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Creators/Authors contains: "Rao, M"

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  1. ; (, IUCrData)
    In the title compound, C8H8ClNO2, the acetamide substituent is twisted out of the phenyl plane, forming a dihedral angle of 58.61 (7)°. In the extended structure, each molecule donates two hydrogen bonds [N—H...O(carbonyl) and O—H...O(carbonyl)] and thus also accepts two such hydrogen bonds. The chlorine atom is not involved in the hydrogen bonding. 
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    Free, publicly-accessible full text available August 1, 2026
  2. ; (, IUCrData)
    In the title compound, C10H12N2O4, the four substituents lie out of the phenyl plane by varying degrees. The methyl C atom lies 0.019 (3) A ˚ out of plane, while the methoxy O and C atoms lie 0.067 (2) and 0.042 (3) A ˚ out of plane, respectively, with the C—C—O—C torsion angle being 3.3 (2). The plane of the nitro group is twisted out of the phenyl plane, forming a dihedral angle of 12.03 (9) with it. The acetamide substituent is twisted considerably more out of the phenyl plane, forming a dihedral angle of 47.24 (6) with it. In the extended structure, the acetamide NH group donates a hydrogen bond to an acetamide carbonyl O atom, thereby forming chains propagating in the [010] direction. 
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    Free, publicly-accessible full text available June 1, 2026
  3. ; ; ; ; (, IUCrData)
    In the title compound, C16H16N2O3, the phenyl groups are twisted away from coplanarity with the ether linkage, forming a dihedral angle of 59.49 (4) with each other. The ether oxygen atom lies somewhat out of both phenyl planes, by 0.066 (2) and 0.097 (2) A ˚ . The acetamide substituents have quite different conformations with respect to the phenyl groups on either side of the molecule. On one side, the C—C—N—C torsion angle is 21.0 (2), while on the other side it is 76.4 (2). In the crystal, the acetamide N—H groups form intermolecular N—H O hydrogen bonds to acetamide O atom, with both NH groups donating to the same molecule. Thus, ladder-like chains exist in the [101] direction. One of the methyl groups has its H atoms disordered into two orientations, and the crystal chosen for data collection was found to be twinned. 
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    Free, publicly-accessible full text available May 1, 2026
  4. ; (, American Meteorological Society)
    Accepted Manuscript Full Text Available
  5. ; (, Transactions American Geophysical Union)
  6. ; (, Transactions American Geophysical Union)
  7. ; (, Transactions American Geophysical Union)
  8. ; ; ; ; ; ; ; ; ; ; et al (, The Astronomical Journal)
    null (Ed.)
    Full Text Available 
  9. ; ; ; ; ; ; ; ; ; (, American Astronomical Society Meeting Abstracts #235)
    Despite the fact that Warm Ionized Medium (WIM) is a major component of the Interstellar Medium our knowledge about it and its relationship with H II regions is very limited. Understanding the WIM better will give us insight into the formation of galaxies and evolution of high-mass star formation regions. Previous surveys of the WIM and H II regions had low spectral and spatial resolutions or looked at Hα, which suffers from extinction. In this project we attempt to get additional value from the GBT Diffuse Ionized Gas Survey (GDIGS), by making continuum maps using the existing data. The goal is to assess whether the GDIGS data can be used to measure the radio recombination line to continuum emission ratio for the diffuse ionized gas. 
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    Accepted Manuscript Full Text Available
  10. ; ; ; ; ; ; ; ; ; (, American Astronomical Society meeting #235)
    The Warm Ionized Medium (WIM) is a low density, diffuse ionized component of the Milky Way. The WIM is the last major component of the interstellar medium to be studied at high spatial and spectral resolution, and therefore many of its fundamental properties are not clear. Radiation from massive, OB-type stars, which live in the inner galaxy, is thought to escape discrete HII regions to ionize the WIM. However, the inner Galaxy has not been well studied due to extinction from dust at optical wavelengths. GDIGS is a fully-sampled Radio Recombination Line (RRL) survey of the inner Galactic Plane at C-band (4-8 GHz). RRL emission is not affected by extinction from dust, and GDIGS has sufficient spatial resolution to distinguish between HII regions and the WIM emission. Here we discuss the status of GDIGS and some preliminary results from the spectral analysis of the RRLs. 
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    Accepted Manuscript Full Text Available