text:
arth-sized exoplanets. We find that sulfur dioxide from large explosive eruptions does present a spectral signal that is remotely detectable especially for secondary eclipse measurements around the closest stars and ground-based telescopes, and report the frequency and magnitude of the expected signatures. The transit probability of a planet in the habitable zone decreases with distance from the host star, making small, nearby host stars the best targets.},
	language = {en},
	number = {5},
	urldate = {2020-06-06},
	journal = {AJ},
	author = {Kaltenegger, L. and Henning, W. G. and Sasselov, D. D.},
	month = oct,
	year = {2010},
	note = {Publisher: IOP Publishing},
	pages = {1370--1380},
	file = {IOP Full Text PDF:/Users/fb90/Zotero/storage/98K79RS9/Kaltenegger et al. - 2010 - DETECTING VOLCANISM ON EXTRASOLAR PLANETS.pdf:application/pdf}
}

@article{luger2017,
	title = {Planet–{Planet} {Occultations} in {TRAPPIST}-1 and {Other} {Exoplanet} {Systems}},
	volume = {851},
	issn = {1538-4357},
	url = {https://iopscience.iop.org/article/10.3847/1538-4357/aa9c43},
	doi = {10.3847/1538-4357/aa9c43},
	abstract = {We explore the occurrence and detectability of planet–planet occultations (PPOs) in exoplanet systems. These are events during which a planet occults the disk of another planet in the same system, imparting a small photometric signal as its thermal or reﬂected light is blocked. We focus on the planets in TRAPPIST-1, whose orbital planes we show are aligned to {\textless}0. 3 at 90\% conﬁdence. We present a photodynamical model for predicting and computing PPOs in TRAPPIST-1 and other systems for various assumptions of the planets’ atmospheric states. When marginalizing over the uncertainties on all orbital parameters, we ﬁnd that the rate of PPOs in TRAPPIST-1 is about 1.4 per day. We investigate the prospects for detection of these events with the James Webb Space Telescope, ﬁnding that ∼10–20 occultations per year of b and c should be above the noise level at 12–15μm. Joint modeling of several of these PPOs could lead to a robust detection. Alternatively, observations with the proposed Origins Space Telescope should be able to detect individual PPOs at high signal-to-noise ratios. We show how PPOs can be used to break transit timing variation degeneracies, imposing strong constraints on the eccentricities and masses of the planets, as well as to constrain the longitudes of nodes and thus the complete three-dimensional structure of the system. We further show how modeling of these events can be used to reveal a planet’s day/night temperature contrast and construct crude surface maps. We make our photodynamical code available on github (https://github.com/rodluger/planetplanet).},
	language = {en},
	number = {2},
	urldate = {2020-06-05},
	journal = {ApJ},
	author = {Luger, Rodrigo and Lustig-Yaeger, Jacob and Agol, Eric},
	month = dec,
	year = {2017},
	pages = {94},
	file = {Luger et al. - 2017 - Planet–Planet Occultations in TRAPPIST-1 and Other.pdf:/Users/fb90/Zotero/storage/MC4JBNP4/Luger et al. - 2017 - Planet–Planet Occultations in TRAPPIST-1 and Other.pdf:application/pdf}
}

@article{henning2018,
	title = {Highly {Volcanic} {Exoplanets}, {Lava} {Worlds}, and {Magma} {Ocean} {Worlds}: {An} {Emerging} {Class} of {Dynamic} {Exoplanets} of {Significant} {Scientific} {Priority}},
	shorttitle = {Highly {Volcanic} {Exoplanets}, {Lava} {Worlds}, and {Magma} {Ocean} {Worlds}},
	url = {http://arxiv.org/abs/1804.05110},
	abstract = {Highly volcanic exoplanets, which can be variously characterized as 'lava worlds', 'magma ocean worlds', or 'super-Ios' are high priority targets for investigation. The term 'lava world' may refer to any planet with extensive surface lava lakes, while the term 'magma ocean world' refers to planets with global or hemispherical magma oceans at their surface. 'Highly volcanic planets', including super-Ios, may simply have large, or large numbers of, active explosive or extrusive volcanoes of any form. They are plausibly highly diverse, with magmatic processes across a wide range of compositions, temperatures, activity rates, volcanic eruption styles, and background gravitational force magnitudes. Worlds in all these classes are likely to be the most characterizable rocky exoplanets in the near future due to observational advantages that stem from their preferential occurrence in short orbital periods and their bright day-side flux in the infrared. Transit techniques should enable a level of characterization of these worlds analogous to hot Jupiters. Understanding processes on highly volcanic worlds is critical to interpret imminent observations. The physical states of these worlds are likely to inform not just geodynamic processes, but also planet formation, and phenomena crucial to habitability. Volcanic and magmatic activity uniquely allows chemical investigation of otherwise spectroscopically inaccessible interior compositions. These worlds will be vital to assess the degree to which planetary interior element abundances compare to their stellar hosts, and may also offer pathways to study both the very young Earth, and the very early form of many silicate planets where magma oceans and surface lava lakes are expected to be more prevalent. We suggest that highly volcanic worlds may become second only to habitable worlds in terms of both scientific and public long-term interest.},
	urldate = {2020-06-05},
	journal = {arXiv:1804.05110 [astro-ph, physics:physics]},
	author = {Henning, Wade G. and Renaud, Joseph P. and Saxena, Prabal and Whelley, Patrick L. and Mandell, Avi M. and Matsumura, Soko and Glaze, Lori S. and Hurford, Terry A. and Livengood, Timothy A. and Hamilton, Christopher W. and Efroimsky, Michael and Makarov, Valeri V. and Berghea, Ciprian T. and Guzewich, Scott D. and Tsigaridis, Kostas and Arney, Giada N. and Cremons, Daniel R. and Kane, Stephen R. and Bleacher, Jacob E. and Kopparapu, Ravi K. and Kohler, Erika and Lee, Yuni and Rushby, Andrew and Kuang, Weijia and Barnes, Rory and Richardson, Jacob A. and Driscoll, Peter and Schmerr, Nicholas C. and Del Genio, Anthony D. and Davies, Ashley Gerard and Kaltenegger, Lisa and Elkins-Tanton, Linda and Fujii, Yuka and Schaefer, Laura and Ranjan, Sukrit and Quintana, Elisa and Barclay, Thomas S. and Hamano, Keiko and Petro, Noah E. and Kendall, Jordan D. and Lopez, Eric D. and Sasselov, Dimitar D.},
	month = apr,
	year = {2018},
	note = {arXiv: 1804.05110},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics, Physics - Geophysics},
	annote = {Comment: A white paper submitted in response to the National Academy of Sciences 2018 Exoplanet Science Strategy solicitation, from the NASA Sellers Exoplanet Environments Collaboration (SEEC) of the Goddard Space Flight Center. 6 pages, 0 figures},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/JJCGSMQ5/Henning et al. - 2018 - Highly Volcanic Exoplanets, Lava Worlds, and Magma.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/RH7AY4ZF/1804.html:text/html}
}

@article{demory2016a,
	title = {A map of the large day-night temperature gradient of a super-{Earth} exoplanet},
	volume = {532},
	issn = {0028-0836, 1476-4687},
	url = {http://arxiv.org/abs/1604.05725},
	doi = {10.1038/nature17169},
	abstract = {Over the past decade, observations of giant exoplanets (Jupiter-size) have provided key insights into their atmospheres, but the properties of lower-mass exoplanets (sub-Neptune) remain largely unconstrained because of the challenges of observing small planets. Numerous efforts to observe the spectra of super-Earths (exoplanets with masses of one to ten times that of Earth) have so far revealed only featureless spectra. Here we report a longitudinal thermal brightness map of the nearby transiting super-Earth 55 Cancri e revealing highly asymmetric dayside thermal emission and a strong day-night temperature contrast. Dedicated space-based monitoring of the planet in the infrared revealed a modulation of the thermal flux as 55 Cancri e revolves around its star in a tidally locked configuration. These observations reveal a hot spot that is located 41 +- 12 degrees east of the substellar point (the point at which incident light from the star is perpendicular to the surface of the planet). From the orbital phase curve, we also constrain the nightside brightness temperature of the planet to 1380 +- 400 kelvin and the temperature of the warmest hemisphere (centred on the hot spot) to be about 1300 kelvin hotter (2700 +- 270 kelvin) at a wavelength of 4.5 microns, which indicates inefficient heat redistribution from the dayside to the nightside. Our observations are consistent with either an optically thick atmosphere with heat recirculation confined to the planetary dayside, or a planet devoid of atmosphere with low-viscosity magma flows at the surface.},
	number = {7598},
	urldate = {2020-06-05},
	journal = {Nature},
	author = {Demory, Brice-Olivier and Gillon, Michael and de Wit, Julien and Madhusudhan, Nikku and Bolmont, Emeline and Heng, Kevin and Kataria, Tiffany and Lewis, Nikole and Hu, Renyu and Krick, Jessica and Stamenkovic, Vlada and Benneke, Bjorn and Kane, Stephen and Queloz, Didier},
	month = apr,
	year = {2016},
	note = {arXiv: 1604.05725},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	pages = {207--209},
	annote = {Comment: Published in Nature on 14 April 2016. Preprint version includes 32 pages, 11 figures and 2 tables},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/HQQTXRDI/Demory et al. - 2016 - A map of the large day-night temperature gradient .pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/WY8F4HSW/1604.html:text/html}
}

@article{demory2016b,
	title = {A map of the large day-night temperature gradient of a super-{Earth} exoplanet},
	volume = {532},
	issn = {0028-0836},
	url = {http://adsabs.harvard.edu/abs/2016Natur.532..207D},
	doi = {10.1038/nature17169},
	abstract = {Over the past decade, observations of giant exoplanets (Jupiter-size) have provided key insights into their atmospheres, but the properties of lower-mass exoplanets (sub-Neptune) remain largely unconstrained because of the challenges of observing small planets. Numerous efforts to observe the spectra of super-Earths—exoplanets with masses of one to ten times that of Earth—have so far revealed only featureless spectra. Here we report a longitudinal thermal brightness map of the nearby transiting super-Earth 55 Cancri e (refs 4, 5) revealing highly asymmetric dayside thermal emission and a strong day-night
temperature contrast. Dedicated space-based monitoring of the planet in the infrared revealed a modulation of the thermal flux as 55 Cancri e revolves around its star in a tidally locked configuration. These observations reveal a hot spot that is located
41 ± 12 degrees east of the substellar point (the
point at which incident light from the star is perpendicular to the surface of the planet). From the orbital phase curve, we also constrain the nightside brightness temperature of the planet to
1,380 ± 400 kelvin and the temperature of the
warmest hemisphere (centred on the hot spot) to be about 1,300 kelvin hotter (2,700 ± 270 kelvin) at a wavelength of 4.5
micrometres, which indicates inefficient heat redistribution from the dayside to the nightside. Our observations are consistent with either an optically thick atmosphere with heat recirculation confined to the planetary dayside, or a planet devoid of atmosphere with low-viscosity magma flows at the surface.},
	urldate = {2020-06-05},
	journal = {Nature},
	author = {Demory, Brice-Olivier and Gillon, Michael and de Wit, Julien and Madhusudhan, Nikku and Bolmont, Emeline and Heng, Kevin and Kataria, Tiffany and Lewis, Nikole and Hu, Renyu and Krick, Jessica and Stamenković, Vlada and Benneke, Björn and Kane, Stephen and Queloz, Didier},
	month = apr,
	year = {2016},
	pages = {207--209},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/8FU2EVPT/Demory et al. - 2016 - A map of the large day-night temperature gradient .pdf:application/pdf}
}

