
month = oct,
year = {1997},
note = {arXiv: astro-ph/9710197},
keywords = {Astrophysics},
annote = {Comment: 4 pages, LaTeX using A\&A macros v3. 1 figure. To appear in A\&A. Also available at http://deneb.ugr.es/work.html}
}
@article{mac_low_control_2004,
title = {Control of star formation by supersonic turbulence},
volume = {76},
issn = {0034-6861, 1539-0756},
url = {http://arxiv.org/abs/astro-ph/0301093},
doi = {10.1103/RevModPhys.76.125},
abstract = {Understanding the formation of stars in galaxies is central to much of modern astrophysics. For several decades it has been thought that stellar birth is primarily controlled by the interplay between gravity and magnetostatic support, modulated by ambipolar diffusion. Recently, however, both observational and numerical work has begun to suggest that support by supersonic turbulence rather than magnetic fields controls star formation. In this review we outline a new theory of star formation relying on the control by turbulence. We demonstrate that although supersonic turbulence can provide global support, it nevertheless produces density enhancements that allow local collapse. Inefficient, isolated star formation is a hallmark of turbulent support, while efficient, clustered star formation occurs in its absence. The consequences of this theory are then explored for both local star formation and galactic scale star formation. (ABSTRACT ABBREVIATED)},
number = {1},
urldate = {2016-11-02},
journal = {Reviews of Modern Physics},
author = {Mac Low, Mordecai-Mark and Klessen, Ralf S.},
month = jan,
year = {2004},
note = {arXiv: astro-ph/0301093},
keywords = {Astrophysics},
pages = {125--194},
annote = {Comment: Invited review for "Reviews of Modern Physics", 87 pages including 28 figures, in press},
file = {arXiv\:astro-ph/0301093 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/NTAF9U6R/Mac Low and Klessen - 2004 - Control of star formation by supersonic turbulence.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/7GMH4RUF/0301093.html:text/html}
}
@article{nakanishi_three-dimensional_2016,
title = {Three-{Dimensional} {Distribution} of the {ISM} in the {Milky} {Way} {Galaxy}: {III}. {The} {Total} {Neutral} {Gas} {Disk}},
volume = {68},
issn = {0004-6264, 2053-051X},
shorttitle = {Three-{Dimensional} {Distribution} of the {ISM} in the {Milky} {Way} {Galaxy}},
url = {http://arxiv.org/abs/1511.08877},
doi = {10.1093/pasj/psv108},
abstract = {We present newly obtained three-dimensional gaseous maps of the Milky Way Galaxy; HI, H\$\_2\$ and total-gas (HI plus H\$\_2\$) maps, which were derived from the HI and \${\textasciicircum}\{12\}\$CO(\$J=1\$--0) survey data and rotation curves based on the kinematic distance. The HI and H\$\_2\$ face-on maps show that the HI disk is extended to the radius of 15--20 kpc and its outskirt is asymmetric to the Galactic center, while most of the H\$\_2\$ gas is distributed inside the solar circle. The total gas mass within radius 30 kpc amounts to \$8.0{\textbackslash}times 10{\textasciicircum}9\$ M\$\_{\textbackslash}odot\$, 89{\textbackslash}\% and 11{\textbackslash}\% of which are HI and H\$\_2\$, \{respectively\}. The vertical slices show that the outer HI disk is strongly warped and the inner HI and H\$\_2\$ disks are corrugated. The total gas map is advantageous to trace spiral structure from the inner to outer disk. Spiral structures such as the Norma-Cygnus, the Perseus, the Sagittarius-Carina, the Scutum-Crux, and the Orion arms are more clearly traced in the total gas map than ever. All the spiral arms are well explained with logarithmic spiral arms with pitch angle of \$11{\textbackslash}degree\$ -- \$15{\textbackslash}degree\$. The molecular fraction to the total gas is high near the Galactic center and decreases with the Galactocentric distance. The molecular fraction also locally enhanced at the spiral arms compared with the inter-arm regions.},
number = {1},
urldate = {2017-02-26},
journal = {Publications of the Astronomical Society of Japan},
author = {Nakanishi, Hiroyuki and Sofue, Yoshiaki},
month = feb,
year = {2016},
note = {arXiv: 1511.08877},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {5},
annote = {Comment: 14 pages, 10 figures, 1 table}
}
@article{schaye_model-independent_2001,
title = {Model-independent {Insights} into the {Nature} of the {Lyα} {Forest} and the {Distribution} of {Matter} in the {Universe}},
volume = {559},
issn = {0004-637X},
url = {http://iopscience.iop.org/article/10.1086/322421/meta},
doi = {10.1086/322421},
language = {en},
number = {2},
urldate = {2017-02-01},
journal = {The Astrophysical Journal},
author = {Schaye, Joop},
month = oct,
year = {2001},
pages = {507},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/J2VM4H27/Schaye - 2001 - Model-independent Insights into the Nature of the .pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/AMXVBVSU/322421.html:text/html}
}
@article{mckee_stars_2015,
title = {Stars, {Gas}, and {Dark} {Matter} in the {Solar} {Neighborhood}},
volume = {814},
issn = {1538-4357},
url = {http://arxiv.org/abs/1509.05334},
doi = {10.1088/0004-637X/814/1/13},
abstract = {The surface density and vertical distribution of stars, stellar remnants, and gas in the solar vicinity form important ingredients for understanding the star formation history of the Galaxy as well as for inferring the local density of dark matter by using stellar kinematics to probe the gravitational potential. In this paper we review the literature for these baryonic components, reanalyze data, and provide tables of the surface densities and exponential scale heights of main sequence stars, giants, brown dwarfs, and stellar remnants. We also review three components of gas (H2, HI, and HII), give their surface densities at the solar circle, and discuss their vertical distribution. We find a local total surface density of M dwarfs of 17.3 pm 2.3 Mo/pc{\textasciicircum}2. Our result for the total local surface density of visible stars, 27.0 pm 2.7 Mo/pc{\textasciicircum}2, is close to previous estimates due to a cancellation of opposing effects: more mass in M dwarfs, less mass in the others. The total local surface density in white dwarfs is 4.9 pm 0.6 Mo/pc{\textasciicircum}2; in brown dwarfs, it is {\textasciitilde}1.2 Mo/pc{\textasciicircum}2. We find that the total local surface density of stars and stellar remnants is 33.4 pm 3 Mo/pc{\textasciicircum}2, somewhat less than previous estimates. We analyze data on 21 cm emission and absorption and obtain good agreement with recent results on the local amount of neutral atomic hydrogen obtained with the Planck satellite. The local surface density of gas is 13.7 pm 1.6 Mo/pc{\textasciicircum}2. The total baryonic mass surface density that we derive for the solar neighborhood is 47.1 pm 3.4 Mo/pc{\textasciicircum}2. Combining these results with others' measurements of the total surface density of matter within 1-1.1 kpc of the plane, we find that the local density of dark matter is 0.013 pm 0.003Mo/pc{\textasciicircum}3.The local density of all matter is 0.097 pm 0.013 Mo/pc{\textasciicircum}3. We discuss limitations on the properties of a possible thin disk of dark matter.},
number = {1},
urldate = {2017-01-12},
journal = {The Astrophysical Journal},
author = {McKee, Christopher F. and Parravano, Antonio and Hollenbach, David J.},
month = nov,
year = {2015},
note = {arXiv: 1509.05334},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {13},
annote = {Comment: 53 pages, 5 tables},
file = {arXiv\:1509.05334 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/MRU9V3PF/McKee et al. - 2015 - Stars, Gas, and Dark Matter in the Solar Neighborh.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/NRWAPAJ5/1509.html:text/html}
}
@book{horedt_polytropes:_2004,
address = {Dordrecht; Boston},
title = {Polytropes: applications in astrophysics and related fields},
isbn = {978-1-4020-2351-4 978-1-4020-2350-7},
shorttitle = {Polytropes},
url = {http://site.ebrary.com/id/10140500},
abstract = {This book provides the most complete academic treatment on the application of polytropes ever published. It is primarily intended for students and scientists working in Astrophysics and related fields. It provides a full overview of past and present research results and is an indispensible guide for everybody wanting to apply polytropes.},
language = {English},
urldate = {2017-02-21},
publisher = {Kluwer Academic Publishers},
author = {Horedt, G. P},
year = {2004},
note = {OCLC: 57385342}
}
@article{krumholz_dynamics_2010,
title = {On the {Dynamics} and {Evolution} of {Gravitational} {Instability}-dominated {Disks}},
volume = {724},
issn = {0004-637X},
url = {http://stacks.iop.org/0004-637X/724/i=2/a=895},
doi = {10.1088/0004-637X/724/2/895},
abstract = {We derive the evolution equations describing a thin axisymmetric disk of gas and stars with an arbitrary rotation curve that is kept in a state of marginal gravitational instability and energy equilibrium due to the balance between energy released by accretion and energy lost due to decay of turbulence. Rather than adopting a parameterized α prescription, we instead use the condition of marginal gravitational instability to self-consistently determine the position- and time-dependent transport rates. We show that there is a steady-state configuration for disks dominated by gravitational instability, and that this steady state persists even when star formation is taken into account if the accretion rate is sufficiently large. For disks in this state, we analytically determine the velocity dispersion, surface density, and rates of mass and angular momentum transport as a function of the gas mass fraction, the rotation curve, and the rate of external accretion onto the disk edge. We show that disks that are initially out of steady state will evolve into it on the viscous timescale of the disk, which is comparable to the orbital period if the accretion rate is high. Finally, we discuss the implications of these results for the structure of disks in a broad range of environments, including high-redshift galaxies, the outer gaseous disks of local galaxies, and accretion disks around protostars.},
language = {en},
number = {2},
urldate = {2016-11-07},
journal = {The Astrophysical Journal},
author = {Krumholz, Mark and Burkert, Andreas},
year = {2010},
pages = {895},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/QHHCENRD/Krumholz and Burkert - 2010 - On the Dynamics and Evolution of Gravitational Ins.pdf:application/pdf}
}
@article{obreschkow_angular_2016,
title = {Angular {Momentum} {Regulates} {Atomic} {Gas} {Fractions} of {Galactic} {Disks}},
volume = {824},
issn = {2041-8213},
url = {http://arxiv.org/abs/1605.04927},
doi = {10.3847/2041-8205/824/2/L26},
abstract = {We show that the mass fraction f\_atm = 1.35*MHI/M of neutral atomic gas (HI and He) in isolated local disk galaxies of baryonic mass M is well described by a straightforward stability model for flat exponential disks. In the outer disk parts, where gas at the characteristic dispersion of the warm neutral medium is stable in the sense of Toomre (1964), the disk consists of neutral atomic gas; conversely the inner part where this medium would be Toomre-unstable, is dominated by stars and molecules. Within this model, f\_atm only depends on a global stability parameter q=j*sigma/(GM), where j is the baryonic specific angular momentum of the disk and sigma the velocity dispersion of the atomic gas. The analytically derived first-order solution f\_atm = min\{1,2.5q{\textasciicircum}1.12\} provides a good fit to all plausible rotation curves. This model, with no free parameters, agrees remarkably well (+-0.2 dex) with measurements of f\_atm in isolated local disk galaxies, even with galaxies that are extremely HI-rich or HI-poor for their mass. The finding that f\_atm increases monotonically with q for pure stability reasons offers a powerful intuitive explanation for the mean variation of f\_atm with M: in a cold dark matter universe galaxies are expected to follow j{\textasciitilde}M{\textasciicircum}(2/3), which implies the average scaling q{\textasciitilde}M{\textasciicircum}(-1/3) and hence f\_atm{\textasciitilde}M{\textasciicircum}(-0.37), in agreement with observations.},
