Page:Epjconf mmUniverse2021 00017.pdf/5

EPJ Web of Conferences 257, 00017 (2022) mm Universe @ NIKA2 despite the large size of the map needed due to the large FoV, the source is well identified in the center with a signal-to-noise ratio (SNR) of ∼10.



Figure 2. Venus brightness temperature as a function of frequency. We present a collection of radio and mm wavelength measurements including those of KISS. The blue and cyan lines represent two models for the Venus brightness temperature. [12]



Figure 3. Uncalibrated spectral mapping of Jupiter with 8 GHz resolution in frequency. The large bin has been adopted to increase the sensitivity. We show the mean value from all detectors. The central frequency in GHz is given at the top of each map.

The presented spectral maps are the result of a portion of the original (typical) 90x90 arcmin2 sky coverage, obtained in 10 minutes of total integration time per observation. We can calibrate the spectral response by exploiting the integrated spectrum of such observations: in other words, we obtain a calibration factor between the detector response and the astrophysical signal per electromagnetic bin. Rh