@article{hammond2017,
	title = {Linking the {Climate} and {Thermal} {Phase} {Curve} of 55 {Cancri} e},
	volume = {849},
	issn = {1538-4357},
	url = {https://iopscience.iop.org/article/10.3847/1538-4357/aa9328},
	doi = {10.3847/1538-4357/aa9328},
	abstract = {The thermal phase curve of 55 Cancri e is the ﬁrst measurement of the temperature distribution of a tidally locked super-Earth, but raises a number of puzzling questions about the planet’s climate. The phase curve has a high amplitude and peak offset, suggesting that it has a signiﬁcant eastward hot-spot shift as well as a large day–night temperature contrast. We use a general circulation model to model potential climates, and investigate the relation between bulk atmospheric composition and the magnitude of these seemingly contradictory features. We conﬁrm theoretical models of tidally locked circulation are consistent with our numerical model of 55 Cnc e, and rule out certain atmospheric compositions based on their thermodynamic properties. Our best-ﬁtting atmosphere has a signiﬁcant hot-spot shift and day–night contrast, although these are not as large as the observed phase curve. We discuss possible physical processes that could explain the observations, and show that night-side cloud formation from species such as SiO from a day-side magma ocean could potentially increase the phase curve amplitude and explain the observations. We conclude that the observations could be explained by an optically thick atmosphere with a low mean molecular weight, a surface pressure of several bars, and a strong eastward circulation, with nightside cloud formation a possible explanation for the difference between our model and the observations.},
	language = {en},
	number = {2},
	urldate = {2020-06-05},
	journal = {ApJ},
	author = {Hammond, Mark and T. Pierrehumbert, Raymond},
	month = nov,
	year = {2017},
	pages = {152},
	file = {Hammond and T. Pierrehumbert - 2017 - Linking the Climate and Thermal Phase Curve of 55 .pdf:/Users/fb90/Zotero/storage/2H6GXXRL/Hammond and T. Pierrehumbert - 2017 - Linking the Climate and Thermal Phase Curve of 55 .pdf:application/pdf}
}

@article{luger2019,
	title = {{TESS} {Photometric} {Mapping} of a {Terrestrial} {Planet} in the {Habitable} {Zone}: {Detection} of {Clouds}, {Oceans}, and {Continents}},
	shorttitle = {{TESS} {Photometric} {Mapping} of a {Terrestrial} {Planet} in the {Habitable} {Zone}},
	url = {http://arxiv.org/abs/1903.12182},
	abstract = {To date, a handful of exoplanets have been photometrically mapped using phase-modulated reflection or emission from their surfaces, but the small amplitudes of such signals have limited previous maps almost exclusively to coarse dipolar features on hot giant planets. In this work, we uncover a signal using recently released data from the Transiting Exoplanet Survey Satellite (TESS), which we show corresponds to time-variable reflection from a terrestrial planet with a rotation period of 0.9972696 days. Using a spherical harmonic-based reflection model developed as an extension of the STARRY package, we are able to reconstruct the surface features of this rocky world. We recover a time-variable albedo map of the planet including persistent regions which we interpret as oceans and cloud banks indicative of continental features. We argue that this planet represents the most promising detection of a habitable world to date, although the potential intelligence of any life on it is yet to be determined.},
	urldate = {2020-06-05},
	journal = {arXiv:1903.12182 [astro-ph]},
	author = {Luger, Rodrigo and Bedell, Megan and Vanderspek, Roland and Burke, Christopher J.},
	month = mar,
	year = {2019},
	note = {arXiv: 1903.12182},
	keywords = {Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 22 pages, 9 figures. To be submitted to AAS journals after slight modifications},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/79ANLXYB/Luger et al. - 2019 - TESS Photometric Mapping of a Terrestrial Planet i.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/2PAMYEDQ/1903.html:text/html}
}

@article{morgado2019,
	title = {The 2014-2015 {Brazilian} mutual phenomena campaign for the {Jovian} satellites and improved results for the 2009 events},
	volume = {179},
	issn = {0032-0633},
	url = {http://adsabs.harvard.edu/abs/2019P%26SS..17904736M},
	doi = {10.1016/j.pss.2019.104736},
	abstract = {Progress in astrometry and orbital modelling of planetary moons in the
last decade enabled better determinations of their orbits. These studies
need accurate positions spread over extended periods. We present the
results of the 2014-2015 Brazilian campaign for 40 mutual events from 47
observed light curves by the Galilean satellites plus one eclipse of
Amalthea by Ganymede. We also reanalysed and updated results for 25
mutual events observed in the 2009 campaign.

All telescopes were equipped with narrow-band filters centred at 889 nm
with a width of 15 nm to eliminate the scattered light from Jupiter. The
albedos' ratio was determined using images before and after each event.
We simulated images of moons, umbra, and penumbra in the sky plane, and
integrated their fluxes to compute albedos, simulate light curves and
fit them to the observed ones using a chi-square fitting procedure. For
that, we used the complete version of the Oren-Nayer reflectance model.
The relative satellite positions mean uncertainty was 11.2 mas ( 35 km)
and 10.1 mas ( 31 km) for the 2014-2015 and 2009 campaigns
respectively. The simulated and observed ASCII light curve files are
freely available in electronic form at the Natural Satellites DataBase
(NSDB).

The 40/25 mutual events from our 2014-2015/2009 campaigns represent a
significant contribution of 17\%/15\% in comparison with the PHEMU
campaigns lead by the IMCCE. Besides that, our result for the eclipse of
Amalthea is only the 4th such measurement ever published
after the three ones observed by the 2014-2015 international PHEMU
campaign. Our results are suitable for new orbital/ephemeris
determinations for the Galilean moons and Amalthea.},
	urldate = {2020-06-05},
	journal = {Planetary and Space Science},
	author = {Morgado, B. and Vieira-Martins, R. and Assafin, M. and Dias-Oliveira, A. and Machado, D. I. and Camargo, J. I. B. and Malacarne, M. and Sfair, R. and Winter, O. C. and Braga-Ribas, F. and Benedetti-Rossi, G. and Boldrin, L. A. and Camargo, B. C. B. and Gaspar, H. S. and Gomes-Júnior, A. R. and Miranda, J. O. and de Santana, T. and Trabuco, L. L.},
	month = dec,
	year = {2019},
	keywords = {Amalthea, Astrometry, Callisto, Europa, Ganymede, Methods: data analysis, Planets and satellites: individual: Io},
	pages = {104736},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/5E7LKSC5/Morgado et al. - 2019 - The 2014-2015 Brazilian mutual phenomena campaign .pdf:application/pdf}
}

@article{saquet2018a,
	title = {The {PHEMU15} catalogue and astrometric results of the {Jupiter}'s {Galilean} satellite mutual occultation and eclipse observations made in 2014-2015},
	volume = {474},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2018MNRAS.474.4730S},
	doi = {10.1093/mnras/stx2957},
	abstract = {During the 2014-2015 mutual events season, the Institut de
Mécanique Céleste et de Calcul des
Éphémérides (IMCCE), Paris, France, and the
Sternberg Astronomical Institute (SAI), Moscow, Russia, led an
international observation campaign to record ground-based photometric
observations of Galilean moon mutual occultations and eclipses. We
focused on processing the complete photometric observations data base to
compute new accurate astrometric positions. We used our method to derive
astrometric positions from the light curves of the events. We developed
an accurate photometric model of mutual occultations and eclipses, while
correcting for the satellite albedos, Hapke's light scattering law, the
phase effect, and the limb darkening. We processed 609 light curves, and
we compared the observed positions of the satellites with the
theoretical positions from IMCCE NOE-5-2010-GAL satellite ephemerides
and INPOP13c planetary ephemeris. The standard deviation after fitting
the light curve in equatorial positions is ±24 mas, or 75 km at
Jupiter. The rms (O-C) in equatorial positions is ±50 mas, or 150
km at Jupiter.},
	urldate = {2020-06-05},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Saquet, E. and Emelyanov, N. and Robert, V. and Arlot, J.-E. and Anbazhagan, P. and Baillié, K. and Bardecker, J. and Berezhnoy, A. A. and Bretton, M. and Campos, F. and Capannoli, L. and Carry, B. and Castet, M. and Charbonnier, Y. and Chernikov, M. M. and Christou, A. and Colas, F. and Coliac, J.-F. and Dangl, G. and Dechambre, O. and Delcroix, M. and Dias-Oliveira, A. and Drillaud, C. and Duchemin, Y. and Dunford, R. and Dupouy, P. and Ellington, C. and Fabre, P. and Filippov, V. A. and Finnegan, J. and Foglia, S. and Font, D. and Gaillard, B. and Galli, G. and Garlitz, J. and Gasmi, A. and Gaspar, H. S. and Gault, D. and Gazeas, K. and George, T. and Gorda, S. Y. and Gorshanov, D. L. and Gualdoni, C. and Guhl, K. and Halir, K. and Hanna, W. and Henry, X. and Herald, D. and Houdin, G. and Ito, Y. and Izmailov, I. S. and Jacobsen, J. and Jones, A. and Kamoun, S. and Kardasis, E. and Karimov, A. M. and Khovritchev, M. Y. and Kulikova, A. M. and Laborde, J. and Lainey, V. and Lavayssiere, M. and Le Guen, P. and Leroy, A. and Loader, B. and Lopez, O. C. and Lyashenko, A. Y. and Lyssenko, P. G. and Machado, D. I. and Maigurova, N. and Manek, J. and Marchini, A. and Midavaine, T. and Montier, J. and Morgado, B. E. and Naumov, K. N. and Nedelcu, A. and Newman, J. and Ohlert, J. M. and Oksanen, A. and Pavlov, H. and Petrescu, E. and Pomazan, A. and Popescu, M. and Pratt, A. and Raskhozhev, V. N. and Resch, J.-M. and Robilliard, D. and Roschina, E. and Rothenberg, E. and Rottenborn, M. and Rusov, S. A. and Saby, F. and Saya, L. F. and Selvakumar, G. and Signoret, F. and Slesarenko, V. Y. and Sokov, E. N. and Soldateschi, J. and Sonka, A. and Soulie, G. and Talbot, J. and Tejfel, V. G. and Thuillot, W. and Timerson, B. and Toma, R. and Torsellini, S. and Trabuco, L. L. and Traverse, P. and Tsamis, V. and Unwin, M. and Abbeel, F. Van Den and Vandenbruaene, H. and Vasundhara, R. and Velikodsky, Y. I. and Vienne, A. and Vilar, J. and Vugnon, J.-M. and Wuensche, N. and Zeleny, P.},
	month = mar,
	year = {2018},
	keywords = {eclipses, astronomical data bases: miscellaneous, ephemerides, occultations, planets and satellites: general, techniques: photometric},
	pages = {4730--4739},
	file = {Submitted Version:/Users/fb90/Zotero/storage/RV6X6T3Q/Saquet et al. - 2018 - The PHEMU15 catalogue and astrometric results of t.pdf:application/pdf}
}

@article{arlot1974,
	title = {Mutual occultation and eclipse of {Jupiter} satellites {J}-1 and {J}-2 on {August} 30, 1973},
	volume = {35},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/1974A%26A....35..115A},
	abstract = {The light curve of the mutual occultation of the Jovian satellites J-2
and J-1 was obtained with the aid of a photoelectric photometer, and the
data were used to determine the radii of the satellites. The calculation
method used assumed uniform brightness for the disk of J-1 and previous
knowledge of the ephemeris values. Theoretical series of light curves
giving the luminous flux emitted by J-2 as a function of the time during
its occultation were calculated for several pairs of values for the
satellites' radii. The curve which most resembled the experimental curve
gave the correct values of the radii. The values found are: radius of
J-1 - 1,830 km; radius of J-2 - 1,457 km. These values are within the
limits of errors of the classical values.-},
	urldate = {2020-06-05},
	journal = {Astronomy and Astrophysics},
	author = {Arlot, J. E. and Camichel, H. and Link, F.},
	month = sep,
	year = {1974},
	keywords = {Astronomical Photometry, Eclipses, Electrophotometry, Ephemerides, Jupiter (Planet), Light Curve, Luminous Intensity, Natural Satellites, Occultation, Radii, Size Determination},
	pages = {115--119},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/W3MS8ZHK/Arlot et al. - 1974 - Mutual occultation and eclipse of Jupiter satellit.pdf:application/pdf}
}

@article{rathbun2006,
	title = {Loki, {Io}: {New} ground-based observations and a model describing the change from periodic overturn},
	volume = {33},
	issn = {0094-8276},
	shorttitle = {Loki, {Io}},
	url = {http://adsabs.harvard.edu/abs/2006GeoRL..3317201R},
	doi = {10.1029/2006GL026844},
	abstract = {Loki Patera is the most powerful volcano in the solar system. We have
obtained measurements of Loki's 3.5 micron brightness from NASA's
Infrared Telescope Facility (IRTF) and have witnessed a major change in
eruptive behavior. While Loki brightened by a factor of several every
540 days prior to 2001, from 2001 through 2004 Loki remained at a
constant, intermediate brightness. We have constructed a quantitative
model of Loki as a basaltic lava lake whose solidified crust overturns
when it becomes buoyantly unstable. By altering the speed at which the
overturn propagates across the patera, we can match our ground-based
brightness data. In addition, we can match other data taken at other
times and wavelengths. By slowing the propagation speed dramatically, we
can match the observations from 2001-2004. Such slowing could be due to
a small change in volatile content in the lava.},
	urldate = {2020-06-04},
	journal = {Geophysical Research Letters},
	author = {Rathbun, J. A. and Spencer, J. R.},
	month = sep,
	year = {2006},
	keywords = {8148, 8450), Planetary Sciences: Solid Surface Planets: Heat flow, Planetary Sciences: Solid Surface Planets: Instruments and techniques, Planetary Sciences: Solid Surface Planets: Origin and evolution, Planetary Sciences: Solid Surface Planets: Volcanism (6063},
	pages = {L17201},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/7LUHYPHW/Rathbun and Spencer - 2006 - Loki, Io New ground-based observations and a mode.pdf:application/pdf}
}

