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TUBIN is a microsatellite mission tasked with the demonstration of microbolometer technology for the detection of high-temperature events. To this end, the spacecraft employs a set of two microbolometers sensitive in the thermal range of the electromagnetic spectrum as well as a complementary CMOS-based imager for the visible spectrum. Additionally, the mission serves to demonstrate the upgraded capabilities of the TUBiX20 microsatellite platform after its initial implementation within the TechnoSat mission, launched in 2017. Here, the platform was upgraded with star trackers for enhanced attitude determination to enable the pointing accuracy required by the mission. Launched in June 2021, TUBIN has already successfully detected wildfires and volcanic activity in different biomes across the globe. Additionally, the sensor suite of the TUBIN mission was applied to examine its capabilities in the assessment of light-pollution in dedicated night time imaging campaigns. In this paper, we present and analyze data sets captured in the first six months of operation to illustrate capabilities, accomplishments, and challenges regarding payload operation, calibration, and data analysis for the TUBIN mission. Finally, the plans for the second half of TUBIN's nominal lifetime are outlined, including an on-orbit calibration campaign and increased automation in payload operations. • Wildfire detection with a small satellite platform in the 20 kg range using uncooled microbolometer technology. • We introduce updates to the highly modular satellite platform. • Initial orbit results are presented to showcase the performance of the payload. • More than a thousand images were taken to demonstrate detection of high-temperature events, calibration routine and other applications. [ABSTRACT FROM AUTHOR]

Technische Universität Berlin has been active in the field of small satellites for more than 25 years and has successfully developed, built and operated 21 satellites to date. One of the recent developments of the university is TUBiX20, a highly modular microsatellite platform that was designed to support various different mission types. At the moment, three missions of Technische Universität Berlin are based on TUBiX20, namely TechnoSat, TUBIN, and QUEEN. Launched in July 2017, TechnoSat is the first mission to demonstrate the TUBiX20 platform in orbit. TechnoSat's mission is the demonstration of seven technology payloads that include an S-band transmitter and a reaction wheel system. This paper presents initial orbit results of the TechnoSat mission, focusing on the payloads relevant for future TUBiX20 missions. Here, the evolution of the experiments towards increasing complexity from the commissioning phase into manoeuvres that combine the use of several payloads underlines the platform's versatility. Furthermore, a quick adaptation of payloads like the S-band transmitter and the reaction wheel system into regular operations was possible by exploiting the platform's modular architecture. TechnoSat achieved all its mission objectives within the nominal mission time and is now used within its extended mission duration primarily to test and demonstrate capabilities for the upcoming missions. • We introduce a highly modular satellite platform architecture. • The platform's first mission is a 20 kg technology demonstration satellite. • Initial orbit results are presented to showcase the performance of the platform. • Thousands of images are taken to demonstrate attitude pointing and operations. [ABSTRACT FROM AUTHOR]

Triton, the largest Solar System satellite beyond Saturn, was probably captured from the Transneptunian population by Neptune. It is mainly covered by N 2 , CO, CO 2 , CH 4 and H 2 O in solid state and, except for H 2 O and CO 2 , these species are also present in gas phase. Sublimation and recondensation of the volatile species may lead to geographical and temporal variation on the surface composition, and could participate to the formation of complex chemical compounds formed from photochemistry occurring in the atmosphere (Krasnopolsky and Cruikshank, 1999) or from irradiation of N 2 : CH 4 : CO layers (Moore and Hudson, 2003). We present new near-IR observations performed at the VLT-ESO with SINFONI in 2010, 2011 and 2013, from which band depths, areas and positions of the main ice features are determined at different longitudes. We also re-reduce and re-analyze earlier data obtained during the last 20 years. Models based on the Hapke theory (Hapke, 1993) are developed to constrain the abundance, grain size, temperature, and state of mixing of the different ices (N 2 , CH 4 , CO, CO 2 , H 2 O) as well as attempt to identify other species. For this purpose, we present and use new optical constants of CO 2 measured at 35 and 54 K. Our analyses confirm the longitudinal variation of the N 2 and CO surface abundances previously evidenced, and suggest additional latitudinal and/or temporal variability of these two species. We confirm the presence of deep N 2 layers in which CO and CH 4 are diluted. In particular, we demonstrate that CO is present in diluted (as opposed to pure ice) form. In contrast, our models support the presence of small and longitudinally variable amounts of pure CH 4 ice, providing an explanation to the enhanced atmospheric CH 4 /N 2 ratio over expectations based on an ideal N 2 -CH 4 -CO mixture. They also suggest significant smaller particles of H 2 O and CO 2 than reported previously in Quirico et al. (1999), with CO 2 being probably distributed over a large area of the surface. We find that the 2.40 µm band is primarily due to 13 CO ice, with a telluric value of the 13 CO/ 12 CO ratio, and not to ethane. We infer a N 2 ice temperature of 37.5  ±  1K, suggesting that the atmospheric pressure over 2010–2013 was similar to that during the Voyager 1989 epoch. [ABSTRACT FROM AUTHOR]