number = {2},
urldate = {2016-10-18},
journal = {The Astrophysical Journal},
author = {Obreschkow, Danail and Glazebrook, Karl and Kilborn, Virginia and Lutz, Katharina},
month = jun,
year = {2016},
note = {arXiv: 1605.04927},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {L26},
annote = {Comment: 5 pages, 3 figures},
file = {arXiv\:1605.04927 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/IID7C5MR/Obreschkow et al. - 2016 - Angular Momentum Regulates Atomic Gas Fractions of.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/W6QJH5J8/1605.html:text/html}
}
@article{schaye_star_2004,
title = {Star formation thresholds and galaxy edges: why and where},
volume = {609},
issn = {0004-637X, 1538-4357},
shorttitle = {Star formation thresholds and galaxy edges},
url = {http://arxiv.org/abs/astro-ph/0205125},
doi = {10.1086/421232},
abstract = {We study global star formation thresholds in the outer parts of galaxies by investigating the stability of disk galaxies embedded in dark halos. The disks are self-gravitating, contain metals and dust, and are exposed to UV radiation. We find that the critical surface density for the existence of a cold interstellar phase depends only weakly on the parameters of the model and coincides with the empirically derived surface density threshold for star formation. Furthermore, it is shown that the drop in the thermal velocity dispersion associated with the transition from the warm to the cold gas phase triggers gravitational instability on a wide range of scales. The presence of strong turbulence does not undermine this conclusion if the disk is self-gravitating. Models based on the hypothesis that the onset of thermal instability determines the star formation threshold in the outer parts of galaxies can reproduce many observations, including the threshold radii, column densities, and the sizes of stellar disks as a function of disk scale length and mass. Finally, prescriptions are given for implementing star formation thresholds in (semi-)analytic models and three-dimensional hydrodynamical simulations of galaxy formation.},
number = {2},
urldate = {2017-01-10},
journal = {The Astrophysical Journal},
author = {Schaye, Joop},
month = jul,
year = {2004},
note = {arXiv: astro-ph/0205125},
keywords = {Astrophysics},
pages = {667--682},
annote = {Comment: 16 pages, 6 figures, accepted for publication in the Astrophysical Journal. Version 2: text significantly revised (major improvements), physics unchanged. Version 3: minor corrections},
file = {arXiv\:astro-ph/0205125 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/BG5D95XP/Schaye - 2004 - Star formation thresholds and galaxy edges why an.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/6PBCGN44/0205125.html:text/html}
}
@article{xing_mori-zwanzig_2009,
title = {Mori-{Zwanzig} projection formalism: from linear to nonlinear},
shorttitle = {Mori-{Zwanzig} projection formalism},
url = {http://arxiv.org/abs/0904.2691},
abstract = {The Mori-Zwanzig projection formalism is widely used in studying systems with many degrees of freedom. We used a system-bath Hamiltonian system to show that the Mori's and Zwanzig's projection procedures are mutual limiting cases of each other depending on the size of the projected Hilbert space. We also derived the dynamic equations of collective coordinates of a Hamiltonian system.},
urldate = {2017-04-09},
journal = {arXiv:0904.2691 [cond-mat]},
author = {Xing, Jianhua},
month = apr,
year = {2009},
note = {arXiv: 0904.2691},
keywords = {Condensed Matter - Statistical Mechanics},
annote = {Comment: 3 pages},
file = {arXiv\:0904.2691 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/VWHJRTN7/Xing - 2009 - Mori-Zwanzig projection formalism from linear to .pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/VFPX9CZT/0904.html:text/html}
}
@article{z_incorporation_2015,
title = {Incorporation of memory effects in coarse-grained modeling via the {Mori}-{Zwanzig} formalism., {Incorporation} of memory effects in coarse-grained modeling via the {Mori}-{Zwanzig} formalism},
volume = {143, 143},
issn = {0021-9606},
url = {http://europepmc.org/abstract/MED/26723613, http://europepmc.org/articles/PMC4644152/?report=abstract},
doi = {10.1063/1.4935490, 10.1063/1.4935490},
abstract = {FULL TEXT Abstract: The Mori-Zwanzig formalism for coarse-graining a complex dynamical system typically introduces memory effects. The Markovian assumption of...},
language = {eng},
number = {24, 24},
urldate = {2017-04-09},
journal = {The Journal of chemical physics, The Journal of Chemical Physics},
author = {Z, Li and X, Bian and X, Li and Ge, Karniadakis},
month = dec,
year = {2015},
pmid = {26723613},
pages = {243128--243128},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/AWM9C97P/Z et al. - 2015 - Incorporation of memory effects in coarse-grained .pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/MFCTRMCK/pmc4644152.html:text/html}
}
@article{kennicutt_jr._star_2007,
title = {Star {Formation} in {NGC} 5194 ({M}51a). {II}. {The} {Spatially}-{Resolved} {Star} {Formation} {Law}},
volume = {671},
issn = {0004-637X, 1538-4357},
url = {http://arxiv.org/abs/0708.0922},
doi = {10.1086/522300},
abstract = {We have studied the relationship between the star formation rate (SFR) surface density and gas surface density in the spiral galaxy M51a (NGC 5194), using multi-wavelength data obtained as part of the Spitzer Infrared Nearby Galaxies Survey (SINGS). We introduce a new SFR index based on a linear combination of H-alpha emission-line and 24 micron continuum luminosities, that provides reliable extinction-corrected ionizing fluxes and SFR densities over a wide range of dust attenuations. The combination of these extinction-corrected SFR densities with aperture synthesis HI and CO maps has allowed us to probe the form of the spatially-resolved star formation law on scales of 0.5 to 2 kpc. We find that the resolved SFR vs gas surface density relation is well represented by a Schmidt power law, which is similar in form and dispersion to the disk-averaged Schmidt law. We observe a comparably strong correlation of the SFR surface density with the molecular gas surface density, but no significant correlation with the surface density of atomic gas. The best-fitting slope of the Schmidt law varies from N = 1.37 to 1.56, with zeropoint and slope that change systematically with the spatial sampling scale. We tentatively attribute these variations to the effects of areal sampling and averaging of a nonlinear intrinsic star formation law. Our data can also be fitted by an alternative parametrization of the SFR surface density in terms of the ratio of gas surface density to local dynamical time, but with a considerable dispersion.},
number = {1},
urldate = {2017-01-12},
journal = {The Astrophysical Journal},
author = {Kennicutt Jr., Robert C. and Calzetti, Daniela and Walter, Fabian and Helou, George and Hollenbach, David J. and Armus, Lee and Bendo, George and Dale, Daniel A. and Draine, Bruce T. and Engelbracht, Charles W. and Gordon, Karl D. and Prescott, Moire K. M. and Regan, Michael W. and Thornley, Michele D. and Bot, Caroline and Brinks, Elias and de Blok, Erwin and de Mello, Duilia and Meyer, Martin and Moustakas, John and Murphy, Eric J. and Sheth, Kartik and Smith, J. D. T.},
month = dec,
year = {2007},
note = {arXiv: 0708.0922},
keywords = {Astrophysics},
pages = {333--348},
annote = {Comment: 46 pages, 10 figures, accepted for publication in The Astrophysical Journal},
file = {arXiv\:0708.0922 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/R8WZ27E2/Kennicutt Jr. et al. - 2007 - Star Formation in NGC 5194 (M51a). II. The Spatial.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/IJ5W9423/0708.html:text/html}
}
@article{mckee_theory_2007,
title = {Theory of {Star} {Formation}},
volume = {45},
issn = {0066-4146, 1545-4282},
url = {http://arxiv.org/abs/0707.3514},
doi = {10.1146/annurev.astro.45.051806.110602},
abstract = {We review current understanding of star formation, outlining an overall theoretical framework and the observations that motivate it. A conception of star formation has emerged in which turbulence plays a dual role, both creating overdensities to initiate gravitational contraction or collapse, and countering the effects of gravity in these overdense regions. The key dynamical processes involved in star formation -- turbulence, magnetic fields, and self-gravity -- are highly nonlinear and multidimensional. Physical arguments are used to identify and explain the features and scalings involved in star formation, and results from numerical simulations are used to quantify these effects. We divide star formation into large-scale and small-scale regimes and review each in turn. Large scales range from galaxies to giant molecular clouds (GMCs) and their substructures. Important problems include how GMCs form and evolve, what determines the star formation rate (SFR), and what determines the initial mass function (IMF). Small scales range from dense cores to the protostellar systems they beget. We discuss formation of both low- and high-mass stars, including ongoing accretion. The development of winds and outflows is increasingly well understood, as are the mechanisms governing angular momentum transport in disks. Although outstanding questions remain, the framework is now in place to build a comprehensive theory of star formation that will be tested by the next generation of telescopes.},
number = {1},
urldate = {2016-12-06},
journal = {Annual Review of Astronomy and Astrophysics},
author = {McKee, Christopher F. and Ostriker, Eve C.},
month = sep,
year = {2007},
note = {arXiv: 0707.3514},
keywords = {Astrophysics},
pages = {565--687},
annote = {Comment: 120 pages, to appear in ARAA. No changes from v1 text; permission statement added},
file = {arXiv\:0707.3514 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/CQ24NGFR/McKee and Ostriker - 2007 - Theory of Star Formation.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/XB2NMPCM/0707.html:text/html}
}
@article{schaye_relation_2007,
title = {On the relation between the {Schmidt} and {Kennicutt}-{Schmidt} star formation laws and its implications for numerical simulations},
volume = {383},
issn = {00358711, 13652966},
url = {http://arxiv.org/abs/0709.0292},
doi = {10.1111/j.1365-2966.2007.12639.x},
