Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH, ¹⁸OH, O I, HCN, and NH₃^⋆

¹ Universidad de Alcalá de HenaresDepartamento de Física, Campus Universitario, 28871 Alcalá de Henares, Madrid, Spain
e-mail: eduardo.gonzalez@uah.es
² Naval Research Laboratory, Remote Sensing Division, 4555 Overlook Ave SW, Washington, DC 20375, USA
³ Max-Planck-Institute for Extraterrestrial Physics (MPE), Giessenbachstraße 1, 85748 Garching, Germany
⁴ Department of Astronomy, University of Maryland, College Park, MD 20742, USA
⁵ Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Code 661, Greenbelt, MD 20771, USA
⁶ Cornell University, Astronomy Department, Ithaca, NY 14853, USA
⁷ University of Oxford, Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK
⁸ Sackler School of Physics & Astronomy, Tel Aviv University, Ramat Aviv 69978, Israel

Received: 6 September 2011
Accepted: 3 February 2012

Abstract

Full range Herschel/PACS spectroscopy of the (ultra)luminous infrared galaxies NGC 4418 and Arp 220, observed as part of the SHINING key programme, reveals high excitation in H₂O, OH, HCN, and NH₃. In NGC 4418, absorption lines were detected with E_lower > 800 K (H₂O), 600 K (OH), 1075 K (HCN), and 600 K (NH₃), while in Arp 220 the excitation is somewhat lower. While outflow signatures in moderate excitation lines are seen in Arp 220 as have been seen in previous studies, in NGC 4418 the lines tracing its outer regions are redshifted relative to the nucleus, suggesting an inflow with Ṁ ≲ 12 M_⊙ yr^-1. Both galaxies have compact and warm (T_dust ≳ 100 K) nuclear continuum components, together with a more extended and colder component that is much more prominent and massive in Arp 220. A chemical dichotomy is found in both sources: on the one hand, the nuclear regions have high H₂O abundances,  ~10^-5, and high HCN/H₂O and HCN/NH₃ column density ratios of 0.1−0.4 and 2−5, respectively, indicating a chemistry typical of evolved hot cores where grain mantle evaporation has occurred. On the other hand, the high OH abundance, with OH/H₂O ratios of  ~0.5, indicates the effects of X-rays and/or cosmic rays. The nuclear media have high surface brightnesses (≳10¹³ L_⊙/kpc²) and are estimated to be very thick (N_H ≳ 10²⁵ cm^-2). While NGC 4418 shows weak absorption in H₂¹⁸O and ¹⁸OH, with a ¹⁶O-to-¹⁸O ratio of  ≳250−500, the relatively strong absorption of the rare isotopologues in Arp 220 indicates ¹⁸O enhancement, with ¹⁶O-to-¹⁸O of 70−130. Further away from the nuclear regions, the H₂O abundance decreases to  ≲10^-7 and the OH/H₂O ratio is reversed relative to the nuclear region to 2.5−10. Despite the different scales and morphologies of NGC 4418, Arp 220, and Mrk 231, preliminary evidence is found for an evolutionary sequence from infall, hot-core like chemistry, and solar oxygen isotope ratio to high velocity outflow, disruption of the hot core chemistry and cumulative high mass stellar processing of ¹⁸O.