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Highlights • We derived vertically-resolved spectral structures of Saturnian polar haze between 375 and 925 km altitude. • The polar haze is dominated by aromatic hydrocarbons. • The haze at lower latitudes mostly consists of aliphatic hydrocarbons. • There is a possibility that the aging process of haze can occur during both horizontal and vertical migrations. Abstract We analyzed the 3-µm emission spectra of Saturn's southern auroral atmosphere observed by the Visual Infrared Mapping Spectrometer (VIMS) on-board Cassini. Extracting adjacent 3-µm H 3 + , CH 4 , and C 2 H 6 emissions, we derived vertically-resolved spectral structures of polar haze between 375 and 925 km altitude. A comparison of the derived polar haze spectra with those of the relatively low-altitudinal (257–520 km) and low-latitudinal haze reported by Kim et al. (2012) indicates that the polar haze is dominated by aromatic hydrocarbons while the haze at lower latitudes mostly consists of aliphatic hydrocarbons. This spectral and chemical variation in the different latitudinal regions suggests a possibility that newly created haze particles at the high altitudes in the auroral regions of Saturn undergo an aging process during latitudinal advection and diffusion from the polar atmosphere to the low altitude and low latitudinal regions, while in the atmosphere of Titan, the aging process occurs during the vertical precipitation process of haze (Courtin et al., 2015a). However, there is a possibility that the aging process can occur during both the horizontal and vertical migrations. Thus, further investigation of the 3-µm spectral structure of the high-altitude haze (>520 km) at low latitudes is needed. [ABSTRACT FROM AUTHOR]

We have derived homopause temperatures of 180–250 K for the 8-µm north-polar hot spot (8NPHS) of Jupiter by fitting CH 4 emission models to 3 and 8 µm spectra of the 8NPHS obtained 24 days apart in 2013. From the fits, we find that CH 4 mixing ratios at the 8NPHS are consistent with those reported by Kim et al. (2014) in equatorial regions. We propose possible mechanisms to account for the temperature of the 8NPHS homopause, which is relatively cool compared with the temperatures of other auroral regions, including locally-fixed and transient but energetic auroral particle precipitation. [ABSTRACT FROM AUTHOR]

We have obtained 3.3–3.4-μm spectro-images of Jupiter including CH 4 and H 3 + emission lines from both polar regions at the Gemini North telescope. We find that the peak of the 3-μm CH 4 northern bright spot is located at ∼200° (SysIII) longitude, ∼20° west of the center of the 8-μm north-polar bright spot, and does not coincide with the 3-μm H 3 + bright spot. We derive high temperatures (500–850 K) from CH 4 rotational lines on the bright spots of both polar regions, above the 1-μbar pressure level, while we find cooler temperatures (<350 K) over the 8-μm spot. The intensity ratios of the various 3-μm vibrational bands of CH 4 are roughly constant, indicating that the upper states of these bands are mostly populated by non-thermal excitation mechanisms, such as auroral particle precipitation and/or Joule heating, in contrast with the 8-μm thermal emission. [ABSTRACT FROM AUTHOR]

Abstract: We have reanalyzed the high-resolution spectrum of Titan between 2.87 and 3.12 μm observed with NIRSPEC/Keck II on 2001 Nov. 21 in southern summer, using updated CH3D and C2H6 line-by-line models. From new synthetic spectra, we identify all but a few of the previously unidentified significant absorption spectral features in this wavelength range as due to these two species, both of which had been previously detected by Voyager and ground-based observations at other wavelengths. We also derive opacities and reflectivities of haze particles as functions of altitude for the 2.87–2.92 μm wavelength range, where Titan''s atmosphere is partially transparent down to the surface. The extinction per unit altitude is observed to increase from 100 km (∼8 mbar) toward lower altitude. The derived total optical depth is approximately 1.1 for the 2.87–2.92 μm range. At wavelengths increasing beyond 2.92 μm the haze layers become much more optically thick, and the surface is rapidly hidden from view. These conclusions apply to equatorial and southern-temperate regions on Titan, excluding polar regions. We also find it unlikely that there is a large enhancement of the tropospheric CH4 mole fraction over the value reported from analysis of the Huygens/GCMS observations. [Copyright &y& Elsevier]

