Abstract
The flat spectrum radio quasar PKS 1510-089 is a monitored target in many wavelength bands due to its high variability. It was detected as a very-high-energy (VHE) γ-ray emitter with H.E.S.S. in 2009, and has since been a regular target of VHE observations by the imaging Cherenkov observatories H.E.S.S. and MAGIC. In this paper, we summarize the current state of results focusing on the monitoring effort with H.E.S.S. and the discovery of a particularly strong VHE flare in 2016 with H.E.S.S. and MAGIC. While the source has now been established as a weak, but regular emitter at VHE, no correlation with other energy bands has been established. This is underlined by the 2016 VHE flare, where the detected optical and high-energy γ-ray counterparts evolve differently than the VHE flux.
Highlights
The correlations between blazar emissions in different energy bands are best probed with long-term monitoring, providing unbiased sampling
The discrete cross-correlation function (DCCF) between the VHE and HE γ-ray fluxes is shown in Figure 3b for the full time frame and 2015-2016, respectively
The HE γ-ray spectra in the two VHE observation windows are compatible within errors being Γ LAT = 1.4 ± 0.2stat during the H.E.S.S. time frame and Γ LAT = 1.7 ± 0.2stat during the MAGIC
Summary
The correlations between blazar emissions in different energy bands are best probed with long-term monitoring, providing unbiased sampling. In the very-high-energy (VHE) γ-ray band (E > 100 GeV) the monitoring effort is limited by sensitivity, e.g., for FACT and HAWC [3], or by time constraints due to competition with other objects. The latter strongly influences the monitoring efforts of the three large imaging atmospheric Cherenkov telescope (IACT) facilities H.E.S.S., MAGIC and VERITAS. The DCCF between the VHE and HE γ-ray fluxes is shown in Figure 3b for the full time frame and 2015-2016, respectively. The black dashed line marks the zero-flux level for the VHE band
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