tokens: Apellániz 2013 ). In Section 2 , we present the characterization and definition of the GALANTE photometric system. In Section 3 , we analyse in detail the set of GALANTE standard stars. Transformation equations between the SDSS and the GALANTE photometric system are obtained in Section 4 , setting up the comparison between the synthetic magnitudes of 378 stars from the Next Generation Spectral Library (NGSL) plus 122 stars from a new catalogue from MAW in both photometric systems. Next, in Section 5 we estimate zero-points from the GALANTE photometry using the SDSS and RefCat2 . Finally, in Section 6 we summarize the results of this paper. 2 THE GALANTE PHOTOMETRIC SYSTEM 2.1 DESCRIPTION Deriving physical stellar (or galaxy) parameters is the main goal of every photometric system. In our case, we achieve this aim with a new filter set designed to plug some gaps found in previous surveys. The GALANTE photometric system has been defined using four J-PLUS filters (Cenarro et al. 2019 ) and three purpose-built filters. This composition of intermediate- and narrow-band filters covers the optical range from 3000 Å to 9000 Å. This filter set has been selected with a direct goal: deriving stellar effective temperatures for hot stars in an optimal way (Maíz Apellániz Sota 2008 ; Maíz Apellániz et al. 2014 ; Maíz Apellániz Barbá 2018 ). We will also be able to obtain the gravity and metallicity (the latter for stars cooler than 10 000 K), allowing us to discriminate between giants, supergiants, dwarfs, and between solar or SMC metallicities. In Figs 1 and 2 , we present the set-up of the filters. Figs 1(a) and (b) show the layout of the J-PLUS and GALANTE filters, respectively, leaning on the Vega spectrum. Note that in this case we only plot the transmission curves of the filters, allowing to the reader a visual location of each one. Focusing on GALANTE, Fig. 1(b) plots the configuration of the selected GALANTE filters, which enable us to measure the key zones in the spectra to derive physical parameters. In Fig. 2 , we plot the response functions of the J-PLUS and the GALANTE photometric system filters. In discontinuous grey, we represent the response curve of the CCD and mirror, while discontinuous green is the CCD, mirror and atmospheric transmission at 1.3 airmass curve. The SDSS response curves are represented in continuous black, and the other continuous curves are the GALANTE and J-PLUS filter response curves convolved with CCD, mirror and atmospheric transmission at 1.3 airmass. Using Fig. 3 , we can also explain the function of each GALANTE filter with greater accuracy. Filter F348M is a u -like filter dispose to measure the continuum from the left of the Balmer jump. We can combine this one with F420N and F450N to measure the Balmer jump on both sides and derive the T eff of stars. Both filters of our design, F420N and F450N, are the most original (compared to other large-scale recent photometric surveys) of the set-up. They have been
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