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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

  • Author(s): Santos-Lleó, M
  • Clavel, J
  • Schulz, B
  • Altieri, B
  • Barr, P
  • Alloin, D
  • Berlind, P
  • Bertram, R
  • Crenshaw, DM
  • Edelson, RA
  • Giveon, U
  • Horne, K
  • Huchra, JP
  • Kaspi, S
  • Kriss, GA
  • Krolik, JH
  • Malkan, MA
  • Malkov, YF
  • Netzer, H
  • O'Brien, PT
  • Peterson, BM
  • Pogge, RW
  • Pronik, VI
  • Qian, BC
  • Reichert, GA
  • Rodríguez-Pascual, PM
  • Sergeev, SG
  • Tao, J
  • Tokarz, S
  • Wagner, RM
  • Wamsteker, W
  • Wilkes, BJ
  • et al.

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 μm 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 μm average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with α = -0.80 ± 0.05 (Fv ∝ vα) and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20 μm. The mid-IR bump is consistent with thermal emission from dust grains at a distance of ≳ 100 lt-d. 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 Hβ line emission in response to the optical continuum variations is τ = 16.7-5.6+5.3 days, consistent with previous measurements.

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