@misc{hiss2017measurement,
  abstract = {We decompose the Lyman-{\alpha} (Ly{\alpha}) forest of an extensive sample of
74 high signal-to-noise ratio and high-resolution quasar spectra into a
collection of Voigt profiles. Absorbers located near caustics in the peculiar
velocity field have the smallest Doppler parameters, resulting in a low-$b$
cutoff in the $b$-$N_{\text{HI}}$ set by the thermal state of intergalactic
medium (IGM). We fit this cutoff as a function of redshift over the range
$2.0\leq z \leq 3.4$, which allows us to measure the evolution of the IGM
temperature-density ($T= T_0 (\rho/ \rho_0)^{\gamma-1}$) relation parameters
$T_0$ and $\gamma$. We calibrate our measurements against Ly$\alpha$ forest
simulations, using 21 different thermal models of the IGM at each redshift,
also allowing for different values of the IGM pressure smoothing scale. We
adopt a forward-modeling approach and self-consistently apply the same
algorithms to both data and simulations, propagating both statistical and
modeling uncertainties via Monte Carlo. The redshift evolution of $T_0$ shows a
suggestive peak at $z=2.8$, while our evolution of $\gamma$ is consistent with
$\gamma\simeq 1.4$ and disfavors inverted temperature-density relations. Our
measured evolution of $T_0$ and $\gamma$ are generally in good agreement with
previous determinations in the literature. Both the peak in the evolution of
$T_0$ at $z = 2.8$, as well as the high temperatures $T_0\simeq 15000-20000\,$K
that we observe at $2.4 < z < 3.4$, strongly suggest that a significant episode
of heating occurred after the end of HI reionization, which was most likely the
cosmic reionization of HeII.},
  added-at = {2017-10-03T09:57:38.000+0200},
  author = {Hiss, Hector and Walther, Michael and Hennawi, Joseph F. and Oñorbe, José and O'Meara, John M. and Rorai, Alberto},
  biburl = {https://www.bibsonomy.org/bibtex/2e6a44747956c7a6378f1ce26b3c54527/miki},
  description = {[1710.00700] A New Measurement of the Temperature Density Relation of the IGM From Voigt Profile Fitting},
  interhash = {b11888400c25a2a2b191e82bf3e96018},
  intrahash = {e6a44747956c7a6378f1ce26b3c54527},
  keywords = {IGM density heating temperature},
  note = {cite arxiv:1710.00700Comment: Submitted to ApJ, 20 pages, 20 figures, machine readable tables will  be made available after publication},
  timestamp = {2017-10-03T09:57:38.000+0200},
  title = {A New Measurement of the Temperature Density Relation of the IGM From
  Voigt Profile Fitting},
  url = {http://arxiv.org/abs/1710.00700},
  year = 2017
}

@misc{zhu2017preheating,
  abstract = {The preheating of intergalactic medium(IGM) by structure collapsing and
ultraviolet background(UVB) are investigated in cosmological hydrodynamical
simulations. When gravitational collapsing is the sole heating mechanism, we
find that (1) $60\%, 45\%$ of the IGM are heated up to $S>8, 17$ kev cm$^2$
respectively at $z=0$, but the fractions drop rapidly to a few percents at
$z=2$, (2) the entropy of the circum-halo gas $S_{\rm{cir}}$ is higher than the
virial entropy for more than $75 \%$ of the halos with masses $M<10^{11.5}$
$M_{\odot}$ since $z=2$, but the fraction higher than the entropy,
$S_{\rm{pr}}$, required in preventive model of galaxies formation is only
$15-20 \%$ for halos with $M<10^{10.5} M_{\odot}$ at $z=0$, and decreases as
redshift increases, (3)assuming a metallicity of $Z \leq 0.03 Z_{\odot}$, the
fraction of halos whose circum-halo gas having a cooling time longer than the
Hubble time $t_{cool,cir}>t_{\rm{H}}$ is merely $5-10 \%$ at $z \lesssim 0.5$,
and even less at $z \geq 1$ for halos with $M<10^{10.5} M_{\odot}$. (4) gas in
the filaments undergoes the strongest preheating. Furthermore, we show that the
UVB can not enhance the fraction of IGM with $S>17$ kev cm$^2$, but can
increase the fraction of low mass halos($<10^{10.5} M_{\odot}$) that having
$S_{\rm{cir}}>S_{\rm{pr}}$ to $\sim 70 \%$ at $z=0$, and that having
$t_{\rm{cool, cir}}>t_{\rm{H}}$ to $15-30 \%$ at $z \lesssim 0.5$. Our results
indicate that preheating due to gravitational collapsing and UVB are inadequate
to fulfil the needs of preventative model, especially for halos with
$10^{10.5}<M<10^{11.5} M_{\odot}$. Nevertheless, these two mechanisms might
cause large scale galactic conformity.},
  added-at = {2017-09-05T11:22:38.000+0200},
  author = {Zhu, Weishan and Feng, Long-Long},
  biburl = {https://www.bibsonomy.org/bibtex/2f46fc0d621e070f6367cf9576c817b71/miki},
  description = {[1709.00709] Pre-heating of the intergalactic medium by gravitational collapse and ultraviolet background},
  interhash = {5d422459cc608f478648703d1fd7d04b},
  intrahash = {f46fc0d621e070f6367cf9576c817b71},
  keywords = {IGM UVB heating},
  note = {cite arxiv:1709.00709Comment: 18 pages, 11 figures, To appear in ApJ},
  timestamp = {2017-09-05T11:22:38.000+0200},
  title = {Pre-heating of the intergalactic medium by gravitational collapse and
  ultraviolet background},
  url = {http://arxiv.org/abs/1709.00709},
  year = 2017
}