abstract = {When averaged over large scales, star formation in galaxies is observed to follow the empirical Kennicutt-Schmidt (KS) law for surface densities above a constant threshold. While the observed law involves surface densities, theoretical models and simulations generally work with volume density laws (i.e. Schmidt laws). We derive analytic relations between star formation laws expressed in terms of surface densities, volume densities, and pressures and we show how these relations depend on parameters such as the effective equation of state of the multiphase interstellar medium. Our analytic relations enable us to implement observed surface density laws into simulations. Because the parameters of our prescription for star formation are observables, we are not free to tune them to match the observations. We test our theoretical framework using high-resolution simulations of isolated disc galaxies that assume an effective equation of state for the multiphase interstellar medium. We are able to reproduce the star formation threshold and both the slope and the normalisation of arbitrary input KS laws without tuning any parameters and with very little scatter, even for unstable galaxies and even if we use poor numerical resolution. Moreover, we can do so for arbitrary effective equations of state. Our prescription therefore enables simulations of galaxies to bypass our current inability to simulate the formation of stars. On the other hand, the fact that we can reproduce arbitrary input thresholds and KS laws, rather than just the particular ones picked out by nature, indicates that simulations that lack the physics and/or resolution to simulate the multiphase interstellar medium can only provide limited insight into the origin of the observed star formation laws.},
number = {3},
urldate = {2016-10-18},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Schaye, Joop and Vecchia, Claudio Dalla},
month = dec,
year = {2007},
note = {arXiv: 0709.0292},
keywords = {Astrophysics},
pages = {1210--1222},
annote = {Comment: Accepted for publication in MNRAS, 14 pages and 9 figures. Minor changes},
file = {arXiv\:0709.0292 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/NFR6QN83/Schaye and Vecchia - 2007 - On the relation between the Schmidt and Kennicutt-.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/URITUMAE/0709.html:text/html}
}
@article{glazebrook_dawes_2013,
title = {The {Dawes} {Review} 1: {Kinematic} {Studies} of {Star}-{Forming} {Galaxies} {Across} {Cosmic} {Time}},
volume = {30},
issn = {1323-3580},
shorttitle = {The {Dawes} {Review} 1},
url = {http://adsabs.harvard.edu/abs/2013PASA...30...56G},
doi = {10.1017/pasa.2013.34},
abstract = {The last seven years have seen an explosion in the number of Integral
Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at
high-redshift. These have taken advantage of the mature capabilities of
8-10 m class telescopes and the development of associated technology
such as AO. Surveys have leveraged both high spectroscopic resolution
enabling internal velocity measurements and high spatial resolution from
AO techniques and sites with excellent natural seeing. For the first
time, we have been able to glimpse the kinematic state of matter in
young, assembling star-forming galaxies and learn detailed astrophysical
information about the physical processes and compare their kinematic
scaling relations with those in the local Universe. Observers have
measured disc galaxy rotation, merger signatures, and
turbulence-enhanced velocity dispersions of gas-rich discs. Theorists
have interpreted kinematic signatures of galaxies in a variety of ways
(rotation, merging, outflows, and feedback) and attempted to discuss
evolution vs. theoretical models and relate it to the evolution in
galaxy morphology. A key point that has emerged from this activity is
that substantial fractions of high-redshift galaxies have regular
kinematic morphologies despite irregular photometric morphologies and
this is likely due to the presence of a large number of highly gas-rich
discs. There has not yet been a review of this burgeoning topic. In this
first Dawes review, I will discuss the extensive kinematic surveys that
have been done and the physical models that have arisen for young
galaxies at high-redshift.},
urldate = {2016-10-31},
journal = {Publications of the Astronomical Society of Australia},
author = {Glazebrook, Karl},
month = nov,
year = {2013},
keywords = {galaxies: evolution, galaxies: formation, galaxies: high-redshift, galaxies: kinematics and dynamics, galaxies: stellar content, galaxies: structure},
pages = {e056},
file = {NASA/ADS Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/6FG6C254/Glazebrook - 2013 - The Dawes Review 1 Kinematic Studies of Star-Form.pdf:application/pdf}
}
@inproceedings{licquia_improved_2013,
title = {Improved {Constraints} on the {Total} {Stellar} {Mass}, {Color}, and {Luminosity} of the {Milky} {Way}},
volume = {221},
url = {http://adsabs.harvard.edu/abs/2013AAS...22125411L},
abstract = {Determining the global properties of the Milky Way presents unique
challenges. Our position within the disk of the Galaxy yields a
distorted view of its overall light emission; interstellar dust alters
the spectral energy density we would otherwise measure in complex ways.
For this reason, measurements of the global properties of the Milky Way,
such as its star formation rate and total stellar mass, have proven to
be historically difficult and remain sparsely studied within the
literature. Here, we utilize updated models of the components of the
Milky Way and constraints from similar galaxies to determine improved
estimates of its total stellar mass. We model the stellar composition of
the Galaxy as an exponential disk, both thin and thick components,
combined with additional mass contributions from a central bulge,
pseudo-bulge, and/or bar (halo contributions are negligible compared to
current uncertainties). We constrain this model with a variety of
measurements from the literature, taking into account the uncertainties
in these estimates. With conservative assumptions we find that the total
stellar mass of the Milky Way is 4.6 (median) +2.0/-1.3 (68\% limit)
×1010 Msun (or +8.2/-2.0
×1010 Msun at 95\% confidence). We then
employ a random selection process that yields a sample of SDSS galaxies
whose distribution in stellar mass and star formation rate matches what
we know about the Milky Way’s (incorporating all uncertainties).
By analyzing the properties of these Milky Way analog galaxies, after
correcting for inclination effects and Eddington bias, we find that the
color of our Galaxy is g-r = 0.671 +0.061/-0.073 mag, and its absolute
magnitude is Mr = -20.87 +0.33/-0.44 mag. We therefore find
that the Milky Way most likely lies in the saddle of the bimodal
distribution of red and blue galaxies.},
urldate = {2017-04-06},
author = {Licquia, Timothy and Newman, J.},
month = jan,
year = {2013},
pages = {254.11}
}
@article{krumholz_universal_2012,
title = {A {Universal}, {Local} {Star} {Formation} {Law} in {Galactic} {Clouds}, {Nearby} {Galaxies}, {High}-{Redshift} {Disks}, and {Starbursts}},
volume = {745},
issn = {0004-637X, 1538-4357},
url = {http://arxiv.org/abs/1109.4150},
doi = {10.1088/0004-637X/745/1/69},
abstract = {[abridged] While observations of Local Group galaxies show a very simple, local star formation law in which the star formation rate per unit area in each patch of a galaxy scales linearly with the molecular gas surface density, recent observations of both Milky Way molecular clouds and high redshift galaxies apparently show a more complicated relationship, in which regions of equal surface density can form stars at quite different rates. These data have been interpreted as implying either that different star formation laws apply in different circumstances, that the star formation law is sensitive to large-scale galaxy properties rather than local properties, or that there are high density thresholds for star formation. Here we collate resolved observations of Milky Way molecular clouds, kpc-scale observations of Local Group galaxies, and unresolved observations of both disk and starburst galaxies in the local universe and at high redshift. We show that all of these data are in fact consistent with a simple, local, volumetric star formation law. The apparent variations stem from the fact that the observed objects have a wide variety of 3D size scales and degrees of internal clumping, so even at fixed gas column density the regions being observed can have wildly varying volume densities. We provide a simple theoretical framework to remove this projection effect, and we show that all the data, from small Solar neighborhood clouds with masses {\textasciitilde}10{\textasciicircum}3 Msun to sub-mm galaxies with masses {\textasciitilde}10{\textasciicircum}11 Msun, fall on a single star formation law in which the SFR is simply {\textasciitilde}1\% of the molecular gas mass per local free-fall time. In contrast, proposed star formation laws in which the star formation timescale is set by the galactic rotation period or the SFR is linearly proportional to the gas mass above some density threshold fail to match at least some of the data.},
number = {1},
urldate = {2017-01-13},
journal = {The Astrophysical Journal},
author = {Krumholz, Mark R. and Dekel, Avishai and McKee, Christopher F.},
month = jan,
year = {2012},
note = {arXiv: 1109.4150},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {69},
annote = {Comment: 20 pages, 4, figures, 4 tables, emulateapj format, accepted to ApJ. This version fixes a minor error in equation 18; no other changes},
file = {arXiv\:1109.4150 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/QWQFKKGN/Krumholz et al. - 2012 - A Universal, Local Star Formation Law in Galactic .pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/KQTUJ6QD/1109.html:text/html}
}
@article{martizzi_supernova_2016,
title = {Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds},
volume = {459},
issn = {0035-8711, 1365-2966},
shorttitle = {Supernova feedback in a local vertically stratified medium},
url = {http://arxiv.org/abs/1601.03399},
doi = {10.1093/mnras/stw745},
abstract = {We use local Cartesian simulations with a vertical gravitational potential to study how supernova (SN) feedback in stratified galactic discs drives turbulence and launches galactic winds. Our analysis includes three disc models with gas surface densities ranging from Milky Way-like galaxies to gas-rich ultra-luminous infrared galaxies (ULIRGs), and two different SN driving schemes (random and correlated with local gas density). In order to isolate the physics of SN feedback, we do not include additional feedback processes. We find that, in these local box calculations, SN feedback excites relatively low mass-weighted gas turbulent velocity dispersions {\textasciitilde}3-7 km/s and low wind mass loading factors {\textless} 1 in all the cases we study. The low turbulent velocities and wind mass loading factors predicted by our local box calculations are significantly below those suggested by observations of gas-rich and rapidly star-forming galaxies; they are also in tension with global simulations of disc galaxies regulated by stellar feedback. Using a combination of numerical tests and analytic arguments, we argue that local Cartesian boxes cannot predict the properties of galactic winds because they do not capture the correct global geometry and gravitational potential of galaxies. The wind mass loading factors are in fact not well-defined in local simulations because they decline significantly with increasing box height. More physically realistic calculations (e.g., including a global galactic potential and disc rotation) will likely be needed to fully understand disc turbulence and galactic outflows, even for the idealized case of feedback by SNe alone.},
number = {3},
urldate = {2016-10-25},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Martizzi, Davide and Fielding, Drummond and Faucher-Giguere, Claude-Andre and Quataert, Eliot},
month = jul,
year = {2016},
note = {arXiv: 1601.03399},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {2311--2326},
annote = {Comment: 17 pages, 12 figures, 4 tables, accepted for publication on MNRAS},
annote = {Three disk models with gas surface densities ranging from
Milky way-like galaxies to
gas rich ULIRGs
Two different SN driving schemes
random
correlated with local gas density
Do not include additional feedback processes (I guess that means star formation).
