Power of SMILES in studying the mid-IR dust properties of galaxies at cosmic noon. Left: The top-left image shows a group of galaxies at z ∼ 0.7 − 2.3 (matching the redshift range in this paper) in F444W/F200W/F090W NIRCam colours (JADES). The pre-JWST mid-IR view of these galaxies is shown in the top row from Spitzer IRAC and MIPS (GOODS survey; Dickinson & FIDEL Team 2007; Ashby et al. 2015). The bottom two rows show the mid-IR images with JWST MIRI at 5.6, 7.7, 10, 12.8, 15, 18, 21, and 25.5 μm (SMILES). The PSF sizes are shown with white circles in the corners (diameter of the circle is the FWHM). The unprecedented improvement of MIRI in spatial resolution (0.19 to 0.86″ from 5.6 to 25.5 μm) compared to that of IRAC (1.72 and 1.88″ at 5.8 and 8 μm) and MIPS 24 μm (6″) makes it possible to observe the mid-IR emission of individual typical galaxies at these redshifts. Right: The IR dust SEDs of typical galaxies at z = 1.8 with IR luminosities of 10^10.5 − 10^11.5 L_⊙ (Rieke et al. 2009; corresponding to obscured SFRs of ∼5 − 50 M_⊙/yr assuming the Kennicutt & Evans 2012 calibration) in grey shaded region, along with 3σ sensitivity limits of the GOODS-S Herschel/PACS (green; Magnelli et al. 2013), Spitzer/MIPS 24 μm confusion limit (red; 56 μJy, Dole et al. 2004), Spitzer IRAC Channels 3 and 4 (blue; Guo et al. 2013), and the MIRI sensitivities of SMILES in ∼10 − 30 min exposures (orange; Section 2.1). MIRI filter transmission curves are shown with orange shaded regions. The high sensitivity and multi-band capability of MIRI enables measurements and characterisations of IR emission of typical galaxies at cosmic noon.