IDENTITY OF THE CARRIER OF λ5797 DIFFUSE INTERSTELLAR BAND and λ5800 RED-RECTANGLE EMISSION BAND

The remarkable Red Rectangle nebula is well known for its emission bands (RRBs), excited by the central binary star HD 44179.\footnote{Schmidt, G. D., \& Witt, A. N. 1991, ApJ, 383:698} The proximity in wavelength between the strong $\lambda$5800~RRB and the long known and intense Diffuse Interstellar Band $\lambda$5797~DIB has led to speculation that these two bands originate from identical molecules. This speculation, however, has been challenged on the grounds that the peak wavelength of $\lambda$5800~RRB fails to converge to 5797~$\AA$ when observed at large angular offsets from HD 44179. Consequently, $\lambda$5800~RRB has been interpreted as being caused by various PAHs.\footnote{Sharp, R. G., Reilly, N. J., Kable, S. H., \& Schmidt, T. W. 2006, ApJ, 639:194} We investigate the possibility that $\lambda$5800~RRB and $\lambda$5797~DIB originate from the same molecule. We speculate that absorption in the foreground gas causes the peak wavelength discrepancy, and that the red-shifting of the $\lambda$5800~RRB peaks is a combined effect of the extended tail toward the red (ETR)\footnote{Oka, T., Welty, D. E., Johnson, S., York, D. G., Dahlstrom, J., \& Hobbs, L. M. 2013, ApJ, 773:42} resulting from the high radiative temperature near HD 44179 and the foreground gas absorption. We use the temperatures and luminosities of the binary star reported by Witt et al.\footnote{Witt, A. N., Vijh, U. P., Hobbs, L. M., Aufdenberg, J. P., Thorburn, J. A., \& York, D. G. 2009, 693:1946} for calculating the emission. However, radio to far infrared radiation emanating directly from the stars is far too weak to produce ETR, and we rely on stellar heating of the environment. We find that radiative temperatures on the order of 1000 K are sufficient to explain the largest tail and red-shifted peak at the smallest angular offset. We believe the molecules causing $\lambda$5797~DIB\footnote{Huang, J. \& Oka, T. 2015, Mol. Phys. 113, 15} and $\lambda$5800~RRB are identical

New 10Be exposure ages improve Holocene ice sheet thinning history near the grounding line of Pope Glacier, Antarctica

Evidence for the timing and pace of past grounding line retreat of the Thwaites Glacier system in the Amundsen Sea embayment (ASE) of Antarctica provides constraints for models that are used to predict the future trajectory of the West Antarctic Ice Sheet (WAIS). Existing cosmogenic nuclide surface exposure ages suggest that Pope Glacier, a former tributary of Thwaites Glacier, experienced rapid thinning in the early to mid-Holocene. There are relatively few exposure ages from the lower ice-free sections of Mt. Murphy (<300 m a.s.l.; metres above sea level) that are uncomplicated by either nuclide inheritance or scatter due to localised topographic complexities; this makes the trajectory for the latter stages of deglaciation uncertain. This paper presents 12 new 10Be exposure ages from erratic cobbles collected from the western flank of Mt. Murphy, within 160 m of the modern ice surface and 1 km from the present grounding line. The ages comprise two tightly clustered populations with mean deglaciation ages of 7.1 ± 0.1 and 6.4 ± 0.1 ka (1 SE). Linear regression analysis applied to the age–elevation array of all available exposure ages from Mt. Murphy indicates that the median rate of thinning of Pope Glacier was 0.27 m yr−1 between 8.1–6.3 ka, occurring 1.5 times faster than previously thought. Furthermore, this analysis better constrains the uncertainty (95 % confidence interval) in the timing of deglaciation at the base of the Mt. Murphy vertical profile (∼ 80 m above the modern ice surface), shifting it to earlier in the Holocene (from 5.2 ± 0.7 to 6.3 ± 0.4 ka). Taken together, the results presented here suggest that early- to mid-Holocene thinning of Pope Glacier occurred over a shorter interval than previously assumed and permit a longer duration over which subsequent late Holocene re-thickening could have occurred

Early planned removal of umbilical venous catheters to prevent infection in newborn infants

