Volume 610, February 2018
|Number of page(s)||7|
|Published online||05 March 2018|
European Space Agency, European Space Astronomy Centre,
C/ Bajo el Castillo s/n,
28692 Villanueva de la Cañada,
2 Astronomical Observatory of Jagiellonian University, ul. Orla 171, 30-244 Krakow, Poland
3 Mt. Suhora Observatory, Pedagogical University, ul. Podchorazych 2, Krakow 30-084, Poland
4 Finnish Centre for Astronomy with ESO, University of Turku, Turku, Finland
5 Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku, Finland
6 Aalto University, Metsähovi Radio Observatory, Metsähovintie 114, 02540 Kylmälä, Finland
7 Aalto University, Department of Electronics and Nanoengineering, PO Box 15500, 00076 Aalto, Finland
8 Tartu Observatory, Observatooriumi 1, 61602 Töravere, Estonia
9 Institute for Astronomy, Astrophysics, Space Applications, and Remote Sensing, National Observatory of Athens, Metaxa & Vas. Pavlou St., 15236 Penteli, Athens, Greece
10 British Astronomical Association Variable Star Section, 67 Ellerton Road, Kingstanding, Birmingham, UK
Accepted: 3 December 2017
Context. The blazar OJ 287 has shown a ≈12 year quasi-periodicity over more than a century, in addition to the common properties of violent variability in all frequency ranges. It is the strongest known candidate to have a binary singularity in its central engine.
Aim. We aim to better understand the different emission components by searching for correlated variability in the flux over four decades of frequency measurements.
Methods. We combined data at frequencies from the millimetric to the visible to characterise the multifrequency light curve in April and May 2010. This includes the only photometric observations of OJ 287 made with the Herschel Space Observatory: five epochs of data obtained over 33 days at 250, 350, and 500 μm with Herschel-SPIRE.
Results. Although we find that the variability at 37 GHz on timescales of a few weeks correlates with the visible to near-IR spectral energy distribution, there is a small degree of reddening in the continuum at lower flux levels that is revealed by the decreasing rate of decline in the light curve at lower frequencies. However, we see no clear evidence that a rapid flare detected in the light curve during our monitoring in the visible to near-IR light curve is seen either in the Herschel data or at 37 GHz, suggesting a low-frequency cut-off in the spectrum of such flares.
Conclusions.We see only marginal evidence of variability in the observations with Herschel over a month, although this may be principally due to the poor sampling. The spectral energy distribution between 37 GHz and the visible can be characterised by two components of approximately constant spectral index: a visible to far-IR component of spectral index α = −0.95, and a far-IR to millimetric spectral index of α = −0.43. There is no evidence of an excess of emission that would be consistent with the 60 μmdust bump found in many active galactic nuclei.
Key words: Galaxies / BL Lacertae objects / individual / OJ 287
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
The photometry data (Table 4) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/610/A74
© ESO 2018
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