Status, sexual capital, and intraminority body stigma in a size-diverse sample of gay men.

Gay men are more likely than heterosexual men to experience social pressure based on body weight, shape, and muscularity, which may drive disparities in body image concerns and eating disorders. Utilizing a sample of 1723 gay men living in the United States, the present study examined whether sociodemographic factors (used as proxies for status and sexual capital) and frequency of attending gay-specific establishments or gatherings (community involvement) were associated with gay men's experiences of negative or discriminatory pressures based on body size and shape specifically from other gay men (intraminority body stigma). Experiences of intraminority body stigma were significantly more common among gay men who identified as higher-weight (r = 0.28), less masculine (r = -0.21), less wealthy (r = -0.21), younger (r = -0.21), or people of color (ds = 0.25-0.28). Furthermore, indicators of low status and sexual capital were indirectly associated with less frequent community involvement via more frequent experiences of intraminority body stigma. In addition to frequency, the valence of interactions between gay men should be considered when assessing body image and eating disorder risk in this population. Future research is encouraged to examine intraminority body stigma as an intersectional source of intraminority stress to inform prevention and treatment efforts for gay men.

Development and Validation of the Gay-Specific Intraminority Stigma Inventory (G-SISI): Initial Evidence Underpinned by Intraminority Stress Theory.

There is currently a lack of measures testing intraminority stress within gay men. Therefore, the current study sought to develop and psychometrically test the Gay-Specific Intraminority Stigma Inventory (G-SISI). Based on a content review of the literature and a panel of experts, a pool of items assessing gay men's perceived exposure to a range of discriminatory attitudes from other gay men was generated. Utilizing a randomly split sample of 1723 gay men between the ages of 19 and 79 years, an exploratory factor analysis was first performed (n = 861). The remaining unexamined data were then used to conduct a confirmatory factor analysis (n = 862). The results support a six-factor model: (1) Age Stigma, (2) Socioeconomic Stigma, (3) Gay Non-Conformity Stigma, (4) Racial Stigma, (5) Gender Expression Stigma, and (6) Body Stigma. Cronbach's alpha for the total scale was 0.90 and for the subscales ranged from 0.60 to 0.85. Sociodemographic factors and measures of community involvement were differentially associated with the G-SISI subscales, providing evidence of construct validity. The findings demonstrate initial support for the dimensionality and validity of the G-SISI, which targets modifiable factors (e.g., identity-based stigma) that may increase stress and reduce community coping resources among gay men with diverse identities.

Geological, multispectral, and meteorological imaging results from the Mars 2020 Perseverance rover in Jezero crater.

Perseverance's Mastcam-Z instrument provides high-resolution stereo and multispectral images with a unique combination of spatial resolution, spatial coverage, and wavelength coverage along the rover's traverse in Jezero crater, Mars. Images reveal rocks consistent with an igneous (including volcanic and/or volcaniclastic) and/or impactite origin and limited aqueous alteration, including polygonally fractured rocks with weathered coatings; massive boulder-forming bedrock consisting of mafic silicates, ferric oxides, and/or iron-bearing alteration minerals; and coarsely layered outcrops dominated by olivine. Pyroxene dominates the iron-bearing mineralogy in the fine-grained regolith, while olivine dominates the coarse-grained regolith. Solar and atmospheric imaging observations show significant intra- and intersol variations in dust optical depth and water ice clouds, as well as unique examples of boundary layer vortex action from both natural (dust devil) and Ingenuity helicopter-induced dust lifting. High-resolution stereo imaging also provides geologic context for rover operations, other instrument observations, and sample selection, characterization, and confirmation.

The dynamic atmospheric and aeolian environment of Jezero crater, Mars.

Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars' ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover's novel environmental sensors and Jezero crater's dusty environment remedy this. In Perseverance's first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty ("dust devils"). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions.

Soil Thermophysical Properties Near the InSight Lander Derived From 50 Sols of Radiometer Measurements.