Context. Taxonomy of trans-Neptunian objects (TNOs) and Centaurs has been made in previous works using broadband filters in the visible and near infrared ranges. This initial investigation led to the establishment of four groups with the aim to provide the mean colors of the different classes with possible links with any physical or chemical properties. However, this taxonomy was only made with the Johnson-Cousins filter system and the ESO J, H, Ks filters combination, and any association with other filter system is not yet available. Aims. We aim to edit complete visible to near infrared taxonomy and extend this work to any possible filters system. To do this, we generate mean spectra for each individual group, from a data set of 43 spectra. This work also presents new spectra of the TNO (38628) Huya, on which aqueous alteration has been suspected, and the Centaur 2007 VH305. Methods. To generate the mean spectra for each taxonomical group, we first averaged the data for each of the four taxonomical groups and checked that spectroscopic and photometric data were consistent according to their relative errors. Results. We obtained four complete spectra corresponding to the different classes from 0.45 to 2.40 microns. Our results based on spectroscopy are in good agreements with those obtained in photometry for the bluest (BB) and reddest (RR) objects. At the contrary, no clear patterns appear for the two intermediate groups (BR and IR). Both BR and IR mean-spectra are almost intermixed, probably due to the fact that part of these objects have not always clear affiliation to one particular taxonomical group. Conclusions. We provide mean spectra that could be used to edit colors in different filters system working in this wavelength range. This work clearly establish the mean spectra of the BB and RR group while the two other groups need probably further refinement. [ABSTRACT FROM AUTHOR]

Aims. Spectral analyses of trans-Neptunan objects (TNOs) and of the linked Centaurs, which are supposed to be among the most primitive minor bodies in the solar system, reveal some chemical and physical properties of their surface. To determine the surface composition of these objects and their surface evolution is essential for gaining clues on the conditions under which the solar system has been formed. Methods. Chemical composition and physical properties of the surface of three objects have been constrained by computing the depth of the absorption features of the spectra in the near-infrared, running spectral models based on radiative transfer theory in the [0.4-2.3] μm range, and analyzing new laboratory measurements of the spectral behavior of thin samples of H2O-CH3OH mixtures. Results. Our investigations allow us to confirm the presence of CH3OH ice on the surface of the Centaur (5145) Pholus and the resonant (55638) TNO 2002 VE95. It may also possibly be found on the classical TNO (120348) 2004 TY364. Our laboratory experiments indicate that the behavior of the methanol and water ice absorption bands is dependent on the ambient temperature and the dilution level of the mixture. These results also suggest that methanol may be diluted in water ice on the surface of the Centaur Pholus. Conclusions. Formation and destruction processes of methanol suggest that a part (at least) of the surface of these objects is younger than the solar system age. If confirmed, this shows that primordial ices could still be detected on the surface of objects that are submitted to irradiation and rejuvenation processes. [ABSTRACT FROM AUTHOR]

Aims. In the framework of a large program, we observed (55638) 2002 VE95 with the ESO-VLT telescope to better constrain its surface composition and to investigate the possible heterogeneity of the surface. Methods. We report new near-infrared observations performed in 2007 and 2008. Using the new constraints of the albedo obtained by Herschel Space Observatory observations, a surface model was computed using the complete set of spectra (from visible to the near-infrared) as well as those of the previous published data to investigate the surface composition properties of (55638) 2002 VE95. Results. The surface is heterogeneous. This red object is covered by different icy compounds, such as water (4-19%) and methanol (10-12%). Different organic compounds, such as titan and triton tholins seem also to be present in the surface. The amount of the components is different depending on the observed area. That methanol ice seems to be present mainly on very red surface favors the hypothesis that surfaces of very red objects are more primordial. [ABSTRACT FROM AUTHOR]

Abstract: We present new photometric and spectroscopic observations of the Pluto–Charon system carried out at the VLT-ESO (Chile) with two 8-m telescopes equipped with the FORS2, ISAAC and SINFONI instruments. The spectra were obtained in the 0.6–2.45μm range with a spectral resolution from 300 to 1500. The SINFONI data were obtained using adaptive optics, allowing a complete separation of the two bodies. We derive both objects’ magnitudes in the near infrared and convert them into albedo values. These first near infrared photometric data allow to adjust the different parts of Pluto’s spectrum, provided by the three instruments. We run spectral models in order to give chemical and physical constraints on the surface of Pluto and Charon. We discuss the dilution properties of the methane ice and its implications on Pluto’s surface. The heterogeneities of the pure and diluted methane ice on Pluto’s surface is also investigated. The high signal-to-noise level of the data and our analyses may support the presence of ethane ice on the surface of Pluto, which is one of the main products of the methane irradiation and photolysis. The analyses of the spectra of Charon suggest that the water ice is almost completely in its crystalline form and that the ammonia compound is hydrated on the surface of this satellite. [ABSTRACT FROM AUTHOR]

