Bibcode
García-Bernete, I.; Ramos Almeida, C.; Acosta-Pulido, J. A.
Bibliographical reference
Highlights of Spanish Astrophysics VIII, Proceedings of the XI Scientific Meeting of the Spanish Astronomical Society held on September 8-12, 2014, in Teruel, Spain, ISBN 978-84-606-8760-3. A. J. Cenarro, F. Figueras, C. Hernández-Monteagudo, J. Trujillo Bueno, and L. Valdivielso (eds.), p. 371-371
Advertised on:
5
2015
Citations
0
Refereed citations
0
Description
We present subarcsecond resolution infrared (IR) imaging and mid-IR
(MIR) spectroscopic observations of the Seyfert 1.9 galaxy NGC 2992. The
data were obtained using the Gemini North telescope and the Gran
Telescopio CANARIAS (GTC). In the N-band, the galaxy was observed with a
spatial resolution of 0.32'' (55 pc) and the imaging data reveal faint
extended emission out to ˜ 3 kpc. By comparing the MIR spectra of
the nuclear and extended emission of the galaxy, we conclude that the
origin of the extended emission is likely dust in the inner galaxy disk,
with some contribution from star formation. We also report arcsecond
resolution MIR and far-IR (FIR) imaging of the interacting system Arp
245 (NGC 2992,NGC 2993 and Arp 245 North), taken with the Spitzer Space
Telescope and the Herschel Space Observatory. For NGC 2992, we obtained
Spitzer MIR and Herschel FIR nuclear fluxes using different methods and
compared them with the subarcsecond resolution data. Using imaging data,
we find that we can only recover the nuclear fluxes obtained from high
angular resolution data at 20--25 μm, where emission from the AGN
dominates. We fitted the nuclear IR spectral energy distribution (SED)
of NGC 2992, including the 7.5--13 μm GTC/CanariCam (CC) nuclear
spectrum, with clumpy torus models. We then used the best-fitting torus
model to decompose the 5--30 μm Spitzer/IRS spectrum (˜ 630 pc)
in AGN and starburst (SB) components, using different SB templates. We
find that, whereas at shorter wavelengths the SB component dominates the
MIR emission, with 64 % contribution at 6 μm, the AGN component
reaches 90 % at 20 μm. Finally, we reproduced the dust emission in
the Arp 245 system using a set of modified blackbodies, from which we
derived dust temperatures, star-formation rates (SFRs) and dust masses.