Probing highly obscured, self-absorbed galaxy nuclei with vibrationally excited HCN
Artikel i vetenskaplig tidskrift, 2015
We present high resolution (0.'' 4) IRAM PdBI and ALMA mm and submm observations of the (ultra) luminous infrared galaxies ((U)LIRGs) IRAS 17208-0014, Arp220, IC 860 and Zw049.057 that reveal intense line emission from vibrationally excited (nu(2) = 1) J = 3-2 and 4-3 HCN. The emission is emerging from buried, compact (r < 17-70 pc) nuclei that have very high implied mid-infrared surface brightness >5 x 10(13) L-circle dot kpc(-2). These nuclei are likely powered by accreting supermassive black holes (SMBHs) and/or hot (>200 K) extreme starbursts. Vibrational, nu(2) = 1, lines of HCN are excited by intense 14 mu m mid-infrared emission and are excellent probes of the dynamics, masses, and physical conditions of (U)LIRG nuclei when H-2 column densities exceed 10(24) cm(-2). It is clear that these lines open up a new interesting avenue to gain access to the most obscured AGNs and starbursts. Vibrationally excited HCN acts as a proxy for the absorbed mid-infrared emission from the embedded nuclei, which allows for reconstruction of the intrinsic, hotter dust SED. In contrast, we show strong evidence that the ground vibrational state (. = 0), J = 3-2 and 4-3 rotational lines of HCN and HCO+ fail to probe the highly enshrouded, compact nuclear regions owing to strong self-and continuum absorption. The HCN and HCO+ line profiles are double-peaked because of the absorption and show evidence of non-circular motions-possibly in the form of in-or outflows. Detections of vibrationally excited HCN in external galaxies are so far limited to ULIRGs and early-type spiral LIRGs, and we discuss possible causes for this. We tentatively suggest that the peak of vibrationally excited HCN emission is connected to a rapid stage of nuclear growth, before the phase of strong feedback.
galaxies: active
galaxies
galaxies: nuclei
galaxies: evolution
Författare
Susanne Aalto
Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik
S. Martin
IRAM Institut de RadioAstronomie Millimetrique
Francesco Costagliola
Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik
E. Gonzalez-Alfonso
Universidad de Alcala
Sebastien Muller
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
K. Sakamoto
Institute of Astrophysics and Astronomy, Academia Sinica Taiwan
G. A. Fuller
University of Manchester
S. G. Burillo
Observatorio Astronomico Nacional
P. van der Werf
Leiden Observatory Research Institute
R. Neri
IRAM Institut de RadioAstronomie Millimetrique
M. Spaans
University of Groningen, Kapteyn Astronomical Institute
F. Combes
LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres
S. Viti
UCL
S. Muhle
Argelander-Institut für Astronomie
L. Armus
California Institute of Technology
A. Evans
University of Virginia
National Radio Astronomy Observatory
E. Sturm
Max Planck Institut fur extraterrestrische Physik
J. Cernicharo
CSIC - Instituto de Ciencia de Materiales de Madrid (ICMM)
C. Henkel
King Abdulaziz University
Max Planck Institut fur Radioastronomie
T. R. Greve
UCL
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 584 A42Molekyler som Diagnostiska Redskap för Aktiva och Skymda Galaxer
Vetenskapsrådet (VR) (2011-4143), 2012-01-01 -- 2014-12-31.
Ämneskategorier (SSIF 2011)
Astronomi, astrofysik och kosmologi
Infrastruktur
Onsala rymdobservatorium
DOI
10.1051/0004-6361/201526410