Abstract: Several different trans-neptunian objects have been studied in order to investigate their physical and chemical properties. New observations in the 1.1–1.4μm range, obtained with the ISAAC instrument, are presented in order to complete previous observations carried out with FORS1 in the visible and SINFONI in the near infrared. All of the observations have been performed at the ESO/Very Large Telescope. We analyze the spectra of six different objects (2003 AZ83, Echeclus, Ixion, 2002 AW197, 1999 DE9 and 2003 FY128) in the 0.45–2.3μm range with the model of Hapke (Hapke, B. [1981]. J. Geophys. Res. 86, 4571–4586) and the method of Shkuratov et al. (Shkuratov, Y., Starukhina, L., Hoffmann, H., Arnold, G. [1999]. Icarus 137, 235–246). Water ice is found on two objects, and in particular it is confirmed in its amorphous and crystalline states on 2003 AZ84 surface. Upper limits on the water ice content are given for the other four TNOs investigated, confirming previous results (Barkume, K.M., Brown, M.E., Schaller, E.L. [2008]. Astron. J. 135, 55–67; Guilbert, A., Alvarez-Candal, A., Merlin, F., Barucci, M.A., Dumas, C., de Bergh, C., Delsanti, A. [2009]. Icarus 201, 272–283). Whatever the absorption features in the near infrared, all objects but one exhibit a moderate red slope in the visible, as most TNOs and Centaurs. We discuss the implications of the presence of water ice and the probable sources of the red slope. [Copyright &y& Elsevier]

ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is planned for launch in 2026 in collaboration with the Israeli Space Agency and NASA. DESY will provide the UV camera, composed by the detector assembly located in the telescope focal plane and the remote electronics unit. The camera is composed out of four back-metallized CMOS Image Sensors (CIS) manufactured in the 4T, dual gain Tower process. As part of the radiation qualification of the camera, Single Event Effect (SEE) testing has been performed by irradiating the sensor with heavy ions at the RADEF, Jyvaskyla facility. Preliminary results of both Single Event Upset (SEU) and Single Event Latch-up (SEL) occurrence rate in the sensor are presented. Additionally, an in-orbit SEE rate simulation has been performed in order to gain preliminary knowledge about the expected effect of SEE on the mission. [ABSTRACT FROM AUTHOR]

Context. A number of bodies in the Solar System are characterized by dark surfaces, from carbonaceous asteroids to the enigmatic surface of Phobos and Deimos. Our understanding of the spectroscopic behavior of low-albedo surfaces remains incomplete. To improve the interpretation of remote sensing data, laboratory studies continue to serve as a pivotal tool for unveiling the physical state and composition of such surfaces. Aims. Several processes can be simulated in the laboratory, however, the preparation and analysis of a complex mixing of analog material is one of the most fundamental among them, while also being one of the most complex when multiple components are used. In this work, we aim to study how dark material mixed with basaltic material at different grain sizes can affect the spectroscopic features from the near- to mid- infrared (1.25–25 µm). Methods. Our sample set includes four series of basaltic mix (feldspar and pyroxene) at different grain sizes from <50 µm to 1000 µm, mixed with amorphous carbon at increasing weight percentages ranging from 1% to 50%. We analyzed several features on the spectrum of each mineral mixture. In particular, we investigated the behavior of the: (i) near-infrared slope; (ii) 2.7 µm OH-stretching band; (iii) Christiansen features; and (iv) Reststrahlen band and Transparency feature. Results. The measurements presented in this work, which take into account a large wavelength range for the first time, point toward a critical effect of dark material, but with a different outcomes for each grain size. Some of the most interesting results involve the slope trend of modification with dark material and the variant behavior of the Reststrahlen band and Transparency feature. Conclusions. This dataset will offer a key support in the interpretation of data collected on dark surfaces by past and future space missions. This knowledge will be also important in the context of linking analyses of returned samples with remote sensing data collected on planetary surfaces. [ABSTRACT FROM AUTHOR]

A letter to the editor is presented regarding the flare-up of discoid lupus erythematosus (DLE)-like lesions in a 58-year-old female patient due to capecitabine.

The dwarf planet (136472) Makemake is one of the largest trans-Neptunian objects discovered to date. Noteworthy, the size and surface temperature of this celestial body put it in a transition region where nitrogen is preferentially lost, while the less volatile methane is retained. Indeed, literature spectra clearly show that the surface of Makemake is dominated by methane ice, though the presence of nitrogen and of irradiation products of methane has been inferred by several authors and a debate is still open about the eventual rotational variability of the surface composition. In this work, we present new visible and near-infrared spectra of Makemake obtained with the TNG telescope (La Palma, Spain) in the time span 2006-2013. Our data sample different rotational phases, covering about 80 per cent of the surface. All of the obtained spectra look very similar, suggesting an overall homogeneous composition. No secular variations appear when comparing our data to literature results (as expected, considering the quite short orbital arc travelled by Makemake since its discovery in 2005). The presence of methane diluted in nitrogen is evidenced by the shift of the observed absorption bands with respect to those of pure methane, with a dilution state looking homogeneous over the surface. We modelled a complete visible and near-infrared spectrum ofMakemake using the Shkuratov formalism, and found that adding irradiation products of methane like ethane and ethylene seems indeed improving the fit of the synthetic spectrum to our data. We found no hints of a localized/temporary atmosphere. [ABSTRACT FROM AUTHOR]

