Dust evolution starts at the earliest stage of star formation, during the formation of cores that slowly contract to form pre-stellar cores (PSC), to the collapse of these PSCs into protostars and protoplanetary disks (PPD). The contraction time of PSCs is still a debated question and ranges from less than 1 My [1,2] to 10 My lifetime [3]. PSCs are dense (>10 5 H . cm −3 ), compact (< 10 4 AU) and cold (5-12 K) objects, making their study difficult. They are very opaque and most gaseous species are depleted onto grains preventing the study of the inner parts. Dust is the only tracer that is present from cloud edge to the densest part, allowing to characterize cloud density structure. Nevertheless, dust itself is a poor tracer in visible and near-infrared (NIR) since its absorption is too high to detect the reddening of the stars above A V ∼ 50 mag. Recent observations of PSCs with Spitzer [4][5][6] and PPDs with SPHERE [7] in scattered light has brought hope to put more constraints on dust properties. Indeed, all parameters involved in the dust emission (dust temperature, density, grain size, emissivity and spectral index) are varying across the cloud leading to degenerate solutions when dust emission is used alone [8]. Studies combining dust scattering and emission reproduced successfully PPD observations, allowing to constrain the geometry and density structure in PPDs [e.g. 9]. On the other hand, a consistent multi-wavelength modeling of PSCs remains an unachieved goal. Grain emissivity in the far-infrared (FIR) has been linked consistently to its absorption efficiency in the near-infrared (NIR) at short wavelengths only [10] or at low resolution with 5 Planck **data** [11], and thus never reproducing observations of the densest part. With our on-going NIKA2 open time Program, we aim at building a consistent multiwavelength picture of two neighbor molecular clouds, L183 and L134 (116±6 pc [C. Zucker priv. comm.] and 107±5 pc [12] respectively) hosting 4 PSCs.