@article{rathbun2006a,
	title = {Loki, {Io}: {New} ground-based observations and a model describing the change from periodic overturn},
	volume = {33},
	copyright = {Copyright 2006 by the American Geophysical Union.},
	issn = {1944-8007},
	shorttitle = {Loki, {Io}},
	url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2006GL026844},
	doi = {10.1029/2006GL026844},
	abstract = {Loki Patera is the most powerful volcano in the solar system. We have obtained measurements of Loki's 3.5 micron brightness from NASA's Infrared Telescope Facility (IRTF) and have witnessed a major change in eruptive behavior. While Loki brightened by a factor of several every 540 days prior to 2001, from 2001 through 2004 Loki remained at a constant, intermediate brightness. We have constructed a quantitative model of Loki as a basaltic lava lake whose solidified crust overturns when it becomes buoyantly unstable. By altering the speed at which the overturn propagates across the patera, we can match our ground-based brightness data. In addition, we can match other data taken at other times and wavelengths. By slowing the propagation speed dramatically, we can match the observations from 2001–2004. Such slowing could be due to a small change in volatile content in the lava.},
	language = {en},
	number = {17},
	urldate = {2020-06-04},
	journal = {Geophysical Research Letters},
	author = {Rathbun, J. A. and Spencer, J. R.},
	year = {2006},
	note = {\_eprint: https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2006GL026844},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/FFDGLFVZ/Rathbun and Spencer - 2006 - Loki, Io New ground-based observations and a mode.pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/EQJVTNJH/2006GL026844.html:text/html}
}

@article{rathbun2002,
	title = {Loki, {Io}: {A} periodic volcano},
	volume = {29},
	issn = {0094-8276},
	shorttitle = {Loki, {Io}},
	url = {http://adsabs.harvard.edu/abs/2002GeoRL..29.1443R},
	doi = {10.1029/2002GL014747},
	abstract = {Not Available},
	urldate = {2020-06-04},
	journal = {Geophysical Research Letters},
	author = {Rathbun, J. A. and Spencer, J. R. and Davies, A. G. and Howell, R. R. and Wilson, L.},
	month = may,
	year = {2002},
	keywords = {Planetary Sciences: Heat flow, Planetary Sciences: Remote sensing, Planetary Sciences: Volcanism (8450), Planetology: Solar System Objects: Jovian satellites, Volcanology: Eruption mechanisms},
	pages = {1443}
}

@misc{zotero-3320,
	title = {Loki, {Io}: {New} ground‐based observations and a model describing the change from periodic overturn - {Rathbun} - 2006 - {Geophysical} {Research} {Letters} - {Wiley} {Online} {Library}},
	url = {https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2006GL026844},
	urldate = {2020-06-04},
	file = {Loki, Io\: New ground‐based observations and a model describing the change from periodic overturn - Rathbun - 2006 - Geophysical Research Letters - Wiley Online Library:/Users/fb90/Zotero/storage/ZIL2BEGQ/2006GL026844.html:text/html}
}

@article{depater2004,
	title = {Keck {AO} observations of {Io} in and out of eclipse},
	volume = {169},
	issn = {0019-1035},
	url = {http://adsabs.harvard.edu/abs/2004Icar..169..250D},
	doi = {10.1016/j.icarus.2003.08.025},
	abstract = {We present adaptive optics (AO) observations of Io taken with the W.M. Keck II telescope on 18 December 2001 (UT) before the satellite went into eclipse, and while it was in Jupiter's shadow. Making these kind of Io-in-eclipse observations, as well as the associated data reduction and analysis are challenging; hence one focus of the paper is to explain the methods and tools used for these data sets. For the sunlit images Io itself was used as the wavefront reference source, while nearby Ganymede was used as reference 'star' when Io was in eclipse. Observations were obtained in K'-, L'-, and M-bands. The sunlit images have been
deconvolved using MISTRAL. The Io-in-eclipse data were deconvolved with IDAC and MISTRAL. The former gives better results, both in absolute photometry and in matching the original images. We determined the flux densities of the hot spots from the original Io-in-eclipse data with StarFinder, as well as from the deconvolved images by integrating the intensity over the relevant areas. We determined the highly
anisoplanatic PSF via a FFT method from the original data, and used this in StarFinder and as a starting PSF for IDAC and MISTRAL. We derived temperatures and areal coverage of all 19 spots detected in both K'- and L'-band images of Io-in-eclipse. We also determined temperatures and areal coverage of the hot spots visible on the L'- and M-band images of sunlit Io. Most volcanoes contain a compact hot 'core' (≲10 km
2 at 600-800 K) within a larger area at lower temperatures (e.g., ∼10 2-10 4 km 2 at 300-500 K). The total heat flow contributed by these active volcanoes is 0.2 W m -2, ∼8\% of the average global heat flow measured at 5-20 μm by Veeder et al. [J. Geophys. Res. 99 (1994) 17095].},
	urldate = {2020-06-04},
	journal = {Icarus},
	author = {de Pater, Imke and Marchis, Franck and Macintosh, Bruce A. and Roe, Henry G. and Le Mignant, David and Graham, James R. and Davies, Ashley G.},
	month = may,
	year = {2004},
	keywords = {Io, Adaptive optics, Eclipse, PSF},
	pages = {250--263}
}

@article{howell1985,
	title = {Infrared speckle observations of {Io} - an eruption in the {Loki} region},
	volume = {230},
	issn = {0036-8075},
	url = {http://adsabs.harvard.edu/abs/1985Sci...230...63H},
	doi = {10.1126/science.230.4721.63},
	abstract = {Speckle observations of Jupiter's satellite Io at a wavelength of 5 micrometers during July 1984 resolved the disk and showed emission from a hot spot in the Loki region. The hot spot contributed a flux
approximately equal to 60 percent of that from the disk. Images
reconstructed by means of the Knox-Thompson algorithm showed the spot moving across the disk as the satellite rotated. It was located at 301 deg + or - 6 deg west longitude, 10 deg + or - 6 deg north latitude, and had a radiance of (2.96 + or - 0.54) x 10 to the 22nd ergs/sec cm sr/A where A is the area of the spot. For an assumed temperature of 400 K, the area of the source would be 11,400 square kilometers. An active 'lava lake' similar to that seen by Voyager may be the source of the infrared emission.},
	urldate = {2020-06-04},
	journal = {Science},
	author = {Howell, R. R. and McGinn, M. T.},
	month = oct,
	year = {1985},
	keywords = {Io, IO, JUPITER, SATELLITES, THERMAL PROPERTIES, VOLCANISM, Algorithms, EMISSIONS, ERUPTIONS, FEATURES, FLUX, HOT SPOTS, IMAGE PROCESSING, Image Reconstruction, IMAGERY, INFRARED, Infrared Interferometers, LOKI REGION, OBSERVATIONS, RADIANCE, ROTATION, SIZE, SOURCE, SPECKLE METHODS, Speckle Patterns, SURFACE, TEMPERATURE, Temperature Distribution, Volcanoes, WAVELENGTHS},
	pages = {63--65}
}

@article{simonelli1986,
	title = {Disk-resolved photometry of {Io}. {I} - {Near}-opposition limb darkening},
	volume = {66},
	issn = {0019-1035},
	url = {http://adsabs.harvard.edu/abs/1986Icar...66..403S},
	doi = {10.1016/0019-1035(86)90083-7},
	abstract = {For conducting a comparison of Voyager photometric measurements of individual areas on the Jovian satellite Io to laboratory data, it is necessary to reduce the two sets of information to a comparable format. In this connection, more accurate normal reflectance spectra for regions on Io are derived by means of a two-step process. The near-opposition limb-darkening characteristics are obtained for areas on the surface of Io. The new limb-darkening results are employed to determine the near-opposition phase behavior of selected regions on the satellite, taking into account also the effects of the opposition surge. A
combination of the phase and limb-darkening data makes it possible to obtain improved normal reflectance spectra for regions on Io. These spectra can be readily compared with laboratory spectra of candidate materials.},
	urldate = {2020-06-04},
	journal = {Icarus},
	author = {Simonelli, D. P. and Veverka, J.},
	month = jun,
	year = {1986},
	keywords = {Io, Voyager Project, Astronomical Photometry, Image Processing, Limb Darkening},
	pages = {403--454}
}

@article{spencer1997,
	title = {A history of high-temperature {Io} volcanism: {February} 1995 to {May} 1997},
	volume = {24},
	issn = {1944-8007},
	shorttitle = {A history of high-temperature {Io} volcanism},
	url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/97GL02591},
	doi = {10.1029/97GL02591},
	abstract = {Ground-based observations of Io's infrared thermal emission between February 1995 and May 1997 show several discrete brightenings for which we can constrain locations, fluxes, and durations. Several of these were brief high-temperature events, with temperatures up to at least 1500 K, similar to but often smaller than the rare “outbursts” seen previously. Loki, Io's most powerful volcano, was relatively active before and probably during Galileo's December 1995 Io flyby, was faint during most of 1996, and began a major, long-lived brightening between February 20 and March 12 1997. Thermal emission was not seen from Ra Patera, site of an active plume in Galileo images. Major outbursts were seen on March 2nd and September 27 1995.},
	language = {en},
	number = {20},
	urldate = {2020-06-04},
	journal = {Geophysical Research Letters},
	author = {Spencer, John R. and Stansberry, John A. and Dumas, Christophe and Vakil, David and Pregler, Randy and Hicks, Michael and Hege, Keith},
	year = {1997},
	note = {\_eprint: https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/97GL02591},
	pages = {2451--2454},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/ZHZ55DVJ/Spencer et al. - 1997 - A history of high-temperature Io volcanism Februa.pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/43TVHMHL/97GL02591.html:text/html}
}

@article{depater2017,
	title = {Three decades of {Loki} {Patera} observations},
	volume = {297},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103516307801},
	doi = {10.1016/j.icarus.2017.03.016},
	abstract = {We present observations of Io’s Loki Patera taken with the 10-m Keck telescopes between 1998 and 2016. Adding these data to those published by Rathbun and Spencer (2006) and the Gemini data of de Kleer and de Pater (2016a, 2017) results in a database of 3.5–3.8 μm emission from Loki Patera over almost 3 decades. Data presented here contain adaptive optics (AO) observations of Io’s sunlit hemisphere at wavelengths between 1.6 and 5 μm, AO observations of Io in eclipse at 2–5 μm, and non-AO observations of Io in eclipse at 1.6–12 μm. The non-AO data were taken in September of 1999, during the early phase of a brightening event that was documented by Howell et al. (2001). Dual-component Io Flow model (IFM) ﬁts to our 1999 observations show a mostly cool lava crust over almost the entire patera ﬂoor, with a relatively small hotter component making up less than 1\% of the total area, consistent with previous observations. The 30-year timeline of Loki Patera revealed that, after an apparent cessation of, or change in, brightening events in 2002, Loki Patera became active again in 2009. The more recent activity may have a slightly shorter periodicity than observed by Rathbun et al. (2002), and the direction of ﬂow propagation appears to have reversed. Since 2009 the ﬂow direction is in the clockwise direction, starting in the north or north-east corner and propagating along the patera towards the south-west. During the Galileo era the propagation was in the counter-clockwise direction, starting in the south-west and propagating towards the east. Both the 30-year timeline and the 1.6–12 μm spectrum that was obtained during the brightening event in 1999 agree well with Matson et al.’s (2006) overturning lava lake model, as modiﬁed by de Kleer and de Pater (2017).},
	language = {en},
	urldate = {2020-06-04},
	journal = {Icarus},
	author = {de Pater, Imke and de Kleer, Katherine and Davies, Ashley G. and Ádámkovics, Máté},
	month = nov,
	year = {2017},
	pages = {265--281},
	file = {de Pater et al. - 2017 - Three decades of Loki Patera observations.pdf:/Users/fb90/Zotero/storage/WVLVW7HJ/de Pater et al. - 2017 - Three decades of Loki Patera observations.pdf:application/pdf}
}