The dwarf planet (136472) Makemake is one of the largest trans-Neptunian objects discovered to date. Noteworthy, the size and surface temperature of this celestial body put it in a transition region where nitrogen is preferentially lost, while the less volatile methane is retained. Indeed, literature spectra clearly show that the surface of Makemake is dominated by methane ice, though the presence of nitrogen and of irradiation products of methane has been inferred by several authors and a debate is still open about the eventual rotational variability of the surface composition. In this work, we present new visible and near-infrared spectra of Makemake obtained with the TNG telescope (La Palma, Spain) in the time span 2006-2013. Our data sample different rotational phases, covering about 80 per cent of the surface. All of the obtained spectra look very similar, suggesting an overall homogeneous composition. No secular variations appear when comparing our data to literature results (as expected, considering the quite short orbital arc travelled by Makemake since its discovery in 2005). The presence of methane diluted in nitrogen is evidenced by the shift of the observed absorption bands with respect to those of pure methane, with a dilution state looking homogeneous over the surface. We modelled a complete visible and near-infrared spectrum of Makemake using the Shkuratov formalism, and found that adding irradiation products of methane like ethane and ethylene seems indeed improving the fit of the synthetic spectrum to our data. We found no hints of a localized/temporary atmosphere. [ABSTRACT FROM AUTHOR]

several authors and a debate is still open about the eventual rotational variability of the surface composition. In this work, we present new visible and near-infrared spectra of Makemake obtained with the TNG telescope (La Palma, Spain) in the time span 2006-2013. Our data sample different rotational phases, covering about 80 per cent of the surface. All of the obtained spectra look very similar, suggesting an overall homogeneous composition. No secular variations appear when comparing our data to literature results (as expected, considering the quite short orbital arc travelled by Makemake since its discovery in 2005). The presence of methane diluted in nitrogen is evidenced by the shift of the observed absorption bands with respect to those of pure methane, with a dilution state looking homogeneous over the surface. We modelled a complete visible and near-infrared spectrum of Makemake using the Shkuratov formalism, and found that adding irradiation products of methane like ethane and ethylene seems indeed improving the fit of the synthetic spectrum to our data. We found no hints of a localized/temporary atmosphere. [ABSTRACT FROM AUTHOR]

We present new results of the observing program which is a part of the NEOROCKS project aimed to improve knowledge on physical properties of near-Earth Objects (NEOs) for planetary defense. Photometric observations were performed using the 1.2-m telescope at the Haute-Provence observatory (France) in the BVRI filters of the Johnson–Cousins photometric systems between June 2021 and April 2022. We obtained new surface colours for 42 NEOs. Based on the measured colours, we classified 20 objects as S-complex, nine as C-complex, nine as X-complex, two as D-type, one object as V-type, and one object remained unclassified. For all the observed objects, we estimated their absolute magnitudes and diameters. Combining these new observations with the previously acquired data within the NEOROCKS project extended our data set to 93 objects. The majority of objects in the data set with diameters D < 500 m belongs to a group of silicate bodies, which could be related to observational bias. Based on MOID and Δ V values we selected 14 objects that could be accessible by a spacecraft. Notably, we find D-type asteroid (163014) 2001 UA5 and A-type asteroid 2017 SE19 to be of particular interest as possible space mission targets. [ABSTRACT FROM AUTHOR]

The number of artificial objects in space increases due to past and present space activities. To analyse the quantity of the small (diameter >100 μm up to cm) space debris and meteoroids, an innovative in-situ impact detection method has been developed at DLR (German Aerospace Center) in Bremen, Germany. The method Solar panel-based Impact Detector "SOLID" uses solar panels for impact detection. Since solar panels provide large detection areas and exist on nearly all satellites, this method enables for the collection of large amounts of data in different orbits. An impacting object generates a permanent damage on a panel. The damage can be determined during analysis scan as well as confirmed or refuted in the frame of subsequent scans of the panels. Those properties of the sensor system can significantly improve the amount as well as the quality of measurement data to be used for environmental model validation. The SOLID method was successfully verified on ground by Hypervelocity Impact (HVI) tests at Fraunhofer EMI, Freiburg, Germany. The ability of the detection method SOLID for impact detection of space debris and meteoroids was clearly demonstrated on ground. Since July 2017, the SOLID sensor system is placed in a 600 km Sun-synchronous orbit on the microsatellite mission TechnoSat of Technische Universität Berlin (TUB). Four solar panels equipped with SOLID technology are installed on the satellite for in-orbit testing and environmental exploration. The total detection area of all panels is about 0.0755 m2. The system was designed to detect space debris or meteoroid objects with a diameter larger than 100 μm. In total 15,570,047 scans were performed over the four years in space. By means of measurement data changes were identified on one panel. However, so far, the telemetry data shows no clear evidence for an impact. • Development of a large area in-situ debris and meteoroid detector SOLID. • In orbit testing of in-situ debris and meteoroid detector SOLID. • Interpretation of in-situ measurement data. • Estimation of expected impacts using environmental model MASTER 8. • Environmental models validation by utilization of measured data. [ABSTRACT FROM AUTHOR]

Aims. We present new near-infrared spectra of the leading and trailing hemispheres of Uranus's icy satellite Miranda. This body is probably the most remarkable of all the satellites of Uranus, because it displays series of surface features such as faults, craters, and large-scale upwelling, a remnant of a geologically very active past. Methods. The observations were obtained with PHARO at Palomar and SpeX at the IRTF Observatory. We performed spectral modelings to further constrain the nature and the chemical and physical states of the compounds possibly present on the surface of Miranda. Results. Water ice signatures are clearly visible in the H and K bands, and it appears to be found in its crystalline state over most of the satellite's surface. Unlike what has been found for Uranus's outer moons, we did not find any significative differences in the abundances of ices covering the leading and trailing hemispheres of Miranda. The signature of carbon dioxide cannot be seen in our spectra, which could still account for the presence of ammonia hydrate, though in small amounts. [ABSTRACT FROM AUTHOR]

