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Herschel FIR continuum data obtained as part of the Hi-GAL survey have beenused, together with the GLIMPSE 8 $\mu$m and MIPSGAL 24 $\mu$m data, to attemptthe first 3D-decomposition of dust emission associated with atomic, molecularand ionized gas at 15 arcmin angular resolution. Our initial test case is a2$\times$2 square degrees region centred on (l,b)=(30$^{\circ}$,0$^{\circ}$), adirection that encompasses the origin point of the Scutum-Crux Arm at the tipof the Galactic Bar. Coupling the IR maps with velocity maps specific fordifferent gas phases (HI 21cm, $^{12}$CO and $^{13}$CO, and RRLs), we estimatethe properties of dust blended with each of the gas components and at differentGalactocentric distances along the LOS. A statistical Pearson's coefficientsanalysis is used to study the correlation between the column densities and theintensity of the IR emission. This analysis provides evidence that the2$\times$2 square degree field under consideration is characterized by thepresence of a gas component not accounted for by the standard tracers, possiblyassociated with warm H$_{2}$ and cold HI. We demonstrate that the IR radiationin the range 8 $\mu$m $<$ $\lambda$ $<$ 500 $\mu$m is systematically dominatedby emission originating within the Scutum-Crux Arm. By applying an inversionmethod, we recover the dust emissivities associated with atomic, molecular andionized gas. Using the DustEM model we obtain an indication for PAHs depletionin the diffuse ionized gas. However, the main goal of this work is to discussthe impact of the missing column density associated with the dark gas componenton the accurate evaluation of the dust properties, and to shed light on thelimitations of the inversion method approach when this is applied to a smallsection of the Galactic Plane and when the working resolution allows sufficientde-blending of the gas components along the LOS.

monthly notices of the royal astronomical society

The pros and cons of the inversion method approach to derive 3D dust  emission properties of the ISM: the Hi-GAL field centred on  (l,b)=(30$^{\circ}$,0$^{\circ}$)