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The 3.3 μm Polycyclic Aromatic Hydrocarbon Emission as a Star Formation Rate Indicator

Kim, Ji Hoon and Im, Myungshin and Lee, Hyung-Mok and Lee, Myung Gyoon and Jun, Hyunsung David and Nakagawa, Takao and Matsuhara, Hideo and Wada, Takehiko and Oyabu, Shinki and Takagi, Toshinobu and Inami, Hanae and Ohyama, Youichi and Yamada, Rika and Helou, George and Armus, Lee and Shi, Yong (2012) The 3.3 μm Polycyclic Aromatic Hydrocarbon Emission as a Star Formation Rate Indicator. Astrophysical Journal, 760 (2). Art. No. 120. ISSN 0004-637X. doi:10.1088/0004-637X/760/2/120. https://resolver.caltech.edu/CaltechAUTHORS:20121219-145701379

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Abstract

Polycyclic aromatic hydrocarbon (PAH) emission features dominate the mid-infrared spectra of star-forming galaxies and can be useful to calibrate star formation rates (SFRs) and diagnose ionized states of grains. However, the PAH 3.3 μm feature has not been studied as much as other PAH features since it is weaker than others and resides outside of Spitzer capability. In order to detect and calibrate the 3.3 μm PAH emission and investigate its potential as an SFR indicator, we carried out an AKARI mission program, AKARI mJy Unbiased Survey of Extragalactic Sources (AMUSES), and compared its sample with various literature samples. We obtained 2-5 μm low-resolution spectra of 20 flux-limited galaxies with mixed spectral energy distribution classes, which yielded the detection of the 3.3 μm PAH emission from 3 out of 20 galaxies. For the combined sample of AMUSES and literature samples, the 3.3 μm PAH luminosities correlate with the infrared luminosities of star-forming galaxies, albeit with a large scatter (1.5 dex). The correlation appears to break down at the domain of ultraluminous infrared galaxies (ULIRGs), and the power of the 3.3 μm PAH luminosity as a proxy for the infrared luminosity is hampered at log[L P_(AH3.3) erg^(–1) s^(–1)] > ~42.0. Possible origins for this deviation in the correlation are discussed, including contributions from active galactic nuclei and strongly obscured young stellar objects, and the destruction of PAH molecules in ULIRGs.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/760/2/120DOIArticle
http://iopscience.iop.org/0004-637X/760/2/120PublisherArticle
ORCID:
AuthorORCID
Im, Myungshin0000-0002-8537-6714
Lee, Hyung-Mok0000-0003-4412-7161
Jun, Hyunsung David0000-0003-1470-5901
Inami, Hanae0000-0003-4268-0393
Ohyama, Youichi0000-0001-9490-3582
Helou, George0000-0003-3367-3415
Armus, Lee0000-0003-3498-2973
Shi, Yong0000-0002-8614-6275
Additional Information:© 2012 American Astronomical Society. Received 2011 December 8; accepted 2012 September 29; published 2012 November 15. The authors sincerely appreciate the anonymous referee’s helpful comments and suggestions to improve the quality of this paper. They also thank Yanling Wu for her work leading to this paper. This work was supported by a Korean Research Foundation (KRF) grant funded by the Korean government (MEST), No. 2010–0000712. This research is based on observations with AKARI, a JAXA project with the participation of ESA.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
National Research Foundation of KoreaUNSPECIFIED
Ministry of Education, Science and Technology (Korea)2010-0000712
Subject Keywords:galaxies: active; galaxies: ISM; galaxies: starburst; galaxies: star formation; infrared: galaxies
Issue or Number:2
DOI:10.1088/0004-637X/760/2/120
Record Number:CaltechAUTHORS:20121219-145701379
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20121219-145701379
Official Citation:The 3.3 μm Polycyclic Aromatic Hydrocarbon Emission as a Star Formation Rate Indicator Ji Hoon Kim, Myungshin Im, Hyung Mok Lee, Myung Gyoon Lee, Hyunsung David Jun, Takao Nakagawa, Hideo Matsuhara, Takehiko Wada, Shinki Oyabu, Toshinobu Takagi, Hanae Inami, Youichi Ohyama, Rika Yamada, George Helou, Lee Armus, and Yong Shi doi:10.1088/0004-637X/760/2/120
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36060
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:19 Dec 2012 23:25
Last Modified:09 Nov 2021 23:19

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