Figure 2 from

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation

Hi-Resolution Export to PDF

Masses, Star Formation Efficiencies, and Dynamical Evolution of 18,000 H II Regions

Authors: Debosmita Pathak, Adam K. Leroy, Ashley. T. Barnes, Todd A. Thompson, Laura A. Lopez, Karin M. Sandstrom, Jiayi Sun, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Kirsten L. Larson, Janice Lee, Sharon Meidt, Patricia Sanchez-Blazquez, Eva Schinnerer, Zein Bazzi, Francesco Belfiore, Médéric Boquien, Ryan Chown, Dario Colombo, Enrico Congiu, Oleg V. Egorov, Cosima Eibensteiner, Sushma Kurapati, Miguel Querejeta, Daniel A. Dale, Timo Kravtsov, Mansi Padave, D. J. Pisano, Erik Rosolowsky, Sumit K. Sarbadhicary, Thomas G. Williams, Remy Indebetouw, Hsi-An Pan, Leonardo Úbeda, Amirnezam Amiri, Frank Bigiel, Guillermo A. Blanc, Kathryn Grasha

Debosmita Pathak et al 2025 The Astrophysical Journal Letters 993 .

Provider: AAS Journals

Caption: Figure 2.

Variation in the different mass components relative to the young cluster mass M_New for the full sample of H II regions, binned in L_H_α^corr (top left) and R_circ (top right) and summarized as histograms (bottom left). M_{Ion, S II}/M_New (dark green), ﹩{M}_{{\rm{Ion}}},{\rm{Str}}\ddot{{\rm{o}}}{\rm{mgren}}/{M}_{{\rm{New}}}﹩ (light green), M_Old/M_New (red), ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}/{M}_{{\rm{New}}}﹩ (dashed pink), and ﹩{M}_{{\rm{Atom}}}^{{\rm{init}}}/{M}_{{\rm{New}}}﹩ (dashed gray) are included for comparison. The dashed line indicates where a mass component is equal to M_New. The bottom right panel includes the distribution of the measured R_circ (black), the estimated radius at which ﹩{M}_{{\rm{New}}}={M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (dashed pink), and the radius where M_New = M_Old (red).

Copyright and Terms & Conditions

Additional terms of reuse

Other Images in This Article

Copyright and Terms & Conditions