@misc{leite2017cosmic,
  abstract = {Cosmic rays (CRs) govern the energetics of present-day galaxies and might
have also played a pivotal role during the Epoch of Reionization. In
particular, energy deposition by low-energy ($E \lesssim 10$ MeV) CRs
accelerated by the first supernovae, might have heated and ionized the neutral
intergalactic medium (IGM) well before ($z \approx 20$) it was reionized,
significantly adding to the similar effect by X-rays or dark matter
annihilations. Using a simple, but physically motivated reionization model, and
a thorough implementation of CR energy losses, we show that CRs contribute
negligibly to IGM ionization, but heat it substantially, raising its
temperature by $\Delta T=10-200$ K by $z=10$, depending on the CR injection
spectrum. Whether this IGM pre-heating is uniform or clustered around the first
galaxies depends on CR diffusion, in turn governed by the efficiency of
self-confinement due to plasma streaming instabilities that we discuss in
detail. This aspect is crucial to interpret future HI 21 cm observations which
can be used to gain unique information on the strength and structure of early
intergalactic magnetic fields, and the efficiency of CR acceleration by the
first supernovae.},
  added-at = {2017-03-29T10:11:55.000+0200},
  author = {Leite, Natacha and Evoli, Carmelo and D'Angelo, Marta and Ciardi, Benedetta and Sigl, Günter and Ferrara, Andrea},
  biburl = {https://www.bibsonomy.org/bibtex/2f7a438c46f29fca44d62d74b44a4af95/miki},
  description = {[1703.09337] Do Cosmic Rays Heat the Early Intergalactic Medium?},
  interhash = {ba4f380fadbe66373151797743c56f76},
  intrahash = {f7a438c46f29fca44d62d74b44a4af95},
  keywords = {cosmic heating igm rays},
  note = {cite arxiv:1703.09337Comment: 10 pages, 7 figures},
  timestamp = {2017-03-29T10:11:55.000+0200},
  title = {Do Cosmic Rays Heat the Early Intergalactic Medium?},
  url = {http://arxiv.org/abs/1703.09337},
  year = 2017
}

@misc{lebouteiller2017neutral,
  abstract = {(abridged) The dominant thermal mechanisms in the neutral interstellar
medium, which acts as a star-forming gas reservoir, are uncertain in extremely
metal-poor galaxies. Our objective is to identify the heating mechanisms in one
such galaxy, IZw18, and assess the diagnostic value of fine-structure cooling
lines. We also seek to constrain the mass of H$_2$, which, despite being an
important catalyst and tracer of star formation, remains elusive in this
object. Building on a previous photoionization model within a multi-sector
topology, we provide additional constraints from the [CII] and [OI] lines and
the dust mass recently measured with Herschel. The heating of the HI region
appears to be mainly due to photoionization by radiation from a bright X-ray
binary source, while photoelectric effect (PE) is negligible. The [CII] and
[OI] lines imply an average X-ray luminosity of $4\times10^{40}$ erg s$^{-1}$,
while the [NeV] upper limits bring strong constraints to the soft X-ray flux
arising from the binary. A negligible amount of H$_2$ is predicted, but
$\lesssim10^7$ M$_\odot$ of H$_2$ may be hidden in sufficiently dense clouds of
order $\lesssim10$ pc in size. Regardless of the presence of significant
amounts of H$_2$, [CII] and [OI] do not trace the so-called CO-dark gas, but
the almost purely atomic medium. Although the [CII]+[OI]/TIR ratio is close to
values found in more metal-rich sources, it cannot be safely used as a PE
heating efficiency proxy. This ratio seems to be kept stable due to a
correlation between the X-ray luminosity and the star-formation rate. We
propose that X-ray heating is an important process in extremely metal-poor
sources. The weak PE heating due to the low dust-to-gas ratio could be
compensated for by the larger occurrence and power of X-ray binaries in
low-metallicity galaxies. We speculate that X-ray heating may quench star
formation.},
  added-at = {2017-02-27T10:36:10.000+0100},
  author = {Lebouteiller, V. and Pequignot, D. and Cormier, D. and Madden, S. and Pakull, M. W. and Kunth, D. and Galliano, F. and Chevance, M. and Heap, S. R. and Lee, M. Y. and Polles, F. L.},
  biburl = {https://www.bibsonomy.org/bibtex/268e696ea94e234ccc10bd001db8de617/miki},
  description = {[1702.07377] Neutral gas heating by X-rays in primitive galaxies: Infrared observations of IZw18 with Herschel},
  interhash = {2274a554ac83fdaa87b5f1633bd313e4},
  intrahash = {68e696ea94e234ccc10bd001db8de617},
  keywords = {heating mechanism metal photoelectric poor x-ray},
  note = {cite arxiv:1702.07377Comment: Accepted for publication in A&A},
  timestamp = {2017-02-27T10:36:10.000+0100},
  title = {Neutral gas heating by X-rays in primitive galaxies: Infrared
  observations of IZw18 with Herschel},
  url = {http://arxiv.org/abs/1702.07377},
  year = 2017
}

