GOALS-JWST: Revealing the Buried Star Clusters in the Luminous Infrared Galaxy VV 114
- Creators
- Linden, Sean T.
- Evans, Aaron S.
- Armus, Lee
- Rich, Jeffrey A.
- Larson, Kirsten L.
- Lai, Thomas
- Privon, George C.
- U, Vivian
- Inami, Hanae
- Bohn, Thomas
- Song, Yiqing
- Barcos-Muñoz, Loreto
- Charmandaris, Vassilis
- Medling, Anne M.
- Stierwalt, Sabrina
- Diaz-Santos, Tanio
- Böker, Torsten
- van der Werf, Paul
- Aalto, Susanne
- Appleton, Philip
- Brown, Michael J. I.
- Hayward, Christopher C.
- Howell, Justin H.
- Iwasawa, Kazushi
- Kemper, Francisca
- Frayer, David T.
- Law, David
- Malkan, Matthew A.
- Marshall, Jason
- Mazzarella, Joseph M.
- Murphy, Eric J.
- Sanders, David
- Surace, Jason
Abstract
We present the results of a James Webb Space Telescope NIRCam investigation into the young massive star cluster (YMC) population in the luminous infrared galaxy VV 114. We identify 374 compact YMC candidates with signal-to-noise ratios ≥ 3, 5, and 5 at F150W, F200W, and F356W, respectively. A direct comparison with our HST cluster catalog reveals that ∼20% of these sources are undetected at optical wavelengths. Based on yggdrasil stellar population models, we identify 17 YMC candidates in our JWST imaging alone with F150W – F200W and F200W – F356W colors suggesting they are all very young, dusty (A_V = 5–15), and massive (10^(5.8) < M_⊙ < 6.1). The discovery of these "hidden" sources, many of which are found in the "overlap" region between the two nuclei, quadruples the number of t < Myr clusters and nearly doubles the number of t < 6 Myr clusters detected in VV 114. Now extending the cluster age distribution (dN/dτ ∝ τ^γ ) to the youngest ages, we find a slope of γ = −1.30 ± 0.39 for 10⁶ < τ(yr) < 10⁷, which is consistent with the previously determined value from 10⁷ < τ(yr) < 10^(8.5), and confirms that VV 114 has a steep age distribution slope for all massive star clusters across the entire range of cluster ages observed. Finally, the consistency between our JWST- and HST-derived age distribution slopes indicates that the balance between cluster formation and destruction has not been significantly altered in VV 114 over the last 0.5 Gyr.
Additional Information
© 2023. 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. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. S.T.L was partially supported through NASA grant HST-GO16914. A.S.E. was supported by NSF grant AST 1816838 and by NASA through grants HST-GO10592.01-A, HST-GO11196.01-A, and HST-GO13364 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. V.U. acknowledges funding support from NASA Astrophysics Data Analysis Program (ADAP) grant 80NSSC20K0450. H.I. and T.B. acknowledge support from JSPS KAKENHI grant No. JP21H01129 and the Ito Foundation for Promotion of Science. F.K. acknowledges support from the Spanish program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M, financed by MCIN/AEI/10.13039/501100011033. This work was also partly supported by the Spanish program Unidad de Excelencia Mariá de Maeztu CEX2020-001058-M, financed by MCIN/AEI/10.13039/501100011033. This research has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Finally, the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.Attached Files
Published - Linden_2023_ApJL_944_L55.pdf
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Additional details
- Eprint ID
- 120279
- Resolver ID
- CaltechAUTHORS:20230321-821906400.73
- HST-GO16914
- NASA
- AST-1816838
- NSF
- HST-GO10592.01-A
- NASA
- HST-GO11196.01-A
- NASA
- HST-GO13364
- NASA
- NAS5-26555
- NASA
- 80NSSC20K0450
- NASA
- JP21H01129
- Japan Society for the Promotion of Science (JSPS)
- Ito Foundation for Promotion of Science
- CEX2020-001058-M
- Unidad de Excelencia María de Maeztu
- MCIN/AEI/10.13039/501100011033
- Ministerio de Ciencia e Innovación (MCINN)
- NASA/JPL/Caltech
- Created
-
2023-05-16Created from EPrint's datestamp field
- Updated
-
2023-05-16Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)