BACKGROUND: Lengthy duration of use may be a risk factor for umbilical venous catheter-associated bloodstream infection in newborn infants. Early planned removal of umbilical venous catheters (UVCs) is recommended to reduce the incidence of infection and associated morbidity and mortality. OBJECTIVES: To compare the effectiveness of early planned removal of UVCs (up to two weeks after insertion) versus an expectant approach or a longer fixed duration in preventing bloodstream infection and other complications in newborn infants.To perform subgroup analyses by gestational age at birth and prespecified planned duration of UVC placement (see "Subgroup analysis and investigation of heterogeneity"). SEARCH METHODS: We used the standard Cochrane Neonatal search strategy including electronic searches of the Cochrane Central Register of Controlled Trials (CENTRAL; 2017, Issue 4), Ovid MEDLINE, Embase, and the Maternity & Infant Care Database (until May 2017), as well as conference proceedings and previous reviews. SELECTION CRITERIA: Randomised and quasi-randomised controlled trials that compared effects of early planned removal of UVCs (up to two weeks after insertion) versus an expectant approach or a longer fixed duration in preventing bloodstream infection and other complications in newborn infants. DATA COLLECTION AND ANALYSIS: Two review authors assessed trial eligibility and risk of bias and independently undertook data extraction. We analysed treatment effects and reported risk ratio (RR) and risk difference (RD) for dichotomous data, and mean difference (MD) for continuous data, with respective 95% confidence intervals (CIs). We planned to use a fixed-effect model in meta-analyses and to explore potential causes of heterogeneity in sensitivity analyses. We assessed the quality of evidence for the main comparison at the outcome level using GRADE methods. MAIN RESULTS: We found one eligible trial. Participants were 210 newborn infants with birth weight less than 1251 grams. The trial was unblinded but otherwise of good methodological quality. This trial compared removal of an umbilical venous catheter within 10 days after insertion (and replacement with a peripheral cannula or a percutaneously inserted central catheter as required) versus expectant management (UVC in place up to 28 days). More infants in the early planned removal group than in the expectant management group (83 vs 33) required percutaneous insertion of a central catheter (PICC). Trial results showed no difference in the incidence of catheter-related bloodstream infection (RR 0.65, 95% CI 0.35 to 1.22), in hospital mortality (RR 1.12, 95% CI 0.42 to 2.98), in catheter-associated thrombus necessitating removal (RR 0.33, 95% confidence interval 0.01 to 7.94), or in other morbidity. GRADE assessment indicated that the quality of evidence was "low" at outcome level principally as the result of imprecision and risk of surveillance bias due to lack of blinding in the included trial. AUTHORS' CONCLUSIONS: Currently available trial data are insufficient to show whether early planned removal of umbilical venous catheters reduces risk of infection, mortality, or other morbidity in newborn infants. A large, simple, and pragmatic randomised controlled trial is needed to resolve this ongoing uncertainty

Surface-wave imaging of the weakly-extended Malawi Rift from ambient-noise and teleseismic Rayleigh waves from onshore and lake-bottom seismometers

Located at the southernmost sector of the Western Branch of the East African Rift System, the Malawi Rift exemplifies an active, magma-poor, weakly extended continental rift. To investigate the controls on rifting, we image crustal and uppermost mantle structure beneath the region using ambient-noise and teleseismic Rayleigh-wave phase velocities between 9 and 100 s period. Our study includes six lake-bottom seismometers located in Lake Malawi (Nyasa), the first time seismometers have been deployed in any of the African rift lakes. Noise-levels in the lake are lower than that of shallow oceanic environments and allow successful application of compliance corrections and instrument orientation determination. Resulting phase-velocity maps reveal slow velocities primarily confined to Lake Malawi at short periods (T 25 s) a prominent low-velocity anomaly exists beneath the Rungwe Volcanic Province at the northern terminus of the rift basin. Estimates of phase-velocity sensitivity indicates these low velocities occur within the lithospheric mantle and potentially uppermost asthenosphere, suggesting that mantle processes may control the association of volcanic centers and the localization of magmatism. Beneath the main portion of the Malawi Rift, a modest reduction in velocity is also observed at periods sensitive to the crust and upper mantle, but these velocities are much higher than those observed beneath Rungwe