@misc{viel2016diagnosing,
  abstract = {We compare the low redshift (z ~ 0.1) Lyman-alpha forest from hydrodynamical
simulations with data from the Cosmic Origin Spectrograph (COS). We find
tension between the observed number of lines with b-parameters in the range
25-45 km/s and the predictions from simulations that incorporate either
vigorous feedback from active galactic nuclei or that exclude feedback
altogether. The gas in these simulations is, respectively, either too hot to
contribute to the Lyman-alpha absorption or too cold to produce the required
line widths. Matching the observed b-parameter distribution therefore requires
feedback processes that thermally or turbulently broaden the absorption
features without collisionally (over-)ionising hydrogen. This suggests the
Lyman-alpha forest b-parameter distribution is a valulable diagnostic of
galactic feedback in the low redshift Universe. We furthermore confirm the low
redshift Lyman-alpha forest column density distribution is better reproduced by
an ultraviolet background with an HI photo-ionisation rate a factor 1.5-3
higher than predicted by Haardt & Madau (2012).},
  added-at = {2016-10-10T09:46:15.000+0200},
  author = {Viel, M. and Haehnelt, M. G. and Bolton, J. S. and Kim, T. S. and Puchwein, E. and Nasir, F. and Wakker, B. P.},
  biburl = {https://www.bibsonomy.org/bibtex/24d9f965be44fd1ec7eb6513cc602cb3c/miki},
  description = {[1610.02046] Diagnosing galactic feedback with the line broadening in the low redshift Lyman-alpha forest},
  interhash = {b57302dc180c8695a10a3f5e6afbd7b4},
  intrahash = {4d9f965be44fd1ec7eb6513cc602cb3c},
  keywords = {feedback forest heating lya},
  note = {cite arxiv:1610.02046Comment: 5 pages - 1 table - 2 figures},
  timestamp = {2016-10-10T09:46:15.000+0200},
  title = {Diagnosing galactic feedback with the line broadening in the low
  redshift Lyman-alpha forest},
  url = {http://arxiv.org/abs/1610.02046},
  year = 2016
}

@misc{onorbe2016selfconsistent,
  abstract = {The ultraviolet background (UVB) emitted by quasars and galaxies governs the
ionization and thermal state of the intergalactic medium (IGM), regulates the
formation of high-redshift galaxies, and is thus a key quantity for modeling
cosmic reionization. The vast majority of cosmological hydrodynamical
simulations implement the UVB via a set of spatially uniform photoionization
and photoheating rates derived from UVB synthesis models. We show that
simulations using canonical UVB rates reionize, and perhaps more importantly,
spuriously heat the IGM, much earlier z ~ 15 than they should. This problem
arises because at z > 6, where observational constraints are non-existent, the
UVB amplitude is far too high. We introduce a new methodology to remedy this
issue, and generate self-consistent photoionization and photoheating rates to
model any chosen reionization history. Following this approach, we run a suite
of hydrodynamical simulations of different reionization scenarios, and explore
the impact of the timing of reionization and its concomitant heat injection on
the the thermal state of the IGM. We present a comprehensive study of the
pressure smoothing scale of IGM gas, illustrating its dependence on the details
of both hydrogen and helium reionization, and argue that it plays a fundamental
role in interpreting Lyman-alpha forest statistics and the thermal evolution of
the IGM. The premature IGM heating we have uncovered implies previous work has
likely dramatically overestimated the impact of photoionization feedback on
galaxy formation, which sets the minimum halo mass able to form stars at high
redshifts. We make our new UVB photoionization and photoheating rates publicly
available for use in future simulations.},
  added-at = {2016-07-15T10:25:31.000+0200},
  author = {Oñorbe, Jose and Hennawi, Joseph F and Lukić, Zarija},
  biburl = {https://www.bibsonomy.org/bibtex/2e635708515a2ef929abc31cf97ebba12/miki},
  description = {[1607.04218] Self-Consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations},
  interhash = {d9dbd69292be0a5d1f4611bfcae11e7a},
  intrahash = {e635708515a2ef929abc31cf97ebba12},
  keywords = {cosmological heating reionisation simulation uvb},
  note = {cite arxiv:1607.04218Comment: 28 pages, 14 figures, 5 tables, submitted to ApJ, comments welcome},
  timestamp = {2016-07-15T10:25:31.000+0200},
  title = {Self-Consistent Modeling of Reionization in Cosmological Hydrodynamical
  Simulations},
  url = {http://arxiv.org/abs/1607.04218},
  year = 2016
}