Finds that SN feedback excites relatively low mass-weighted gas turbulent velocity dispersions (approx 3-7 km/s) and low wind mass loading factors n {\textless} 1 in all cases they study.
These are significantly below those suggested by observations of gas-rich and rapidly star-forming galaxies; also in tension with global simulations of disk galaxies regulated by stellar feedback.
Argues that local Cartesian boxes cannot predict the properties of galactic winds - do not capture the correct global geometry and gravitational potential of galaxies.
Needs more physically realistic simulations.},
file = {arXiv\:1601.03399 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/UNIHT8CH/Martizzi et al. - 2016 - Supernova feedback in a local vertically stratifie.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/3G2V44HT/1601.html:text/html}
}
@article{robertson_disk_2004,
title = {Disk {Galaxy} {Formation} in a \${\textbackslash}{Lambda}\$ {Cold} {Dark} {Matter} {Universe}},
volume = {606},
issn = {0004-637X},
url = {http://iopscience.iop.org/article/10.1086/382871/meta},
doi = {10.1086/382871},
language = {en},
number = {1},
urldate = {2017-01-18},
journal = {The Astrophysical Journal},
author = {Robertson, Brant and Yoshida, Naoki and Springel, Volker and Hernquist, Lars},
month = may,
year = {2004},
pages = {32},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/6CQ56DG7/Robertson et al. - 2004 - Disk Galaxy Formation in a Λ Cold Dark Matter Univ.pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/5DZXVKEF/382871.html:text/html}
}
@article{rafikov_local_2001,
title = {The local axisymmetric instability criterion in a thin, rotating, multicomponent disc},
volume = {323},
issn = {0035-8711},
url = {https://academic.oup.com/mnras/article/323/2/445/1246378/The-local-axisymmetric-instability-criterion-in-a},
doi = {10.1046/j.1365-8711.2001.04201.x},
number = {2},
urldate = {2017-04-03},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Rafikov, R. R.},
month = may,
year = {2001},
pages = {445--452},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/3TT5XGME/Rafikov - 2001 - The local axisymmetric instability criterion in a .pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/8FTVI6Q5/The-local-axisymmetric-instability-criterion-in-a.html:text/html}
}
@article{springel_cosmological_2003,
title = {Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation},
volume = {339},
issn = {0035-8711, 1365-2966},
shorttitle = {Cosmological smoothed particle hydrodynamics simulations},
url = {http://mnras.oxfordjournals.org/content/339/2/289},
doi = {10.1046/j.1365-8711.2003.06206.x},
abstract = {We present a model for star formation and supernova feedback that describes the multiphase structure of star-forming gas on scales that are typically not resolved in cosmological simulations. Our approach includes radiative heating and cooling, the growth of cold clouds embedded in an ambient hot medium, star formation in these clouds, feedback from supernovae in the form of thermal heating and cloud evaporation, galactic winds and outflows, and metal enrichment. Implemented using smoothed particle hydrodynamics, our scheme is a significantly modified and extended version of the grid-based method of Yepes et al., and enables us to achieve a high dynamic range in simulations of structure formation.
We discuss properties of the feedback model in detail and show that it predicts a self-regulated, quiescent mode of star formation, which, in particular, stabilizes the star-forming gaseous layers of disc galaxies. The parametrization of this mode can be reduced to a single free quantity that determines the overall time-scale for star formation. We fix this parameter numerically to match the observed rates of star formation in local disc galaxies. When normalized in this manner, cosmological simulations employing our model nevertheless overproduce the observed cosmic abundance of stellar material. We are thus motivated to extend our feedback model to include galactic winds associated with star formation.
Using small-scale simulations of individual star-forming disc galaxies, we show that these winds produce either galactic fountains or outflows, depending on the depth of the gravitational potential. In low-mass haloes, winds can greatly suppress the overall efficiency of star formation. When incorporated into cosmological simulations, our combined model for star formation and winds predicts a cosmic star formation density that is consistent with observations, provided that the winds are sufficiently energetic. Moreover, outflows from galaxies in these simulations drive chemical enrichment of the intergalactic medium — in principle, accounting for the presence of metals in the Lyman α forest.},
language = {en},
number = {2},
urldate = {2017-01-05},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Springel, Volker and Hernquist, Lars},
month = feb,
year = {2003},
keywords = {galaxies: evolution, galaxies: formation, methods: numerical},
pages = {289--311},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/QICBSUXB/Springel and Hernquist - 2003 - Cosmological smoothed particle hydrodynamics simul.pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/9PDHH5A9/289.html:text/html}
}
@article{geach_evolution_2011,
title = {On the {Evolution} of the {Molecular} {Gas} {Fraction} of {Star}-{Forming} {Galaxies}},
volume = {730},
issn = {2041-8205},
url = {http://stacks.iop.org/2041-8205/730/i=2/a=L19},
doi = {10.1088/2041-8205/730/2/L19},
abstract = {We present IRAM Plateau de Bure interferometric detections of CO ( J = 1 → 0) emission from a 24 μm-selected sample of star-forming galaxies at z = 0.4. The galaxies have polycyclic aromatic hydrocarbon 7.7 μm-derived star formation rates of SFR 30-60 M ☉ yr –1 and stellar masses M \#\#IMG\#\# [http://ej.iop.org/icons/Entities/sstarf.gif] sstarf 10 11 M ☉ . The CO ( J = 1 → 0) luminosities of the galaxies imply that the disks still contain a large reservoir of molecular gas, contributing 20\% of the baryonic mass, but have star formation "efficiencies" similar to local quiescent disks and gas-dominated disks at z 1.5-2. We reveal evidence that the average molecular gas fraction has undergone strong evolution since z 2, with f gas \#\#IMG\#\# [http://ej.iop.org/icons/Entities/vprop.gif] vprop (1 + z ) 2±0.5 . The evolution of f gas encodes fundamental information about the relative depletion/replenishment of molecular fuel in galaxies and is expected to be a strong function of halo mass. We show that the latest predictions for the evolution of the molecular gas fraction in semi-analytic models of galaxy formation within a ΛCDM universe are supported by these new observations.},
language = {en},
number = {2},
urldate = {2017-01-12},
journal = {The Astrophysical Journal Letters},
author = {Geach, James E. and Smail, Ian and Moran, Sean M. and MacArthur, Lauren A. and Lagos, Claudia del P. and Edge, Alastair C.},
year = {2011},
pages = {L19},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/N2XCDUSV/Geach et al. - 2011 - On the Evolution of the Molecular Gas Fraction of .pdf:application/pdf}
}
@article{noauthor_ensemble_1960,
title = {Ensemble {Method} in the {Theory} of {Irreversibility}},
volume = {33},
issn = {0021-9606},
url = {http://aip.scitation.org/doi/abs/10.1063/1.1731409},
doi = {10.1063/1.1731409},
number = {5},
urldate = {2017-04-09},
journal = {The Journal of Chemical Physics},
month = nov,
year = {1960},
pages = {1338--1341},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/5V32ZMJV/1.html:text/html}
}
@article{livermore_hubble_2012,
title = {Hubble {Space} {Telescope} {Hα} imaging of star-forming galaxies at z ≃ 1-1.5: evolution in the size and luminosity of giant {H} {II} regions},
volume = {427},
shorttitle = {Hubble {Space} {Telescope} {Hα} imaging of star-forming galaxies at z ≃ 1-1.5},
url = {https://ui.adsabs.harvard.edu/#abs/2012MNRAS.427..688L/abstract},
doi = {10.1111/j.1365-2966.2012.21900.x},
abstract = {A powerful, streamlined new way to search the Astrophysics Data System},
urldate = {2017-03-17},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Livermore, R. C. and Jones, T. and Richard, J. and Bower, R. G. and Ellis, R. S. and Swinbank, A. M. and Rigby, J. R. and Smail, Ian and Arribas, S. and Rodriguez Zaurin, J. and Colina, L. and Ebeling, H. and Crain, R. A.},
month = nov,
year = {2012},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/3A5IJX28/ui.adsabs.harvard.edu.html:text/html}
}
@article{mo_formation_1998,
title = {The formation of galactic discs},
volume = {295},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/1998MNRAS.295..319M},
doi = {10.1046/j.1365-8711.1998.01227.x},
abstract = {We study the population of galactic discs expected in current hierarchical clustering models for structure formation. A rotationally supported disc with exponential surface density profile is assumed to form with a mass and angular momentum which are fixed fractions of those of its surrounding dark halo. We assume that haloes respond
adiabatically to disc formation, and that only stable discs can
correspond to real systems. With these assumptions the predicted population can match both present-day discs and the damped Lyalpha absorbers in QSO spectra. Good agreement is found provided that: (i) the masses of discs are a few per cent of those of their haloes; (ii) the specific angular momenta of discs are similar to those of their haloes; (iii) present-day discs were assembled recently (at z{\textless}=1). In
particular, the observed scatter in the size-rotation velocity plane is reproduced, as are the slope and scatter of the Tully-Fisher (TF) relation. The zero-point of the TF relation is matched for a stellar mass-to-light ratio of 1 to 2 h in the I-band, consistent with
observational values derived from disc dynamics. High-redshift discs are predicted to be small and dense, and could plausibly merge together to form the observed population of elliptical galaxies. In many (but not all) currently popular cosmogonies, discs with rotation velocities exceeding 200 kms{\textasciicircum}-1 can account for a third or more of the observed damped Lyalpha systems at z{\textasciitilde}2.5. Half of the lines of sight to such systems are predicted to intersect the absorber at r{\textgreater}{\textasciitilde}3h{\textasciicircum}-1kpc and about 10 per cent at r{\textgreater}10h{\textasciicircum}-1kpc. The cross-section for absorption is strongly weighted towards discs with large angular momentum and