We have obtained Gemini/GNIRS 3.3–3.4 μm spectra of Jupiter at 65o North latitude over a range of longitudes roughly centered on the 8-μm CH 4 north polar hot spot (8CNPHS). The spectra were measured on four occasions during a four-month period in 2018, in order to search for variability of the 3-μm emissions of CH 4 and C 2 H 6. The observed locations of the brightest spots of the C 2 H 6 and CH 4 emissions at 65oN differed in longitude typically by 20o during this period. The peak emission intensities of these species showed large variations, with the highest intensities 3–4 times greater than the lowest intensities. In addition, the brightest 3-μm CH 4 emissions and hottest temperatures at the 8CNPHS were significantly less than those at the 3-μm CH 4 north polar hot spot (3CNPHS, Kim et al., 2015). Recently, Sinclair et al. (2019) reported a coincidence between solar wind dynamical pressure and the 8-μm brightening of the 8CNPHS. In contrast, we find lack of correlation in our data between the 3-μm hydrocarbon emission intensities at the 8CNPHS and the solar wind strength. We also find lack of correlation between H 3 + intensities and the solar wind strength during the period. However, due to the limited observational data, it is too early to conclude whether this lack of correlation indicates that the solar wind activity induced no significant changes in local temperatures (<40 K) and/or mixing ratios of these molecules. Our observing period was close to the historic grand solar minimum. The detailed influence of the solar activity on the 3 and 8 μm brightness at the 8CNPHS is not quantitatively understood at the present time. • Gemini/GNIRS 3.3–3.4 μm spectra of the 8-μm CH 4 north polar hot spot (8CNPHS) of Jupiter were obtained. • Four occasions during a five-month period in 2018 were observed. • The variability of the 3-μm emission intensities of CH 4 , C 2 H 6 , and H 3 + was studied. • The peak intensities of these species showed the highest 3–4 times greater than the lowest. • We find lack of correlation between the 3-μm hydrocarbon intensities at the 8CNPHS and the solar wind strength. [ABSTRACT FROM AUTHOR]

We have analyzed spectroscopic observations of Titan performed in January 1997 by the Short Wavelength Spectrometer (SWS) on the Infrared Space Observatory in the wavelength range from 5.3 to 7.0 μm (1422–1890 cm −1 ). This spectral interval is of particular interest because it contains various molecular transitions, particularly the ν 2 band of CH 4 and the ν 8 band of C 2 H 6 , as well as a spectral feature characteristic of the laboratory analogs of Titan’s haze—or tholins—which have been studied for decades. In addition, this region is expected to show the transition between the thermal emission and reflected sunlight regimes of Titan’s atmospheric radiation around 6 μm. All these features are indeed observed in the SWS spectrum, for the first time in the case of the ν 2 band of CH 4 at 6.5 μm. We present a radiative transfer model of these observations from which we derive the extinction cross section of the haze particles at 140 ± 20 km altitude. This result complements similar determinations recently obtained at shorter and longer wavelengths from Cassini VIMS and CIRS measurements, although large uncertainties still remain at 1700–1800 cm −1 , as well as a gap at 1800–2000 cm −1 . A comparison between the available extinction cross section determinations for the Titan haze and those derived for laboratory-synthesized tholins, from the near- to the far-infrared, shows some similarities but also striking discrepancies, thus reinforcing the idea that there is not a unique tholin analogue to the Titan haze material. [ABSTRACT FROM AUTHOR]

Using the LACE data from Apollo 17 we have found measured neon densities consistent with the 20Ne surface number densities reported by Cook et al. (2013) for normal conditions, terminator surface densities of 3 (±1.5) × 103 cm−3. These values are almost an order of magnitude less than those reported by Benna et al. (2015) for CME conditions. Using a Monte Carlo model and assuming the normal solar wind and a photoionization lifetime for Ne of 300 days, our result was more consistent with the Benna (2015) result than our measured result. Two lunations showed an increase in Ne during the night, consistent with the simulation, but two of the lunations showed a decrease in surface number density through the night. We have shown that explaining the Ne distribution is not as simple as assuming dynamic equilibrium with the solar wind and an exosphere accommodated to the local surface temperature. • LACE data from Apollo 17 have been reanalyzed. • The 20Ne nightside surface number densities are 3 (±1.5) × 103 cm−3. • Ne cannot be modeled assuming dynamic equilibrium with the solar wind. [ABSTRACT FROM AUTHOR]