@misc{yang2016intracluster,
  abstract = {Feedback from active galactic nuclei (AGN) is believed to prevent
catastrophic cooling in galaxy clusters. However, how the feedback energy is
transformed into heat, and how the AGN jets heat the intracluster medium (ICM)
isotropically, still remain elusive. In this work, we gain insights into the
relative importance of different heating mechanisms using three-dimensional
hydrodynamic simulations including cold gas accretion and momentum-driven jet
feedback, which are the most successful models to date in terms reproducing the
properties of cool cores. We find that there is net heating within two `jet
cones' (within ~30 degrees from the axis of jet precession) where the ICM gains
entropy by shock heating and mixing with the hot thermal gas within bubbles.
Outside the jet cones, the ambient gas is heated by weak shocks, but not enough
to overcome radiative cooling, therefore forming a `reduced' cooling flow.
Consequently, the cluster core is in a process of `gentle circulation' over
billions of years. Within the jet cones, there is significant adiabatic cooling
as the gas is uplifted by buoyantly rising bubbles; outside the cones, energy
is supplied by inflow of already-heated gas from the jet cones as well as
adiabatic compression as the gas moves toward the center. In other words, the
fluid dynamics self-adjusts such that it compensates and transports the heat
provided by the AGN, and hence no fine-tuning of the heating profile of any
process is necessary. Throughout the cluster evolution, turbulent energy is
only at the percent level compared to gas thermal energy, and thus turbulent
heating is not the main source of heating in our simulation.},
  added-at = {2016-05-09T10:10:18.000+0200},
  author = {Yang, H. Y. K. and Reynolds, C. S.},
  biburl = {https://www.bibsonomy.org/bibtex/2a36919dc6946490eb77aeea2d4c7facd/miki},
  description = {[1605.01725] How AGN Jets Heat the Intracluster Medium -- Insights from Hydrodynamic Simulations},
  interhash = {f9d542a4a602e179d99eee63609795db},
  intrahash = {a36919dc6946490eb77aeea2d4c7facd},
  keywords = {agn heating icm jets simulations},
  note = {cite arxiv:1605.01725Comment: 17 pages, 12 figures, submitted to ApJ},
  timestamp = {2016-05-09T10:10:29.000+0200},
  title = {How AGN Jets Heat the Intracluster Medium -- Insights from Hydrodynamic
  Simulations},
  url = {http://arxiv.org/abs/1605.01725},
  year = 2016
}

@misc{grand2015vertical,
  abstract = {Vertically extended, high velocity dispersion stellar distributions appear to
be a ubiquitous feature of disc galaxies, and both internal and external
mechanisms have been proposed to be the major driver of their formation.
However, it is unclear to what extent each mechanism can generate such a
distribution, which is likely to depend on the assembly history of the galaxy.
To this end, we perform 16 high resolution cosmological-zoom simulations of
Milky Way-sized galaxies using the state-of-the-art cosmological
magneto-hydrodynamical code \textlcsc{AREPO}, and analyse the evolution of the
vertical kinematics of the stellar disc in connection with various heating
mechanisms. We find that the bar is the dominant heating mechanism in most
cases, whereas spiral arms, radial migration, and adiabatic heating from
mid-plane density growth are all sub-dominant. The strongest source, though
less prevalent than bars, originates from external perturbations from
satellites/sub-halos of masses log$_{10} (M/\rm M_{\odot}) \gtrsim 10$.
However, in many simulations the orbits of newborn star particles become cooler
with time, such that they dominate the shape of the age-velocity dispersion
relation and overall vertical disc structure unless a strong external
perturbation takes place.},
  added-at = {2015-12-09T10:17:42.000+0100},
  author = {Grand, Robert J. J. and Springel, Volker and Gómez, Facundo A. and Marinacci, Federico and Pakmor, Rüdiger and Campbell, David J. R. and Jenkins, Adrian},
  biburl = {https://www.bibsonomy.org/bibtex/2161b6299d18b1d8a29ebbf7b6cb2328a/miki},
  description = {[1512.02219] Vertical disc heating in Milky Way-sized galaxies in a cosmological context},
  interhash = {ed8b15a2418bc4726f70a9e1e287442a},
  intrahash = {161b6299d18b1d8a29ebbf7b6cb2328a},
  keywords = {bar disc formation heating},
  note = {cite arxiv:1512.02219Comment: 21 pages, 14 figures. MNRAS submitted. Comments welcomed},
  timestamp = {2015-12-09T10:17:42.000+0100},
  title = {Vertical disc heating in Milky Way-sized galaxies in a cosmological
  context},
  url = {http://arxiv.org/abs/1512.02219},
  year = 2015
}