therefore large size for their mass. The galaxy population associated with damped absorbers should thus be biased towards low surface
brightness systems.},
urldate = {2017-01-18},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Mo, H. J. and Mao, Shude and White, Simon D. M.},
month = apr,
year = {1998},
keywords = {COSMOLOGY: THEORY, Dark Matter, galaxies: formation, GALAXIES: SPIRAL, galaxies: structure},
pages = {319--336},
file = {NASA/ADS Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/7FQEWFAF/Mo et al. - 1998 - The formation of galactic discs.pdf:application/pdf}
}
@article{hijon_morizwanzig_2009,
title = {Mori–{Zwanzig} formalism as a practical computational tool},
volume = {144},
issn = {1364-5498},
url = {http://pubs.rsc.org/en/content/articlelanding/2010/fd/b902479b},
doi = {10.1039/B902479B},
abstract = {An operational procedure is presented to compute explicitly the different terms in the generalized Langevin equation (GLE) for a few relevant variables obtained within Mori–Zwanzig formalism. The procedure amounts to introducing an artificial controlled parameter which can be tuned in such a way that the so-called projected dynamics becomes explicit and the GLE reduces to a Markovian equation. The projected dynamics can be realised in practice by introducing constraints, and it is shown that the Green–Kubo formulae computed with these dynamics do not suffer from the plateau problem. The methodology is illustrated in the example of star polymer molecules in a melt using their center of mass as relevant variables. Through this example, we show that not only the effective potentials, but also the friction forces and the noise play a very important role in the dynamics.},
language = {en},
number = {0},
urldate = {2017-04-08},
journal = {Faraday Discussions},
author = {Hijón, Carmen and Español, Pep and Vanden-Eijnden, Eric and Delgado-Buscalioni, Rafael},
month = oct,
year = {2009},
pages = {301--322},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/KCR3SAXP/Hijón et al. - 2009 - Mori–Zwanzig formalism as a practical computationa.html:text/html}
}
@article{kalberla_hi_2009,
title = {The {Hi} {Distribution} of the {Milky} {Way}},
volume = {47},
url = {http://dx.doi.org/10.1146/annurev-astro-082708-101823},
doi = {10.1146/annurev-astro-082708-101823},
abstract = {Neutral atomic hydrogen (Hi) traces the interstellar medium (ISM) over a broad range of physical conditions. Its 21-cm emission line is a key probe of the structure and dynamics of the Milky Way Galaxy. About 50 years after the first detection of the 21-cm line the exploration of the Hi distribution of the Milky Way has undergone a true renaissance. This was triggered by several large-scale 21-cm surveys that became available within the past decade. New all-sky surveys unravel the shape and volume density distribution of the gaseous disk up to its borders. High-resolution Galactic plane surveys disclose a wealth of shells, filaments, and spurs that bear witness to the recycling of matter between stars and the ISM. All these observational results indicate that the Hi gas traces a dynamical Galactic ISM with structures on all scales, from tens of astronomical units to kiloparsecs. The Galaxy can be considered to be a violent, breathing disk surrounded by highly turbulent extra-planar gas.},
number = {1},
urldate = {2017-01-23},
journal = {Annual Review of Astronomy and Astrophysics},
author = {Kalberla, Peter and Jürgen, Kerp},
year = {2009},
pages = {27--61}
}
@article{drimmel_three-dimensional_2001,
title = {Three-dimensional {Structure} of the {Milky} {Way} {Disk}: {The} {Distribution} of {Stars} and {Dust} beyond 0.35 {R}\$\_{\textbackslash}odot\$},
volume = {556},
issn = {0004-637X},
shorttitle = {Three-dimensional {Structure} of the {Milky} {Way} {Disk}},
url = {http://stacks.iop.org/0004-637X/556/i=1/a=181},
doi = {10.1086/321556},
abstract = {We present a three-dimensional model for the Milky Way fitted to the far-infrared (FIR) and near-infrared (NIR) data from the COBE /DIRBE instrument for Galactic latitudes {\textbar} b {\textbar} {\textless} 30 ° and to within 20° of the Galactic center. Because of the low optical depth at 240 μm, the FIR emission traces the distribution of Galactic dust in the Galaxy. We model the dust distribution as due to three components: a warped exponential disk with scale length 0.28 R ☉ and a flaring scale height, a spiral arm component with four arms as traced by Galactic H II regions, and the local (Orion) arm, which produces prominent emission features at Galactic longitudes l \#\#IMG\#\# [http://ej.iop.org/icons/Entities/simeq.gif] simeq 80 and -100°. A cosmic infrared background of 1.07 MJy sr -1 is recovered, consistent with previous determinations. The dust distribution is then used to calculate absorption in J and K , and the stellar emission in these wavebands is modeled with two components: a warped exponential disk with a scale length of 0.28 R ☉ and a spiral arm component dominated by two arms. This small scale length is consistent with a maximal disk model for our Galaxy, which is inconsistent with the cuspy dark matter halos predicted in CDM models. We find different amplitudes for the warp in the stars and dust, which starts within the solar circle.},
language = {en},
number = {1},
urldate = {2017-01-23},
journal = {The Astrophysical Journal},
author = {Drimmel, Ronald and Spergel, David N.},
year = {2001},
pages = {181},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/6X48MXTI/Drimmel and Spergel - 2001 - Three-dimensional Structure of the Milky Way Disk.pdf:application/pdf}
}
@article{kim_three_2013,
title = {Three {Dimensional} {Hydrodynamic} {Simulations} of {Multiphase} {Galactic} {Disks} with {Star} {Formation} {Feedback}: {I}. {Regulation} of {Star} {Formation} {Rates}},
volume = {776},
issn = {0004-637X, 1538-4357},
shorttitle = {Three {Dimensional} {Hydrodynamic} {Simulations} of {Multiphase} {Galactic} {Disks} with {Star} {Formation} {Feedback}},
url = {http://arxiv.org/abs/1308.3231},
doi = {10.1088/0004-637X/776/1/1},
abstract = {The energy and momentum feedback from young stars has a profound impact on the interstellar medium (ISM), including heating and driving turbulence in the neutral gas that fuels future star formation. Recent theory has argued that this leads to a quasi-equilibrium self-regulated state, and for outer atomic-dominated disks results in the surface density of star formation \${\textbackslash}Sigma\_\{SFR\}\$ varying approximately linearly with the weight of the ISM (or midplane turbulent + thermal pressure). We use three-dimensional numerical hydrodynamic simulations to test the theoretical predictions for thermal, turbulent, and vertical dynamical equilibrium, and the implied functional dependence of \${\textbackslash}Sigma\_\{SFR\}\$ on local disk properties. Our models demonstrate that all equilibria are established rapidly, and that the expected proportionalities between mean thermal and turbulent pressures and \${\textbackslash}Sigma\_\{SFR\}\$ apply. For outer disk regions, this results in \${\textbackslash}Sigma\_\{SFR\} {\textbackslash}propto {\textbackslash}Sigma {\textbackslash}sqrt\{{\textbackslash}rho\_\{sd\}\}\$, where \${\textbackslash}Sigma\$ is the total gas surface density and \${\textbackslash}rho\_\{sd\}\$ is the midplane density of the stellar disk (plus dark matter). This scaling law arises because \${\textbackslash}rho\_\{sd\}\$ sets the vertical dynamical time in our models (and outer disk regions generally). The coefficient in the star formation law varies inversely with the specific energy and momentum yield from massive stars. We find proportions of warm and cold atomic gas, turbulent-to-thermal pressure, and mean velocity dispersions that are consistent with Solar-neighborhood and other outer-disk observations. This study confirms the conclusions of a previous set of simulations, which incorporated the same physics treatment but was restricted to radial-vertical slices through the ISM.},
number = {1},
urldate = {2016-10-18},
journal = {The Astrophysical Journal},
author = {Kim, Chang-Goo and Ostriker, Eve C. and Kim, Woong-Tae},
month = oct,
year = {2013},
note = {arXiv: 1308.3231},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {1},
annote = {Comment: 20 pages, 17 figures. Accepted for publication in ApJ},
file = {arXiv\:1308.3231 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/CG8KGVCQ/Kim et al. - 2013 - Three Dimensional Hydrodynamic Simulations of Mult.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/ZSRZE8CU/1308.html:text/html}
}
@book{press_numerical_2007,
title = {Numerical {Recipes} 3rd {Edition}: {The} {Art} of {Scientific} {Computing}},
isbn = {978-0-521-88068-8},
shorttitle = {Numerical {Recipes} 3rd {Edition}},
abstract = {Co-authored by four leading scientists from academia and industry, Numerical Recipes Third Edition starts with basic mathematics and computer science and proceeds to complete, working routines. Widely recognized as the most comprehensive, accessible and practical basis for scientific computing, this new edition incorporates more than 400 Numerical Recipes routines, many of them new or upgraded. The executable C++ code, now printed in color for easy reading, adopts an object-oriented style particularly suited to scientific applications. The whole book is presented in the informal, easy-to-read style that made earlier editions so popular. Please visit www.nr.com or www.cambridge.org/us/numericalrecipes for more details. More information concerning licenses is available at: www.nr.com/licenses New key features: 2 new chapters, 25 new sections, 25\% longer than Second Edition Thorough upgrades throughout the text Over 100 completely new routines and upgrades of many more. New Classification and Inference chapter, including Gaussian mixture models, HMMs, hierarchical clustering, Support Vector MachinesNew Computational Geometry chapter covers KD trees, quad- and octrees, Delaunay triangulation, and algorithms for lines, polygons, triangles, and spheres New sections include interior point methods for linear programming, Monte Carlo Markov Chains, spectral and pseudospectral methods for PDEs, and many new statistical distributions An expanded treatment of ODEs with completely new routines Plus comprehensive coverage of linear algebra, interpolation, special functions, random numbers, nonlinear sets of equations, optimization, eigensystems, Fourier methods and wavelets, statistical tests, ODEs and PDEs, integral equations, and inverse theory},
