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tokens: in the standard manner for mid-infrared ground-based imaging observations, including dark subtractions and flat fielding. The flux calibration of V1280 Sco was achieved using measurements of the two standard stars listed in Cohen et al. ( 1999 ): λ Sgr for N8.8, N11.7, and Q18.8, and μ Cep for Q24.5. The aperture size for the photometry was set to be 2′′ in radius. For the NL spectroscopy of V1280 Sco on Day 150, a slit width of 033 was used. As in the case of the imaging observations, only the secondary mirror chopping was performed at a frequency of ∼0.5 Hz with a 10′′ throw in the north–south direction. The position angle (PA) of the slit was set to 0° so that images at both chopping positions would fall on the slit. Spectra collected at both chopping positions were co-added, resulting in the total on-source integration time of 20 s for NL spectroscopy (see Table 2 ). The data reduction was performed in the standard manner for mid-infrared ground-based spectroscopic observations, including dark subtraction, flat fielding using domeflat, wavelength calibration using atmospheric lines, and distortion correction. Finally, a one-dimensional spectrum of V1280 Sco was extracted. Atmospheric absorption in the extracted spectrum was corrected by division by the spectrum of a standard star, λ Sgr, whose absolute spectrum is provided in Cohen et al. ( 1999 ). The absolute flux calibration including the correction for slit efficiency was performed by simply scaling the flux level of the obtained spectrum to match the photometric data in the 8.8 and 11.7 μ m bands. Table 2 Summary of Spectroscopic Observations Note. a The epochs of the observations with Subaru/COMICS, Gemini-S/T-ReCS, and AKARI /IRC in days after the discovery. 2.2. Gemini-S/T-ReCS data Mid-infrared imaging and spectroscopic observations of V1280 Sco on Days 1272, 1616, and 1947 were carried out at the Gemini-South observatory under the Subaru/Gemini Time Exchange Programmes GS-2010B-C-7 on 2010 August 1, GS-2011B-C-4 on 2011 July 10, and GS-2012A-C-5 on 2012 June 6. For the imaging portion, five medium-band filters, Si-1, Si-3, Si-5, Qa, and Qb, were used. The center wavelength, λ c , and bandwidth, Δ λ , are summarized in Table 1 . The pixel scale of the T-ReCS detector was 009 and the FOV was 288 × 216. Both chopping and nodding were performed to cancel out the high background radiation and the chopping residual pattern. The chopping was performed at a frequency of ∼3 Hz with a 15′′ throw in the north–south direction. The on-source integration time is summarized in Table 1 . The mireduce task included in the Gemini IRAF package ( https://www.gemini.edu/node/10795 ) was used to produce final co-added, chop-subtracted, and nod-subtracted data from the raw data files. The flux calibration was accomplished by observing the Cohen standard star HD 151680 (Cohen et al. 1999 ). The aperture size for the photometry was set to be 2′′ in radius. A slit width of 035 was used for the N-band