@misc{bocchio2015detection,
  abstract = {Observations of edge-on galaxies allow us to investigate the vertical extent
and properties of dust, gas and stellar distributions. NGC 891 has been studied
for decades and represents one of the best studied cases of an edge-on galaxy.
We use deep PACS data together with IRAC, MIPS and SPIRE data to study the
vertical extent of dust emission around NGC 891. We also test the presence of a
more extended, thick dust component. By performing a convolution of an
intrinsic vertical profile emission with each instrument PSF and comparing it
with observations we derived the scaleheight of a thin and thick dust disc
component. For all wavelengths considered the emission is best fit with the sum
of a thin and a thick dust component. The scaleheight of both dust components
shows a gradient passing from 70 $\mu$m to 250 $\mu$m. This could be due to a
drop in dust heating (and thus dust temperature) with the distance from the
plane, or to a sizable contribution ($\sim 15 - 80%$) of an unresolved thin
disc of hotter dust to the observed surface brightness at shorter wavelengths.
The scaleheight of the thick dust component, using observations from 70 $\mu$m
to 250 $\mu$m has been estimated to be $(1.44\pm 0.12)$ kpc, consistent with
previous estimates (extinction and scattering in optical bands and MIR
emission). The amount of dust mass at distances larger than $\sim 2$ kpc from
the midplane represents $2 - 3.3$ % of the total galactic dust mass and the
relative abundance of small grains with respect to large grains is almost
halved comparing to that in the midplane. The paucity of small grains high
above the midplane might indicate that dust is hit by interstellar shocks or
galactic fountains and entrained together with gas. The halo dust component is
likely to be embedded in an atomic / molecular gas and heated by a thick
stellar disc.},
  added-at = {2015-09-28T10:43:35.000+0200},
  author = {Bocchio, M. and Bianchi, S. and Hunt, L. K. and Schneider, R.},
  biburl = {https://www.bibsonomy.org/bibtex/22c7b508ffe4b8abdbc5e528b653dec51/miki},
  description = {[1509.07677] Halo dust detection around NGC 891},
  interhash = {8fc23bafa86fa42f6b4ff3a3095162aa},
  intrahash = {2c7b508ffe4b8abdbc5e528b653dec51},
  keywords = {dust halo heating},
  note = {cite arxiv:1509.07677Comment: 15 pages, 13 figures, A&A accepted},
  timestamp = {2015-09-28T10:43:35.000+0200},
  title = {Halo dust detection around NGC 891},
  url = {http://arxiv.org/abs/1509.07677},
  year = 2015
}

@misc{lamberts2015patchy,
  abstract = {TeV-blazars potentially heat the intergalactic medium (IGM) as their gamma
rays interact with photons of the extragalactic background light to produce
electron-positron pairs, which lose their kinetic energy to the surrounding
medium through plasma instabilities. This results in a heating mechanism that
is only weakly sensitive to the local density, and therefore approximately
spatially uniform, naturally producing an inverted temperature-density relation
in underdense regions. In this paper we go beyond the approximation of uniform
heating and quantify the heating rate fluctuations due to the clustered
distribution of blazars and how this impacts on the thermal history of the IGM.
We analytically compute a filtering function that relates the heating rate
fluctuations to the underlying dark matter density field. We implement it in
the cosmological code GADGET-3 and perform large scale simulations to determine
the impact of inhomogeneous heating. We show that, because of blazar
clustering, blazar heating is inhomogeneous for z>= 2. At high redshift, the
temperature-density relation shows an important scatter and presents a low
temperature envelope of unheated regions, in particular at low densities and
within voids. However, the median temperature of the IGM is close to that in
the uniform case, albeit slightly lower at low redshift. We find that blazar
heating is more complex than initially assumed and that the temperature-density
relation is not unique. Our analytic model for the heating rate fluctuations
couples well with large scale simulations and provides a cost-effective
alternative to subgrid models.},
  added-at = {2015-03-02T09:58:10.000+0100},
  author = {Lamberts, Astrid and Chang, Philip and Pfrommer, Christoph and Puchwein, Ewald and Broderich, Avery E. and Shalaby, Mohamad},
  biburl = {https://www.bibsonomy.org/bibtex/2c7c961628c1d615a953d0cb1378ee232/miki},
  description = {[1502.07980] Patchy blazar heating: diversifying the thermal history of the intergalactic medium},
  interhash = {e846f5be3eba55f6da7fbe96cff52772},
  intrahash = {c7c961628c1d615a953d0cb1378ee232},
  keywords = {blazar heating igm thermal},
  note = {cite arxiv:1502.07980Comment: 17 pages, 9 figures, submitted to ApJ},
  timestamp = {2015-03-02T09:58:10.000+0100},
  title = {Patchy blazar heating: diversifying the thermal history of the
  intergalactic medium},
  url = {http://arxiv.org/abs/1502.07980},
  year = 2015
}

