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"Bayliss, Daniel"
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Jim Henson's Labyrinth : coronation
The untold origin of the Goblin King from Jim Henson's cult-classic film, Labyrinth. Long before Sarah ventured to save her baby brother from the clutches of the Goblin King, another young woman sought to save her child from an unknown fate within the Labyrinth. Set in 18th-century Venice, Jim Henson's Labyrinth: Coronation is a striking look into the mysteries of the Labyrinth itself, uncovering the fate of a small boy named Jareth who would one day be King. Simon Spurrier (The Spire, Jim Henson's The Power of the Dark Crystal) and Daniel Bayliss (Jim Henson's The Storyteller: Dragons, Big Trouble in Little China/Escape from New York) present a look into a magical world where nothing is as it seems and introduce Maria, a heroine instilled with courage, hope, and determination.
Book
A remnant planetary core in the hot-Neptune desert
The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune ‘desert’ (a region in mass–radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b and NGTS-4b, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune’s but an anomalously large mass of 39.1(+2.7−2.6) Earth masses and a density of 5.2(+0.7−0.8) grams per cubic centimetre, similar to Earth’s. Interior-structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9(+0.8−0.9) per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet.
Journal Article
SuperLupus: A Deep, Long Duration Transit Survey
SuperLupus is a deep transit survey monitoring a Galactic Plane field in the Southern hemisphere. The project is building on the successful Lupus Survey, and will double the number of images of the field from 1700 to 3400, making it one of the longest duration deep transit surveys. The immediate motivation for this expansion is to search for longer period transiting planets (5-8 days) and smaller radii planets. It will also provide near complete recovery for the shorter period planets (1-3 days). In March, April, and May 2008 we obtained the new images and work is currently in progress reducing these new data.
Journal Article
Transits against Fainter Stars: The Power of Image Deconvolution
Compared to bright star searches, surveys for transiting planets against fainter (V = 12–18) stars have the advantage of much higher sky densities of dwarf star primaries, which afford easier detection of small transiting bodies. Furthermore, deep searches are capable of probing a wider range of stellar environments. On the other hand, for a given spatial resolution and transit depth, deep searches are more prone to confusion from blended eclipsing binaries. We present a powerful mitigation strategy for the blending problem that includes the use of image deconvolution and high-resolution imaging. The techniques are illustrated with Lupus-TR-3 and very recent IR imaging with PANIC on Magellan. The results are likely to have implications for the CoRoT and KEPLER missions designed to detect transiting planets of terrestrial size.
Journal Article
The storyteller.: (Dragons)
Following Witches, this is our second in a themed series of Jim Henson's The Storyteller tales, this time centered around dragons. Includes four tales of dragons, inspired by folklore from around the world and told in the spirit of Jim Henson's beloved television series.Collects the complete limited series and also includes an exclusive behind-the-scenes look at the process and care taken in adapting each of these timeless legends.
eBook
Revisiting WASP-47 with ESPRESSO and TESS
WASP-47 hosts a remarkable planetary system containing a hot Jupiter (WASP-47 b; P = 4.159 days) with an inner super-Earth (WASP-47 e; P = 0.7896 days), a close-orbiting outer Neptune (WASP-47 d; P = 9.031 days), and a long period giant planet (WASP-47 c; P = 588.4 days). We use the new TESS photometry to refine the orbital ephemerides of the transiting planets in the system, particularly the hot Jupiter WASP-47 b, for which we find an update equating to a 17.4 min shift in the transit time. We report new radial velocity measurements from the ESPRESSO spectrograph for WASP-47, which we use to refine the masses of WASP-47 d and WASP-47 e, with a high cadence observing strategy aimed to focus on the super-Earth WASP-47 e. We detect a periodic modulation in the K2 photometry that corresponds to a 32.5\\(\\pm\\)3.9 day stellar rotation, and find further stellar activity signals in our ESPRESSO data consistent with this rotation period. For WASP-47 e we measure a mass of 6.77\\(\\pm\\)0.57 M\\(_{\\oplus}\\) and a bulk density of 6.29\\(\\pm\\)0.60 gcm\\(^{-3}\\), giving WASP-47 e the second most precisely measured density to date of any super-Earth. The mass and radius of WASP-47 e, combined with the exotic configuration of the planetary system, suggest the WASP-47 system formed through a mechanism different to systems with multiple small planets or more typical isolated hot Jupiters.