Artificial Intelligence for Science in Quantum, Atomistic, and Continuum Systems

Advances in artificial intelligence (AI) are fueling a new paradigm of discoveries in natural sciences. Today, AI has started to advance natural sciences by improving, accelerating, and enabling our understanding of natural phenomena at a wide range of spatial and temporal scales, giving rise to a new area of research known as AI for science (AI4Science). Being an emerging research paradigm, AI4Science is unique in that it is an enormous and highly interdisciplinary area. Thus, a unified and technical treatment of this field is needed yet challenging. This work aims to provide a technically thorough account of a subarea of AI4Science; namely, AI for quantum, atomistic, and continuum systems. These areas aim at understanding the physical world from the subatomic (wavefunctions and electron density), atomic (molecules, proteins, materials, and interactions), to macro (fluids, climate, and subsurface) scales and form an important subarea of AI4Science. A unique advantage of focusing on these areas is that they largely share a common set of challenges, thereby allowing a unified and foundational treatment. A key common challenge is how to capture physics first principles, especially symmetries, in natural systems by deep learning methods. We provide an in-depth yet intuitive account of techniques to achieve equivariance to symmetry transformations. We also discuss other common technical challenges, including explainability, out-of-distribution generalization, knowledge transfer with foundation and large language models, and uncertainty quantification. To facilitate learning and education, we provide categorized lists of resources that we found to be useful. We strive to be thorough and unified and hope this initial effort may trigger more community interests and efforts to further advance AI4Science

FoxP3+ T regulatory cells in cancer : prognostic biomarkers and therapeutic targets

T Regulatory cells (Tregs) can have both protective and pathological roles. They maintain immune homeostasis and inhibit immune responses in various diseases, including cancer. Proportions of Tregs in the peripheral blood of some cancer patients increase by five-to ten-folds, compared to those in healthy individuals. Tregs contribute to cancer development and progression by suppressing T effector cell functions, thereby compromising tumor killing and promoting tumor growth. Highly immunosuppressive Tregs express upregulated levels of the transcription factor, Forkhead box protein P3 (FoxP3). Elevated levels of FoxP3+ Tregs within the tumor microenvironment (TME) showed a positive correlation with poor prognosis in various cancer patients. Despite the success of immunotherapy, including the use of immune checkpoint inhibitors, a significant proportion of patients show low response rates as a result of primary or acquired resistance against therapy. Some of the mechanisms which underlie the development of therapy resistance are associated with Treg suppressive function. In this review, we describe Treg contribution to cancer development/progression, and the mechanisms of Treg-mediated immunosuppression. We discuss the prognostic significance of FoxP3+ Tregs in different cancers and their potential use as prognostic biomarkers. We also describe potential therapeutic strategies to target Tregs in combination with other types of immunotherapies aiming to overcome tumor resistance and improve clinical outcomes in cancer patients. Overall, understanding the prognostic significance of FoxP3+ Tregs in various cancers and their contribution to therapeutic resistance could help in the development of more effective targeted therapeutic strategies to enhance the clinical outcomes in cancer patients

IDENTITY OF THE CARRIER OF λ5797 DIFFUSE INTERSTELLAR BAND and λ5800 RED-RECTANGLE EMISSION BAND

The remarkable Red Rectangle nebula is well known for its emission bands (RRBs), excited by the central binary star HD 44179.\footnote{Schmidt, G. D., \& Witt, A. N. 1991, ApJ, 383:698} The proximity in wavelength between the strong $\lambda$5800~RRB and the long known and intense Diffuse Interstellar Band $\lambda$5797~DIB has led to speculation that these two bands originate from identical molecules. This speculation, however, has been challenged on the grounds that the peak wavelength of $\lambda$5800~RRB fails to converge to 5797~$\AA$ when observed at large angular offsets from HD 44179. Consequently, $\lambda$5800~RRB has been interpreted as being caused by various PAHs.\footnote{Sharp, R. G., Reilly, N. J., Kable, S. H., \& Schmidt, T. W. 2006, ApJ, 639:194} We investigate the possibility that $\lambda$5800~RRB and $\lambda$5797~DIB originate from the same molecule. We speculate that absorption in the foreground gas causes the peak wavelength discrepancy, and that the red-shifting of the $\lambda$5800~RRB peaks is a combined effect of the extended tail toward the red (ETR)\footnote{Oka, T., Welty, D. E., Johnson, S., York, D. G., Dahlstrom, J., \& Hobbs, L. M. 2013, ApJ, 773:42} resulting from the high radiative temperature near HD 44179 and the foreground gas absorption. We use the temperatures and luminosities of the binary star reported by Witt et al.\footnote{Witt, A. N., Vijh, U. P., Hobbs, L. M., Aufdenberg, J. P., Thorburn, J. A., \& York, D. G. 2009, 693:1946} for calculating the emission. However, radio to far infrared radiation emanating directly from the stars is far too weak to produce ETR, and we rely on stellar heating of the environment. We find that radiative temperatures on the order of 1000 K are sufficient to explain the largest tail and red-shifted peak at the smallest angular offset. We believe the molecules causing $\lambda$5797~DIB\footnote{Huang, J. \& Oka, T. 2015, Mol. Phys. 113, 15} and $\lambda$5800~RRB are identical