@misc{hunt2014heating,
  abstract = {Physical conditions of the interstellar medium in galaxies are closely linked
to the ambient radiation field and the heating of dust grains. In order to
characterize dust properties in galaxies over a wide range of physical
conditions, we present here the radial surface brightness profiles of the
entire sample of 61 galaxies from Key Insights into Nearby Galaxies:
Far-Infrared Survey with Herschel (KINGFISH). The main goal of our work is the
characterization of the grain emissivities, dust temperatures, and interstellar
radiation fields responsible for heating the dust. After fitting the dust and
stellar radial profiles with exponential functions, we fit the far-infrared
spectral energy distribution (SED) in each annular region with
single-temperature modified black bodies using both variable (MBBV) and fixed
(MBBF) emissivity indices beta, as well as with physically motivated dust
models. Results show that while most SED parameters decrease with radius, the
emissivity index beta also decreases with radius in some galaxies, but in
others is increasing, or rising in the inner regions and falling in the outer
ones. Despite the fixed grain emissivity (average beta~ 2.1) of the
physically-motivated models, they are well able to accommodate flat spectral
slopes with beta<= 1. We find that flatter slopes (beta<= 1.5) are associated
with cooler temperatures, contrary to what would be expected from the usual
Tdust-beta degeneracy. This trend is related to variations in Umin since beta
and Umin are very closely linked over the entire range in Umin sampled by the
KINGFISH galaxies: low Umin is associated with flat beta<=1. Both these results
strongly suggest that the low apparent \beta values (flat slopes) in MBBV fits
are caused by temperature mixing along the line-of-sight, rather than by
intrinsic variations in grain properties. Abstract truncated for arXiv.},
  added-at = {2014-09-23T09:41:18.000+0200},
  author = {Hunt, L. K. and Draine, B. T. and Bianchi, S. and Gordon, K. D. and Aniano, G. and Calzetti, D. and Dale, D. A. and Helou, G. and Hinz, J. L. and Kennicutt, R. C. and Roussel, H. and Wilson, C. D. and Bolatto, A. and Boquien, M. and Croxall, K. V. and Galametz, M. and de Paz, A. Gil and Koda, J. and Munoz-Mateos, J. C. and Sandstrom, K. M. and Sauvage, M. and Vigroux, L. and Zibetti, S.},
  biburl = {https://www.bibsonomy.org/bibtex/216f15eb0119f7fd0e8573460aa2ad02a/miki},
  description = {[1409.5916] Cool dust heating and temperature mixing in nearby star-forming galaxies},
  interhash = {0a223551f147444741c8e471514c54a0},
  intrahash = {16f15eb0119f7fd0e8573460aa2ad02a},
  keywords = {dust forming galaxy heating nearby star},
  note = {cite arxiv:1409.5916Comment: 28 pages, 20 figures, accepted for publication in A&A},
  timestamp = {2014-09-23T09:41:18.000+0200},
  title = {Cool dust heating and temperature mixing in nearby star-forming galaxies},
  url = {http://arxiv.org/abs/1409.5916},
  year = 2014
}

@misc{barnes2014photoionisation,
  abstract = {The Diffuse Ionised Gas (DIG) in galaxies traces photoionisation feedback
from massive stars. Through three dimensional photoionisation simulations, we
study the propagation of ionising photons, photoionisation heating and the
resulting distribution of ionised and neutral gas within snapshots of
magnetohydrodynamic simulations of a supernova driven turbulent interstellar
medium. We also investigate the impact of non-photoionisation heating on
observed optical emission line ratios. Inclusion of a heating term which scales
less steeply with electron density than photoionisation is required to produce
diagnostic emission line ratios similar to those observed with the Wisconsin
H{\alpha} Mapper. Once such heating terms have been included, we are also able
to produce temperatures similar to those inferred from observations of the DIG,
with temperatures increasing to above 15000 K at heights |z| > 1 kpc. We find
that ionising photons travel through low density regions close to the midplane
of the simulations, while travelling through diffuse low density regions at
large heights. The majority of photons travel small distances (< 100pc);
however some travel kiloparsecs and ionise the DIG.},
  added-at = {2014-03-14T09:49:30.000+0100},
  author = {Barnes, J. E. and Wood, Kenneth and Hill, Alex S. and Haffner, L. M.},
  biburl = {https://www.bibsonomy.org/bibtex/22fe5a6910a3244ca0c520b910ccbafb1/miki},
  description = {[1403.3261] Photoionisation and Heating of a Supernova Driven, Turbulent, Interstellar Medium},
  interhash = {c17e03d4663081372453e81caa89b3c4},
  intrahash = {2fe5a6910a3244ca0c520b910ccbafb1},
  keywords = {heating ism photoionisation supernova},
  note = {cite arxiv:1403.3261Comment: 10 pages, 13 figures, accepted to MNRAS},
  timestamp = {2014-03-14T09:49:30.000+0100},
  title = {Photoionisation and Heating of a Supernova Driven, Turbulent,
  Interstellar Medium},
  url = {http://arxiv.org/abs/1403.3261},
  year = 2014
}