In this work, we aim to investigate the presence of absorption bands around 3.4 μm in the infrared spectra of primitive asteroids. We collected the published reflectance spectra of low-albedo asteroids from the literature and analysed the 2.4–3.8 μm region using the same techniques. From the initial data set of 92 asteroids, we restricted our analysis to 42 spectra of low-albedo asteroids with a good signal-to-noise (S/N) ratio, and we found the absorption feature around 3.4 μm in the spectra of 16 objects. For objects that are classified by the 3 μm band into the 'rounded', Ceres-like, and Europa-like groups, the depth of the 3.4 μm feature is strongly correlated with that of the 3 μm band. The majority of objects in our data set not showing the 3.4 μm absorption band have lower S/N spectra and belong to Ch or Chg classes, while asteroids with a detected 3.4 μm bands mostly belong to C, B, and also P types. Additionally, asteroids with a detected 3.4 μm band tend to have a lower albedo, redder J-K colours, and more neutral U-V colours. We observe that the analysed objects larger than ∼300 km in diameter show features due to carbon-bearing materials, which could be explained by their higher S/N ratio in our data set. Finally, we found that the distributions of asteroids showing the 3.4 μm feature appear to be shifted towards larger distances from the Sun compared to those not showing this band. [ABSTRACT FROM AUTHOR]

Abstract: A Large Program (LP) has been carried out at ESO–VLT using almost simultaneously the UT1, UT2 and UT4 telescopes (Cerro Paranal, Chile). The aim of this Large Program was to obtain simultaneous visible and near-IR spectroscopic measurements (using FORS, ISAAC and SINFONI instruments) with a S/N ratio as high as possible for almost all objects among different dynamical groups observable within the VLT capability. In this paper we present results on the second half of the Large Program which includes new near-infrared spectroscopy data of 20 objects. For 12 of them for which we had obtained the complete spectral range (V+J+H+K bands), we apply a radiative transfer model to the entire spectral range to constrain their surface composition. We also present an analysis of all near-IR spectral data available on TNOs and Centaurs from both the complete LP and the literature. An overview for a total sample of 75 objects is thus carried out analyzing the ice content with respect to the physical and dynamical characteristics. The major new results are: (i) all objects classified as BB class seem to have icy surfaces; (ii) the possible presence of CH3OH has primarily been detected on very red surfaces (RR class objects) and (iii) the majority of Centaurs observed multiple times have an heterogeneous composition. [Copyright &y& Elsevier]

Abstract: Comet 133P/Elst-Pizarro, known to be a main-belt asteroid with a cometary activity, was observed with the near-infrared integral field spectrograph SINFONI at the 8.2-m Very Large Telescope in J, H, and K bands during its 2007 perihelion passage. The goal of these observations was to attempt detection of water ice absorption bands. We present here the details of the data processing, the results of these observations, and our compositional modeling of the final spectrum. No water ice absorptions were detected within the noise of the spectrum but we show that this spectrum is compatible with a reasonable near-infrared albedo value of 7–10% and a mixture of water ice, black carbon, Tholin and silicates. This interpretation, nevertheless, is not unique. [ABSTRACT FROM AUTHOR]

Background and aims: Inflammatory bowel diseases (IBD), including Crohn's disease (CD) and ulcerative colitis (UC), are complex genetic disorders. CARD15/NOD2, a member of the Ced4 superfamily which includes Apaf-1 and CARD4/NOD1, has recently been associated with genetic predisposition to CD but additional genetic factors remain to be identified. Because CARD4/NOD1 shares many structural and functional similarities with CARD15, we tested its putative role in IBD. Patients and methods: The 11 exons of CARD4 were screened for the presence of variants in 63 unrelated IBD patients. The only non-private genetic variation encoding for a substitution in the peptidic chain was genotyped in 381 IBD families (235 CD, 58 UC, 81 mixed, and seven indeterminate colitis families) using a polymerase chain reaction-restriction fragment length polymorphism procedure. Genotyping data were analysed by the transmission disequilibrium test. Results: Five of nine sequence variations identified in the coding sequence of the gene encoded for non-conservative changes (E266K, D372N, R705Q, T787M, and T787K). Four were present in only one family. The remaining variant (E266K), which exhibited an allele frequency of 0.28, was not associated with CD, UC, or IBD. Furthermore, IBD patients carrying sequence variations in their CARD4 gene had a similar phenotype to those with a normal sequence. Conclusion: Our results suggest that CARD4 does not play a major role in genetic susceptibility to IBD. [ABSTRACT FROM AUTHOR]

