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We show a Swift /XRT spectrum in the 0.3 − 6 keV energy range with 2.5 ks integration in Figure 2, taken on September 6, 2009. We used XSPEC version 12.5 to fit an absorbed power-law to the spectrum with a fixed Galactic neutral hydrogen column density of 2.79 × 10 20 cm − 2 [10], and obtained a photon index of 1.53 ± 0.11. The value of the Cash statistic after fitting is 21.2 with 20 degrees of freedom. The photon statistics above 6 keV were not sufficient to obtain spectral data. 

We show a weekly-binned Fermi LAT light curve (100 MeV − 100 GeV) from August 2008 to July 2009 in Figure 3, which is the first 11-month of the mis- sion. We used Fermi Science Tools version v9r10 and instrumental response functions (IRFs) version P6 V3 DIFFUSE to analyze LAT data. From Figure 3, we could see that there is a gradual rise in the flux density with time, especially when time approached to July 2009. 

We present a preliminary broadband SED of PKS 2052 − 47 from radio to gamma-ray in Figure 4. As shown in Figure 4, the synchrotron self-Compton 

(SSC) peak appears to be higher than the synchrotron emission peak in our result. This is consistent with the results of [11], which was based on the historical data. To further understand the physical processes involved in the active phase of PKS 2052 − 47, SED modeling is needed. The results of this will be presented else- where. 

## 4. Outlook 

The multiwavelength campaign of PKS 2052 − 47 provides an opportunity to investigate the emission mechanisms and physical processes involved in this ra- dio quasar during its flaring state. When all datasets will be collected, we will be able to compare the VLBI parsec-scale images at 8 GHz and 22 GHz with the re- sults from the other wavelengths, especially that of high energies, to probe the source of high-energy emis- sion. Also, the varying broadband SED modeling will be necessary to understand the source in its active phase. 

