Comparing models of an exoplanet-earth to earthshine observations

Polarimetry is widely becoming recognized as a powerful technique for enhancing the contrast between a star and an exoplanet, and thus improving upon the direct detection of exoplanets. The real power of polarimetry, however, is in its ability to characterize the physical properties of these worlds. This is because the state of the polarization of the light from the planet is very sensitive to the composition and structure of the planetary atmosphere and surface, being affected by properties such as the mixing ratios of atmospheric absorbing gases, cloud optical thickness, cloud top pressure, cloud particle size, and surface albedo. Various groups have theoretically studied the optical linear polarimetric signals of Earth-like exoplanets as functions of both orbital phase and wavelength. This project aims to validate the accuracy of these theoretical models against the only known observations of an Earth-like planet thus far: Earthshine. Using atmospheric and surface data taken by the MODIS instrument aboard the Terra and Aqua satellites, as well as surface albedo spectra from the EcoStress Spectral Library, we created a detailed model of the Earth. Then, using this model data as input for three separate radiative transfer algorithms, we generate the flux and linear polarization spectra for the model exoplanet-Earth from the optical to near-infrared wavelengths. We compare the results from all three codes to each other and to observational linear spectropolarimetric data of the Earthshine obtained by a member of our group. We identify similarities and potential pitfalls between these codes in an effort to improve our future characterizations of Earth-like exoplanets.Stars and planetary system

Earth-as-an-exoplanet: comparing earthshine observations to models of an exo-Earth

Traditional methods of exoplanet characterization that only make use of emitted or reflected flux lack the ability to fully distinguish between different physical features of the target, such as cloud layers, hazes, or surface features. Polarimetry, however, is a powerful, more sensitive technique that has this ability, as it measures light as a vector (by the orientation of the electric field) rather than a scalar intensity. It is therefore extremely sensitive to the composition and structure of the planetary atmosphere and surface, being affected by properties such as the mixing ratios of atmospheric absorbing gases, cloud optical thickness, cloud top pressure, cloud particle size, and surface albedo. Various groups have theoretically studied the optical linear polarimetric signals of Earth-like exoplanets as functions of both orbital phase and wavelength. With this project we assess the accuracy of these theoretical models against observations of the Earthshine, the only known observations of an Earth-like planet thus far. Using data of the atmosphere and surface taken by the MODIS instrument aboard the Terra and Aqua satellites, as well as surface reflectance spectra from the JPL EcoStress Spectral Library, we created a gridded model of the Earth. Then, using this model data as input for three separate radiative transfer algorithms, we generate the flux and linear polarization spectra for the model exoplanet-Earth across the optical to near-infrared wavelengths. We compare the results from all three codes to each other and to the observational linear spectropolarimetric data of the Earthshine obtained by a member of our group. We identify similarities and potential pitfalls between the codes, and make necessary adjustments to them, in an effort to improve our future characterizations of terrestrial exoplanets.Stars and planetary system

Polarized signatures of a habitable world: comparing models of an exoplanet-earth with VNIR earthshine spectra

n the James Webb Space Telescope and Extremely Large Telescopes era we expect to characterize a number of potentially habitable Earth-like exoplanets. However, the characterization of these worlds depends crucially on the accuracy of theoretical models. Validating these models against observations of planets with known properties will be key for the future characterization of terrestrial exoplanets. Due to its sensitivity to the micro- and macro-physical properties of an atmosphere, spectropolarimetry will be an important tool that in tandem with traditional flux-only observations will enhance the capabilities of characterizing Earth-like planets. In this presentation we benchmark two separate polarization-enabled radiative transfer codes against each other and against unique linear spectropolarimetric observations of the Earthshine (i.e., sunlight scattered by the dayside of the Earth and reflected back to the planet by the nightside of the Moon) that cover wavelengths from ~ 0.4 μm to ~ 2.3 μm. We find that the results from the two codes agree with each other but both underestimate the level of polarization of the Earthshine. We discuss how we plan to update the two codes to better fit the observations. We also report an interesting discrepancy between our models and the observed 1.27 μm O2 feature in the Earthshine, together with an analysis of potential methods for matching this feature and a discussion on the implications this has for future observations of habitable exoplanets.Stars and planetary system

Polarized signatures of a habitable world: comparing models of an exoplanet Earth with visible and near-infrared Earthshine spectra

Stars and planetary system

First report of a bucephalid digenean from an apogonid teleost: Prosorhynchoides apogonis n. sp from Cheilodipterus macrodon on the southern Great Barrier Reef, Australia

Prosorhynchoides apogonis n. sp. (Digenea: Bucephalidae) is described from the intestine of the apogonid Cheilodipterus macrodon on the southern Great Barrier Reef, Australia. The new species is differentiated from other species of Prosorhynchoides Dollfus, 1929 by the configuration of its digestive system, shape and distribution of its vitelline follicles, and the shape and extent of its uterus. This is the first bucephalid to be described from the teleost family Apogonidae, and our records suggest that this species is strongly host-specific, at least to the genus Cheilodipterus. The host family is consistent with the pattern of Prosorhynchoides being reported from a very wide range of piscivorous fish families. As a result of comparisons made in the description of this species, 18 species formerly included in Bucephaloides Hopkins, 1954, Bucephalopsis Diesing, 1855 and Neobucephalopsis Dayal, 1948 are transferred to Prosorhynchoides, 16 as new combinations and two as replacement names to prevent secondary homonymy