@article{veeder1994a,
	title = {Io's {Heat} {Flow} {From} {Infrared} {Radiometry}: 1983-1993},
	shorttitle = {Io's {Heat} {Flow} {From} {Infrared} {Radiometry}},
	url = {https://trs.jpl.nasa.gov/handle/2014/33536},
	abstract = {This paper presents results from a decade of infrared radiometry of IO. Results indicated that a new thermophysical model is required to match all the data. The thermal anomalies are modeled with a total of 10 source components at five locations.},
	language = {en\_US},
	urldate = {2020-06-04},
	author = {Veeder, G. and Matson, D. and Johnson, T. and Blaney, D. and Goguen, J.},
	year = {1994},
	note = {Accepted: 2004-10-05T06:23:33Z},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/N9FP6XYR/Veeder et al. - 1994 - Io's Heat Flow From Infrared Radiometry 1983-1993.pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/5QIQYFNS/33536.html:text/html}
}

@article{marchis2000,
	title = {Adaptive {Optics} {Mapping} of {Io}'s {Volcanism} in the {Thermal} {IR} (3.8 μm)},
	volume = {148},
	issn = {0019-1035},
	url = {http://adsabs.harvard.edu/abs/2000Icar..148..384M},
	doi = {10.1006/icar.2000.6506},
	abstract = {Two opposite hemispheres of Io were observed on October 20 and 21, 1996, through an L' broadband filter, using the high-resolution capability of the Adaptive Optics (AO) system implemented on the ESO 3.6-m telescope at La Silla, Chile. These observations, performed at thermal wavelengths when Io is in daylight, have been carefully processed to improve the sharpness of the initial, diffraction-limited, images. The myopic deconvolution process used ( idac) achieved an angular resolution estimated to be 0.15 arcsec, corresponding to a spatial resolution of ∼570 km on Io's disc at the time of the observations. The final
images show a number of bright features which have been compared with the Galileo/NIMS data, the only data set with a comparable resolution available for the anti-Jovian side of the satellite as well as its Jupiter-facing side. Our maps of the hot spot distribution are quite consistent with the Galileo data. The Jupiter-facing side is dominated by emission from Loki, which accounts for ∼25\% of the total hot spot emission from that side (and 45\% of that we were able to resolve and identify), although Loki was in a phase of decreasing activity (but not yet quiescent), as derived from ground-based monitoring observations. A few more hot sources are detected, including Pele-Pillan. The other hemisphere is characterized by a large number of moderately bright hot spots which are distributed around Bosphorus Regio. These preliminary observations fully demonstrate the capabilities of an AO system coupled with a thermal camera to monitor the volcanic activity of Io, in terms of morphology as well as thermal output. These monitoring capabilities will become especially important when the Galileo mission ends.},
	urldate = {2020-06-04},
	journal = {Icarus},
	author = {Marchis, Franck and Prangé, Renée and Christou, Julian},
	month = dec,
	year = {2000},
	pages = {384--396}
}

@article{marchis2001,
	title = {A survey of {Io}'s vocanism by adaptive optics observations in the 3.8-μm thermal band (1996-1999)},
	volume = {106},
	issn = {0148-0227},
	url = {http://adsabs.harvard.edu/abs/2001JGR...10633141M},
	doi = {10.1029/2000JE001376},
	abstract = {In this study, we analyze a series of images of Io obtained with the
European Southern Observatory adaptive optics system (Adaptive Optics
Near Infrared System, ADONIS) at 3.8 μm from 1996 to 1999, with
particular emphasis on the observations carried out in late 1999 in
support of the Galileo flybys of Io. Use of a new myopic deconvolution
method, Myopic Iterative Step Preserving Algorithm (MISTRAL), especially
designed for planetary objects, significantly improves the quality and
the reliability of the reconstructed images. Using a simulation of
artificial images of Io, we estimate the extent to which this algorithm
is able to prevent noise amplification, to better restore sharp edges,
and to preserve the initial photometry. Once this algorithm has been
applied to our data and the solar-reflected background has been
subtracted, we have 89 images of Io available for search and temporal
survey of the hot spots over 4 years. In most cases, the data, acquired
during two consecutive nights, provide an almost global view of the
surface of Io. We identify 20 hot spots for which we determine the
coordinates and the brightness at 3.8 μm (as a function of time).
More than half of the hot spots were detected on all the images and were
considered as persistent. Particular emphasis has been put on the
brightest two hot spots, Loki and Pele, for which we obtain a
center-to-limb variation curve (a cosine curve for Loki and a curve
decreasing slightly faster than a cosine law for Pele with possible
physical interpretations). The temporal variations of their activity
have been derived over these 4 years and, for Loki, compared with the
results of other ground-based surveys. The variability of the other,
fainter, sources has also been derived but with less accuracy. We have
also identified a few new hot spots, some of which are transient, such
as a diffuse emission seen in September and November 1999 at the
location of the upcoming Tvashtar outburst. The data are based on
observations (58.F-1003, 63.S-0260, and 64.S-0661) collected at the
European Southern Observatory in La Silla, Chile.},
	urldate = {2020-06-04},
	journal = {Journal of Geophysical Research},
	author = {Marchis, Franck and Prangé, Renée and Fusco, Thierry},
	month = dec,
	year = {2001},
	keywords = {Planetology: Solar System Objects: Jovian satellites, Planetology: Solid Surface Planets: Remote sensing, Planetology: Solid Surface Planets: Volcanism, Volcanology: Lava rheology and morphology},
	pages = {33141--33160}
}

@article{mura2020,
	title = {Infrared observations of {Io} from {Juno}},
	volume = {341},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103519304427},
	doi = {10.1016/j.icarus.2019.113607},
	abstract = {The Jovian InfraRed Auroral Mapper (JIRAM) on board the NASA Juno spacecraft is a dual-band imager and spectrometer, primarily designed to study the Jovian atmosphere and aurorae. In addition to its primary goal, JIRAM has been used to obtain images and spectra of the Galilean satellites, Jupiter's largest moons, when the spacecraft attitude was favourable to achieve this goal. Here we present JIRAM’s first images and spectra of Io. These observations are used to characterize the location and possible morphology, and some temperatures, of Io’s volcanic thermal sources; the identification of SO2 and the possible identification of other materials. A new hot spot/volcano is identified close to the South Pole of Io, and others are seen in lower latitude regions, which were previously unmapped. Images of the same region taken 2 months apart also show variations of hot spot intensity, possibly due to new lava flows or to lava flow breakouts.},
	language = {en},
	urldate = {2020-06-04},
	journal = {Icarus},
	author = {Mura, A. and Adriani, A. and Tosi, F. and Lopes, R.M.C. and Sindoni, G. and Filacchione, G. and Williams, D.A. and Davies, A.G. and Plainaki, C. and Bolton, S. and Altieri, F. and Cicchetti, A. and Grassi, D. and Migliorini, A. and Moriconi, M.L. and Noschese, R. and Olivieri, A. and Piccioni, G. and Sordini, R.},
	month = may,
	year = {2020},
	pages = {113607},
	file = {Mura et al. - 2020 - Infrared observations of Io from Juno.pdf:/Users/fb90/Zotero/storage/9VB4EXS9/Mura et al. - 2020 - Infrared observations of Io from Juno.pdf:application/pdf}
}

@article{belton1996,
	title = {Galileo's {First} {Images} of {Jupiter} and the {Galilean} {Satellites}},
	volume = {274},
	issn = {0036-8075},
	url = {http://adsabs.harvard.edu/abs/1996Sci...274..377B},
	doi = {10.1126/science.274.5286.377},
	abstract = {The first images of Jupiter, Io, Europa, and Ganymede from the Galileo spacecraft reveal new information about Jupiter's Great Red Spot (GRS) and the surfaces of the Galilean satellites. Features similar to clusters of thunderstorms were found in the GRS. Nearby wave structures suggest that the GRS may be a shallow atmospheric feature. Changes in surface color and plume distribution indicate differences in resurfacing processes near hot spots on Io. Patchy emissions were seen while Io was in eclipse by Jupiter. The outer margins of prominent linear markings (triple bands) on Europa are diffuse, suggesting that material has been vented from fractures. Numerous small circular craters indicate
localized areas of relatively old surface. Pervasive brittle deformation of an ice layer appears to have formed grooves on Ganymede. Dark terrain unexpectedly shows distinctive albedo variations to the limit of resolution.},
	urldate = {2020-06-04},
	journal = {Science},
	author = {Belton, M. J. S. and Head, III, J. W. and Ingersoll, A. P. and Greeley, R. and McEwen, A. S. and Klaasen, K. P. and Senske, D. and Pappalardo, R. and Collins, G. and Vasavada, A. R. and Sullivan, R. and Simonelli, D. and Geissler, P. and Carr, M. H. and Davies, M. E. and Veverka, J. and Gierasch, P. J. and Banfield, D. and Bell, M. and Chapman, C. R. and Anger, C. and Greenberg, R. and Neukum, G. and Pilcher, C. B. and Beebe, R. F. and Burns, J. A. and Fanale, F. and Ip, W. and Johnson, T. V. and Morrison, D. and Moore, J. and Orton, G. S. and Thomas, P. and West, R. A.},
	month = oct,
	year = {1996},
	pages = {377--385}
}

@article{smith1979,
	title = {The {Jupiter} system through the eyes of {Voyager} 1},
	volume = {204},
	issn = {0036-8075},
	url = {http://adsabs.harvard.edu/abs/1979Sci...204..951S},
	doi = {10.1126/science.204.4396.951},
	abstract = {The cameras aboard Voyager 1 have provided a closeup view of the Jupiter system, revealing heretofore unknown characteristics and phenomena associated with the planet's atmosphere and the surfaces of its five major satellites. On Jupiter itself, atmospheric motions - the
interaction of cloud systems - display complex vorticity. On its dark side, lightening and auroras are observed. A ring was discovered surrounding Jupiter. The satellite surfaces display dramatic differences including extensive active volcanism on Io, complex tectonism on Ganymede and possibly Europa, and flattened remnants of enormous impact features on Callisto.},
	urldate = {2020-06-04},
	journal = {Science},
	author = {Smith, Bradford A. and Soderblom, Laurence A. and Johnson, Torrence V. and Ingersoll, Andrew P. and Collins, Stewart A. and Shoemaker, Eugene M. and Hunt, G. E. and Masursky, Harold and Carr, Michael H. and Davies, Merton E. and Cook, II, Allan F. and Boyce, Joseph and Danielson, G. Edward and Owen, Tobias and Sagan, Carl and Beebe, Reta F. and Veverka, Joseph and Strom, Robert G. and McCauley, John F. and Morrison, David and Briggs, Geoffrey A. and Suomi, Verner E.},
	month = jun,
	year = {1979},
	keywords = {Galilean Satellites, IO, JUPITER, SATELLITES, VOLCANISM, VOYAGER 1, Voyager Project, Amalthea, Jupiter (Planet), OBSERVATIONS, SURFACE, Volcanoes, AMALTHEA, ATMOSPHERE, CALLISTO, Cameras, Color, Craters, CRATERS, DIASTROPHISM, EUROPA, FLATTENING, GENYMEDE, Global Atmospheric Research Program, GREAT RED SPOT, Imaging Techniques, Jupiter Atmosphere, MORPHOLOGY, Planetary Rotation, Planetary Structure, Planetary Surfaces, RINGS, Time Response, Vertical Motion, Vortices},
	pages = {951--957}
}

@article{howell2001,
	title = {Ground-based observations of volcanism on {Io} in 1999 and early 2000},
	volume = {106},
	issn = {0148-0227},
	url = {http://adsabs.harvard.edu/abs/2001JGR...10633129H},
	doi = {10.1029/2000JE001382},
	abstract = {Ground-based observations of volcanism on Io during the period of the 1999 and early 2000 Galileo close flybys have detected several types of activity, providing information which complements the spacecraft observations. At Loki a brightening began between August 25 and
September 9 and continued through February. On August 2 a major outburst was observed near (14°N, 74°W) whose brightness corresponds to
an area of approximately 350 km2 at a temperature of 1100 K. Observations of eruptions in late June (9906A) and in late November (9911A, at Tvashtar) provide temporal and photometric constraints on activity also seen by Galileo. High-resolution adaptive optics images provide further information on the fainter sources distributed across the surface.},
	urldate = {2020-06-03},
	journal = {Journal of Geophysical Research},
	author = {Howell, Robert R. and Spencer, John R. and Goguen, Jay D. and Marchis, Franck and Prangé, Renée and Fusco, Thierry and Blaney, Diana L. and Veeder, Glenn J. and Rathbun, Julie A. and Orton, Glenn S. and Grocholski, Aaron J. and Stansberry, John A. and Kanner, Gary S. and Hege, E. Keith},
	month = dec,
	year = {2001},
	keywords = {Planetology: Solar System Objects: Jovian satellites, Planetology: Solid Surface Planets: Remote sensing, Planetology: Solid Surface Planets: Volcanism, Planetology: Solid Surface Planets: Interactions with particles and fields},
	pages = {33129--33140}
}