Background The use of different 3D T1-weighted magnetic resonance (T1 MR) imaging protocols induces image incompatibility across multicenter studies, negating the many advantages of multicenter studies. A few methods have been developed to address this problem, but significant image incompatibility still remains. Thus, we developed a novel and convenient method to improve image compatibility. Methods W-score standardization creates quality reference values by using a healthy group to obtain normalized disease values. We developed a protocol-specific w-score standardization to control the protocol effect, which is applied to each protocol separately. We used three data sets. In dataset 1, brain T1 MR images of normal controls (NC) and patients with Alzheimer’s disease (AD) from two centers, acquired with different T1 MR protocols, were used (Protocol 1 and 2, n = 45/group). In dataset 2, data from six subjects, who underwent MRI with two different protocols (Protocol 1 and 2), were used with different repetition times, echo times, and slice thicknesses. In dataset 3, T1 MR images from a large number of healthy normal controls (Protocol 1: n = 148, Protocol 2: n = 343) were collected for w-score standardization. The protocol effect and disease effect on subjects' cortical thickness were analyzed before and after the application of protocol-specific w-score standardization. Results As expected, different protocols resulted in differing cortical thickness measurements in both NC and AD subjects. Different measurements were obtained for the same subject when imaged with different protocols. Multivariate pattern difference between measurements was observed between the protocols. Classification accuracy between two protocols was nearly 90%. After applying protocol-specific w-score standardization, the differences between the protocols substantially decreased. Most importantly, protocol-specific w-score standardization reduced both univariate and multivariate differences in the images while maintaining the AD disease effect. Compared to conventional regression methods, our method showed the best performance for in terms of controlling the protocol effect while preserving disease information. Conclusions Protocol-specific w-score standardization effectively resolved the concerns of conventional regression methods. It showed the best performance for improving the compatibility of a T1 MR post-processed feature, cortical thickness. [ABSTRACT FROM AUTHOR]

Abstract: Transglutaminase2 (TGase2) activates Rho-associated kinase (ROCK), an important mediator of ischemia–reperfusion (IR) injury, through polyamination of RhoA. Cystamine, an oxidized dimer of cysteamine inhibits the transamidation activity of TGase2. We examined whether addition of cystamine to an organ preservation solution protects rat cardiomyocyte cells (H9C2) from cell death in IR injury. H9C2 cells were stored under hypoxic conditions at 4°C in laboratory-made preservation solution (SNU) or SNU solution supplemented with cystamine (SNU-C1), and cell preservation in the two solutions was compared by measuring the release of lactate dehydrogenase. The cells were preserved more effectively in SNU-C1 than in SNU solution. Cystamine inhibited the intracellular activity of TGase2 which increased during cold storage or reoxygenation. The inhibition of TGase2 by cystamine reduced the polyamination of RhoA, the interaction between RhoA and ROCK2, and F-actin formation. Cystamine also prevented the activation of caspases during cold storage. These results suggest that addition of cystamine to the organ preservation solution significantly enhances cardiomyocytes preservation apparently by inhibiting TGase2-mediated RhoA-ROCK pathway and that TGase2 may play an important role in IR injury by regulating ROCK. [Copyright &y& Elsevier]

Human cytomegalovirus UL18, a MHC class I homologue, is known to serve as a natural killer cell (NK) decoy and to ligate NK inhibitory receptors to prevent lysis of an infected target cell. To explore whether the cell surface expression of UL18 represents a potential immune suppressive approach to evade NK-mediated cytotoxicity in the prevention of xenograft rejection, we examined the effect of the UL18 expression in vitro upon human NK-mediated cytotoxicity against swine endothelial cells (SECs). UL18 expression on SECs by a retroviral vector (PLNCX2) significantly suppressed NK-mediated SEC lysis by approximately 25–100%. The protective effect of UL18 could be mediated through ILT-2 inhibitory receptor on NKs. Additionally, the interaction between UL18 and NKs resulted in the significant reduction of IFN-γ production. This study demonstrates that UL18 can serve as an effective tool for the evasion of NK-mediated cytotoxicity and for the inhibition of IFN-γ production during xenograft rejection. [Copyright &y& Elsevier]