Hydrogen 2p--2s transition: signals from the epochs of recombination and reionization

We propose a method to study the epoch of reionization based on the possible observation of 2p--2s fine structure lines from the neutral hydrogen outside the cosmological H {\sc ii} regions enveloping QSOs and other ionizing sources in the reionization era. We show that for parameters typical of luminous sources observed at $z \simeq 6.3$ the strength of this signal, which is proportional to the H {\sc i} fraction, has a brightness temperature $\simeq 20 \mu K$ for a fully neutral medium. The fine structure line from this redshift is observable at $\nu \simeq 1 \rm GHz$ and we discuss prospects for the detection with several operational and future radio telescopes. We also compute the characteristics of this signal from the epoch of recombination: the peak brightness is expected to be $\simeq 100 \mu K$; this signal appears in the frequency range 5-10 MHz. The signal from the recombination era is nearly impossible to detect owing to the extreme brightness of the Galactic emission at these frequencies.Comment: 17 pages, 1 figure, to appear in Ap

Do no harm: health systems' duty to promote clinician well-being

Burnout and mental health disorders plague the health care workforce. Since the pandemic began, there has been an uptick in symptoms of anxiety, depression, and suicidality among health care professionals. These threats to the workforce existed before the pandemic, have been exacerbated by the pandemic, and are likely to persist for years ahead.Anish K. Agarwal (MD, MPH, MS, Department of Emergency Medicine, Perelman School of Medicine, University of Pennsylvania, Philadelphia, Center for Health Care Innovation, University of Pennsylvania, Philadelphia), Thea Gallagher (PsyD, Department of Psychiatry, Grossman School of Medicine, New York University, New York City). Corresponding author: Anish K. Agarwal MD, MPH, MS, Assistant Professor and Chief Well-Being Officer | Department of Emergency Medicine.Includes bibliographical reference

STRUCTURAL AND FUNCTIONAL IMPACT OF G2032R MUTATION IN ROS1 – A THEORETICAL PERSPECTIVE

Objective: Drug resistance is an imperative issue in the treatment of patients with lung cancer. In this work, investigation of the drug resistance mechanism of G2032R mutation in ROS1 is carried out using computational simulation techniques.Methods: Molecular docking and molecular dynamics (MD) simulation approach have been utilized to uncover the mechanism behind crizotinib resistance in ROS1 at a molecular level. Normal mode analysis was carried out using ElNemo server which examines the movements and conformational changes in the protein structure. ArgusLab, PEARLS, and Autodock were employed for the docking analysis, whereas GROMACS package 4.5.3 was used for MD simulation approach.Results: The results from our analysis indicates that wild-type ROS1 (Protein Data Bank Code 3ZBF) could be more crucial for the crizotinib binding as it indicates largest binding affinity, minimum number of H-bonds, and higher flexibility than mutant-type ROS1. Moreover, the theoretical basis for the cause of drug insensitivity is the differences in the electrostatic properties of binding site residues between the wild and mutant ROS1 structures. Our analysis theoretically suggests that E-2027 is a key residue responsible for the ROS1 drug selectivity.Conclusion: Molecular docking and MD simulation results provide an explanation of the resistance caused by G2032R and may give a key clue for the drug design to encounter drug resistance.Â

Hydrogen recombination lines near 327 MHz. III. physical properties and origin of the low-density ionized gas in the inner galaxy

We present constraints on the physical properties of the ionized gas responsible for hydrogen radio recombination lines (RRLs) near 327 MHz detected in a recent Galactic plane survey made with the Ooty Radio Telescope. To obtain these constraints, we combined the data at 327 MHz with previously published RRL observations near 1.4 GHz. The density of the ionized gas is well constrained and is in the range of 1 to 10 cm-3. The data implies upper limits to the temperature and size of the line emitting regions of ~12,000 K and ~500 pc, respectively. Assuming an electron temperature of 7000 K, the derived path lengths of the line emitting region are in the range of 20 to 200 pc. The derived properties of the ionized gas responsible for the RRL emission near 327 MHz suggest that most of the [N II] 205 µm emission and a considerable fraction of the [C II] 158 µm emission observed in the Galactic plane by the COBE satellite could also originate in the same gas. The Hα emission from these ionized gases is mostly undetected in the existing Hα surveys because of large interstellar extinction. About 50% of the free-free absorption of the Galactic nonthermal radiation observed at frequencies less than 100 MHz can be accounted for by the same ionized gas. We also discuss the origin of this low-density ionized gas in the inner Galaxy. The derived low line-of-sight filling factor (<1%) for this ionized gas indicates that it does not form a pervasive medium. On the basis of the similarity of the distribution of this gas in the Galactic disk with that of the star-forming regions and the range of derived physical properties, we support the earlier suggestion that the low-frequency RRL emission originates from low-density ionized gas, which forms envelopes of normal H II regions

Hydrogen recombination lines near 327 MHz. I. distribution of low-density ionized gas in the galactic disk

We present the results of a low-resolution (2° × 2°) survey of radio recombination lines (RRLs) near 327 MHz in the Galactic plane made with the Ooty Radio Telescope (ORT). Although the angular resolution is coarse, these observations represent the first contiguous survey of low-frequency RRL emission in the longitude range l = 330°-0°-89° (inner Galaxy). Hydrogen RRLs were detected in almost all directions in the inner Galaxy and carbon lines in several positions. In the outer Galaxy (l = 172°-252°), an unbiased set of 14 positions were observed and lines were detected toward three of them. To study the extent of the ionized gas above the Galactic disk, we have observed RRLs along the Galactic latitude at two specific longitudes (l = 0°.0 and 13°.9). RRLs were detected up to b = ±3°. The l-ν diagram and the radial distribution, obtained from RRL emission near 327 MHz, show good similarity with that of RRL emission near 1.4 GHz, "intense" 12CO emission and to some extent with the RRLs observed near 3 cm from normal H II region. These distributions are distinctly different from those of Hα and H I emission from the Galactic disk. Based on a comparison of the radial distribution of different components in the Galactic disk, we conclude that the diffuse RRL emission is associated with star-forming regions and possibly with a low-density component of known H II regions in the inner Galaxy