Santos-Lleó, M.Clavel, J.Schulz, B.Altieri, B.Barr, P.Alloin, D.Berlind, PerryBertram, 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, Belinda2017-02-142001Santos-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:10.1051/0004-6361:20010103.0004-6361http://nrs.harvard.edu/urn-3:HUL.InstRepos:30248639Mid-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.en-USGalaxies: activeGalaxies: individual: Mrk 279Galaxies: nucleiGalaxies: SeyfertInfrared: galaxiesJournal Article2017-02-1410.1051/0004-6361:20010103