A Caltech Library Service

Keck OSIRIS AO LIRG Analysis (KOALA): Feedback in the Nuclei of Luminous Infrared Galaxies

U, Vivian and Medling, Anne M. and Inami, Hanae and Armus, Lee and Díaz-Santos, Tanio and Charmandaris, Vassilis and Howell, Justin and Stierwalt, Sabrina and Privon, George C. and Linden, Sean T. and Sanders, David B. and Max, Claire E. and Evans, Aaron S. and Barcos-Muñoz, Loreto and Chiang, Charleston W. K. and Appleton, Phil and Canalizo, Gabriela and Fazio, Giovanni and Iwasawa, Kazushi and Larson, Kirsten and Mazzarella, Joseph and Murphy, Eric and Rich, Jeffrey and Surace, Jason (2019) Keck OSIRIS AO LIRG Analysis (KOALA): Feedback in the Nuclei of Luminous Infrared Galaxies. Astrophysical Journal, 871 (2). Art. No. 166. ISSN 1538-4357. doi:10.3847/1538-4357/aaf1c2.

[img] PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


The role of feedback in triggering or quenching star formation and hence driving galaxy evolution can be directly studied with high-resolution integral field observations. The manifestation of feedback in shocks is particularly important to examine in galaxy mergers, where violent interactions of gas take place in the interstellar medium during the course of the galactic collision. As part of our effort to systematically study the local population of luminous infrared galaxies within the Great Observatories All-Sky LIRG Survey, we undertook the Keck OSIRIS AO LIRG Analysis observing campaign to study the gas dynamics in the inner kiloparsec regions of these systems at spatial scales of a few tens of pc. With high-resolution near-infrared adaptive optics–assisted integral field observations taken with OSIRIS on the Keck Telescopes, we employ near-infrared diagnostics such as Brγ and the rovibrationally excited H_2 lines to quantify the nuclear star formation rate and identify feedback associated with shocked molecular gas seen in 21 nearby luminous infrared galaxies. Shocked molecular gas is preferentially found in the ultraluminous infrared systems but may also be triggered at a lower-luminosity, earlier merging stage. On circumnuclear scales, AGNs have a strong effect on heating the surrounding molecular gas, though their coupling is not simply driven by AGN strength but rather is complicated by orientation, dust shielding, density, and other factors. We find that nuclear star formation correlates with merger class and diminishing projected nuclear separations. These trends are largely consistent with the picture of merger-induced starbursts in the center of galaxy mergers.

Item Type:Article
Related URLs:
URLURL TypeDescription
U, Vivian0000-0002-1912-0024
Medling, Anne M.0000-0001-7421-2944
Inami, Hanae0000-0003-4268-0393
Armus, Lee0000-0003-3498-2973
Díaz-Santos, Tanio0000-0003-0699-6083
Charmandaris, Vassilis0000-0002-2688-1956
Howell, Justin0000-0002-5924-0629
Stierwalt, Sabrina0000-0002-2596-8531
Privon, George C.0000-0003-3474-1125
Linden, Sean T.0000-0002-1000-6081
Sanders, David B.0000-0002-1233-9998
Max, Claire E.0000-0003-0682-5436
Evans, Aaron S.0000-0003-2638-1334
Barcos-Muñoz, Loreto0000-0003-0057-8892
Chiang, Charleston W. K.0000-0002-0668-7865
Appleton, Phil0000-0002-7607-8766
Canalizo, Gabriela0000-0003-4693-6157
Fazio, Giovanni0000-0002-0670-0708
Iwasawa, Kazushi0000-0002-4923-3281
Larson, Kirsten0000-0003-3917-6460
Mazzarella, Joseph0000-0002-8204-8619
Murphy, Eric0000-0001-7089-7325
Rich, Jeffrey0000-0002-5807-5078
Surace, Jason0000-0001-7291-0087
Additional Information:© 2019. The American Astronomical Society. Received 2018 August 1; revised 2018 November 8; accepted 2018 November 16; published 2019 January 29. We thank the anonymous referee and the statistical editor for thoughtful suggestions that significantly improved our manuscript. We appreciate informative discussions with B. Groves and P. Creasey regarding photoionization models and wish to acknowledge helpful communication with D. Calzetti regarding dust extinction curves. We thank all of the Keck staff for help with carrying out the observations. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We also acknowledge the Evans Remote Observing Room at UC Irvine for a number of the remote observing sessions carried out there. VU acknowledges funding support from the University of California Chancellor's Postdoctoral Fellowship, JPL Contract/IRAC GTO grant No. 1256790, and NSF grant AST-1412693. Support for AMM is provided by NASA through Hubble Fellowship grant #HST-HF2-51377, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. TD-S acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT project 1151239. GCP acknowledges support from the University of Florida. This work was conducted in part at the Aspen Center for Physics, which is supported by NSF grant PHY-1607611; we thank the center for its hospitality during the Astrophysics of Massive Black Hole Mergers workshop in 2018 June and July. This research has 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. Facilities: Keck: I/II (OSIRIS - , AO) - .
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
University of CaliforniaUNSPECIFIED
NASA Hubble FellowshipHST-HF2-51377
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)31130005
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1151239
University of FloridaUNSPECIFIED
Subject Keywords:galaxies: active; galaxies: interactions; galaxies: nuclei
Issue or Number:2
Record Number:CaltechAUTHORS:20190130-121937282
Persistent URL:
Official Citation:Vivian U et al 2019 ApJ 871 166
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:92529
Deposited By: George Porter
Deposited On:31 Jan 2019 00:07
Last Modified:16 Nov 2021 03:51

Repository Staff Only: item control page