Measurements from the InSight lander radiometer acquired after landing are used to characterize the thermophysical properties of the Martian soil in Homestead hollow. This data set is unique as it stems from a high measurement cadence fixed platform studying a simple well-characterized surface, and it benefits from the environmental characterization provided by other instruments. We focus on observations acquired before the arrival of a regional dust storm (near Sol 50), on the furthest observed patch of soil (i.e., ∼3.5 m away from the edge of the lander deck) where temperatures are least impacted by the presence of the lander and where the soil has been least disrupted during landing. Diurnal temperature cycles are fit using a homogenous soil configuration with a thermal inertia of 183 ± 25 J m-2 K-1 s-1/2 and an albedo of 0.16, corresponding to very fine to fine sand with the vast majority of particles smaller than 140 µm. A pre-landing assessment leveraging orbital thermal infrared data is consistent with these results, but our analysis of the full diurnal temperature cycle acquired from the ground further indicates that near surface layers with different thermophysical properties must be thin (i.e., typically within the top few mm) and deep layering with different thermophysical properties must be at least below ∼4 cm. The low thermal inertia value indicates limited soil cementation within the upper one or two skin depths (i.e., ∼4-8 cm and more), with cement volumes <<1%, which is challenging to reconcile with visible images of overhangs in pits.

Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars.

Records of solar array currents recorded by the InSight lander during its first 200 sols on Mars are presented. In addition to the geometric variation in illumination on seasonal and diurnal timescales, the data are influenced by dust suspended in the atmosphere and deposited on the solar panels. Although no dust devils have been detected by InSight's cameras, brief excursions in solar array currents suggest that at least some of the vortices detected by transient pressure drops are accompanied by dust. A step increase in array output (i.e., a "cleaning event") was observed to be directly associated with the passage of a strong vortex. Some quasiperiodic variations in solar array current are suggestive of dust variations in the planetary boundary layer. Nonzero array outputs before sunrise and after sunset are indicative of scattering in the atmosphere: A notable increase in evening twilight currents is observed associated with noctilucent clouds, likely of water or carbon dioxide ice. Finally, although the observations are intermittent (typically a few hours per sol) and at a modest sample rate (one to two samples per minute), three single-sample light dips are seen associated with Phobos eclipses. These results demonstrate that engineering data from solar arrays provide valuable scientific situational awareness of the Martian environment.

The Mars Science Laboratory (MSL) Mast cameras and Descent imager: Investigation and instrument descriptions.

The Mars Science Laboratory Mast camera and Descent Imager investigations were designed, built, and operated by Malin Space Science Systems of San Diego, CA. They share common electronics and focal plane designs but have different optics. There are two Mastcams of dissimilar focal length. The Mastcam-34 has an f/8, 34 mm focal length lens, and the M-100 an f/10, 100 mm focal length lens. The M-34 field of view is about 20° × 15° with an instantaneous field of view (IFOV) of 218 µrad; the M-100 field of view (FOV) is 6.8° × 5.1° with an IFOV of 74 µrad. The M-34 can focus from 0.5 m to infinity, and the M-100 from ~1.6 m to infinity. All three cameras can acquire color images through a Bayer color filter array, and the Mastcams can also acquire images through seven science filters. Images are ≤1600 pixels wide by 1200 pixels tall. The Mastcams, mounted on the ~2 m tall Remote Sensing Mast, have a 360° azimuth and ~180° elevation field of regard. Mars Descent Imager is fixed-mounted to the bottom left front side of the rover at ~66 cm above the surface. Its fixed focus lens is in focus from ~2 m to infinity, but out of focus at 66 cm. The f/3 lens has a FOV of ~70° by 52° across and along the direction of motion, with an IFOV of 0.76 mrad. All cameras can acquire video at 4 frames/second for full frames or 720p HD at 6 fps. Images can be processed using lossy Joint Photographic Experts Group and predictive lossless compression.