language = {en},
publisher = {Cambridge University Press},
author = {Press, William H.},
month = sep,
year = {2007},
note = {Google-Books-ID: 1aAOdzK3FegC},
keywords = {Computers / Mathematical \& Statistical Software, Mathematics / Applied, Mathematics / General, Mathematics / Numerical Analysis}
}
@article{silk_feedback_1997,
title = {Feedback, {Disk} {Self}-{Regulation}, and {Galaxy} {Formation}},
volume = {481},
url = {https://ui.adsabs.harvard.edu/#abs/1997ApJ...481..703S/abstract},
doi = {10.1086/304073},
abstract = {A powerful, streamlined new way to search the Astrophysics Data System},
urldate = {2017-04-04},
journal = {The Astrophysical Journal},
author = {Silk, Joseph},
month = may,
year = {1997},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/C2WCQ6QG/ui.adsabs.harvard.edu.html:text/html}
}
@article{noauthor_markoff_1952,
title = {Markoff {Random} {Processes} and the {Statistical} {Mechanics} of {Time}‐{Dependent} {Phenomena}},
volume = {20},
issn = {0021-9606},
url = {http://aip.scitation.org/doi/abs/10.1063/1.1700722},
doi = {10.1063/1.1700722},
number = {8},
urldate = {2017-04-09},
journal = {The Journal of Chemical Physics},
month = aug,
year = {1952},
pages = {1281--1295},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/R93IH6JC/1.html:text/html}
}
@article{leroy_star_2008,
title = {The {Star} {Formation} {Efficiency} in {Nearby} {Galaxies}: {Measuring} {Where} {Gas} {Forms} {Stars} {Effectively}},
volume = {136},
shorttitle = {The {Star} {Formation} {Efficiency} in {Nearby} {Galaxies}},
url = {https://ui.adsabs.harvard.edu/#abs/2008AJ....136.2782L/abstract},
doi = {10.1088/0004-6256/136/6/2782},
abstract = {A powerful, streamlined new way to search the Astrophysics Data System},
urldate = {2017-01-31},
journal = {The Astronomical Journal},
author = {Leroy, Adam K. and Walter, Fabian and Brinks, Elias and Bigiel, Frank and Blok, De and G, W. J. and Madore, Barry and Thornley, M. D.},
month = dec,
year = {2008},
file = {Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/J4HP7ZU4/ui.adsabs.harvard.edu.html:text/html}
}
@article{licquia_improved_2015,
title = {Improved {Estimates} of the {Milky} {Way}'s {Stellar} {Mass} and {Star} {Formation} {Rate} from {Hierarchical} {Bayesian} {Meta}-{Analysis}},
volume = {806},
issn = {1538-4357},
url = {http://arxiv.org/abs/1407.1078},
doi = {10.1088/0004-637X/806/1/96},
abstract = {We present improved estimates of several global properties of the Milky Way, including its current star formation rate (SFR), the stellar mass contained in its disk and bulge+bar components, as well as its total stellar mass. We do so by combining previous measurements from the literature using a hierarchical Bayesian (HB) statistical method that allows us to account for the possibility that any value may be incorrect or have underestimated errors. We show that this method is robust to a wide variety of assumptions about the nature of problems in individual measurements or error estimates. Ultimately, our analysis yields a SFR for the Galaxy of \${\textbackslash}dot\{{\textbackslash}mathrm\{M\}\}\_{\textbackslash}star=1.65{\textbackslash}pm0.19\$ \${\textbackslash}textrm\{M\}\_{\textbackslash}odot {\textbackslash}textrm\{yr\}{\textasciicircum}\{-1\}\$, assuming a Kroupa initial mass function (IMF). By combining HB methods with Monte Carlo simulations that incorporate the latest estimates of the Galactocentric radius of the Sun, \$R\_0\$, the exponential scale length of the disk, \$L\_d\$, and the local surface density of stellar mass, \${\textbackslash}Sigma\_{\textbackslash}star(R\_0)\$, we show that the mass of the Galactic bulge+bar is \${\textbackslash}textrm\{M\}\_{\textbackslash}star{\textasciicircum}B=0.91{\textbackslash}pm0.07{\textbackslash}times10{\textasciicircum}\{10\}\$ \${\textbackslash}textrm\{M\}\_{\textbackslash}odot\$, the disk mass is \${\textbackslash}textrm\{M\}\_{\textbackslash}star{\textasciicircum}D=5.17{\textbackslash}pm1.11{\textbackslash}times10{\textasciicircum}\{10\}\$ \${\textbackslash}textrm\{M\}\_{\textbackslash}odot\$, and their combination yields a total stellar mass of \${\textbackslash}textrm\{M\}\_{\textbackslash}star=6.08{\textbackslash}pm1.14{\textbackslash}times10{\textasciicircum}\{10\}\$ \${\textbackslash}textrm\{M\}\_{\textbackslash}odot\$ (assuming a Kroupa IMF and an exponential disk profile). This analysis is based upon a new compilation of literature bulge mass estimates, normalized to common assumptions about the stellar initial mass function and Galactic disk properties, presented herein. We additionally find a bulge-to-total mass ratio for the Milky Way of \$B/T=0.150{\textasciicircum}\{+0.028\}\_\{-0.019\}\$ and a specific star formation rate of \${\textbackslash}dot\{{\textbackslash}mathrm\{M\}\}\_{\textbackslash}star/{\textbackslash}textrm\{M\}\_{\textbackslash}star=2.71{\textbackslash}pm0.59{\textbackslash}times10{\textasciicircum}\{-11\} {\textbackslash}textrm\{yr\}{\textasciicircum}\{-1\}\$.},
number = {1},
urldate = {2017-02-26},
journal = {The Astrophysical Journal},
author = {Licquia, Timothy C. and Newman, Jeffrey A.},
month = jun,
year = {2015},
note = {arXiv: 1407.1078},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {96},
annote = {Comment: 21 pages, 8 figures, 6 tables, 1 appendix}
}
@article{zwanzig_memory_1961,
title = {Memory {Effects} in {Irreversible} {Thermodynamics}},
volume = {124},
url = {https://link.aps.org/doi/10.1103/PhysRev.124.983},
doi = {10.1103/PhysRev.124.983},
abstract = {A new generalization of Onsager's theory of irreversible processes is presented. The main purpose is to allow for memory effects or causal time behavior, so that the response to a thermodynamic force comes later than the application of the force. This is accomplished by a statistical mechanical derivation of an exact non-Markoffian kinetic equation for the probability distribution in the space of macroscopic state variables. The memory effect in the resulting transport equations is represented by a time convolution of the thermodynamic forces with memory functions. The latter are time-correlation functions in the rates of change of the phase functions corresponding to macroscopic quantities. The resulting transport equations are not restricted to small deviations from thermal equilibrium. Onsager's theory is shown to be the low-frequency limit of our causal theory.},
number = {4},
urldate = {2017-04-09},
journal = {Physical Review},
author = {Zwanzig, Robert},
month = nov,
year = {1961},
pages = {983--992},
file = {APS Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/T32KRAEK/PhysRev.124.html:text/html}
}
@article{vecchia_simulating_2008,
title = {Simulating galactic outflows with kinetic supernova feedback},
volume = {387},
issn = {00358711, 13652966},
url = {http://arxiv.org/abs/0801.2770},
doi = {10.1111/j.1365-2966.2008.13322.x},
abstract = {Feedback from star formation is thought to play a key role in the formation and evolution of galaxies, but its implementation in cosmological simulations is currently hampered by a lack of numerical resolution. We present and test a sub-grid recipe to model feedback from massive stars in cosmological smoothed particle hydrodynamics simulations. The energy is distributed in kinetic form among the gas particles surrounding recently formed stars. The impact of the feedback is studied using a suite of high-resolution simulations of isolated disc galaxies embedded in dark halos with total mass 10{\textasciicircum}\{10\} and 10{\textasciicircum}\{12\} Msol/h. We focus in particular on the effect of pressure forces on wind particles within the disc, which we turn off temporarily in some of our runs to mimic a recipe that has been widely used in the literature. We find that this popular recipe gives dramatically different results because (ram) pressure forces on expanding superbubbles determine both the structure of the disc and the development of large-scale outflows. Pressure forces exerted by expanding superbubbles puff up the disc, giving the dwarf galaxy an irregular morphology and creating a galactic fountain in the massive galaxy. Hydrodynamic drag within the disc results in a strong increase of the effective mass loading of the wind for the dwarf galaxy, but quenches much of the outflow in the case of the high-mass galaxy.},
number = {4},
urldate = {2016-10-18},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Vecchia, Claudio Dalla and Schaye, Joop},
month = jul,
year = {2008},
note = {arXiv: 0801.2770},
keywords = {Astrophysics},
pages = {1431--1444},
annote = {Comment: 15 pages, 11 figures, accepted for publication in MNRAS. Added 4 new figures and made minor textual changes. Simulation videos available at http://www.strw.leidenuniv.nl/DS08/},
file = {arXiv\:0801.2770 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/PPPE8V3T/Vecchia and Schaye - 2008 - Simulating galactic outflows with kinetic supernov.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/ERWF4UV9/0801.html:text/html}
}
@article{murray_disruption_2010,
title = {The {Disruption} of {Giant} {Molecular} {Clouds} by {Radiation} {Pressure} and the {Efficiency} of {Star} {Formation} in {Galaxies}},
volume = {709},
issn = {0004-637X, 1538-4357},
url = {http://arxiv.org/abs/0906.5358},
doi = {10.1088/0004-637X/709/1/191},
