Title: Phased-Array Mode for TP-array Continuum Observations Authors: Seiji Kameno, Tsuyoshi Sawada, Shun Ishii, and Edward Fomalont (JAO) ALMA Total-Power (TP) array observing mode compensates zero-spacing visibilities for image fidelity of extended sources. Sensitivity on TP-array for continuum observation is significantly affected by factor of 100 due to receiver gain variation (Sawada, Ishii, and Siringo 2019). We propose a multi-field phase-array capability to improve the sensitivity in TP-array continuum observations. This capability employs the Morita array, consisting of twelve 7-m antennas, as a multi-pixel camera with a field of view (FoV) of the 7-m antennas and a resolution identical to the synthesized beam. Thus, spatial frequency range of 0 – 45m spacing will be seamlessly acquired. The multi-pixel capability is realized by parallel processing of phasing (see left figure) giving phase shift of fj,k = 2p (ujlk + vjmk) /l , where l is wavelength, uj and vj stand for the j-th antenna coordinates projected to the source direction and lk and mk are directional cosine of the k-th pixel. The right figure shows a tentative configuration of Nyquist-sampled 121 pixels within the 7-m antenna FoV. These pixels are numerically formed, then, they can overlap to mediate contamination from sidelobes. Receiver gain variation influences all of pixels equally and won’t affect uniformity inside the FoV. Antenna fast scanning under the phased-array mode allows us to take images wider than the FoV. Image sampling should be frequent enough to have overlap between adjacent FoVs for stitching. Scan pattern and speed should be optimized to discriminate the celestial signal from fluctuations of the atmosphere and receiver gain. We will discuss about expected performance of the phase array.