@article{luger2019a,
	title = {starry: {Analytic} {Occultation} {Light} {Curves}},
	volume = {157},
	issn = {0004-6256},
	shorttitle = {starry},
	url = {http://adsabs.harvard.edu/abs/2019AJ....157...64L},
	doi = {10.3847/1538-3881/aae8e5},
	abstract = {We derive analytic, closed form, numerically stable solutions for the total flux received from a spherical planet, moon, or star during an occultation if the specific intensity map of the body is expressed as a sum of spherical harmonics. Our expressions are valid to arbitrary degree and may be computed recursively for speed. The formalism we develop here applies to the computation of stellar transit light curves, planetary secondary eclipse light curves, and
planet-planet/planet-moon occultation light curves, as well
as thermal (rotational) phase curves. In this paper, we also introduce starry, an open-source package written in C++ and wrapped in Python that computes these light curves. The algorithm in starry is six orders of magnitude faster than direct numerical integration and several orders of magnitude more precise. starry also computes analytic derivatives of the light curves with respect to all input parameters for use in
gradient-based optimization and inference, such as Hamiltonian Monte Carlo (HMC), allowing users to quickly and efficiently fit observed light curves to infer properties of a celestial body’s surface
map. (Please see https://github.com/rodluger/starry,
https://rodluger.github.io/starry/,
and https://doi.org/10.5281/zenodo.1312286).},
	urldate = {2020-06-03},
	journal = {The Astronomical Journal},
	author = {Luger, Rodrigo and Agol, Eric and Foreman-Mackey, Daniel and Fleming, David P. and Lustig-Yaeger, Jacob and Deitrick, Russell},
	month = feb,
	year = {2019},
	keywords = {eclipses, occultations, techniques: photometric, methods: analytical},
	pages = {64},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/KVUC7CUU/Luger et al. - 2019 - starry Analytic Occultation Light Curves.pdf:application/pdf}
}

@article{rathbun2010,
	title = {Ground-based observations of time variability in multiple active volcanoes on {Io}},
	volume = {209},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103510002113},
	doi = {10.1016/j.icarus.2010.05.019},
	abstract = {Since before the beginning of the Galileo spacecraft’s Jupiter orbital tour, we have observed Io from the ground using NASA’s Infrared Telescope Facility (IRTF). We obtained images of Io in reﬂected sunlight and in-eclipse at 2.3, 3.5, and 4.8 lm. In addition, we have measured the 3.5 lm brightness of an eclipsed Io as it is occulted by Jupiter. These lightcurves enable us to measure the brightness and one-dimensional location of active volcanoes on the surface. During the Galileo era, two volcanoes were observed to be regularly active: Loki and either Kanehekili and/or Janus. At least 12 other active volcanoes were observed for shorter periods of time, including one distinguishable in images that include reﬂected sunlight. These data can be used to compare volcano types and test volcano eruption models, such as the lava lake model for Loki.},
	language = {en},
	number = {2},
	urldate = {2020-06-03},
	journal = {Icarus},
	author = {Rathbun, Julie A. and Spencer, John R.},
	month = oct,
	year = {2010},
	pages = {625--630},
	file = {Rathbun and Spencer - 2010 - Ground-based observations of time variability in m.pdf:/Users/fb90/Zotero/storage/E3HEFYL5/Rathbun and Spencer - 2010 - Ground-based observations of time variability in m.pdf:application/pdf}
}

@incollection{asteris2015,
	title = {Orthogonal {NMF} through {Subspace} {Exploration}},
	url = {http://papers.nips.cc/paper/5998-orthogonal-nmf-through-subspace-exploration.pdf},
	urldate = {2020-05-31},
	booktitle = {Advances in {Neural} {Information} {Processing} {Systems} 28},
	publisher = {Curran Associates, Inc.},
	author = {Asteris, Megasthenis and Papailiopoulos, Dimitris and Dimakis, Alexandros G},
	editor = {Cortes, C. and Lawrence, N. D. and Lee, D. D. and Sugiyama, M. and Garnett, R.},
	year = {2015},
	pages = {343--351},
	file = {NIPS Full Text PDF:/Users/fb90/Zotero/storage/SBYDXWCF/Asteris et al. - 2015 - Orthogonal NMF through Subspace Exploration.pdf:application/pdf;NIPS Snapshot:/Users/fb90/Zotero/storage/P5GTTTIU/5998-orthogonal-nmf-through-subspace-exploration.html:text/html}
}

@article{yoo,
	title = {Nonnegative {Matrix} {Factorization} with {Orthogonality} {Constraints}},
	language = {en},
	author = {Yoo, Jiho and Choi, Seungjin},
	pages = {12},
	file = {Yoo and Choi - Nonnegative Matrix Factorization with Orthogonalit.pdf:/Users/fb90/Zotero/storage/WTFDR5DP/Yoo and Choi - Nonnegative Matrix Factorization with Orthogonalit.pdf:application/pdf}
}

@article{kumar2020,
	title = {On {The} {Geological} {Time} {Evolution} of {Volcanism} in the {Inner} {Solar} {System}},
	url = {http://arxiv.org/abs/2005.13200},
	abstract = {We have studied the geological time evolution of volcanism in Earth and other inner solar system planetary bodies (Mercury, Moon, Mars and Venus) in both geophysical and biophysical perspective. The record of Large Igneous Provinces in Earth and other planetary objects suggest the existence of increasing, decreasing and cessation phases of major volcanic activity over geological time scales. We have extended the existing scale of measuring intensity of volcanic eruptions based on Earth based observations to accommodate intense and extreme volcanic activity. The mass of a rocky planetary object is found to be related to the magnitude of the internal heat, occurrences of Large Igneous Provinces and the duration of major volcanic activity from relevant data available for the inner solar system. The internal heat magnitude may also decide the intensity of volcanism in these planetary objects. The time evolution of volcanism in Earth and Mars has probably influenced the origin of life and biological evolution in these planets.},
	urldate = {2020-05-29},
	journal = {arXiv:2005.13200 [astro-ph]},
	author = {Kumar, Varnana M. and Girish, T. E. and Sathyan, Thara N. and Longhinos, Biju and Panicker, Anjana A. V. and Binoy, J.},
	month = may,
	year = {2020},
	note = {arXiv: 2005.13200},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 30 Pages and 15 Figures},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/UJYIFIL3/Kumar et al. - 2020 - On The Geological Time Evolution of Volcanism in t.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/N238DTRH/2005.html:text/html}
}

@article{yao2018a,
	title = {Yes, but {Did} {It} {Work}?: {Evaluating} {Variational} {Inference}},
	shorttitle = {Yes, but {Did} {It} {Work}?},
	url = {http://arxiv.org/abs/1802.02538},
	abstract = {While it's always possible to compute a variational approximation to a posterior distribution, it can be difficult to discover problems with this approximation. We propose two diagnostic algorithms to alleviate this problem. The Pareto-smoothed importance sampling (PSIS) diagnostic gives a goodness of fit measurement for joint distributions, while simultaneously improving the error in the estimate. The variational simulation-based calibration (VSBC) assesses the average performance of point estimates.},
	urldate = {2020-05-26},
	journal = {arXiv:1802.02538 [stat]},
	author = {Yao, Yuling and Vehtari, Aki and Simpson, Daniel and Gelman, Andrew},
	month = jul,
	year = {2018},
	note = {arXiv: 1802.02538},
	keywords = {Statistics - Computation, Statistics - Machine Learning},
	annote = {Comment: Appearing at International Conference on Machine Learning 2018},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/E8QT63QU/Yao et al. - 2018 - Yes, but Did It Work Evaluating Variational Infe.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/4T2U8PBI/1802.html:text/html}
}

@article{moolekamp2018,
	title = {Block-simultaneous direction method of multipliers: a proximal primal-dual splitting algorithm for nonconvex problems with multiple constraints},
	volume = {19},
	issn = {1389-4420, 1573-2924},
	shorttitle = {Block-simultaneous direction method of multipliers},
	url = {http://link.springer.com/10.1007/s11081-018-9380-y},
	doi = {10.1007/s11081-018-9380-y},
	abstract = {We introduce a generalization of the linearized Alternating Direction Method of Multipliers to optimize a real-valued function f of multiple arguments with potentially multiple constraints g  on each of them. The function f may be nonconvex as long as it is convex in every argument, while the constraints g  need to be convex but not smooth. If f is smooth, the proposed Block-Simultaneous Direction Method of Multipliers (bSDMM) can be interpreted as a proximal analog to inexact coordinate descent methods under constraints. Unlike alternative approaches for joint solvers of multiple-constraint problems, we do not require linear operators L of a constraint function gðL ÁÞ to be invertible or linked between each other. bSDMM is well-suited for a range of optimization problems, in particular for data analysis, where f is the likelihood function of a model and L could be a transformation matrix describing e.g. ﬁnite differences or basis transforms. We apply bSDMM to the Non-negative Matrix Factorization task of a hyperspectral unmixing problem and demonstrate convergence and effectiveness of multiple constraints on both matrix factors. The algorithms are implemented in python and released as an open-source package.},
	language = {en},
	number = {4},
	urldate = {2020-05-26},
	journal = {Optim Eng},
	author = {Moolekamp, Fred and Melchior, Peter},
	month = dec,
	year = {2018},
	pages = {871--885},
	file = {Moolekamp and Melchior - 2018 - Block-simultaneous direction method of multipliers.pdf:/Users/fb90/Zotero/storage/KPEZ27UN/Moolekamp and Melchior - 2018 - Block-simultaneous direction method of multipliers.pdf:application/pdf}
}

@article{yao,
	title = {Yes, but {Did} {It} {Work}?: {Evaluating} {Variational} {Inference}},
	abstract = {While it’s always possible to compute a variational approximation to a posterior distribution, it can be difﬁcult to discover problems with this approximation. We propose two diagnostic algorithms to alleviate this problem. The Paretosmoothed importance sampling (PSIS) diagnostic gives a goodness of ﬁt measurement for joint distributions, while simultaneously improving the error in the estimate. The variational simulationbased calibration (VSBC) assesses the average performance of point estimates.},
	language = {en},
	author = {Yao, Yuling and Vehtari, Aki and Simpson, Daniel and Gelman, Andrew},
	pages = {16},
	file = {Yao et al. - Yes, but Did It Work Evaluating Variational Infe.pdf:/Users/fb90/Zotero/storage/ATWS9UUT/Yao et al. - Yes, but Did It Work Evaluating Variational Infe.pdf:application/pdf}
}

@incollection{mnih2008,
	title = {Probabilistic {Matrix} {Factorization}},
	url = {http://papers.nips.cc/paper/3208-probabilistic-matrix-factorization.pdf},
	urldate = {2020-05-19},
	booktitle = {Advances in {Neural} {Information} {Processing} {Systems} 20},
	publisher = {Curran Associates, Inc.},
	author = {Mnih, Andriy and Salakhutdinov, Russ R},
	editor = {Platt, J. C. and Koller, D. and Singer, Y. and Roweis, S. T.},
	year = {2008},
	pages = {1257--1264},
	file = {NIPS Full Text PDF:/Users/fb90/Zotero/storage/I6UQ5QIC/Mnih and Salakhutdinov - 2008 - Probabilistic Matrix Factorization.pdf:application/pdf;NIPS Snapshot:/Users/fb90/Zotero/storage/FHBGJ2SA/3208-probabilistic-matrix-factorization.html:text/html}
}

