Bibcode
Sacchi, N.; Spinoglio, L.; Wilson, C. D.; Kamenetzky, J.; Rangwala, N.; Rykala, A.; Isaak, K. G.; Bendo, G. J.; Bradford, M.; Glenn, J.; Maloney, P. R.; Schirm, M. R. P.; Auld, R.; Baes, M.; Barlow, M. J.; Bock, J. J.; Boselli, A.; Buat, V.; Castro-Rodriguez, N.; Chanial, P.; Charlot, S.; Ciesla, L.; Clements, D. L.; Cooray, A.; Cormier, D.; Cortese, L.; Davies, J. I.; Dwek, E.; Eales, S. A.; Elbaz, D.; Galametz, M.; Galliano, F.; Gear, W. K.; Gomez, H. L.; Griffin, M.; Hony, S.; Levenson, L. R.; Lu, N.; Madden, S.; O'Halloran, B.; Okumura, K.; Oliver, S.; Page, M. J.; Panuzzo, P.; Papageorgiou, A.; Parkin, T. J.; Perez-Fournon, I.; Pohlen, M.; Rigby, E. E.; Roussel, H.; Sauvage, M.; Schulz, B.; Smith, M. W. L.; Stevens, J. A.; Sundar, S.; Symeonidis, M.; Trichas, M.; Vaccari, M.; Vigroux, L.; Wozniak, H.; Wright, G. S.; Zeilinger, W. W.
Bibliographical reference
The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Toledo, Spain, May 30-June 3, 2011, #322
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5
2011
Citations
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Description
We present the 450-1550 GHz spectra of three nearby Seyfert galaxies (NGC1068,
NGC7130 and NGC7582) taken with the Herschel SPIRE FTS. For the case of NGC1068
we reconstruct the nuclear spectral line energy distribution (SLED) of the CO
lines, applying nonLTE radiative transfer and a Bayesian likelihood analysis to
estimate the physical properties of the molecular gas in the circumnuclear region.
Groundbased observations of the low-J transitions with high (few arcsec) angular
resolution are required to reconstruct the nuclear SLED avoiding contamination
from colder molecular gas on larger galactic scales. We find evidence for a very
warm molecular gas component with a density ~10^3.9 cm-3, similar to that found in
previous works (Papadopoulos & Seaquist 1999, Usero et al. 2004, Kamenetzky et
al. 2011), but with a much higher temperature (~ 550 K instead of 20-160 K). The
higher-J transitions of CO are compatible with being excited in X-ray dissociation
regions (XDR). However, in order to explain the entire CO SLED a comparable
contribution from photodissociation regions (PDR) is required.