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GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114

Evans, A. S. and Frayer, D. T. and Charmandaris, Vassilis and Armus, Lee and Inami, Hanae and Surace, Jason and Linden, Sean and Soifer, B. T. and Diaz-Santos, Tanio and Larson, Kirsten L. and Rich, Jeffrey A. and Song, Yiqing and Barcos-Munoz, Loreto and Mazzarella, Joseph M. and Privon, George C. and U, Vivian and Medling, Anne M. and Böker, Torsten and Aalto, Susanne and Iwasawa, Kazushi and Howell, Justin H. and van der Werf, Paul and Appleton, Philip and Bohn, Thomas and Brown, Michael J. I. and Hayward, Christopher C. and Hoshioka, Shunshi and Kemper, Francisca and Lai, Thomas and Law, David and Malkan, Matthew A. and Marshall, Jason and Murphy, Eric J. and Sanders, David and Stierwalt, Sabrina (2022) GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114. Astrophysical Journal Letters, 940 (1). Art. No. L8. ISSN 2041-8205. doi:10.3847/2041-8213/ac9971.

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James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) images of the luminous infrared (IR) galaxy VV 114 are presented. This redshift ∼0.020 merger has a western component (VV 114W) rich in optical star clusters and an eastern component (VV 114E) hosting a luminous mid-IR nucleus hidden at UV and optical wavelengths by dust lanes. With MIRI, the VV 114E nucleus resolves primarily into bright NE and SW cores separated by 630 pc. This nucleus comprises 45% of the 15 μm light of VV 114, with the NE and SW cores having IR luminosities, L_(IR)(8 − 1000 μm) ∼ 8 ± 0.8 × 10¹⁰ L_⊙ and ∼ 5 ± 0.5 × 10¹⁰ L_⊙, respectively, and IR densities, Σ_(IR) ≳ 2 ± 0.2 × 10¹³ L_⊙ kpc⁻² and ≳ 7 ± 0.7 × 10¹² L_⊙ kpc⁻², respectively—in the range of Σ_(IR) for the Orion star-forming core and the nuclei of Arp 220. The NE core, previously speculated to have an active galactic nucleus (AGN), has starburst-like mid-IR colors. In contrast, the VV 114E SW core has AGN-like colors. Approximately 40 star-forming knots with L_(IR) ∼ 0.02–5 × 10¹⁰ L_⊙ are identified, 28% of which have no optical counterpart. Finally, diffuse emission accounts for 40%–60% of the mid-IR emission. Mostly notably, filamentary polycyclic aromatic hydrocarbon (PAH) emission stochastically excited by UV and optical photons accounts for half of the 7.7 μm light of VV 114. This study illustrates the ability of JWST to detect obscured compact activity and distributed PAH emission in the most extreme starburst galaxies in the local universe.

Item Type:Article
Related URLs:
URLURL TypeDescription
Evans, A. S.0000-0003-2638-1334
Frayer, D. T.0000-0003-1924-1122
Charmandaris, Vassilis0000-0002-2688-1956
Armus, Lee0000-0003-3498-2973
Inami, Hanae0000-0003-4268-0393
Surace, Jason0000-0001-7291-0087
Linden, Sean0000-0002-1000-6081
Soifer, B. T.0000-0002-8112-1132
Diaz-Santos, Tanio0000-0003-0699-6083
Larson, Kirsten L.0000-0003-3917-6460
Rich, Jeffrey A.0000-0002-5807-5078
Song, Yiqing0000-0002-3139-3041
Barcos-Munoz, Loreto0000-0003-0057-8892
Mazzarella, Joseph M.0000-0002-8204-8619
Privon, George C.0000-0003-3474-1125
U, Vivian0000-0002-1912-0024
Medling, Anne M.0000-0001-7421-2944
Böker, Torsten0000-0002-5666-7782
Aalto, Susanne0000-0002-5828-7660
Iwasawa, Kazushi0000-0002-4923-3281
Howell, Justin H.0000-0001-6028-8059
van der Werf, Paul0000-0001-5434-5942
Appleton, Philip0000-0002-7607-8766
Bohn, Thomas0000-0002-4375-254X
Brown, Michael J. I.0000-0002-1207-9137
Hayward, Christopher C.0000-0003-4073-3236
Kemper, Francisca0000-0003-2743-8240
Lai, Thomas0000-0001-8490-6632
Law, David0000-0002-9402-186X
Malkan, Matthew A.0000-0001-6919-1237
Marshall, Jason0000-0001-7712-8465
Murphy, Eric J.0000-0001-7089-7325
Sanders, David0000-0002-1233-9998
Stierwalt, Sabrina0000-0002-7532-3328
Additional Information:The authors thank the anonymous referee for comments that improved the overall quality of the manuscript. The authors also thank the members of the international MIRI Instrument Team for their work to bring the MIRI instrument to fruition. The research was supported by NASA grants JWST-ERS-01328, HST-GO-15472, and HST-GO-16914. Y.S. was funded in part by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. V.U acknowledges funding support from NASA Astrophysics Data Analysis Program (ADAP) grant 80NSSC20K0450. K.I. acknowledges support by the Spanish MCIN under grant PID2019-105510GB-C33/AEI/10.13039/501100011033. S.A. gratefully acknowledges support from an ERC Advanced grant 789410, from the Swedish Research Council and from the Knut and Alice Wallenberg (KAW) Foundation. H.I. and T.B. acknowledge support from JSPS KAKENHI Grant Number JP21H01129 and the Ito Foundation for Promotion of Science. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors acknowledge the usage of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology, and CARTA (Comrie et al. 2021).
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
National Radio Astronomy ObservatoryUNSPECIFIED
Ministerio de Ciencia e Innovación (MICINN)PID2019-105510GB-C33/AEI/10.13039/501100011033
European Research Council (ERC)789410
Swedish Research CouncilUNSPECIFIED
Knut and Alice Wallenberg FoundationUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP21H01129
Ito Foundation for Promotion of ScienceUNSPECIFIED
Issue or Number:1
Record Number:CaltechAUTHORS:20221205-666301600.21
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:118244
Deposited By: Research Services Depository
Deposited On:06 Jan 2023 23:20
Last Modified:06 Jan 2023 23:20

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