abstract = {Star formation is slow, in the sense that the gas consumption time is much longer than the dynamical time. It is also inefficient; essentially all star formation in local galaxies takes place in giant molecular clouds (GMCs), but the fraction of a GMC converted to stars is very small, {\textasciitilde}5\%. In the most luminous starbursts, the GMC lifetime is shorter than the main sequence lifetime of even the most massive stars, so that supernovae can play no role in GMC disruption. We investigate the disruption of GMCs across a wide range of galaxies, from normal spirals to the densest starbursts; we take into account the effects of HII gas pressure, shocked stellar winds, protostellar jets, and radiation pressure produced by the absorption and scattering of starlight on dust grains. In the Milky Way, we find that a combination of three mechanisms, jets, HII gas pressure, and radiation pressure, disrupts the clouds. In more rapidly star forming galaxies such as ``clump'' galaxies at high-redshift, ultra-luminous infrared galaxies (ULIRGs) and submillimeter galaxies, radiation pressure dominates natal cloud distribution. We predict the presence of 10-20 clusters with masses {\textasciitilde}10{\textasciicircum}7 Msun in local ULIRGs such as Arp 220 and a similar number of clusters with M\_* {\textasciitilde} 10{\textasciicircum}8 Msun in high redshift clump galaxies; submillimeter galaxies will have even more massive clusters. We find that the mass fraction of a GMC that ends up in stars is an increasing function of the gas surface density of a galaxy, reaching {\textasciitilde}35\% in the most luminous starbursts. Furthermore, the disruption of bubbles by radiation pressure stirs the interstellar medium to velocities of {\textasciitilde}10 km/s in normal galaxies and to {\textasciitilde}100 km/s in ULIRGs like Arp 220, consistent with observations. Thus, radiation pressure may play a dominant role in the ISM of star-forming galaxies.},
number = {1},
urldate = {2017-01-31},
journal = {The Astrophysical Journal},
author = {Murray, Norman and Quataert, Eliot and Thompson, Todd A.},
month = jan,
year = {2010},
note = {arXiv: 0906.5358},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {191--209},
annote = {Comment: 17 pages, 5 figures, submitted to ApJ},
file = {arXiv\:0906.5358 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/RSEIRV8C/Murray et al. - 2010 - The Disruption of Giant Molecular Clouds by Radiat.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/378RDHUW/0906.html:text/html}
}
@article{schaye_eagle_2015,
title = {The {EAGLE} project: simulating the evolution and assembly of galaxies and their environments},
volume = {446},
issn = {0035-8711},
shorttitle = {The {EAGLE} project},
url = {https://academic.oup.com/mnras/article/446/1/521/1316115/The-EAGLE-project-simulating-the-evolution-and},
doi = {10.1093/mnras/stu2058},
number = {1},
urldate = {2017-04-04},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Schaye, Joop and Crain, Robert A. and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and Dalla Vecchia, Claudio and Frenk, Carlos S. and McCarthy, I. G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Y. M. and White, Simon D. M. and Baes, Maarten and Booth, C. M. and Camps, Peter and Navarro, Julio F. and Qu, Yan and Rahmati, Alireza and Sawala, Till and Thomas, Peter A. and Trayford, James},
month = jan,
year = {2015},
pages = {521--554},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/K3E2M8WW/Schaye et al. - 2015 - The EAGLE project simulating the evolution and as.pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/ZU3ZZ4VD/stu2058.html:text/html}
}
@article{faucher-giguere_feedback-regulated_2013,
title = {Feedback-regulated star formation in molecular clouds and galactic discs},
volume = {433},
issn = {0035-8711, 1365-2966},
url = {http://mnras.oxfordjournals.org/content/433/3/1970},
doi = {10.1093/mnras/stt866},
abstract = {We present a two-zone theory for feedback-regulated star formation in galactic discs, consistently connecting the galaxy-averaged star formation law with star formation proceeding in giant molecular clouds (GMCs). Our focus is on galaxies with gas surface density Σg ≳ 100 M⊙ pc−2, where the interstellar medium (ISM) can be assumed to be fully molecular. This regime includes most star formation in the Universe and our basic framework can be extended to other galaxies. In our theory, the galactic disc consists of Toomre-mass GMCs embedded in a volume-filling ISM. Radiation pressure on dust disperses GMCs and most supernovae explode in the volume-filling medium. A galaxy-averaged star formation law is derived by balancing the momentum input from supernova feedback with the vertical gravitational weight of the disc gas. This star formation law is in good agreement with observations for a CO conversion factor depending continuously on Σg. We argue that the galaxy-averaged star formation efficiency per free-fall time, ϵgalffϵffgal{\textbackslash}epsilon \_\{{\textbackslash}rm ff\}{\textasciicircum}\{{\textbackslash}rm gal\}, is only a weak function of the efficiency with which GMCs convert their gas into stars, ϵGMCintϵintGMC{\textbackslash}epsilon \_\{{\textbackslash}rm int\}{\textasciicircum}\{{\textbackslash}rm GMC\}. This is possible because the rate limiting step for star formation is the rate at which GMCs form: for large efficiency of star formation in GMCs, the Toomre Q parameter obtains a value slightly above unity so that the GMC formation rate is consistent with the galaxy-averaged star formation law. We contrast our results with other theories of turbulence-regulated star formation and discuss predictions of our model. Using a compilation of data from the literature, we show that the galaxy-averaged star formation efficiency per free-fall time is non-universal and increases with increasing gas fraction, as predicted by our model. We also predict that the fraction of the disc gas mass in bound GMCs decreases for increasing values of the GMC star formation efficiency. This is qualitatively consistent with the smooth molecular gas distribution inferred in local ultraluminous infrared galaxies and the small mass fraction in giant clumps in high-redshift galaxies.},
language = {en},
number = {3},
urldate = {2016-11-14},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Faucher-Giguère, Claude-André and Quataert, Eliot and Hopkins, Philip F.},
month = aug,
year = {2013},
keywords = {galaxies: evolution, galaxies: formation, galaxies: high-redshift, galaxies: ISM, galaxies: starburst, stars: formation},
pages = {1970--1990},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/AC658QSK/Faucher-Giguère et al. - 2013 - Feedback-regulated star formation in molecular clo.pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/8W44ZADK/1970.html:text/html}
}
@article{martizzi_supernova_2015,
title = {Supernova {Feedback} in an {Inhomogeneous} {Interstellar} {Medium}},
volume = {450},
issn = {0035-8711, 1365-2966},
url = {http://arxiv.org/abs/1409.4425},
doi = {10.1093/mnras/stv562},
abstract = {Supernova (SN) feedback is one of the key processes shaping the interstellar medium (ISM) of galaxies. SNe contribute to (and in some cases may dominate) driving turbulence in the ISM and accelerating galactic winds. Modern cosmological simulations have sufficient resolution to capture the main structures in the ISM of galaxies, but are typically still not capable of explicitly resolving all of the small-scale stellar feedback processes, including the expansion of supernova remnants (SNRs). We perform a series of controlled three-dimensional hydrodynamic (adaptive mesh refinement) simulations of single SNRs expanding in an inhomogeneous density field with statistics motivated by those of the turbulent ISM. We use these to quantify the momentum and thermal energy injection from SNe as a function of spatial scale and the density, metallicity, and structure of the ambient medium. We develop a series of analytic formulae that we fit to the simulations. These formulae can be used as a basis for a more predictive sub-resolution model for SN feedback for galaxy formation simulations. We then use simulations of multiple, stochastically driven SNe that resolve the key phases of SNRs to test the sub-resolution model, and show that it accurately captures the turbulent kinetic energy and thermal energy in the ISM. By contrast, proposed SN feedback models in the literature based on `delayed cooling' significantly overpredict the late-time thermal energy and momentum in SNRs.},
number = {1},
urldate = {2016-10-27},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Martizzi, Davide and Faucher-Giguere, Claude-Andre and Quataert, Eliot},
month = apr,
year = {2015},
note = {arXiv: 1409.4425},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {504--522},
annote = {Comment: 21 pages, 11 figures, 4 tables. Published on MNRAS},
file = {arXiv\:1409.4425 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/A5V6W5S8/Martizzi et al. - 2015 - Supernova Feedback in an Inhomogeneous Interstella.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/7HIM9B2J/1409.html:text/html}
}
@article{daddi_different_2010,
title = {Different {Star} {Formation} {Laws} for {Disks} {Versus} {Starbursts} at {Low} and {High} {Redshifts}},
volume = {714},
issn = {2041-8205},
url = {http://stacks.iop.org/2041-8205/714/i=1/a=L118},
doi = {10.1088/2041-8205/714/1/L118},
abstract = {We present evidence that bona fide disks and starburst systems occupy distinct regions in the gas mass versus star formation rate (SFR) plane, both for the integrated quantities and for the respective surface densities. This result is based on carbon monoxide (CO) observations of galaxy populations at low and high redshifts, and on the current consensus for the CO luminosity to gas mass conversion factors. The data suggest the existence of two different SF regimes: a long-lasting mode for disks and a more rapid mode for starbursts, the latter probably occurring during major mergers or in dense nuclear SF regions. Both modes are observable over a large range of SFRs. The detection of CO emission from distant near-IR selected galaxies reveals such bimodal behavior for the first time, as they allow us to probe gas in disk galaxies with much higher SFRs than are seen locally. The different regimes can potentially be interpreted as the effect of a top-heavy initial mass function in starbursts. However, we favor a different physical origin related to the fraction of molecular gas in dense clouds. The IR luminosity to gas mass ratio (i.e., the SF efficiency) appears to be inversely proportional to the dynamical (rotation) timescale. Only when accounting for the dynamical timescale, a universal SF law is obtained, suggesting a direct link between global galaxy properties and the local SFR.},
