Dark Hydrogen in the Galactic Plane

Gibson, Steven J.; Taylor, A. R.; Stil, J. M.; Higgs, L. A.; Dewdney, P. E.; Brunt, C. M.

doi:10.1007/1-4020-2620-x_7

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“…The same peak of emission in 12 CO and 13 CO is also observed in correspondence of Ring 3. However, in this case, as mentioned in Section 2 and Section 4.3.1, a cold HI layer is also found, as reported by Gibson et al (2004). The existence of cold (i.e.…”

Section: Ring 2-3-4: Missing Column Density and Dark Gassupporting

confidence: 82%

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

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Paladini

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et al. 2014

Monthly Notices of the Royal Astronomical Society

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Herschel far-infrared (FIR) continuum data obtained as part of the Hi-GAL survey have been used, together with the GLIMPSE 8 µm and MIPSGAL 24 µm data, to attempt the first 3Ddecomposition of dust emission associated with atomic, molecular and ionized gas at 15 arcmin angular resolution. Our initial test case is a 2×2 square degrees region centred on (l,b)=(30 • ,0 • ), a direction that encompasses the origin point of the Scutum-Crux Arm at the tip of the Galactic Bar. Coupling the IR maps with velocity maps specific for different gas phases (HI 21cm, 12 CO and 13 CO, and Radio Recombination Lines, RRLs), we estimate the properties of dust blended with each of the gas components and at different Galactocentric distances along the Line of Sight (LOS).A statistical Pearson's coefficients analysis is used to study the correlation between the column densities estimated for each gas component and the intensity of the IR emission. This analysis provides evidence that the 2×2 square degree field under consideration is characterized by the presence of a gas component not accounted for by the standard tracers, possibly associated with warm H 2 and cold HI.We demonstrate that the IR radiation in the range 8 µm < λ < 500 µm is systematically dominated by emission originating within the Scutum-Crux Arm. By applying an inversion method, we recover the dust emissivities associated with atomic, molecular and ionized gas. Using the DustEM model, we fit the Spectral Energy Distributions (SEDs) for each gas phase, and find average dust temperatures of T d, HI =18.82±0.47 K, T d, H 2 =18.84±1.06 K and T d, HII =22.56±0.64 K, respectively. We also obtain an indication for Polycyclic Aromatic Hydrocarbons (PAHs) depletion in the diffuse ionized gas.We demonstrate the importance of including the ionized component in 3Ddecompositions of the total IR emission.However, the main goal of this work is to discuss the impact of the missing column density associated with the dark gas component on the accurate evaluation of the dust properties, and to shed light on the limitations of the inversion method approach when this is applied to a small section of the Galactic Plane and when the working resolution allows sufficient de-blending of the gas components along the LOS.

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Section: Ring 2-3-4: Missing Column Density and Dark Gassupporting

confidence: 82%

“…A cold layer of atomic hydrogen (Gibson et al 2004) has also been observed in SDPF1. As discussed in Section 6.2, this layer is seen in absorption in the HI 21cm line.…”

Section: The Content Of Sdpf1mentioning

confidence: 86%