The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). III. The Mass Function of Young Stellar Clusters in M33
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Author
Wainer, T.M.Johnson, L.C.
Seth, A.C.
Torresvillanueva, E.E.
Dalcanton, J.J.
Durbin, M.J.
Dolphin, A.
Weisz, D.R.
Williams, B.F.
PHATTER Collaboration
Affiliation
Steward Observatory, University of ArizonaIssue Date
2022
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IOP Publishing LtdCitation
Wainer, T. M., Johnson, L. C., Seth, A. C., Torresvillanueva, E. E., Dalcanton, J. J., Durbin, M. J., Dolphin, A., Weisz, D. R., Williams, B. F., & PHATTER Collaboration. (2022). The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). III. The Mass Function of Young Stellar Clusters in M33. Astrophysical Journal.Journal
Astrophysical JournalRights
Copyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We measure the star cluster mass function (CMF) for the Local Group galaxy M33. We use the catalog of stellar clusters selected from the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region survey. We analyze 711 clusters in M33 with 7.0<log(Age/yr)<8.5, and log(M/M) > 3.0 as determined from color-magnitude diagram fits to individual stars. The M33 CMF is best described by a Schechter function with power-law slope α = - 2.06-0.13+0.14, and truncation mass log(M c /M) =4.24-0.13+0.16 . The data show strong evidence for a high-mass truncation, thus strongly favoring a Schechter function fit over a pure power law. M33's truncation mass is consistent with the previously identified linear trend between M c , and star formation rate surface density, ςSFR. We also explore the effect that individual cluster mass uncertainties have on derived mass function parameters, and find evidence to suggest that large cluster mass uncertainties have the potential to bias the truncation mass of fitted mass functions at the 1σ level. © 2022. The Author(s). Published by the American Astronomical Society.Note
Open access journalISSN
0004-637XVersion
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ac51cf
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Except where otherwise noted, this item's license is described as Copyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.