@article{babacan2009,
	title = {Variational {Bayesian} {Blind} {Deconvolution} {Using} a {Total} {Variation} {Prior}},
	volume = {18},
	issn = {1057-7149, 1941-0042},
	url = {http://ieeexplore.ieee.org/document/4689325/},
	doi = {10.1109/TIP.2008.2007354},
	abstract = {In this paper, we present novel algorithms for total variation (TV) based blind deconvolution and parameter estimation utilizing a variational framework. Using a hierarchical Bayesian model, the unknown image, blur, and hyperparameters for the image, blur, and noise priors are estimated simultaneously. A variational inference approach is utilized so that approximations of the posterior distributions of the unknowns are obtained, thus providing a measure of the uncertainty of the estimates. Experimental results demonstrate that the proposed approaches provide higher restoration performance than non-TV-based methods without any assumptions about the unknown hyperparameters.},
	language = {en},
	number = {1},
	urldate = {2020-05-18},
	journal = {IEEE Trans. on Image Process.},
	author = {Babacan, S.D. and Molina, R. and Katsaggelos, A.K.},
	month = jan,
	year = {2009},
	pages = {12--26},
	file = {Babacan et al. - 2009 - Variational Bayesian Blind Deconvolution Using a T.pdf:/Users/fb90/Zotero/storage/6PUX4GNM/Babacan et al. - 2009 - Variational Bayesian Blind Deconvolution Using a T.pdf:application/pdf}
}

@article{melchior2018,
	title = {{SCARLET}: {Source} separation in multi-band images by {Constrained} {Matrix} {Factorization}},
	volume = {24},
	issn = {22131337},
	shorttitle = {{SCARLET}},
	url = {http://arxiv.org/abs/1802.10157},
	doi = {10.1016/j.ascom.2018.07.001},
	abstract = {We present the source separation framework SCARLET for multi-band images, which is based on a generalization of the Non-negative Matrix Factorization to alternative and several simultaneous constraints. Our approach describes the observed scene as a mixture of components with compact spatial support and uniform spectra over their support. We present the algorithm to perform the matrix factorization and introduce constraints that are useful for optical images of stars and distinct stellar populations in galaxies, in particular symmetry and monotonicity with respect to the source peak position. We also derive the treatment of correlated noise and convolutions with band-dependent point spread functions, rendering our approach applicable to coadded images observed under variable seeing conditions. SCARLET thus yields a PSF-matched photometry measurement with an optimally chosen weight function given by the mean morphology in all available bands. We demonstrate the performance of SCARLET for deblending crowded extragalactic scenes and on an AGN jet -- host galaxy separation problem in deep 5-band imaging from the Hyper Suprime-Cam Stategic Survey Program. Using simulations with prominent crowding we show that SCARLET yields superior results to the HSC-SDSS deblender for the recovery of total fluxes, colors, and morphologies. Due to its non-parametric nature, a conceptual limitation of SCARLET is its sensitivity to undetected sources or multiple stellar population within detected sources, but an iterative strategy that adds components at the location of significant residuals appears promising. The code is implemented in Python with C++ extensions and is available at https://github.com/fred3m/scarlet},
	urldate = {2020-05-18},
	journal = {Astronomy and Computing},
	author = {Melchior, Peter and Moolekamp, Fred and Jerdee, Maximilian and Armstrong, Robert and Sun, Ai-Lei and Bosch, James and Lupton, Robert},
	month = jul,
	year = {2018},
	note = {arXiv: 1802.10157},
	keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
	pages = {129--142},
	annote = {Comment: accepted by Astronomy \& Computing},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/BWWT73TW/Melchior et al. - 2018 - SCARLET Source separation in multi-band images by.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/DTJJGJRK/1802.html:text/html}
}

@article{tichy2019,
	title = {Bayesian {Non}-{Negative} {Matrix} {Factorization} {With} {Adaptive} {Sparsity} and {Smoothness} {Prior}},
	volume = {26},
	issn = {1070-9908, 1558-2361},
	url = {https://ieeexplore.ieee.org/document/8633424/},
	doi = {10.1109/LSP.2019.2897230},
	number = {3},
	urldate = {2020-05-18},
	journal = {IEEE Signal Process. Lett.},
	author = {Tichy, Ondrej and Bodiova, Lenka and Smidl, Vaclav},
	month = mar,
	year = {2019},
	pages = {510--514}
}

@article{kawahara2020a,
	title = {Global {Mapping} of the {Surface} {Composition} on an {Exo}-{Earth} {Using} {Color} {Variability}},
	volume = {894},
	issn = {1538-4357},
	url = {https://iopscience.iop.org/article/10.3847/1538-4357/ab87a1},
	doi = {10.3847/1538-4357/ab87a1},
	number = {1},
	urldate = {2020-05-17},
	journal = {ApJ},
	author = {Kawahara, Hajime},
	month = may,
	year = {2020},
	pages = {58},
	file = {Submitted Version:/Users/fb90/Zotero/storage/ZMMK3XT3/Kawahara - 2020 - Global Mapping of the Surface Composition on an Ex.pdf:application/pdf}
}

@article{bertin,
	title = {Enforcing {Harmonicity} and {Smoothness} in {Bayesian} {Non}-negative {Matrix} {Factorization} {Applied} to {Polyphonic} {Music} {Transcription}.},
	abstract = {This article presents theoretical and experimental results about constrained non-negative matrix factorization (NMF) in a Bayesian framework. A model of superimposed Gaussian components including harmonicity is proposed, while temporal continuity is enforced through an inverse-Gamma Markov chain prior. We then exhibit a space-alternating generalized expectation-maximization (SAGE) algorithm to estimate the parameters. Computational time is reduced by initializing the system with an original variant of multiplicative harmonic NMF, which is described as well. The algorithm is then applied to perform polyphonic piano music transcription. It is compared to other state-of-the-art algorithms, especially NMF-based. Convergence issues are also discussed on a theoretical and experimental point of view.},
	language = {en},
	author = {Bertin, Nancy and Badeau, Roland and Vincent, Emmanuel},
	pages = {11},
	file = {Bertin et al. - Enforcing Harmonicity and Smoothness in Bayesian N.pdf:/Users/fb90/Zotero/storage/DZKN9GL9/Bertin et al. - Enforcing Harmonicity and Smoothness in Bayesian N.pdf:application/pdf}
}

@article{pascual-montano2006,
	title = {Nonsmooth nonnegative matrix factorization ({nsNMF})},
	volume = {28},
	issn = {0162-8828},
	url = {http://ieeexplore.ieee.org/document/1580485/},
	doi = {10.1109/TPAMI.2006.60},
	number = {3},
	urldate = {2020-05-17},
	journal = {IEEE Trans. Pattern Anal. Machine Intell.},
	author = {Pascual-Montano, A. and Carazo, J.M. and Kochi, K. and Lehmann, D. and Pascual-Marqui, R.D.},
	month = mar,
	year = {2006},
	pages = {403--415}
}

@article{babacan2009a,
	title = {Variational {Bayesian} {Blind} {Deconvolution} {Using} a {Total} {Variation} {Prior}},
	volume = {18},
	issn = {1057-7149, 1941-0042},
	url = {http://ieeexplore.ieee.org/document/4689325/},
	doi = {10.1109/TIP.2008.2007354},
	abstract = {In this paper, we present novel algorithms for total variation (TV) based blind deconvolution and parameter estimation utilizing a variational framework. Using a hierarchical Bayesian model, the unknown image, blur, and hyperparameters for the image, blur, and noise priors are estimated simultaneously. A variational inference approach is utilized so that approximations of the posterior distributions of the unknowns are obtained, thus providing a measure of the uncertainty of the estimates. Experimental results demonstrate that the proposed approaches provide higher restoration performance than non-TV-based methods without any assumptions about the unknown hyperparameters.},
	language = {en},
	number = {1},
	urldate = {2020-05-16},
	journal = {IEEE Trans. on Image Process.},
	author = {Babacan, S.D. and Molina, R. and Katsaggelos, A.K.},
	month = jan,
	year = {2009},
	pages = {12--26},
	file = {Babacan et al. - 2009 - Variational Bayesian Blind Deconvolution Using a T.pdf:/Users/fb90/Zotero/storage/YVN29DTV/Babacan et al. - 2009 - Variational Bayesian Blind Deconvolution Using a T.pdf:application/pdf}
}

@article{chantas2010,
	title = {Variational {Bayesian} {Image} {Restoration} {With} a {Product} of {Spatially} {Weighted} {Total} {Variation} {Image} {Priors}},
	volume = {19},
	issn = {1057-7149, 1941-0042},
	url = {http://ieeexplore.ieee.org/document/5272318/},
	doi = {10.1109/TIP.2009.2033398},
	number = {2},
	urldate = {2020-05-16},
	journal = {IEEE Trans. on Image Process.},
	author = {Chantas, Giannis and Galatsanos, Nikolaos P. and Molina, Rafael and Katsaggelos, Aggelos K.},
	month = feb,
	year = {2010},
	pages = {351--362}
}

@article{lee2013,
	title = {Bayesian inversion with total variation prior for discrete geologic structure identification},
	volume = {49},
	issn = {1944-7973},
	url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1002/2012WR013431},
	doi = {10.1002/2012WR013431},
	abstract = {The characterization of geologic heterogeneity that affects flow and transport phenomena in the subsurface is essential for cost-effective and reliable decision-making in applications such as groundwater supply and contaminant cleanup. In the last decades, geostatistical inversion approaches have been widely used to tackle subsurface characterization problems and quantify their corresponding uncertainty. Some well-established geostatistical methods use models that assume gradually varying parameters. However, in many cases, the subsurface can often be better represented as consisting of a few relatively uniform geologic facies or zones with abrupt changes at their boundaries. We advance a Bayesian inversion approach with the gradient represented not through a Gaussian but a Laplace prior, also known as total variation prior, for the case that there are reasons to believe that discrete geologic structures with relatively homogeneous properties predominate in the subsurface but their number, locations, and shapes are unknown a priori. Structural parameters (or hyperparameters of the inversion scheme) are determined in a Bayesian framework by maximizing the marginal distribution of these parameters using an expectation-maximization approach; this allows proper weighting of prior versus data information and produces results with realistic uncertainty quantification. We present here three applications of the method: a time-varying extraction rate estimation at a well, a linear cross-well seismic tomography, and a nonlinear hydraulic tomography. These results are compared with those achieved in the classical geostatistical method and it is shown that the Bayesian inversion approach with total variation prior can be a useful tool to identify discrete geologic structures.},
	language = {en},
	number = {11},
	urldate = {2020-05-16},
	journal = {Water Resources Research},
	author = {Lee, J. and Kitanidis, P. K.},
	year = {2013},
	note = {\_eprint: https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2012WR013431},
	keywords = {compressed sensing, discrete geologic structure identification, facies detection, Laplace prior},
	pages = {7658--7669},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/MLFQEKAG/Lee and Kitanidis - 2013 - Bayesian inversion with total variation prior for .pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/KHL7VMCH/2012WR013431.html:text/html}
}

@article{fu2019,
	title = {Nonnegative {Matrix} {Factorization} for {Signal} and {Data} {Analytics}: {Identifiability}, {Algorithms}, and {Applications}},
	volume = {36},
	issn = {1053-5888, 1558-0792},
	shorttitle = {Nonnegative {Matrix} {Factorization} for {Signal} and {Data} {Analytics}},
	url = {http://arxiv.org/abs/1803.01257},
	doi = {10.1109/MSP.2018.2877582},
	abstract = {Nonnegative matrix factorization (NMF) has become a workhorse for signal and data analytics, triggered by its model parsimony and interpretability. Perhaps a bit surprisingly, the understanding to its model identifiability---the major reason behind the interpretability in many applications such as topic mining and hyperspectral imaging---had been rather limited until recent years. Beginning from the 2010s, the identifiability research of NMF has progressed considerably: Many interesting and important results have been discovered by the signal processing (SP) and machine learning (ML) communities. NMF identifiability has a great impact on many aspects in practice, such as ill-posed formulation avoidance and performance-guaranteed algorithm design. On the other hand, there is no tutorial paper that introduces NMF from an identifiability viewpoint. In this paper, we aim at filling this gap by offering a comprehensive and deep tutorial on model identifiability of NMF as well as the connections to algorithms and applications. This tutorial will help researchers and graduate students grasp the essence and insights of NMF, thereby avoiding typical `pitfalls' that are often times due to unidentifiable NMF formulations. This paper will also help practitioners pick/design suitable factorization tools for their own problems.},
	number = {2},
	urldate = {2020-05-14},
	journal = {IEEE Signal Process. Mag.},
	author = {Fu, Xiao and Huang, Kejun and Sidiropoulos, Nicholas D. and Ma, Wing-Kin},
	month = mar,
	year = {2019},
	note = {arXiv: 1803.01257},
	keywords = {Statistics - Machine Learning, Computer Science - Machine Learning, Electrical Engineering and Systems Science - Signal Processing},
	pages = {59--80},
	annote = {Comment: accepted version, IEEE Signal Processing Magazine; supplementary materials added. Some minor revisions implemented},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/L9PWL7KD/Fu et al. - 2019 - Nonnegative Matrix Factorization for Signal and Da.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/YTDPF4PU/1803.html:text/html}
}

