tokens: filter wheels. The gray cylindrical object below the filter and shutter unit represents the cryogenic camera. Center panel : same view of the T80Cam model after cover removal, showing the two filter wheels and the shutter. Right panel : T80Cam integrated at the Cassegrain focus of the JAST/T80 telescope. A summary of the technical characteristics of T80Cam is presented in Table 2 . In addition, full technical and managerial details on T80Cam can be found in Marín-Franch et al. (2012a , 2015) . Table 2. Main technical performances of the T80Cam panoramic camera at the JAST/T80 telescope. 2.3. J-PLUS filter set The main goals of J-PLUS depend on the accurate determination of SEDs of MW stars and nearby galaxies. It is therefore clear that the J-PLUS filter set must be sensitive to both the optical continuum and the most prominent spectral features. In this context, it has been frequently demonstrated that it is possible to retrieve reliable stellar SEDs with a set of around 10–15 intermediate- to broad-band optical filters centered at key spectral regions (e.g., Bailer-Jones 2004 ; Jordi et al. 2006 ; Carrasco 2006 ). Following this strategy, the J-PLUS filter set consists of the 12 filters defined in Table 3 . Four of these are SDSS filters ( g , r , i , and z ; Fukugita et al. 1996 ) that provide the low-frequency continuum, and six are intermediate-band filters of 200–400 Å width, centered on key absorption features. These are the u filter, in common with J-PAS and located at the blue side of the 3700–4000 Å Balmer-break region, and the filters J 0395 for Ca H+K, J 0410 for H δ , J 0430 for the G band, J 0515 for the Mg b triplet, and J 0861 for the Ca triplet. The J-PLUS filter set is completed with two narrow-band filters, J 0378 and J 0660, also in common with the J-PAS filter set. These two filters are sensitive to the [O II ]/ λ 3727 and H α / λ 6563 emission lines, respectively. The three filters in common with J-PAS are envisioned as an added value for the overall calibration procedure, as they will allow second-order corrections of the ZPs to anchor the J-PAS calibration. Table 3. J-PLUS filter system. Notes. (a) In common with J-PAS; (b) SDSS. Rest-frame key spectral features matching the location of narrow- and intermediate-band filters are also indicated. The J-PLUS filters have been manufactured by Schott (Switzerland). A detailed technical description of the filter requirements and design can be found in Marín-Franch et al. (2012b) . Figure 3 shows the overall efficiency of the transmission curves of the filters, whose tabulated data can be found at the J-PLUS website 4 . Fig. 3. Overall transmission curves measured for the set of 12 J-PLUS filters, including the effect of the entire system (sky, mirrors, lenses, and CCD). The filter arrangement is tuned to provide scientifically valuable data for many fields of Astrophysics. Since the intermediate-band filters are sensitive to the strengths of key features of old stellar
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