2 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 Figure 1: The TANAMI VLBI images of PKS 2052 − 47 at 8 GHz (left, February 7, 2008) and 22 GHz (right, February 6, 2008). The axes are relative right ascension (RA) and declination (DEC) in milli-arcsecond (mas). On the bottom right, the scale of 10 parsec (pc) is shown. The scales are different in both images. Table I Observation log Start date End date Facility Band Comments 2009-09-05 2009-09-06 CHI 6.6 GHz - 2009-09-05 2009-09-06 TANAMI 8 & 22 GHz - 2009-09-02 2009-09-06 APEX 345 GHz - 2009-09-04 2009-09-08 Swift UVOT 2000–3500 ˚ A ∼ 2 ks per day 2009-09-04 2009-09-08 Swift XRT 0.3–10 keV ∼ 2 ks per day 2008-06-11 present Fermi LAT 100 MeV–300 GeV All-sky survey since June 11, 2008 (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. 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 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. 4. Outlook eConf C091122