@article{melchior2019,
	title = {Adaptive {Proximal} {Gradient} {Method} for {Constrained} {Matrix} {Factorization}},
	url = {http://arxiv.org/abs/1910.10094},
	abstract = {The Proximal Gradient Method (PGM) is a robust and efficient way to minimize the sum of a smooth convex function \$f\$ and a non-differentiable convex function \$r\$. It determines the sizes of gradient steps according to the Lipschitz constant of the gradient of \$f\$. For many problems in data analysis, the Lipschitz constants are expensive or impossible to compute analytically because they depend on details of the experimental setup and the noise properties of the data. Adaptive optimization methods like AdaGrad choose step sizes according to on-the-fly estimates of the Hessian of \$f\$. As quasi-Newton methods, they generally outperform first-order gradient methods like PGM and adjust step sizes iteratively and with low computational cost. We propose an iterative proximal quasi-Newton algorithm, AdaProx, that utilizes the adaptive schemes of Adam and its variants (AMSGrad, AdamX, PAdam) and works for arbitrary proxable penalty functions \$r\$. In test cases for Constrained Matrix Factorization we demonstrate the advantages of AdaProx in fidelity and performance over PGM, especially when factorization components are poorly balanced. The python implementation of the algorithm presented here is available as an open-source package at https://github.com/pmelchior/proxmin},
	urldate = {2020-05-11},
	journal = {arXiv:1910.10094 [astro-ph]},
	author = {Melchior, Peter and Joseph, Rémy and Moolekamp, Fred},
	month = oct,
	year = {2019},
	note = {arXiv: 1910.10094},
	keywords = {Astrophysics - Instrumentation and Methods for Astrophysics, Electrical Engineering and Systems Science - Image and Video Processing, Mathematics - Optimization and Control},
	annote = {Comment: 12 pages, 5 figures; submitted to Optimization \& Engineering},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/TLXEV26J/Melchior et al. - 2019 - Adaptive Proximal Gradient Method for Constrained .pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/V5QRGBRD/1910.html:text/html}
}

@article{paananen,
	title = {Implicitly {Adaptive} {Importance} {Sampling}},
	abstract = {Adaptive importance sampling is a class of techniques for ﬁnding good proposal distributions for importance sampling. Often the proposal distributions are standard probability distributions whose parameters are adapted based on the mismatch between the current proposal and a target distribution. In this work, we present an implicit adaptive importance sampling method that applies to complicated distributions which are not available in closed form. The method iteratively matches the moments of a set of Monte Carlo draws to weighted moments based on importance weights. We apply the method to Bayesian leave-one-out cross-validation and show that it performs better than many existing parametric adaptive importance sampling methods while being computationally inexpensive.},
	language = {en},
	author = {Paananen, Topi and Piironen, Juho and Burkner, Paul-Christian and Vehtari, Aki},
	pages = {29},
	file = {Paananen et al. - Implicitly Adaptive Importance Sampling.pdf:/Users/fb90/Zotero/storage/DG59XEMK/Paananen et al. - Implicitly Adaptive Importance Sampling.pdf:application/pdf;veeder1994 (1).pdf:/Users/fb90/Zotero/storage/NVADUPZK/veeder1994 (1).pdf:application/pdf}
}

@article{rathbun2010a,
	title = {Ground-based observations of time variability in multiple active volcanoes on {Io}},
	volume = {209},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103510002113},
	doi = {10.1016/j.icarus.2010.05.019},
	language = {en},
	number = {2},
	urldate = {2020-05-06},
	journal = {Icarus},
	author = {Rathbun, Julie A. and Spencer, John R.},
	month = oct,
	year = {2010},
	pages = {625--630}
}

@article{depater2017a,
	title = {Three decades of {Loki} {Patera} observations},
	volume = {297},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103516307801},
	doi = {10.1016/j.icarus.2017.03.016},
	language = {en},
	urldate = {2020-04-14},
	journal = {Icarus},
	author = {de Pater, Imke and de Kleer, Katherine and Davies, Ashley G. and Ádámkovics, Máté},
	month = nov,
	year = {2017},
	pages = {265--281}
}

@book{2017,
	address = {Paris},
	title = {Natural satellites astrometric data from either space probes and ground-based observatories produced by the {European} consortium {ESPaCE}},
	isbn = {978-2-910015-76-3},
	language = {en},
	publisher = {Institut de mécanique céleste et de calcul des éphémérides},
	year = {2017},
	note = {OCLC: 1018389102},
	file = {2017 - Natural satellites astrometric data from either sp.pdf:/Users/fb90/Zotero/storage/VRFMG2I6/2017 - Natural satellites astrometric data from either sp.pdf:application/pdf}
}

@article{tsumura2014,
	title = {{NEAR}-{INFRARED} {BRIGHTNESS} {OF} {THE} {GALILEAN} {SATELLITES} {ECLIPSED} {IN} {JOVIAN} {SHADOW}: {A} {NEW} {TECHNIQUE} {TO} {INVESTIGATE} {JOVIAN} {UPPER} {ATMOSPHERE}},
	volume = {789},
	issn = {0004-637X, 1538-4357},
	shorttitle = {{NEAR}-{INFRARED} {BRIGHTNESS} {OF} {THE} {GALILEAN} {SATELLITES} {ECLIPSED} {IN} {JOVIAN} {SHADOW}},
	url = {http://stacks.iop.org/0004-637X/789/i=2/a=122?key=crossref.036189d28338175e6fcb6dfb4ddcbade},
	doi = {10.1088/0004-637X/789/2/122},
	abstract = {Based on observations from the Hubble Space Telescope and the Subaru Telescope, we have discovered that Europa, Ganymede, and Callisto are bright around 1.5 μm even when not directly lit by sunlight. The observations were conducted with non-sidereal tracking on Jupiter outside of the ﬁeld of view to reduce the stray light subtraction uncertainty due to the close proximity of Jupiter. Their eclipsed luminosity was 10−6–10−7 of their uneclipsed brightness, which is low enough that this phenomenon has been undiscovered until now. In addition, Europa in eclipse was {\textless}1/10 of the others at 1.5 μm, a potential clue to the origin of the source of luminosity. Likewise, Ganymede observations were attempted at 3.6 μm by the Spitzer Space Telescope, but it was not detected, suggesting a signiﬁcant wavelength dependence. It is still unknown why they are luminous even when in the Jovian shadow, but forward-scattered sunlight by hazes in the Jovian upper atmosphere is proposed as the most plausible candidate. If this is the case, observations of these Galilean satellites while eclipsed by the Jovian shadow provide us with a new technique to investigate the Jovian atmospheric composition. Investigating the transmission spectrum of Jupiter by this method is important for investigating the atmosphere of extrasolar giant planets by transit spectroscopy.},
	language = {en},
	number = {2},
	urldate = {2020-02-25},
	journal = {ApJ},
	author = {Tsumura, K. and Arimatsu, K. and Egami, E. and Hayano, Y. and Honda, C. and Kimura, J. and Kuramoto, K. and Matsuura, S. and Minowa, Y. and Nakajima, K. and Nakamoto, T. and Shirahata, M. and Surace, J. and Takahashi, Y. and Wada, T.},
	month = jun,
	year = {2014},
	pages = {122},
	file = {Tsumura et al. - 2014 - NEAR-INFRARED BRIGHTNESS OF THE GALILEAN SATELLITE.pdf:/Users/fb90/Zotero/storage/L2APLJ7C/Tsumura et al. - 2014 - NEAR-INFRARED BRIGHTNESS OF THE GALILEAN SATELLITE.pdf:application/pdf}
}

@article{marchis2005,
	title = {Keck {AO} survey of {Io} global volcanic activity between 2 and 5 μm},
	volume = {176},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103505000096},
	doi = {10.1016/j.icarus.2004.12.014},
	abstract = {We present in this Keck AO paper the ﬁrst global high angular resolution observations of Io in three broadband near-infrared ﬁlters: Kc (2.3 µm), Lp (3.8 µm), and Ms (4.7 µm). The Keck AO observations are composed of 13 data sets taken during short time intervals spanning 10 nights in December, 2001. The MISTRAL deconvolution process, which is speciﬁcally aimed for planetary images, was applied to each image. The spatial resolution achieved with those ground-based observations is 150, 240, and 300 km in the Kc, Lp, and Ms band, respectively, making them similar in quality to most of the distant observations of the Galileo/NIMS instrument. Eleven images per ﬁlter were selected and stitched together after being deprojected to build a cylindrical map of the entire surface of the satellite. In Kc-band, surface albedo features, such as paterae (R {\textgreater} 60 km) are easily identiﬁable. The Babbar region is characterized by extremely low albedo at 2.2 µm, and shows an absorption band at 0.9 µm in Galileo/SSI data. These suggest that this region is covered by dark silicate deposits, possibly made of orthopyroxene. In the Lp–Ms (3–5 µm) bands, the thermal emission from active centers is easily identiﬁed. We detected 26 hot spots in both broadband ﬁlters over the entire surface of the minor planet; two have never been seen active before, nine more are seen in the Ms band. We focused our study on the hot spots detected in both broadband ﬁlters. Using the measurements of their brightness, we derived the temperature and area covered by 100 brightness measurements. Loki displayed a relatively quiescent activity. Dazhbog, a new eruption detected by Galileo/NIMS in August 2001, is a major feature in our survey. We also point out the fading of Tvashtar volcanic activity after more than two years of energetic activity, and the presence of a hot, but small, active center at the location of Surt, possibly a remnant of its exceptional eruption detected in February 2001. Two new active centers, labeled F and V on our data, are detected. Using the best temperature and the surface area derived from the L and M band intensities, we calculated the thermal output of each active center. The most energetic hot spots are Loki and Dazhbog, representing respectively 36 and 19\% of the total output calculated from a temperature ﬁt of all hot spots (20.6 × 1012 W). Based on the temperature derived from hot spots (∼400 K), our measurement can unambiguously identify the contribution to the heat ﬂux from the silicate portion of the surface. Because the entire surface was observed, no extrapolation was required to calculate that ﬂux. It is also important to note that we measured the brightness of the individual hot spots when they were located close to the Central Meridian. This minimizes the line-of-sight effect which does not follow strictly a classical cosine law. Finally, we argue that despite the widespread volcanic activity detected, Io was relatively quiescent in December 2001, with a minimum mean total output of 0.4–1.2 W m−2. This output is at least a factor of two lower than those inferred from observations made at longer wavelengths and at different epochs.},
	language = {en},
	number = {1},
	urldate = {2020-02-24},
	journal = {Icarus},
	author = {Marchis, F and Lemignant, D and Chaffee, F and Davies, A and Kwok, S and Prange, R and Depater, I and Amico, P and Campbell, R and Fusco, T},
	month = jul,
	year = {2005},
	pages = {96--122},
	file = {Marchis et al. - 2005 - Keck AO survey of Io global volcanic activity betw.pdf:/Users/fb90/Zotero/storage/H48AR44W/Marchis et al. - 2005 - Keck AO survey of Io global volcanic activity betw.pdf:application/pdf}
}

