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The AKARI IRC all-sky survey provided more than twenty thousand thermal infrared observations of over five thousand asteroids. Diameters and albedos were obtained by fitting an empirically calibrated version of the standard thermal model to these data. After the publication of the flux catalogue in October 2016, our aim here is to present the AKARI IRC all-sky survey data and discuss valuable scientific applications in the field of small body physical properties studies. As an example, we update the catalogue of asteroid diameters and albedos based on AKARI using the near-Earth asteroid thermal model (NEATM). We fit the NEATM to derive asteroid diameters and, whenever possible, infrared beaming parameters. We fit groups of observations taken for the same object at different epochs of the survey separately, so we compute more than one diameter for approximately half of the catalogue. We obtained a total of 8097 diameters and albedos for 5170 asteroids, and we fitted the beaming parameter for almost two thousand of them. When it was not possible to fit the beaming parameter, we used a straight line fit to our sample’s beaming parameter-versus-phase angle plot to set the default value for each fit individually instead of using a single average value. Our diameters agree with stellar-occultation-based diameters well within the accuracy expected for the model. They also match the previous AKARI-based catalogue at phase angles lower than 50° , but we find a systematic deviation at higher phase angles, at which near-Earth and Mars-crossing asteroids were observed. The AKARI IRC All-sky survey is an essential source of information about asteroids, especially the large ones, since, it provides observations at different observation geometries, rotational coverages and aspect angles. For example, by comparing in more detail a few asteroids for which dimensions were derived from occultations, we discuss how the multiple observations per object may already provide three-dimensional information about elongated objects even based on an idealised model like the NEATM. Finally, we enumerate additional expected applications for more complex models, especially in combination with other catalogues. [ABSTRACT FROM AUTHOR]

A wealth of near infrared spectroscopic data for a large number of galactic objects was recorded with AKARI during its active lifetime. The hydrocarbon emission features around 3.3 – 3.5 m are modelled here as a series of 6 Voigt profiles arising due to hydrogen atoms found in different molecular structures within the emitting spectroscopic carriers. This model is compared and contrasted with a model consisting of 3 Gaussian profiles and found to produce a superior fit to AKARI data. Analysis of the 6 Voigt model shows that the 3.3 m aromatic hydrocarbon band is well described by two components at 3.28 m and 3.30 m . We confirm that the 3.28 μ m band is due to emission from aromatic molecules, and find a good correlation between the 3.28 μ m and 3.41 m bands, assigned to bay-hydrogen sites and linking methylene groups respectively. Results are discussed in terms of molecular processing and dust formation. [ABSTRACT FROM AUTHOR]

In avian species, primordial germ cells (PGC) use the vascular system as a vehicle to transport them to the future gonadal region. The aim of this study was to elucidate the details of migration system and size of the PGC population in the early chicken embryo. We analyzed whole chicken embryos during stages X and 2 to 17 by immunohistochemical staining using specific antibody raised against chicken vasa homolog. At stage X, PGC were dense in the central zone of the area pellucida. Following the formation of the primitive streak, PGC moved anteriorly to the edge of the extraembryonic region. The size of the PGC population increased gradually during stages X (130.4 ± 31.9) to 10 (439.3 ± 93.6). At stage 10, PGC began to accumulate in the region anterior to the head, and then we could observe that PGC invaded into the vascular system in this region. At stage 11, the number of PGC decreased in the region anterior to the head (129.8 ± 42.5 to 46.7 ± 4.2) and increased in the blood vessels (194.0 ± 41.6 to 285.0 ± 7.5). No PGC could be recognized in the intermediate mesoderm, the future gonadal region, until stage 14, but they first appeared there at stage 15. The number of PGC recognized in the intermediate mesoderm increased from stage 15 to 17. Interestingly, the number of PGC between the left and right sides of this region was consistently and significantly different (P < 0.05) in females and males. The present study mainly clarified that chicken PGC continue to proliferate throughout early development, many PGC invaded into the vascular system from the region anterior to the head in stage 11, and PGC actively left the blood vessels and migrated to the intermediate mesoderm from stage 15. [ABSTRACT FROM AUTHOR]

