The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system

TLDR: The MAGIC telescopes as mentioned in this paper are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma, Spain, which are designed to measure Cherennikov light from air showers initiated by gamma rays in the energy regime from around 50GeV to more than 50TeV.

About: This article is published in Astroparticle Physics.The article was published on 2016-01-01 and is currently open access. It has received 210 citations till now. The article focuses on the topics: MAGIC (telescope) & Cherenkov Telescope Array.

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Figure 4: View of the electronics room of the MAGIC telescopes. The six closed racks can be seen. They are placed on a technical raised floor (20 cm height) allowing for better cable routing.

Table 2: Contribution to noise from different hardware components as well as from the NSB for MAGIC-I pixels and MAGIC-II (in terms of pedestal RMS).

Figure 10: Schematic view on the computing network of the DAQ and the data analysis machines in MAGIC.

Figure 16: Distribution of the L0 trigger delays in MAGIC-I and MAGIC-II after applying the HYDRA optimization procedure.

Figure 17: Distribution of the L0 discriminator thresholds (DTs) applied in MAGIC-I and MAGIC-II receiver boards after the charge flatfielding procedure in order to achieve a charge threshold of 4.25 phe.

Figure 15: Example of the adjustment of the L0 delays between neighboring pixels of the 3NN logic. Shown are 4 macrocells with an example of 3NN combination between pixels pA, pB and pC. The result of the scan is shown by the blue cross. See text for details.