@article{jindal2020,
	title = {Arid or {Cloudy}: {Characterizing} the {Atmosphere} of the super-{Earth} 55 {Cancri} e using {High}-{Resolution} {Spectroscopy}},
	shorttitle = {Arid or {Cloudy}},
	url = {http://arxiv.org/abs/2007.03115},
	abstract = {The nearby super-Earth 55 Cnc e orbits a bright (V = 5.95 mag) star with a period of {\textasciitilde} 18 hours and a mass of {\textasciitilde} 8 Earth masses. Its atmosphere may be water-rich and have a large scale-height, though attempts to characterize it have yielded ambiguous results. Here we present a sensitive search for water and TiO in its atmosphere at high spectral resolution using the Gemini North telescope and the GRACES spectrograph. We combine observations with previous observations from Subaru and CFHT, improving the constraints on the presence of water vapor. We adopt parametric models with an updated planet radius based on recent measurements, and use a cross-correlation technique to maximize sensitivity. Our results are consistent with atmospheres that are cloudy or contain minimal amounts of water and TiO. Using these parametric models, we rule out a water-rich atmosphere (VMR {\textgreater}= 0.1\%) with a mean molecular weight of {\textless}= 15 g/mol at a 3 sigma confidence level, improving on the previous limit by a significant margin. For TiO, we rule out a mean molecular weight of {\textless}= 5 g/mol with a 3 sigma confidence level for a VMR greater than 10{\textasciicircum}-8; for a VMR of greater than 10{\textasciicircum}-7, the limit rises to a mean molecular weight of {\textless}= 10 g/mol. We can rule out low mean-molecular-weight chemical equilibrium models both including and excluding TiO/VO at very high confidence levels ({\textgreater} 10 sigma). Overall, our results are consistent with an atmosphere with a high mean molecular weight and/or clouds, or no atmosphere.},
	urldate = {2020-07-08},
	journal = {arXiv:2007.03115 [astro-ph]},
	author = {Jindal, A. and de Mooij, E. J. W. and Jayawardhana, R. and Deibert, E. K. and Brogi, M. and Rustamkulov, Z. and Fortney, J. J. and Hood, C. E. and Morley, C. V.},
	month = jul,
	year = {2020},
	note = {arXiv: 2007.03115},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 15 pages, 12 figures, 1 table},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/KT6AAPJQ/Jindal et al. - 2020 - Arid or Cloudy Characterizing the Atmosphere of t.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/V5T9NJDU/2007.html:text/html}
}

@article{cowan2018,
	title = {Mapping {Exoplanets}},
	url = {http://adsabs.harvard.edu/abs/2018haex.bookE.147C},
	abstract = {The varied surfaces and atmospheres of planets make them interesting places to live, explore, and study from afar. Unfortunately, the great distance to even the closest exoplanets makes it impossible to resolve their disk with current or near-term technology. It is still possible, however, to deduce spatial inhomogeneities in exoplanets provided that different regions are visible at different times - this can be due to rotation, orbital motion, and occultations by a star, planet, or moon. Astronomers have so far constructed maps of thermal emission and albedo for short-period giant planets. These maps constrain atmospheric dynamics and cloud patterns in exotic atmospheres. In the future, exo-cartography could yield surface maps of terrestrial planets, hinting at the geophysical and geochemical processes that shape them.},
	urldate = {2020-07-09},
	journal = {Handbook of Exoplanets},
	author = {Cowan, Nicolas B. and Fujii, Yuka},
	year = {2018},
	doi = {10.1007/978-3-319-55333-7_147},
	keywords = {Physics},
	pages = {147},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/VZF5S64P/Cowan and Fujii - 2018 - Mapping Exoplanets.pdf:application/pdf}
}

@article{lindal1981,
	title = {The atmosphere of {Jupiter}: {An} analysis of the {Voyager} radio occultation measurements},
	volume = {86},
	issn = {01480227},
	shorttitle = {The atmosphere of {Jupiter}},
	url = {http://doi.wiley.com/10.1029/JA086iA10p08721},
	doi = {10.1029/JA086iA10p08721},
	language = {en},
	number = {A10},
	urldate = {2020-07-14},
	journal = {J. Geophys. Res.},
	author = {Lindal, G. F. and Wood, G. E. and Levy, G. S. and Anderson, J. D. and Sweetnam, D. N. and Hotz, H. B. and Buckles, B. J. and Holmes, D. P. and Doms, P. E. and Eshleman, V. R. and Tyler, G. L. and Croft, T. A.},
	month = sep,
	year = {1981},
	pages = {8721--8727},
	file = {Lindal et al. - 1981 - The atmosphere of Jupiter An analysis of the Voya.pdf:/Users/fb90/Zotero/storage/SXZPQZQ3/Lindal et al. - 1981 - The atmosphere of Jupiter An analysis of the Voya.pdf:application/pdf}
}

@article{barth2020,
	title = {Magma ocean evolution of the {TRAPPIST}-1 planets},
	url = {http://arxiv.org/abs/2008.09599},
	abstract = {Recent observations of the potentially habitable planets TRAPPIST-1 e, f, and g suggest that they possess large water mass fractions of possibly several tens of wt\% of water, even though the host star's activity should drive rapid atmospheric escape. These processes can photolyze water, generating free oxygen and possibly desiccating the planet. After the planets formed, their mantles were likely completely molten with volatiles dissolving and exsolving from the melt. In order to understand these planets and prepare for future observations, the magma ocean phase of these worlds must be understood. To simulate these planets, we have combined existing models of stellar evolution, atmospheric escape, tidal heating, radiogenic heating, magma ocean cooling, planetary radiation, and water-oxygen-iron geochemistry. We present magmoc, a versatile magma ocean evolution model, validated against the rocky Super-Earth GJ 1132b and early Earth. We simulate the coupled magma ocean-atmospheric evolution of TRAPPIST-1 e, f, and g for a range of tidal and radiogenic heating rates, as well as initial water contents between 1 and 100 Earth-oceans. We find that TRAPPIST-1 f and g most likely followed the extremely wet scenario with a prolonged magma ocean phase of at least 250 Myr. Planet e probably followed the dry or intermediate track, and may or may not have possessed little water vapour or oxygen in the atmosphere at the time of mantle solidification. For all planets that we investigated, we find that only 3-5\% of the initial water will be locked in the mantle after the magma ocean solidified.},
	urldate = {2020-08-24},
	journal = {arXiv:2008.09599 [astro-ph]},
	author = {Barth, Patrick and Carone, Ludmila and Barnes, Rory and Noack, Lena and Mollière, Paul and Henning, Thomas},
	month = aug,
	year = {2020},
	note = {arXiv: 2008.09599},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: Submitted to Astrobiology, 25 pages, 9 figures},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/UMINEGGX/Barth et al. - 2020 - Magma ocean evolution of the TRAPPIST-1 planets.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/IALEXPVA/2008.html:text/html}
}

@misc{zotero-3522,
	title = {Build software better, together},
	url = {https://github.com},
	abstract = {GitHub is where people build software. More than 50 million people use GitHub to discover, fork, and contribute to over 100 million projects.},
	language = {en},
	urldate = {2020-09-02},
	journal = {GitHub},
	file = {Snapshot:/Users/fb90/Zotero/storage/JTMK8Y9L/github.com.html:text/html}
}

@article{depater2020,
	title = {{ALMA} {Observations} of {Io} {Going} into and {Coming} out of {Eclipse}},
	url = {http://arxiv.org/abs/2009.07729},
	abstract = {We present 1-mm observations constructed from ALMA [Atacama Large (sub)Millimeter Array] data of SO\$\_2\$, SO and KCl when Io went from sunlight into eclipse (20 March 2018), and vice versa (2 and 11 September 2018). There is clear evidence of volcanic plumes on 20 March and 2 September. The plumes distort the line profiles, causing high-velocity (\${\textbackslash}gtrsim\$500 m/s) wings, and red/blue-shifted shoulders in the line profiles. During eclipse ingress, the SO\$\_2\$ flux density dropped exponentially, and the atmosphere reformed in a linear fashion when re-emerging in sunlight, with a "post-eclipse brightening" after \${\textbackslash}sim\$10 minutes. While both the in-eclipse decrease and in-sunlight increase in SO was more gradual than for SO\$\_2\$, the fact that SO decreased at all is evidence that self-reactions at the surface are important and fast, and that in-sunlight photolysis of SO\$\_2\$ is the dominant source of SO. Disk-integrated SO\$\_2\$ in-sunlight flux densities are \${\textbackslash}sim\$2--3 times higher than in-eclipse, indicative of a roughly 30--50{\textbackslash}\% contribution from volcanic sources to the atmosphere. Typical column densities and temperatures are \$N {\textbackslash}approx (1.5 {\textbackslash}pm 0.3) {\textbackslash}times 10{\textasciicircum}\{16\}\$ cm\${\textasciicircum}\{-2\}\$ and \$T {\textbackslash}approx 220-320\$ K both in-sunlight and in-eclipse, while the fractional coverage of the gas is 2--3 times lower in-eclipse than in-sunlight. The low level SO\$\_2\$ emissions present during eclipse may be sourced by stealth volcanism or be evidence of a layer of non-condensible gases preventing complete collapse of the SO\$\_2\$ atmosphere. The melt in magma chambers at different volcanoes must differ in composition to explain the absence of SO and SO\$\_2\$, but simultaneous presence of KCl over Ulgen Patera.},
	urldate = {2020-09-18},
	journal = {arXiv:2009.07729 [astro-ph]},
	author = {de Pater, Imke and Luszcz-Cook, Statia and Rojo, Patricio and Redwing, Erin and de Kleer, Katherine and Moullet, Arielle},
	month = sep,
	year = {2020},
	note = {arXiv: 2009.07729},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 20 pages, 15 figures. Planetary Science Journal, 2020, In Press},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/RCMMEDTH/de Pater et al. - 2020 - ALMA Observations of Io Going into and Coming out .pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/N39W97GC/2009.html:text/html}
}

@article{seon2007,
	title = {Smoothing of an {All}-sky {Survey} {Map} with a {Fisher}-von {Mises} {Function}},
	url = {http://arxiv.org/abs/astro-ph/0703168},
	abstract = {A convolution of the all-sky survey data with a smoothing function is crucial in calculating the smooth surface brightness of the sky survey data. The convolution is usually performed using a spherical version of the convolution theorem. However, a Gaussian function, applicable only in the flat-sky approximation, has been usually adopted as a smoothing kernel. In this paper, we present an exact analytic solution of the spherical-harmonics transformation of a Fisher-von Mises function, the mathematical version of a Gaussian function in spherical space. We also obtain the approximate solutions exp[-l(l + 1)/2k]. The exact and the approximate solutions may be useful when an astrophysical survey map is convolved with a smoothing function of k{\textgreater}1.},
	urldate = {2020-09-18},
	journal = {arXiv:astro-ph/0703168},
	author = {Seon, Kwang-Il},
	month = mar,
	year = {2007},
	note = {arXiv: astro-ph/0703168},
	keywords = {Astrophysics},
	annote = {Comment: 4 pages, 2 figures, preprint version of the paper published in JKPS on March 15, 2006},
	file = {arXiv Fulltext PDF:/Users/fb90/Zotero/storage/THMW638P/Seon - 2007 - Smoothing of an All-sky Survey Map with a Fisher-v.pdf:application/pdf;arXiv.org Snapshot:/Users/fb90/Zotero/storage/N9AXL3M8/0703168.html:text/html}
}

@article{white1995,
	title = {Window functions of cosmic microwave background experiments},
	volume = {443},
	url = {http://adsabs.harvard.edu/abs/1995ApJ...443....6W},
	doi = {10.1086/175497},
	abstract = {We discuss the applicability and derivation of window functions for cosmic microwave background experiments on large and intermediate angular scales. These window functions describe the response of the experiment to power in a particular mode of the fluctuation spectrum. We give general formulae, illustrated with specific examples, for the most common observing strategies.},
	urldate = {2020-09-19},
	journal = {The Astrophysical Journal},
	author = {White, Martin and Srednicki, M.},
	month = apr,
	year = {1995},
	keywords = {Background Radiation, Cosmology, Functions (Mathematics), Infrared Windows, Microwaves, Numerical Analysis, Spectra, Variations},
	pages = {6--10},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/TADU6B3W/White and Srednicki - 1995 - Window functions of cosmic microwave background ex.pdf:application/pdf}
}

@misc{zotero-3534,
	title = {Geologic {Map} of {Io}},
	url = {https://pubs.usgs.gov/sim/3168/},
	urldate = {2020-09-26},
	file = {Geologic Map of Io:/Users/fb90/Zotero/storage/VA4RNW8U/3168.html:text/html}
}

@misc{williamsd.a.keszthelyil.p.crownd.a.yffj.a.jaegerw.l.schenkp.m.geisslerp.e.andbeckert.l.2011,
	title = {Geologic map of {Io}: {U}.{S}. {Geological} {Survey} {Scientific} {Investigations} {Map} 3168, scale 1:15,000,000, 25 p.},
	url = {https://pubs.usgs.gov/sim/3168/.},
	author = {, D.A., Keszthelyi, L.P., Crown, D.A., Yff, J.A., Jaeger, W.L., Schenk, P.M., Geissler, P.E., {and} Becker, T.L., Williams},
	year = {2011}
}

license: MIT

license_type: permissive

branch_name: refs/heads/main

extension: bib