@misc{oklopcic2013lymanalpha,
  abstract = {The intergalactic medium (IGM) prior to the epoch of reionization consists
mostly of neutral hydrogen gas. Ly-alpha photons produced by early stars
resonantly scatter off hydrogen atoms, causing energy exchange between the
radiation field and the gas. This interaction results in moderate heating of
the gas due to the recoil of the atoms upon scattering, which is of great
interest for future studies of the pre-reionization IGM in the HI 21 cm line.
We investigate the effect of this Ly-alpha heating in the IGM with linear
density, temperature and velocity perturbations. Perturbations smaller than the
diffusion length of photons could be damped due to heat conduction by Ly-alpha
photons. The scale at which damping occurs and the strength of this effect
depend on various properties of the gas, the flux of Ly-alpha photons and the
way in which photon frequencies are redistributed upon scattering. To find the
relevant length scale and the extent to which Ly-alpha heating affects
perturbations, we calculate the gas heating rates by numerically solving
linearized Boltzmann equations in which scattering is treated by the
Fokker-Planck approximation. We find that (i) perturbations add a small
correction to the gas heating rate, and (ii) the damping of temperature
perturbations occurs at scales with comoving wavenumber k>10^4 Mpc^{-1}, which
are much smaller than the Jeans scale and thus unlikely to substantially affect
the observed 21 cm signal.},
  added-at = {2013-07-29T13:40:50.000+0200},
  author = {Oklopcic, Antonija and Hirata, Christopher M.},
  biburl = {https://www.bibsonomy.org/bibtex/2f4cc87a915a030311ff35f44458fcd1e/miki},
  description = {[1307.6859] Lyman-alpha Heating of Inhomogeneous High-redshift Intergalactic Medium},
  interhash = {9c8dd141dc87832161f48af1d9461478},
  intrahash = {f4cc87a915a030311ff35f44458fcd1e},
  keywords = {heating igm lya scatter},
  note = {cite arxiv:1307.6859Comment: 10 pages, 4 figures},
  timestamp = {2013-07-29T13:40:50.000+0200},
  title = {Lyman-alpha Heating of Inhomogeneous High-redshift Intergalactic Medium},
  url = {http://arxiv.org/abs/1307.6859},
  year = 2013
}

@misc{krumholz2013despotic,
  abstract = {I describe DESPOTIC, a code to Derive the Energetics and SPectra of Optically
Thick Interstellar Clouds. DESPOTIC represents such clouds using a one-zone
model, and can calculate line luminosities, line cooling rates, and in
restricted cases line profiles using an escape probability formalism. It also
includes approximate treatments of the other dominant heating and cooling
processes for the cold interstellar medium, including cosmic ray and X-ray
heating, grain photoelectric heating, heating of the dust by infrared and
ultraviolet radiation, thermal cooling of the dust, and collisional energy
exchange between dust and gas. Based on these heating and cooling rates,
DESPOTIC can calculate clouds' equilibrium gas and dust temperatures, and their
time-dependent thermal evolution. The software is intended to allow rapid and
interactive calculation of clouds' characteristic temperatures, identification
of their dominant heating and cooling mechanisms, and prediction of their
observable spectra across a wide range of interstellar environments. DESPOTIC
is implemented as a Python package, and is released under the GNU General
Public License.},
  added-at = {2013-04-10T19:02:55.000+0200},
  author = {Krumholz, Mark R.},
  biburl = {https://www.bibsonomy.org/bibtex/2522530413495438b0cf9f73656f1aa1b/miki},
  description = {[1304.2404] DESPOTIC -- A New Software Library to Derive the Energetics and SPectra of Optically Thick Interstellar Clouds},
  interhash = {3cf23d411be16219aa65bdb210083c12},
  intrahash = {522530413495438b0cf9f73656f1aa1b},
  keywords = {clouds code cooling heating},
  note = {cite arxiv:1304.2404Comment: 20 pages, 11 figures, submitted to MNRAS},
  timestamp = {2013-04-10T19:02:55.000+0200},
  title = {DESPOTIC -- A New Software Library to Derive the Energetics and SPectra
  of Optically Thick Interstellar Clouds},
  url = {http://arxiv.org/abs/1304.2404},
  year = 2013
}

