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Near-infrared (Fe II) and Paβ imaging and spectroscopy of ARP 220

Armus, L. and Shupe, D. L. and Matthews, K. and Soifer, B. T. and Neugebauer, G. (1995) Near-infrared (Fe II) and Paβ imaging and spectroscopy of ARP 220. Astrophysical Journal, 440 (2). pp. 200-209. ISSN 0004-637X. doi:10.1086/175261.

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We have imaged the ultraluminous infrared galaxy Arp 220 in light of the near-infrared [Fe II] 1.257 μm and Paβ lines, and have obtained spectra in the J- and H-band atmospheric windows. Arp 220 is a strong source of [Fe II] and Paβ emission, with luminosities of 1.3 x 10^(41) and 9.2 x 10^(40) ergs s^(-1), respectively. The [Fe II] and Paβ emission are both extended over the central 2"-3", but with different morphologies. The Paβ line is strongly peaked at the position of the western nucleus seen at 2.2 μm (Graham et al. 1990) with a fainter "spur" in the direction of the eastern nucleus. The [Fe II] emission line shows a weak peak at the western nucleus along with diffuse emission extending to the east, but with no indication of a secondary maximum. The [Fe II] is more extended in the north-south direction than the Paβ line. Nearly 75% of the detected [Fe II] emission is spatially resolved. The overall [Fe II]-to-Paβ line flux ratio in Arp 220 is consistent with that seen over similar spatial scales in Seyfert 2 galaxies, yet larger than what is measured in galaxies with nuclear starbursts. The [Fe II]-to-Paβ line flux ratio is spatially variable being approximately 0.8 at the position of the western nucleus and approximately 2.0 at radii of up to 500 pc. We suggest that the extended [Fe II] emission is produced through the interaction of fast shocks with ambient gas in the ISM at the base of the outflowing, supernovae-driven superwind mapped by Heckman et al. (1987). The bolometric luminosity of the starburst required to power this wind is estimated to be at least 2 x 10^(11) L_☉. If the spatially unresolved [Fe II] emission is produced via a large number of supernova remnants, the implied rate is ~0.6 yr^(-1). The overall luminosity of such a starburst could account for a large fraction (1/2-1/3) of the Arp 220 energy budget, but the large deficit of ionizing photons (as counted by the Paβ luminosity) requires that the starburst be rapidly declining and/or have a low upper mass cutoff. Alternatively, dust may effectively compete with the gas for ionizing photons, or much of the ionizing radiation may escape through "holes" in the ISM. It is also possible that a buried AGN produces a large fraction of the unresolved [Fe II] and Paβ emission. We briefly discuss these possibilities in light of these new imaging and spectroscopic data.

Item Type:Article
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Armus, L.0000-0003-3498-2973
Shupe, D. L.0000-0003-4401-0430
Additional Information:© 1995 American Astronomical Society. Received 1994 July 13; accepted 1994 August 26 We would like to thank the night assistants at the Hale telescope, J. Carasco, S. Staples, and W. KcKinley, and the entire staff at the Palomar Observatory for their assistance in obtaining these data. Discussions with James Graham, Tim Heckman, and Matt Lehnert were most helpful, as were the suggestions of the referee. Infrared astronomy at Caltech is supported by grants from NASA and the NSF. This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Subject Keywords:galaxies: individual (Arp 220) - infrared: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20170214-134731167
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Official Citation:Near-infrared (Fe II) and PA Beta imaging and spectroscopy of ARP 220 Armus, L.; Shupe, D. L.; Matthews, K.; Soifer, B. T.; Neugebauer, G. Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 440, no. 1, p. 200-209 10.1086/175261
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74301
Deposited By: Ruth Sustaita
Deposited On:15 Feb 2017 05:14
Last Modified:11 Nov 2021 05:26

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