language = {en},
number = {1},
urldate = {2017-01-12},
journal = {The Astrophysical Journal Letters},
author = {Daddi, E. and Elbaz, D. and Walter, F. and Bournaud, F. and Salmi, F. and Carilli, C. and Dannerbauer, H. and Dickinson, M. and Monaco, P. and {D. Riechers}},
year = {2010},
pages = {L118},
file = {IOP Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/2DH3IJP9/Daddi et al. - 2010 - Different Star Formation Laws for Disks Versus Sta.pdf:application/pdf}
}
@article{jeans_stability_1902,
title = {The {Stability} of a {Spherical} {Nebula}},
volume = {199},
issn = {1364-503X, 1471-2962},
url = {http://rsta.royalsocietypublishing.org/content/199/312-320/1},
doi = {10.1098/rsta.1902.0012},
language = {en},
number = {312-320},
urldate = {2017-01-16},
journal = {Philosophical Transactions of the Royal Society of London A: Mathematical, Physical and Engineering Sciences},
author = {Jeans, J. H.},
month = jan,
year = {1902},
pages = {1--53},
file = {Full Text PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/XAAAB8F3/Jeans - 1902 - The Stability of a Spherical Nebula.pdf:application/pdf;Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/9H5UM44P/1.html:text/html}
}
@article{schaye_eagle_2014,
title = {The {EAGLE} project: {Simulating} the evolution and assembly of galaxies and their environments},
volume = {446},
issn = {0035-8711, 1365-2966},
shorttitle = {The {EAGLE} project},
url = {http://arxiv.org/abs/1407.7040},
doi = {10.1093/mnras/stu2058},
abstract = {We introduce the Virgo Consortium's EAGLE project, a suite of hydrodynamical simulations that follow the formation of galaxies and black holes in representative volumes. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and AGN in which thermal energy is injected into the gas without the need to turn off cooling or hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the z{\textasciitilde}0 galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy mass function is reproduced to \${\textbackslash}lesssim 0.2\$ dex over the full mass range, \$10{\textasciicircum}8 {\textless} M\_*/M\_{\textbackslash}odot {\textbackslash}lesssim 10{\textasciicircum}\{11\}\$, a level of agreement close to that attained by semi-analytic models, and unprecedented for hydrodynamical simulations. We compare our results to a representative set of low-redshift observables not considered in the calibration, and find good agreement with the observed galaxy specific star formation rates, passive fractions, Tully-Fisher relation, total stellar luminosities of galaxy clusters, and column density distributions of intergalactic CIV and OVI. While the mass-metallicity relations for gas and stars are consistent with observations for \$M\_* {\textbackslash}gtrsim 10{\textasciicircum}9 M\_{\textbackslash}odot\$, they are insufficiently steep at lower masses. The gas fractions and temperatures are too high for clusters of galaxies, but for groups these discrepancies can be resolved by adopting a higher heating temperature in the subgrid prescription for AGN feedback. EAGLE constitutes a valuable new resource for studies of galaxy formation.},
number = {1},
urldate = {2016-10-18},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Schaye, Joop and Crain, Robert A. and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and Vecchia, Claudio Dalla and Frenk, Carlos S. and McCarthy, I. G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Y. M. and White, Simon D. M. and Baes, Maarten and Booth, C. M. and Camps, Peter and Navarro, Julio F. and Qu, Yan and Rahmati, Alireza and Sawala, Till and Thomas, Peter A. and Trayford, James},
month = nov,
year = {2014},
note = {arXiv: 1407.7040},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {521--554},
annote = {Comment: Accepted for publication in MNRAS. V2: Minor changes. For images and videos, see http://eagle.strw.leidenuniv.nl/ and http://icc.dur.ac.uk/Eagle/},
file = {arXiv\:1407.7040 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/8VFGQGN8/Schaye et al. - 2014 - The EAGLE project Simulating the evolution and as.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/74CTK3X6/1407.html:text/html}
}
@article{bigiel_star_2008,
title = {The {Star} {Formation} {Law} in {Nearby} {Galaxies} on {Sub}-{Kpc} {Scales}},
volume = {136},
issn = {0004-6256, 1538-3881},
url = {http://arxiv.org/abs/0810.2541},
doi = {10.1088/0004-6256/136/6/2846},
abstract = {(Abridged) We present a comprehensive analysis of the relationship between star formation rate surface density (SFR SD) and gas surface density (gas SD) at sub-kpc resolution in a sample of 18 nearby galaxies. We use high resolution HI data from THINGS, CO data from HERACLES and BIMA SONG, 24 micron data from the Spitzer Space Telescope, and UV data from GALEX. We target 7 spiral galaxies and 11 late-type/dwarf galaxies and investigate how the star formation law differs between the H2-dominated centers of spiral galaxies, their HI-dominated outskirts and the HI-rich late-type/dwarf galaxies. We find that a Schmidt-type power law with index N=1.0+-0.2 relates the SFR SD and the H2 SD across our sample of spiral galaxies, i.e., that H2 forms stars at a constant efficiency in spirals. The average molecular gas depletion time is {\textasciitilde}2*10{\textasciicircum}9 yrs. We interpret the linear relation and constant depletion time as evidence that stars are forming in GMCs with approximately uniform properties and that the H2 SD may be more a measure of the filling fraction of giant molecular clouds than changing conditions in the molecular gas. The relationship between total gas SD and SFR SD varies dramatically among and within spiral galaxies. Most galaxies show little or no correlation between the HI SD and the SFR SD. As a result, the star formation efficiency (SFE = SFR SD / gas SD) varies strongly across our sample and within individual galaxies. We show that in spirals the SFE is a clear function of radius, while the dwarf galaxies in our sample display SFEs similar to those found in the outer optical disks of the spirals. Another general feature of our sample is a sharp saturation of the HI SD at {\textasciitilde}9 M\_sol/pc{\textasciicircum}2 in both the spiral and dwarf galaxies.},
number = {6},
urldate = {2016-11-07},
journal = {The Astronomical Journal},
author = {Bigiel, Frank and Leroy, Adam and Walter, Fabian and Brinks, Elias and de Blok, W. J. G. and Madore, Barry and Thornley, Michele D.},
month = dec,
year = {2008},
note = {arXiv: 0810.2541},
keywords = {Astrophysics},
pages = {2846--2871},
annote = {Comment: Accepted for publication in the AJ special THINGS issue. For a high-resolution version visit: http://www.mpia.de/THINGS/Publications.html},
file = {arXiv\:0810.2541 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/KR8AZ9HI/Bigiel et al. - 2008 - The Star Formation Law in Nearby Galaxies on Sub-K.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/FZI68CMB/0810.html:text/html}
}
@article{vecchia_simulating_2012,
title = {Simulating galactic outflows with thermal supernova feedback},
volume = {426},
issn = {00358711},
url = {http://arxiv.org/abs/1203.5667},
doi = {10.1111/j.1365-2966.2012.21704.x},
abstract = {Cosmological simulations make use of sub-grid recipes for the implementation of galactic winds driven by massive stars because direct injection of supernova energy in thermal form leads to strong radiative losses, rendering the feedback inefficient. We argue that the main cause of the catastrophic cooling is a mismatch between the mass of the gas in which the energy is injected and the mass of the parent stellar population. Because too much mass is heated, the temperatures are too low and the cooling times too short. We use analytic arguments to estimate, as a function of the gas density and the numerical resolution, the minimum heating temperature that is required for the injected thermal energy to be efficiently converted into kinetic energy. We then propose and test a stochastic implementation of thermal feedback that uses this minimum temperature increase as an input parameter and that can be employed in both particle- and grid-based codes. We use smoothed particle hydrodynamics simulations to test the method on models of isolated disc galaxies in dark matter haloes with total mass 10{\textasciicircum}10 and 10{\textasciicircum}12 h{\textasciicircum}-1 solar masses. The thermal feedback strongly suppresses the star formation rate and can drive massive, large-scale outflows without the need to turn off radiative cooling temporarily. In accord with expectations derived from analytic arguments, for sufficiently high resolution the results become insensitive to the imposed temperature jump and also agree with high-resolution simulations employing kinetic feedback.},
number = {1},
urldate = {2016-10-18},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Vecchia, Claudio Dalla and Schaye, Joop},
month = oct,
year = {2012},
note = {arXiv: 1203.5667},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {140--158},
annote = {Comment: 21 pages, 14 figures, accepted for publication in MNRAS. High resolution pictures and movies can be found at http://www.strw.leidenuniv.nl/DS12/ (cleaner version, unchanged manuscript)},
file = {arXiv\:1203.5667 PDF:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/6PV7N76S/Vecchia and Schaye - 2012 - Simulating galactic outflows with thermal supernov.pdf:application/pdf;arXiv.org Snapshot:/Users/josh/Library/Application Support/Zotero/Profiles/c4whbwdy.default/zotero/storage/4C6QQSHG/1203.html:text/html}
}
@article{vogelsberger_introducing_2014,
title = {Introducing the {Illustris} {Project}: {Simulating} the coevolution of dark and visible matter in the {Universe}},