@misc{groves2012heating,
  abstract = {We use new Herschel multi-band imaging of the Andromeda galaxy to analyze how
dust heating occurs in the central regions of galaxy spheroids that are
essentially devoid of young stars. We construct a dust temperature map of M31
through fitting modified blackbody SEDs to the Herschel data, and find that the
temperature within 2 kpc rises strongly from the mean value in the disk of 17
pm 1K to \sim35K at the centre. UV to near-IR imaging of the central few kpc
shows directly the absence of young stellar populations, delineates the radial
profile of the stellar density, and demonstrates that even the near-UV dust
extinction is optically thin in M31's bulge. This allows the direct calculation
of the stellar radiation heating in the bulge, U\ast(r), as a function of
radius. The increasing temperature profile in the centre matches that expected
from the stellar heating, i.e. that the dust heating and cooling rates track
each other over nearly two orders of magnitude in U\ast. The modelled dust
heating is in excess of the observed dust temperatures, suggesting that it is
more than sufficient to explain the observed IR emission. Together with the
wavelength dependent absorption cross section of the dust, this demonstrates
directly that it is the optical, not UV, radiation that sets the heating rate.
This analysis shows that neither young stellar populations nor stellar near-UV
radiation are necessary to heat dust to warm temperatures in galaxy spheroids.
Rather, it is the high densities of Gyr-old stellar populations that provide a
sufficiently strong diffuse radiation field to heat the dust. To the extent
which these results pertain to the tenuous dust found in the centres of
early-type galaxies remains yet to be explored.},
  added-at = {2012-06-15T08:46:09.000+0200},
  author = {Groves, Brent and Krause, Oliver and Sandstrom, Karin and Schmiedeke, Anika and Leroy, Adam and Linz, Hendrik and Kapala, Maria and Rix, Hans-Walter and Schinnerer, Eva and Tabatabaei, Fatemeh and Walter, Fabian and da Cunha, Elisabete},
  biburl = {https://www.bibsonomy.org/bibtex/2c9391efa5105d27c46dd197bcea506bc/miki},
  description = {[1206.2925] The heating of dust by old stellar populations in the Bulge of M31},
  interhash = {92d8b6d81eebb442a078088c75583394},
  intrahash = {c9391efa5105d27c46dd197bcea506bc},
  keywords = {dust heating optical},
  note = {cite arxiv:1206.2925Comment: 11 pages. Accepted for publication in MNRAS},
  timestamp = {2012-06-15T08:46:09.000+0200},
  title = {The heating of dust by old stellar populations in the Bulge of M31},
  url = {http://arxiv.org/abs/1206.2925},
  year = 2012
}

@misc{Gnedin2012,
  abstract = {  Cooling functions of cosmic gas are a crucial ingredient for any study of gas
dynamics and thermodynamics in the interstellar and intergalactic medium. As
such, they have been studied extensively in the past under the assumption of
collisional ionization equilibrium. However, for a wide range of applications,
the local radiation field introduces a non-negligible, often dominant,
modification to the cooling and heating functions. In the most general case,
these modifications cannot be described in simple terms, and would require a
detailed calculation with a large set of chemical species using a radiative
transfer code (the well-known code Cloudy, for example). We show, however, that
for a sufficiently general variation in the spectral shape and intensity of the
incident radiation field, the cooling and heating functions can be
\emph{approximated} as depending only on (1) the photo-dissociation rate of
molecular hydrogen, (2) the hydrogen photo-ionization rate, and (3) the
photo-ionization rate of OVIII; more complex and more accurate approximations
also exist. Such dependence is easy to tabulate and implement in cosmological
or galactic-scale simulations, thus economically accounting for an important
but rarely-included factor in the evolution of cosmic gas. We also show a few
examples where the radiation environment has a large effect, the most
spectacular of which is a quasar that suppresses gas cooling in its host halo
without any mechanical or non-radiative thermal feedback.
},
  added-at = {2012-01-26T20:18:16.000+0100},
  author = {Gnedin, Nickolay Y. and Hollon, Nicholas},
  biburl = {https://www.bibsonomy.org/bibtex/2b549a52a07e1a544b7c640e3eb6a011d/miki},
  description = {[1201.5116] Cooling and Heating Functions of Photoionized Gas},
  interhash = {2af6fdd4e52db8e0e66c4de89be35a4c},
  intrahash = {b549a52a07e1a544b7c640e3eb6a011d},
  keywords = {cooling heating photionization},
  note = {cite arxiv:1201.5116
Comment: submitted to ApJS},
  timestamp = {2012-01-26T20:18:16.000+0100},
  title = {Cooling and Heating Functions of Photoionized Gas},
  url = {http://arxiv.org/abs/1201.5116},
  year = 2012
}