tokens: high count rates occasionally occurred in the so-called tentacle region (Forster et al. 2014 ) near the SAA. Thus, we ran nupipeline to reject times with high count rates by setting options saamode=optimized and tentacle=yes . Background rates during the J0822+2241 observation were stable and low, and thus we adopted saamode=none and tentacle=no . We defined source regions as 30′′-radius circles centered at each optical position by taking account of the FWHM of the NuSTAR point-spread function (PSF; ≈18′′). The size is much larger than the typical size of GPs (1′′; Cardamone et al. 2009 ). Background regions were off-source circular regions with a 30′′-radius on the same detector. Then, we produced source and background spectra, and response files using the nuproducts task. The products of FPMA and FPMB were combined to provide better statistics by using the addascaspec command. The systematic uncertainty between the two modules is likely much smaller than the statistical uncertainty. Figure 3 shows the obtained spectra, as well as the background contribution. This clearly illustrates that we detected no significant emission from J0749+3337 and J0822+2241 even in the most sensitive 8–24 keV band. Count rate upper limits at 3 σ in the energy range are 5.7 × 10 −4 counts s −1 and 4.5 × 10 −4 counts s −1 , respectively. They are converted into 2–10 keV luminosities of ≈2 × 10 43 erg s −1 and ≈1 × 10 43 erg s −1 , respectively, by adopting a power-law model with Γ = 1.7. In Section 5.2 , we further investigate how large absorbing column densities are needed to be consistent with the nondetection if there are AGNs with (Section 2 ). Figure 3. NuSTAR 3–50 keV and XMM-Newton 0.2–9 keV spectra taken from the source (black crosses with circles) and background (blue dashed crosses with diamonds) regions. The figures suggest that the GPs are detected in the soft band, but not in the hard band. 4. <italic>XMM-Newton</italic> Soft X-Ray Data Analysis The XMM-Newton data for J0749+3337 and J0822+2241 were obtained through the European Photon Imaging Camera/MOS (1 and 2) and PN detectors with a duration time of ≈44 ks and ≈34 ks. All observations were performed by adopting the Prime Full Window mode and the thin filter. We reduced the data following the XMM-Newton ABC guide. 13 13 https://heasarc.gsfc.nasa.gov/docs/xmm/abc/ The raw PN and MOS data were reprocessed using pipelines of epchain and emchain , respectively. To filter periods with a high background, we created PN background light curves in the 10–12 keV band with PATTERN=0 (single events), and those of the MOS in energies above 10 keV with the same pattern selection. Regarding the J0822+2241 data, we adopted background count rate thresholds of 0.35 s −1 and 0.40 counts s −1 for the MOS and PN cameras, respectively. These are the recommended values in the guide. In contrast, we found two high-background flares during the J0749+3337 observation, and could not clearly remove the tails of the flares
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