We present the results of the first-ever visible spectroscopic survey fully dedicated to the small (absolute magnitude H ≥ 20) near-Earth asteroid (NEA) population. Observations have been performed at the New Technology Telescope (NTT) of the European Southern Observatory (ESO), during a 30-night Guaranteed Time Observations programme, in the framework of the European Commission financed NEOShield-2 project. The visible spectra of 147 objects have been obtained and taxonomically classified. They show a peculiar taxonomic distribution, with respect to larger NEAs. In particular, olivine-rich A-types and organic-rich D-types are more abundant than what could be expected by extrapolating the taxonomic distribution of larger NEAs. Such results have implications for the investigation of the first phases of solar system history, including the delivery of prebiotic material on the early Earth. Having been obtained over a large range of solar phase angles, our data allowed us to evidence peculiar phase reddening behaviours for asteroids belonging to different taxonomic types. Low-albedo asteroids display no or limited phase reddening, compared to moderate- and high-albedo objects. This result suggests a promising novel way to distinguish primitive asteroids in the X-complex. In agreement with previous laboratory experiments, olivine-rich surfaces are the most affected by phase reddening. [ABSTRACT FROM AUTHOR]

In the framework of the Near Earth Objects (NEOs) observational campaign carried out within the NEOShield-2 project, we identify nine new small D-type asteroids with estimated diameter less than 600 m. The link with meteorites for this class of asteroids is weak and the best fit obtained is with the Tagish Lake meteorite for seven of them. D-type asteroids are believed to contain the most pristine material of the Solar system and could have delivered the prebiotic material to the Earth. Our results double the known sample of the D-types in the NEO population and triple the candidates of this class for a sample-return mission (at very low ΔV). Our finding increases considerably the number of targets for sample-return mission. A sample-return mission to a D-type asteroid will provide a major progress in understanding the early history of the Solar system and to investigate the origin of life on the Earth. [ABSTRACT FROM AUTHOR]

ULTRASAT (ULtraviolet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform deep time-resolved surveys in the near-ultraviolet spectrum. ULTRASAT is a space mission led by the Weizmann Institute of Science and the Israel Space Agency and is planned for launch in 2025. The camera implements backside-illuminated, stitched pixel sensors. The pixel has a dual-conversion-gain 4T architecture, with a pitch of 9.5 μ m and is produced in a 180 nm process by Tower Semiconductor. Before the final sensor was available for testing, test sensors provided by Tower were used to gain first insights into the pixel's radiation tolerance. One of the main contributions to sensor degradation due to radiation for the ULTRASAT mission is Total Ionizing Dose (TID). TID measurements on the test sensors have been performed with a Co-60 gamma source at Helmholz Zentrum Berlin and CC-60 facility at CERN and preliminary results are presented. [ABSTRACT FROM AUTHOR]

We present an analysis of the colors available for seven trans-neptunian objects (TNOs) and three centaurs among the reddest known, aimed at characterizing their surface chemical properties. In particular we seek to obtain evidence in support of the proposed correlation between the visible coloration of the surface of TNOs and their surface compositions (Brown, M.E., Schaller, E.L., Fraser, W.C. [2011]. Astrophys. J. 739, L60). The analysis focuses on nine available colors in the visible–near IR (0.3–4.5 μm) spectral range scaled to the V albedo to provide a proxy for the spectral shape of the objects. The colors include Spitzer IRAC data never published before, key in providing an effective constraint in the discrimination of ices contributing to the surface composition of the objects. Compositions are obtained by comparing the data to a grid of radiative transfer models convolved by the filter response functions of the colors adopted in the spectrum-proxies to match the resolution of the observations. We find evidence suggesting the presence of hydrocarbons and/or methanol on the surfaces of most objects in our sample, supporting the hypothesis by Brown et al. (Brown, M.E., Schaller, E.L., Fraser, W.C. [2011]. Astrophys. J. 739, L60) that the coloration of red TNOs could be linked to their methanol content. From our finding of methanol/hydrocarbon ices on the surfaces of the objects in our sample of very red TNOs and centaurs we infer that ultra-red objects in general might contain these ices and therefore might have formed in the outer part of the Solar System. We also deduce that the surfaces of most of the very red TNOs in our dataset are probably still quite pristine, and that their organic materials could have been produced by irradiation of the volatile ices whose traces are still present on their surface. Although our sample is small, we infer that the irradiation process is still in progress, as hinted by the centaurs’ slightly elevated organic amounts at smaller perihelion distances. However, considering the relatively similar amounts of organics found in our data at a wide variety of perihelion distances, we also infer that it could have started before Neptune’s migration. The technique used to constrain the composition described as part of this study introduces a new approach at investigating the surface chemistry of the very small and numerous objects that constitute the bulk of the TNO and centaur populations. This innovative method has the potential to provide constraints for irradiation theories and for models of dynamical and chemical evolution of the Solar System. [ABSTRACT FROM AUTHOR]

