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1. Star cluster formation in Orion A

   https://doi.org/10.1093/pasj/psaa035  

   Lim, Wanggi; Nakamura, Fumitaka; Wu, Benjamin; Bisbas, Thomas G; Tan, Jonathan C; Chambers, Edward; Bally, John; Kong, Shuo; McGehee, Peregrine; Lis, Dariusz C; et al (May 2020, Publications of the Astronomical Society of Japan)

   null (Ed.)

   Abstract We introduce new analysis methods for studying the star cluster formation processes in Orion A, especially examining the scenario of a cloud–cloud collision. We utilize the CARMA–NRO Orion survey 13CO (1–0) data to compare molecular gas to the properties of young stellar objects from the SDSS III IN-SYNC survey. We show that the increase of $$v_{\rm {}^{13}CO} - v_{\rm YSO}$$ and Σ scatter of older YSOs can be signals of cloud–cloud collision. SOFIA-upGREAT 158 μm [C ii] archival data toward the northern part of Orion A are also compared to the 13CO data to test whether the position and velocity offsets between the emission from these two transitions resemble those predicted by a cloud–cloud collision model. We find that the northern part of Orion A, including regions ONC-OMC-1, OMC-2, OMC-3, and OMC-4, shows qualitative agreements with the cloud–cloud collision scenario, while in one of the southern regions, NGC 1999, there is no indication of such a process in causing the birth of new stars. On the other hand, another southern cluster, L 1641 N, shows slight tendencies of cloud–cloud collision. Overall, our results support the cloud–cloud collision process as being an important mechanism for star cluster formation in Orion A. 

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2. A radio counterpart to a neutron star merger

   https://doi.org/10.1126/science.aap9855  

   Hallinan, G.; Corsi, A.; Mooley, K. P.; Hotokezaka, K.; Nakar, E.; Kasliwal, M. M.; Kaplan, D. L.; Frail, D. A.; Myers, S. T.; Murphy, T.; et al (December 2017, Science)
3. ORION2: A magnetohydrodynamics code for star formation

   https://doi.org/10.21105/joss.03771  

   Li, Pak; Cunningham, Andrew; Gaches, Brandt; Klein, Richard; Krumholz, Mark; Lee, Aaron; McKee, Christopher; Offner, Stella; Rosen, Anna; Skinner, Aaron (December 2021, Journal of Open Source Software)
4. A highly magnified star at redshift 6.2

   https://doi.org/10.1038/s41586-022-04449-y  

   Welch, Brian; Coe, Dan; Diego, Jose M.; Zitrin, Adi; Zackrisson, Erik; Dimauro, Paola; Jiménez-Teja, Yolanda; Kelly, Patrick; Mahler, Guillaume; Oguri, Masamune; et al (March 2022, Nature)
5. Proper Motion of the Faint Star near KIC 8462852 (Boyajian's Star)—Not a Binary System

   https://doi.org/https://doi.org/10.3847/2041-8213/aab492  

   Clemens, Dan P.; Maheshwari, Kush; Jagani, Roshan; Montgomery, J.; El Batal, A. M.; Ellis, T. G.; Wright, J. T. (March 2018, The astrophysical journal. Letters)

   A faint star located 2 arcsec from KIC 8462852 was discovered in Keck 10 m adaptive optics imaging in the JHK near-infrared (NIR) in 2014 by Boyajian et al. (2016). The closeness of the star to KIC 8462852 suggested that the two could constitute a binary, which might have implications for the cause of the brightness dips seen by Kepler and in ground-based optical studies. Here, NIR imaging in 2017 using the Mimir instrument resolved the pair and enabled measuring their separation. The faint star had moved 67 ± 7 milliarcsec (mas) relative to KIC 8462852 since 2014. The relative proper motion of the faint star is 23.9 ± 2.6 mas yr-1, for a tangential velocity of 45 ± 5 km s-1 if it is at the same 390 pc distance as KIC 8462852. Circular velocity at the 750 au current projected separation is 1.5 km s-1, hence the star pair cannot be bound. 

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