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1. Crystal structures of [Cu(phen)(H 2 O) 3 ( M F 6 )]·H 2 O ( M = Ti, Zr, Hf) and [Cu(phen)(H 2 O) 2 F] 2 [HfF 6 ]·H 2 O

   https://doi.org/10.1107/S2056989021000645  

   Nisbet, Matthew L.; Poeppelmeier, Kenneth R. (February 2021, Acta Crystallographica Section E Crystallographic Communications)

   null (Ed.)

   The crystal structures of three bridged bimetallic molecular compounds, namely, triaqua-2κ 3 O -μ-fluorido-pentafluorido-1κ 5 F -(1,10-phenanthroline-2κ 2 N , N ′)copper(II)titanium(IV) monohydrate, [Cu(TiF 6 )(phen)(H 2 O) 3 ]·H 2 O (phen is 1,10-phenanthroline, C 12 H 8 N 2 ), (I), triaqua-2κ 3 O -μ-fluorido-pentafluorido-1κ 5 F -(1,10-phenanthroline-2κ 2 N , N ′)copper(II)zirconium(IV) monohydrate, [Cu(ZrF 6 )(phen)(H 2 O) 3 ]·H 2 O, (II), and triaqua-2κ 3 O -μ-fluorido-pentafluorido-1κ 5 F -(1,10-phenanthroline-2κ 2 N , N ′)copper(II)hafnium(IV) monohydrate, [Cu(HfF 6 )(phen)(H 2 O) 3 ]·H 2 O, (III), and one molecular salt, bis[diaquafluorido(1,10-phenanthroline-κ 2 N , N ′)copper(II)] hexafluoridohafnate(IV) dihydrate, [CuF(phen)(H 2 O) 2 ] 2 [HfF 6 ]·2H 2 O, (IV), are reported. The bridged bimetallic compounds adopt Λ-shaped configurations, with the octahedrally coordinated copper(II) center linked to the fluorinated early transition metal via a fluoride linkage. The extended structures of these Λ-shaped compounds are organized through both intra- and intermolecular hydrogen bonds and intermolecular π–π stacking. The salt compound [Cu(phen)(H 2 O) 2 F] 2 [HfF 6 ]·H 2 O displays an isolated square-pyramidal Cu(phen)(H 2 O) 2 F + complex linked to other cationic complexes and isolated HfF 6 2− anions through intermolecular hydrogen-bonding interactions. 

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2. Mixture rules and falloff are now major uncertainties in experimentally derived rate parameters for H + O2 (+M) ↔ HO2 (+M)

   https://doi.org/10.1016/j.combustflame.2019.11.041  

   Lei, Lei; Burke, Michael P. (March 2020, Combustion and Flame)
3. H-Representation of the Kimura-3 Polytope for the $$m$$-Claw Tree

   https://doi.org/10.1137/15M1051890  

   Mauhar, Marie; Rusinko, Joseph; Vernon, Zoe (January 2017, SIAM Journal on Discrete Mathematics)
4. H ₂ Fluorescence in M Dwarf Systems: A Stellar Origin

   https://doi.org/10.3847/1538-4357/aa7b79  

   Kruczek, Nicholas; France, Kevin; Evonosky, William; Loyd, R. O.; Youngblood, Allison; Roberge, Aki; Wittenmyer, Robert A.; Stocke, John T.; Fleming, Brian; Hoadley, Keri (August 2017, The Astrophysical Journal)
5. DIISC-I: The Discovery of Kinematically Anomalous H i Clouds in M 100

   https://doi.org/10.3847/1538-4357/ac2303  

   Gim, Hansung B.; Borthakur, Sanchayeeta; Momjian, Emmanuel; Padave, Mansi; Jansen, Rolf A.; Nelson, Dylan; Heckman, Timothy M.; Kennicutt Jr., Robert C.; Fox, Andrew J.; Pineda, Jorge L.; et al (November 2021, The Astrophysical Journal)

   Abstract We report the discovery of two kinematically anomalous atomic hydrogen (H i ) clouds in M 100 (NGC 4321), which was observed as part of the Deciphering the Interplay between the Interstellar medium, Stars, and the Circumgalactic medium (DIISC) survey in H i 21 cm at 3.3 km s −1 spectroscopic and 44″ × 30″ spatial resolution using the Karl G. Jansky Very Large Array. 15 15 The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. These clouds were identified as structures that show significant kinematic offsets from the rotating disk of M 100. The velocity offsets of 40 km s −1 observed in these clouds are comparable to the offsets seen in intermediate-velocity clouds (IVCs) in the circumgalactic medium (CGM) of the Milky Way and nearby galaxies. We find that one anomalous cloud in M 100 is associated with star-forming regions detected in H α and far-ultraviolet imaging. Our investigation shows that anomalous clouds in M 100 may originate from multiple mechanisms, such as star formation feedback-driven outflows, ram pressure stripping, and tidal interactions with satellite galaxies. Moreover, we do not detect any cool CGM at 38.8 kpc from the center of M 100, giving an upper limit of N(H i ) ≤1.7 × 10 13 cm −2 (3 σ ). Since M 100 is in the Virgo cluster, the nonexistence of neutral/cool CGM is a likely pathway for turning it into a red galaxy. 

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