Abstract: The Deep Impact spacecraft flew by Comet 103P/Hartley 2 on November 4th, 2010 (EPOXI mission) and Comet 9P/Tempel 1 on July 4th, 2005 (Deep Impact mission). During the two flybys, spatially resolved infrared (1.05–4.8μm) spectra of the surface of the nucleus were acquired by the HRI-IR instrument. The analysis of these two data sets, obtained by the same instrument, offers a unique opportunity to understand, compare and contrast the surface thermal properties of these two comets. For this paper, we use spectral cubes with a spatial resolution of 30m/pixel to 40m/pixel for Hartley 2 and 160m/pixel for Tempel 1. We focus our analysis on the color, temperature, thermal inertia and roughness of the nucleus. The two comets have the same color, moderately red, with an average slope of 3.0±0.9% per kÅ to 3.5±1.1% per kÅ. There are very small variations of the color across the surface, except for regions with water ice that are neutral to blue, and two dark spots with redder (4.5±1.4% per kÅ) materials on Hartley2. The nucleus thermal emission at all resolved spatial scales differs from that of a gray body with an infrared emissivity of 0.9–1.0, the discrepancy being more important for larger incidence angles. Moreover, the color temperature of Comets Hartley 2 and Tempel 1 is relatively homogeneous across the surface and does not vary strongly with incidence angle. These two effects mainly result from surface roughness and associated projected shadows. From the temperature rise on the morning terminator, we derive a thermal inertia lower than 250W/K/m2/s1/2 for Hartley2 and lower than 45W/K/m2/s1/2 for Tempel1 (3σ upper limits). For Hartley2 and Tempel1, the temperature of the regions with exposed water ice is more than 100K above the sublimation temperature of water ice (∼200K). This observation indicates that the thermal emission is dominated by dust, and that water ice is not intimately mixed with dust at the scale of observation, with water ice patches at the meter or sub-meter scale. [Copyright &y& Elsevier]

Neptune's moon Triton shares many similarities with Pluto, including volatile cycles of N 2 , CH 4 and CO, and represents a benchmark case for the study of surface-atmosphere interactions on volatile-rich Kuiper Belt objects. The observations of Pluto by New Horizons acquired during the 2015 flyby and their analysis with volatile transport models (VTMs) shed light on how volatile sublimation-condensation cycles control the climate and shape the surface of such objects. Within the context of New Horizons observations as well as recent Earth-based observations of Triton, we adapt a Plutonian VTM to Triton, and test its ability to simulate its volatile cycles, thereby aiding our understanding of its climate. Here we present numerical VTM simulations exploring the volatile cycles of N 2 , CH 4 and CO on Triton over long-term and seasonal timescales (cap extent, surface temperatures, surface pressure, sublimation rates) for varying model parameters (including the surface ice reservoir, albedo, thermal inertia, and the internal heat flux). We explore what scenarios and model parameters allow for a best match of the available observations. In particular, our set of observational constraints include Voyager 2 observations (surface pressure and cap extent), ground-based near-infrared (0.8–2.4 μm) disk-integrated spectra (the relative surface area of volatile vs. non-volatile ice) and the evolution of surface pressure as retrieved from stellar occultations. Our results show that Triton's poles act as cold traps for volatile ices and favor the formation of polar caps extending to lower latitudes through glacial flow or through the formation of thinner seasonal deposits. As previously evidenced by other VTMs, North-South asymmetries in surface properties can favor the development of one cap over the other. Our best-case simulations are obtained for a bedrock surface albedo of 0.6–0.7, a global reservoir of N 2 ice thicker than 200 m, and a bedrock thermal inertia larger than 500 SI (or smaller but with a large internal heat flux). The large N 2 ice reservoir implies a permanent N 2 southern cap (several 100 m thick) extending to the equatorial regions with higher amounts of volatile ice at the south pole, which is not inconsistent with Voyager 2 images but does not fit well with observed full-disk near-infrared spectra. Our results also suggest that a small permanent polar cap exists in the northern (currently winter) hemisphere if the internal heat flux remains relatively low (e.g. radiogenic, < 3 mW m−2). A non-permanent northern polar cap was only obtained in some of our simulations with high internal heat flux (30 mW m−2). The northern cap will possibly extend to 30°N in the next decade, thus becoming visible by Earth-based telescopes. On the basis of our model results, we also discuss the composition of several surface units seen by Voyager 2 in 1989, including the bright equatorial fringe and dark surface patches. Finally, we provide predictions for the evolution of ice distribution, surface pressure and CO and CH 4 atmospheric mixing ratios in the next decades. According to our model, the surface pressure should slowly decrease but remain larger than 0.5 Pa by 2060. We also model the thermal lightcurves of Triton for different climate scenarios in 2022, which serve as predictions for future James Webb Space Telescope observations. • Results suggest large global N 2 reservoir (>200 m) and thermal inertia (>500 SI or smaller if internal heat flux >30 mW m−2). • Results suggest a permanent N 2 southern cap (100 m to 1.5 km thick) extending to the equator with max. thickness at the pole. • Results suggest a small permanent polar cap should exist in the northern hemisphere, and could extend to 30°N by 2030. • Modeled surface pressures are consistent with a moderate increase of pressure during the 1990-2000 period. • JWST/MIRI will help in discriminating climate scenarios and in providing constraints on thermal/energetic surface properties. [ABSTRACT FROM AUTHOR]

