PAPER / ARXIV:2609.16190
Kaitlyn E. Sheriff (University of Kansas), Elisabeth A. C. Mills (University of Kansas), Xinyu Mai (University of Kansas), Utsav Siwakoti (University of Kansas), Sara E. Duval (University of Toledo), Alberto D. Bolatto (University of Maryland), Rebecca C. Levy (Space Telescope Science Institute), Jia Wei Teh (Heidelberg University), Torsten Böker (European Space Agency), Serena A. Cronin (University of Maryland), Daniel A. Dale (University of Wyoming), Keaton Donaghue (University of Maryland), Kimberly Emig (National Radio Astronomy Observatory), Simon C. O. Glover (Heidelberg University), Rodrigo Herrera-Camus (University of Concepción, Millennium Nucleus for Galaxies), Ralf S. Klessen (Heidelberg University), Thomas S.-Y Lai (California Institute of Technology), Ashley E. Lieber (University of Kansas), Laura Lenkić (California Institute of Technology), Sebastian Lopez (The Ohio State University), David S. Meier (New Mexico Institute of Mining and Technology), Jüergen Ott (National Radio Astronomy Observatory), J. D. T. Smith (University of Toledo), Yu-Hsuan Teng (University of Maryland), Paul P. van der Werf (Leiden Observatory), Sylvain Veilleux (University of Maryland), Vicente Villanueva (Universidad Diego Portales Instituto de Estudios Astrofísicos, Millennium Nucleus for Galaxies), Rachel Cionitti (University of Kansas), Joseph Havens (University of Kansas), Maleah Rhem (University of Kansas), Nathan Shaw (University of Kansas), Kai Smith (University of Kansas), Hazel B. Wright (University of Kansas), Md. Abdullah Al Zaman (University of Kansas)
RESUMO
We present a multi-wavelength analysis of a young bubble in the nuclear starburst of NGC 253 using new JWST MIRI-MRS observations together with archival ALMA (100, 350, 690 GHz) and Chandra data. The MIRI maps reveal a prominent bubble-like structure in both ionized and molecular emission lines. The bubble is spatially coincident with one of the least embedded massive young clusters detected with ALMA, suggesting that the cluster is driving the expansion. We measure a radius of $\sim 11.5 \pm 3.4$ pc and an expansion velocity of $\sim 90 \pm 44$ km s$^{-1}$, implying a dynamical age of $\sim 0.1 \pm 0.1$ Myr. Using RADEX modeling of multiple CO transitions, we infer a molecular mass in the range of $(1.3 \pm 0.3) \times 10^4$ to $(2.8 \pm 0.8) \times 10^5$ $M_\odot$. We derive a kinetic energy of order $10^{51}$-$10^{52}$ erg, consistent with mechanical input from Wolf-Rayet stellar winds or supernovae in a $\sim 10^6$ $M_\odot$ cluster. The existence of a large population of Wolf-Rayet stars or past supernovae is supported by the presence of coincident X-ray emission. Our results provide direct evidence that individual clusters in a nuclear environment can carve out coherent structures on parsec scales and inject significant energy and momentum into the surrounding interstellar medium, which can contribute to the nuclear outflow in NGC 253.
NO MESMO MAPA