Spectroscopy of MRK 231 and NGC 4151 in the 3 MU M Region

Details Spectroscopy of MRK 231 and NGC 4151 in the 3 MU M Region Spectroscopy of MRK 231 and NGC 4151 in the 3 MU M Region

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998pasj...50..399i&link_type=abstract

Publications of the Astronomical Society of Japan, v.50, p.399-404.

Astronomy and Astrophysics

Astronomy

5

Galaxies: Active, Galaxies: Individual (Mrk 231, Ngc 4151), Infrared: Spectra

Scientific paper

We present the results of spectroscopic studies of Mrk 231 and NGC 4151 in the 3 mu m region. In the spectrum of Mrk 231, the strengths of the 3.3 mu m emission feature and the 3.4 mu m carbonaceous absorption feature are smaller than expected. The weakness of the 3.3 mu m emission feature implies that large fractions of extended H2 emission detected by Krabbe et al. (1997, AAA 67.158.058) are excited by SMBH-driven activities, and/or the 3.3 mu m emission carriers in the circumnuclear starburst region are destroyed by being exposed to energetic radiation from SMBH-driven activities. The weakness of the 3.4 mu m carbonaceous absorption feature may be due to the destruction of C--H stretching bonds in dust grains and/or lower abundance of C relative to Si, O, and Mg than that in our Galaxy, consistent to the fact that Mrk 231 is now undergoing starburst activities. In the spectrum of NGC 4151, we detect the broad Bralpha emission line, but do not detect the 3.3 mu m emission feature nor the 3.4 mu m carbonaceous absorption feature. The non-detection of the 3.3 mu m emission feature implies that nuclear starburst activities just outside the obscuring torus are weak (L_FIR< 3.7 times 10(9) LO ).

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