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tokens: of LLAGNs, its 2–10 keV intrinsic luminosity is only , or ∼10 −8.5 of the Eddington luminosity of the putative SMBH (Yang et al. 2015 , hereafter Y15 ). Using NSF’s Karl G. Jansky Very Large Array (VLA) observations at a central frequency of 6.6 GHz with a bandwidth of 2 GHz, Y15 detected a weak radio source (with a luminosity of νL ν [6.6 GHz] ) coincident with the optical nucleus of M32, which they argued is most likely the radio counterpart of the SMBH. Together with Sgr A* and M31* (Crane et al. 1992 ; Yang et al. 2017 ), the LLAGN in M32 provides a rare but promising opportunity to study feedback from the most under-luminous SMBHs on parsec-scales. In this work, we present follow-up high-resolution, dual-band VLA observations to further explore the nuclear radio source in M32. Section 2 describes our new VLA observations and data reduction procedures. Section 3 presents the main observational results, in particular, morphological and spectral properties of the nuclear source. Section 4 is devoted to understanding the nature of this source. To be consistent with previous work, we adopt a distance of 780 kpc for M32 (1′′ corresponds to 3.8 pc; Young et al. 2008 ). Quoted errors are at the 1 σ confidence level, unless otherwise stated. 2. Observations and Data Preparation Our VLA A-configuration observations of M32 were initially scheduled for the 2015A semester (Project ID: 15A-049, PI: L. Sjouwerman). However, due to a failure in the antenna control system, only one of the three requested observing epochs was successfully conducted, which resulted in two 3 hr integrations on 2015 July 20, one in C -band and the other in Ku-band. Subsequently, on 2016 December 13, 2016 December 14, and 2017 January 22, we conducted three additional epochs of dual-band observations through a new program (Project ID: 16B-073) with the same setting as in 15A-049. In all four epochs, the C -band (Ku-band) observation was centered at 6.0 (15.0) GHz, with a bandwidth of 4 (6) GHz as captured with the 3 bit samplers. Using a visibility integration time of 2 s, the available bandwidth was divided into 1 MHz dual polarization channels to aid the selective removal of RFI. A phase-referenced mode was adopted, with J0038+4137 serving as phase calibrator every 10 minutes for C -band and every 8 minutes for Ku-band. 3C48 7 7 3C48 underwent a major event since 2016; however, it did not significantly affect our data analysis and result (private communication with NRAO helpdesk). See also https://science.nrao.edu/facilities/vla/docs/manuals/obsguide/modes/pol . was used as flux and bandpass calibrator with a 3% systematic uncertainty (Perley Butler 2013 ). In total, we obtained 8.5 hr on-source integration for C -band and 10.0 hr for Ku-band. A log of the VLA observations is given in Table 1 . Table 1 Log of VLA observations Note. (1) Observation date. (2) Central frequency. (3) Synthesized beam FWHM of major and minor axes, and position angle of the major axis.