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Testing afterglow models of FRB 200428 with early post-burst observations of SGR 1935+2154

ArXiv 2210.06547 (2022)

Authors:

AJ Cooper, A Rowlinson, RAMJ Wijers, C Bassa, K Gourdji, J Hessels, AJ van der Horst, V Kondratiev, Z Pleunis, T Shimwell, S ter Veen
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A refined dynamical mass for the black hole in the X-ray transient XTE J1859+226

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 517:1 (2022) 1476-1482

Authors:

IV Yanes-Rizo, MAP Torres, J Casares, SE Motta, T Muñoz-Darias, P Rodríguez-Gil, M Armas Padilla, F Jiménez-Ibarra, PG Jonker, JM Corral-Santana, R Fender
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MIGHTEE-HI: The HI mass-stellar mass relation over the last billion years

(2022)

Authors:

Hengxing Pan, Matt J Jarvis, Mario G Santos, Natasha Maddox, Bradley S Frank, Anastasia A Ponomareva, Isabella Prandoni, Sushma Kurapati, Maarten Baes, Pavel E Mancera Piña, Giulia Rodighiero, Martin J Meyer, Romeel Davé, Gauri Sharma, Sambatriniaina HA Rajohnson, Nathan J Adams, Rebecca AA Bowler, Francesco Sinigaglia, Thijs van der Hulst, Peter W Hatfield, Srikrishna Sekhar, Jordan D Collier
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WISDOM Project – XII. Clump properties and turbulence regulated by clump–clump collisions in the dwarf galaxy NGC 404

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 517:1 (2022) 632-656

Authors:

Lijie Liu, Martin Bureau, Guang-Xing Li, Timothy A Davis, Dieu D Nguyen, Fu-Heng Liang, Woorak Choi, Mark R Smith, Satoru Iguchi

Abstract:

ABSTRACT We present a study of molecular structures (clumps and clouds) in the dwarf galaxy NGC 404 using high-resolution (≈0.86 × 0.51 pc2) Atacama Large Millimeter/sub-millimeter Array 12CO(2-1) observations. We find two distinct regions in NGC 404: a gravitationally stable central region (Toomre parameter Q = 3–30) and a gravitationally unstable molecular ring (Q ≲ 1). The molecular structures in the central region have a steeper size–linewidth relation and larger virial parameters than those in the molecular ring, suggesting gas is more turbulent in the former. In the molecular ring, clumps exhibit a shallower mass–size relation and larger virial parameters than clouds, implying density structures and dynamics are regulated by different physical mechanisms at different spatial scales. We construct an analytical model of clump–clump collisions to explain the results in the molecular ring. We propose that clump–clump collisions are driven by gravitational instabilities coupled with galactic shear, which lead to a population of clumps whose accumulation lengths (i.e. average separations) are approximately equal to their tidal radii. Our model-predicted clump masses and sizes (and mass–size relation) and turbulence energy injection rates (and size–linewidth relation) match the observations in the molecular ring very well, suggesting clump–clump collisions are the main mechanism regulating clump properties and gas turbulence in that region. As expected, our collision model does not apply to the central region, where turbulence is likely driven by clump migration.
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Late-time H/He-poor circumstellar interaction in the type-Ic supernova SN 2021ocs: an exposed oxygen-magnesium layer and extreme stripping of the progenitor

ArXiv 2210.01755 (2022)

Authors:

H Kuncarayakti, K Maeda, L Dessart, T Nagao, M Fulton, CP Gutierrez, ME Huber, DR Young, R Kotak, S Mattila, JP Anderson, L Ferrari, G Folatelli, H Gao, E Magnier, KW Smith, S Srivastav
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