Dwarfs galaxies (DG) – galaxies with baryonic mass of 𝑀𝑏∼109𝑀⊙, are commonly thought to be the building blocks for the entire hierarchy of mass distribution in the Universe, being progressed during its evolution since post-recombination epochs through merging process (White & Rees 1978). Within this concept, DG in local Universe can serve as laboratories for understanding the details of physical processes regulating formation of the very first galaxies in early Universe (see review by Tolstoy et al. 2009, and more recent discussions in Henkel et al. (2022); Annibali & Tosi (2022)). Among the most important traits of DGs are their metal-poor interstellar medium (ISM) and, correspondingly, a low dust content (Henkel et al. 2022) – the features that are also commonly expected for early Universe galaxies. Observations of bright galaxies at 𝑧 > 10 conducted first by the Hubble Space Telescope (HST), and subsequently by the James Webb Space Telescope (JWST), have indeed indicated a deficient amount of dust in a set of high-𝑧 galaxies (see discussion in Finkelstein et al. 2022; Ferrara et al. 2023). In order for local DGs to indeed provide relevant information for understanding of their more distant congeners, the comparative analysis of their global emission characteristics, along with the respective properties on smaller scales, is of a high importance (relevant discussion can be found in Izotov et al. 2021; Henkel et al. 2022). A good example of a DG in local Universe is the Holmberg II (Ho II) galaxy belonging to the nearby M81 group at a distance of ≃ 3.4 Mpc. Its modest inclination angle (≈27◦ ; Sánchez-Salcedo et al. (2014)) makes Ho II a very informative source of distribution of gas and dust in the interstellar discs. Spitzer and Herschel space telescopes with the angular resolution of ∼ 2 ′′ − 5 ′′ can probe the Ho II interstellar disc with a high scrutiny. Scanning the interstellar medium (ISM) with such resolution can allow to distinguish isolated star forming regions (SFR), photodissociation (PDR) and HII regions, supernovae remnants, and can provide information about relevant physical processes. In this Letter we analyze spectra of dust emission in the range 𝜆𝜆 = 4.5, . . . 160 𝜇m from Spitzer and Herschel archival data, focusing on a few rather small-area locations. It allows us to distinguish IR emission which cannot be attributed to the isothermal dust, thus requiring existence of at least two populations of dust with different temperatures.Since the primary source of dust heating is the absorption of UV/optical photons by the dust grains, we have also utilised the highest available resolution (1.2 ′′ −1.6 ′′) FUV observations of Ho II galaxy obtained by the UVIT instrument of India’s AstroSat mission (Singh et al. 2014) as part of this study. The data correspond to 3 epochs in 2016, 2 epochs in 2019, and 3 epochs in 2020 (Vinokurov et al. 2022). These observations are crucial in understanding the UV radiation fields, responsible for modifying the dust populations and © their thermal IR emission profiles at these locations.