Here we report a comparison between reflectance spectroscopy of meteorites under asteroidal environment (high vacuum and temperature) and Main Belt and Near Earth Asteroids spectra. Focusing on the –OH absorption feature around 3 μm, we show that the asteroidal environment induces a reduction of depth and width of the band, as well as a shift of the reflectance minimum. We then decompose the –OH feature into several components with a new model using Exponentially Modified Gaussians. Unlike previous studies, we confirme the link between these components, the aqueous alteration history and the amount of water molecules inside of the sample, using the shape of this spectral feature only. We then apply this deconvolution model to asteroids spectra which were obtained with a space-borne telescope and two space probes, and find a strong similarity with the components detected on meteorites, and among asteroids from a same type. Based on the conclusions drawn from our meteorites experiment, we suggest to use the 3-μm band as a tracer of the alteration history of the small bodies. Using the 3-μm band only, we show that Ryugu has been heavily altered by water, which is consistent with its parent body being covered with water ice, then went through a high temperature sequence, over 400 °C. We also point out that the 3-μm band of Bennu shows signs of its newly discovered surface activity. • Exponentially Modified Gaussians are used to model the shape of the 3-μm band. • The components of the band depend on the aqueous alteration and relative humidity. • Similar components are detected on the asteroids spectra. • The components are used to retrieve the alteration history of the asteroids. • Signs of activity on Bennu and two Cgh-types are detected through the –OH band. [ABSTRACT FROM AUTHOR]

The near-Earth asteroid 308635 (2005 YU55) is a potentially hazardous asteroid which was discovered in 2005 and passed Earth on Nov. 8, 2011 at 0.85 lunar distances. This was the closest known approach by an asteroid of several hundred metres in diameter since 1976 when an object of similar size passed at 0.5 lunar distances. We observed 2005 YU55 from the ground with a recently developed mid-IR camera (miniTAO/MAX38) in N and Q bands and with the Submillimeter Array (SMA) at 1.3 mm. In addition, we obtained space observations with Herschel/PACS at 70, 100, and 160 μm. Our thermal measurements cover a wide range of wavelengths from 8.9 μm to 1.3 mm and were taken after opposition at phase angles between -97° and -18°. We performed a radiometric analysis via a thermophysical model and combined our derived properties with results from radar, adaptive optics, lightcurve observations, speckle, and auxiliary thermal data. We find that 308635 (2005 YU55) has an almost spherical shape with an effective diameter of 300 to 312 m and a geometric albedo pV of 0.055 to 0.075. Its spin axis is oriented towards celestial directions (λecl, βecl) = (60° ± 30°, -60° ± 15°), which means it has a retrograde sense of rotation. The analysis of all available data combined revealed a discrepancy with the radar-derived size. Our radiometric analysis of the thermal data together with the problem to find a unique rotation period might be connected to a non-principal axis rotation. A low to intermediate level of surface roughness (rms mean slope in the range 0.1-0.3) is required to explain the available thermal measurements. We found a thermal inertia in the range 350-800 Jm-2 s-0.5 K-1, very similar to the rubble-pile asteroid 25 143 Itokawa and indicating a surface with a mixture of low conductivity fine regolith with larger rocks and boulders of high thermal inertia. [ABSTRACT FROM AUTHOR]

Abstract: Cometary dust trails were first observed by IRAS; they are widely known to be the origins of meteoric showers. A new window has been opened for the study of dust trails, using ground-based observations. We succeeded in obtaining direct images of the 22P/Kopff dust trail with the Kiso 1.05-m Schmidt telescope. Following this initial success, we have continued to perform a dust trail survey at Kiso. As a result of this survey, we have detected dust trails along the orbit of six periodic comets, between February 2002 and March 2004. The optical depth of these dust trails are 10−9 to 10−8, which is consistent with IRAS measurements. In this paper, we describe the observations and data reduction procedures, and report the brief result obtained between February 2002 and March 2004. [Copyright &y& Elsevier]