OBJECTIVES:Infl ammatory bowel disease (IBD), e.g., Crohn's disease (CD) and ulcerative colitis (UC), is a complex genetic disorder. Tumor necrosis factor (ligand) superfamily, member 15 (TNFSF15) has been previously identified as a susceptibility gene for CD in Japanese and UK cohorts. This replication study was designed in order to confirm and further validate the role of TNFSF15 in IBD.METHODS:A total of 666 IBD families (corresponding to 2,982 relatives) with European ancestry were genotyped for the rs6478108 and rs7869487 polymorphisms, which define the main TNFSF15 haplotypes previously associated with CD. An association between the main haplotypes and CD, UC and IBD was tested using the Genehunter TDT and Unphased statistics. Caspase recruitment domain 15 (CARD15)/TNFSF15 interaction and genotype/phenotype correlations were also studied.RESULTS:The previously reported “high-risk” haplotype (A) was associated with IBD (P=0.001) (OR=1.25 (1.05–1.50)) and CD (P=0.02) (OR=1.31 (1.03–1.67)) whereas the “protective” (B) haplotype was significantly less transmitted to IBD and CD patients. No interaction between CARD15 and TNFSF15 was detected. We also failed to define a clinical subgroup of CD patients specifically associated with TNFSF15 haplotype A.CONCLUSIONS:This study confirms that TNFSF15 or a closely linked gene is involved in the genetic predisposition to CD.Am J Gastroenterol 2009; 104:384–391; doi:10.1038/ajg.2008.36; published online 13 January 2009 [ABSTRACT FROM AUTHOR]

Asteroids were likely a major source of volatiles and water to early Earth. Quantifying the hydration of asteroids is necessary to constrain models of the formation and evolution of the Solar System and the origin of Life on Earth. The OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer) mission showed that near-Earth asteroid (101955) Bennu contains widespread, abundant hydrated phyllosilicates, indicated by a ubiquitous absorption at ~ 2.7 μm. The objective of this work is to quantify the hydration—that is, the hydrogen content—of phyllosilicates on Bennu's surface and investigate how this hydration varies spatially. We analyse spectral parameters (normalized optical path length, NOPL; effective single-scattering albedo, ESPAT; and Gaussian modeling) computed from the hydrated phyllosilicate absorption band of spatially resolved visible–near-infrared spectra acquired by OVIRS (the OSIRIS-REx Visible and InfraRed Spectrometer). We also computed the same spectral parameters using laboratory-measured spectra of meteorites including CMs, CIs, and the ungrouped C2 Tagish Lake. We estimate the mean hydrogen content of water and hydroxyl groups in hydrated phyllosilicates on Bennu's surface to be 0.71 ± 0.16 wt%. This value is consistent with the hydration range of some aqueously altered meteorites (CMs, C2 Tagish Lake), but not the most aqueously altered group (CIs). The sample collection site of the OSIRIS-REx mission has slightly higher hydrogen content than average. Spatial variations in hydrogen content on Bennu's surface are linked to geomorphology, and may have been partially inherited from its parent body. • Hydrated phyllosilicate OH−, H 2 O hydrogen (H) content is estimated. • First spatially resolved H content quantified, on asteroid (101955) Bennu. • H content variation is associated with asteroid Bennu geomorphology. • Bennu mean H content is similar to CMs and Tagish Lake. • Our results will be compared to Bennu's samples. [ABSTRACT FROM AUTHOR]

Using data acquired by the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer) mission, we investigate spectral properties of craters on the near-Earth asteroid (101955) Bennu. We compare Bennu's craters with its global average by means of four spectral parameters: (a) minimum position of the band at 2.7 μ m, (b) depth of the hydrated phyllosilicate absorption band at 2.7 μ m, (c) normalized spectral slope from 0.55 to 2.0 μ m, and (d) reflectance factor at 0.55 μ m. We examine 45 craters using spectral data obtained under various observing conditions. For 20 craters, we find a shortward shift of the 2.7- μ m band minimum relative to the global 2.7- μ m band minimum, which we attribute to the presence of relatively fresh (less space-weathered) material excavated from the sub-surface by crater-forming impacts. For three craters, we find an anti-correlation between spectral slopes and reflectance factor for a series of spectra acquired during a specific scan, where we observe that spectra become redder and darker towards the center of the crater. We attribute this to the presence of fine-particulate regolith. Localized spectral heterogeneities are apparent inside a prominent equatorial crater on Bennu, which is one of the asteroid's oldest geological features. We propose that such local spectral heterogeneities could be used as a tracer of mass movement on Bennu. We show that younger craters are redder, brighter, and have deeper 2.7- μ m bands. Comparing global average spectral values of Bennu and crater frequency distributions as a function of the chosen spectral parameters, we find that craters evolve to assume the global average spectral properties of Bennu. A positive correlation identified between the reflectance factor and 2.7- μ m band depth suggests that brighter craters tend to be more hydrated. Finally, we put into context, the results from the Small Carry-on Impactor experiment by the Hayabusa2 spacecraft, which created an artificial crater on the near-Earth asteroid (162173) Ryugu. • The shortward shift of the 2.7-μm band inside craters indicates the presence of freshly excavated sub-surface material. • A scan-dependentant anti-correlation between REFF0.55 μm and spectral slopes hints at the presence of fine particulates. • Younger craters are brighter and have deeper 2.7-μm hydration bands and redder spectral slopes. • Nightingale crater, the primary sample site of the OSIRIS-REx mission, is the reddest and the darkest crater [ABSTRACT FROM AUTHOR]

Presents a letter to the editor related to gene mutation.