Spectrum of an IBH inside a molecular cloud core for the parameters listed in Table 1. The dotted and solid lines represent the absorbed and unabsorbed spectra, respectively. The VLA sensitivity curve corresponds to a total observation time of 1 h, while the ALMA sensitivity curve corresponds to an on-sourve time of 1 h. We extracted the 10 ks MIRI sensitivity curve from the instrument user documentation (https://jwst-docs.stsci.edu/jwst-mid-infrared-instrument/miri-performance/miri-sensitivity). The NEOWISE sensitivity is taken from Mainzer et al. (2011). The Chandra, XMM-Newton and NuSTAR sensitivity curves correspond to observation times of 100 ks, and were taken from https://chandra.harvard.edu/about/specs.html, Ferrando (2002) and Koglin et al. (2005), respectively. The COSI sensitivity corresponds to a 2 yr survey time (Tomsick et al. 2019). The Fermi sensitivity curve corresponds to a 10 yr observation for sources with Galactic latitude |b|< 30° (see https://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm). The CTA sensitivity curve corresponds to a 50 h observation time (Cherenkov Telescope Array Consortium 2019). We assumed a distance to the source of 2 kpc. First panel: accretion emission. The hot electrons emit via synchrotron and bremsstrahlung, and also Comptonise the low-energy photons. Second panel: shocked medium thermal emission and shocked outflow non-thermal emission. Third panel: non-thermal emission from protons and electrons diffusing through the core (solid lines) and the outer regions of the molecular cloud (dashed lines). Fourth panel: total spectrum, including the emission from the molecular cloud dust.