Monitoring of the optical and 2.5 – 11.7 µm spectrum and mid-IR imaging of the Seyfert 1 galaxy Mrk 279 with ISO

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Monitoring of the optical and 2.5 – 11.7 µm spectrum and mid-IR imaging of the Seyfert 1 galaxy Mrk 279 with ISO

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Title: Monitoring of the optical and 2.5 – 11.7 µm spectrum and mid-IR imaging of the Seyfert 1 galaxy Mrk 279 with ISO
Author: Santos-Lleó, M.; Clavel, J.; Schulz, B.; Altieri, B.; Barr, P.; Alloin, D.; Berlind, Perry; Bertram, R.; Crenshaw, D. M.; Edelson, R. A.; Giveon, U.; Horne, K.; Huchra, J. P.; Kaspi, S.; Kriss, G. A.; Krolik, J. H.; Malkan, M. A.; Malkov, Yu. F.; Netzer, H.; O, P. T.; Peterson, B. M.; Pogge, R. W.; Pronik, V. I.; Qian, B.-C.; Reichert, G. A.; Rodríguez-Pascual, P. M.; Sergeev, S. G.; Tao, J.; Tokarz, S.; Wagner, R. M.; Wamsteker, W.; Wilkes, Belinda Jane

Note: Order does not necessarily reflect citation order of authors.

Citation: Santos-Lleó, M., J. Clavel, B. Schulz, B. Altieri, P. Barr, D. Alloin, P. Berlind, et al. 2001. “Monitoring of the optical and 2.5 – 11.7 µm spectrum and mid-IR imaging of the Seyfert 1 galaxy Mrk 279 with ISO.” Astronomy and Astrophysics 369 (1) (April): 57–64. doi:10.1051/0004-6361:20010103.
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Abstract: Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7 micron spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the ISOCAM instrument, 4-5". The 2.5-11.7 micron average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with a spectral index alpha = -0.80+/-0.05 and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20 micron . The mid-IR bump is consistent with thermal emission from dust grains at a distance of >= 100 light-days. No significant variations of the mid-IR flux have been detected during our observing campaign, consistent with the relatively low amplitude (~10 % rms) of the optical variability during the campaign. The time delay for the Hbeta line emission in response to the optical continuum variations is 16.7 +5.3/5.6 days, consistent with previous measurements.
Published Version: doi:10.1051/0004-6361:20010103
Other Sources: https://arxiv.org/abs/astro-ph/0102356
Terms of Use: This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#LAA
Citable link to this page: http://nrs.harvard.edu/urn-3:HUL.InstRepos:30248639
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