Paper
The atmosphere of WASP-17b: Optical high-resolution transmission spectroscopy
High-resolution transmission spectroscopy is a method for understanding the chemical and physical properties of upper exoplanetary atmospheres. Due to large absorption cross-sections, resonance lines of atomic sodium D-lines (at 5889.95 \\(\\AA\\) and 5895.92 \\(\\AA\\)) produce large transmission signals. Our aim is to unveil the physical properties of WASP-17b through an accurate measurement of the sodium absorption in the transmission spectrum. We analyze 37 high-resolution spectra observed during a single transit of WASP-17b with the MIKE instrument on the 6.5 meter Magellan Telescopes. We exclude stellar flaring activity during the observations by analyzing the temporal variations of H\\(_{\\alpha}\\) and Ca II infra-red triplet (IRT) lines. Then we obtain the excess absorption light curves in wavelength bands of 0.75, 1, 1.5 and 3 \\(\\AA\\) around the center of each sodium line (i.e., the light curve approach). We model the effects of differential limb-darkening, and the changing planetary radial velocity on the light curves. We also analyze the sodium absorption directly in the transmission spectrum, which is obtained through dividing in-transit by out-of-transit spectra (i.e., the division approach). We then compare our measurements with a radiative transfer atmospheric model. Our analysis results in a tentative detection of exoplanetary sodium: we measure the width and amplitude of the exoplanetary sodium feature to be \\(\\sigma_{\\mathrm{Na}}\\) = (0.128 \\(\\pm\\) 0.078) \\(\\AA\\) and A\\(_{\\mathrm{Na}}\\) = (1.7 \\(\\pm\\) 0.9)% in the excess light curve approach and \\(\\sigma_{\\mathrm{Na}}\\) = (0.850 \\(\\pm\\) 0.034) \\(\\AA\\) and A\\(_{\\mathrm{Na}}\\) = (1.3 \\(\\pm\\) 0.6)% in the division approach. By comparing our measurements with a simple atmospheric model, we retrieve an atmospheric temperature of 1550 \\(^{+170} _{-200}\\) K and radius (at 0.1 bar) of 1.81 \\(\\pm\\) 0.02 R\\(_{\\rm Jup}\\) for WASP-17b.
Paper
Investigating the Planet-Metallicity Correlation for Hot Jupiters
We investigate the giant planet-metallicity correlation for a homogeneous, unbiased set of 217 hot Jupiters taken from nearly 15 years of wide-field ground-based surveys. We compare the host star metallicity to that of field stars using the Besançon Galaxy model, allowing for a metallicity measurement offset between the two sets. We find that hot Jupiters preferentially orbit metal rich stars. However, we find the correlation consistent, though marginally weaker, for hot Jupiters (\\(\\beta=0.71^{+0.56}_{-0.34}\\)) than it is for other longer period gas giant planets from radial velocity surveys. This suggests that the population of hot Jupiters probably formed in a similar process to other gas giant planets, and differ only in their migration histories.
Paper
Examining the broadband emission spectrum of WASP-19b: A new z band eclipse detection
WASP-19b is one of the most irradiated hot-Jupiters known. Its secondary eclipse is the deepest of all transiting planets, and has been measured in multiple optical and infrared bands. We obtained a z band eclipse observation, with measured depth of 0.080 +/- 0.029 %, using the 2m Faulkes Telescope South, that is consistent with the results of previous observations. We combine our measurement of the z band eclipse with previous observations to explore atmosphere models of WASP-19b that are consistent with the its broadband spectrum. We use the VSTAR radiative transfer code to examine the effect of varying pressure-temperature profiles and C/O abundance ratios on the emission spectrum of the planet. We find models with super-solar carbon enrichment best match the observations, consistent with previous model retrieval studies. We also include upper atmosphere haze as another dimension in the interpretation of exoplanet emission spectra, and find that particles <0.5 micron in size are unlikely to be present in WASP-19b.
Paper
Author Correction: An ultrahot Neptune in the Neptune desert
An amendment to this paper has been published and can be accessed via a link at the top of the paper.
Journal Article