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How does Evolutionary Distinctiveness change when we place fossils in the tree?
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Time-binning rates of continuous character evolution on a phylogeny: the orig...
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A novel metatree approach to generating large phylogenetic hypotheses of exti...
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HotJupiters are amongthebest-studied exoplanets, but it is still poorly understood how their chemical composition and cloud properties vary with longitude. Theoretical models predict that clouds may condense on the nightside and that molecular abundances can be driven out of equilibrium by zonal winds. Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43b measured from 5–12µ 5–12µ 5–12µm with JWST’s Mid-Infrared Instrument (MIRI). 1524 ±35 1524 ±35 and 863±23 The spectra reveal a large day–night temperature contrast (with average brightness temperatures of 1524 ± 35 863 ±23 863 ±23Kelvin, respectively) and evidence for water absorption at all orbital phases. Comparisons with three-dimensional atmospheric models show that both the phase curve shape and emission spectra strongly suggest the presence of nightside clouds which become optically thick to thermal emission at pressures greater than ∼100mbar. The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Con3trary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1–6 parts per million, depending on model assumptions).
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Context. WASP-76 b has been a recurrent subject of study since the detection of a signature in high-resolution transit spectroscopy data indicating an asymmetry between the two limbs of the planet. The existence of this asymmetric signature has been confirmed by multiple studies, but its physical origin is still under debate. In addition, it contrasts with the absence of asymmetry reported in the infrared (IR) phase curve. Aims. We provide a more comprehensive dataset of WASP-76 b with the goal of drawing a complete view of the physical processes at work in this atmosphere. In particular, we attempt to reconcile visible high-resolution transit spectroscopy data and IR broadband phase curves. Methods. We gathered 3 phase curves, 20 occultations, and 6 transits for WASP-76 b in the visible with the CHEOPS space telescope. We also report the analysis of three unpublished sectors observed by the TESS space telescope (also in the visible), which represents 34 phase curves. Results. WASP-76 b displays an occultation of 260±11 and 152±10 ppm in TESS and CHEOPS bandpasses respectively. Depending on the composition assumed for the atmosphere and the data reduction used for the IR data, we derived geometric albedo estimates that range from 0.05 ± 0.023 to 0.146 ± 0.013 and from <0.13 to 0.189 ± 0.017 in the CHEOPS and TESS bandpasses, respectively. As expected from the IR phase curves, a low-order model of the phase curves does not yield any detectable asymmetry in the visible either. However, an empirical model allowing for sharper phase curve variations offers a hint of a flux excess before the occultation, with an amplitude of ∼40 ppm, an orbital offset of ∼−30◦ , and a width of ∼20◦ . We also constrained the orbital eccentricity of WASP-76 b to a value lower than 0.0067, with a 99.7% confidence level. This result contradicts earlier proposed scenarios aimed at explaining the asymmetry observed in high-resolution transit spectroscopy. Conclusions. In light of these findings, we hypothesise that WASP-76 b could have night-side clouds that extend predominantly towards its eastern limb. At this limb, the clouds would be associated with spherical droplets or spherically shaped aerosols of an unknown species, which would be responsible for a glory effect in the visible phase curves.
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Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b
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How does Evolutionary Distinctiveness change when we place fossils in the tree?
1.
How does Evolutionary Distinctiveness
change when we place fossils in the tree? Graeme T. Lloyd @GraemeTLloyd
2.
EDGE species Evolutionary Distinctiveness Extinction Risk Isaac
et al. 2007
3.
EDGE species Evolutionary Distinctiveness Extinction Risk EDGE Isaac
et al. 2007
4.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma)
5.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma) 3 5 1 1 1 1 1 1Branch Duration
6.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma) 4 1 2 2 1 1 1 1N Descendants
7.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma) 3 / 4 5 / 1 1 / 2 1 / 2 1 / 1 1 / 1 1 / 1 1 / 1Branch Duration / N Descendants
8.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma) 0.75 5 0.5 0.5 1 1 1 1ED
9.
Evolutionary Distinctiveness Isaac et
al. 2007 012345 Time (Ma) 0.75 + 5 = 0.5 + 0.5 + 1 = 1 = 1 = 1 = 2.25 2.25 2.25 2.25 5 ED
10.
Evolutionary Distinctiveness 012345 Time (Ma) 0.75
+ 5 = 0.5 + 0.5 + 1 = 1 = 1 = 1 = 2.25 2.25 2.25 2.25 5 ED Isaac et al. 2007 ?
11.
Case study
12.
Tree without fossils Oaks
2011
13.
ED without fossils
14.
ED without fossils Alligator
sinensis
15.
Tree with fossils
16.
Change in EDDecreaseinED IncreaseinED
17.
ED with fossils
18.
ED with fossils Gavialis
gangeticus Tomistoma schlegelii
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