PDRs4All IX. Sulfur elemental abundance in the Orion Bar
arxiv(2024)
摘要
One of the main problems in astrochemistry is determining the amount of
sulfur in volatiles and refractories in the interstellar medium. The detection
of the main sulfur reservoirs (icy H_2S and atomic gas) has been challenging,
and estimates are based on the reliability of models to account for the
abundances of species containing less than 1
sensitivity of the James Webb Space Telescope provides an unprecedented
opportunity to estimate the sulfur abundance through the observation of the [S
I] 25.249 μm line. We used the [S III] 18.7 μm, [S IV] 10.5 μm, and
[S l] 25.249 μm lines to estimate the amount of sulfur in the ionized and
molecular gas along the Orion Bar. For the theoretical part, we used an
upgraded version of the Meudon photodissociation region (PDR) code to model the
observations. New inelastic collision rates of neutral atomic sulfur with
ortho- and para- molecular hydrogen were calculated to predict the line
intensities. The [S III] 18.7 μm and [S IV] 10.5 μm lines are detected
over the imaged region with a shallow increase (by a factor of 4) toward the
HII region. We estimate a moderate sulfur depletion, by a factor of ∼2, in
the ionized gas. The corrugated interface between the molecular and atomic
phases gives rise to several edge-on dissociation fronts we refer to as DF1,
DF2, and DF3. The [S l] 25.249 μm line is only detected toward DF2 and DF3,
the dissociation fronts located farthest from the HII region. The detailed
modeling of DF3 using the Meudon PDR code shows that the emission of the [S l]
25.249 μm line is coming from warm (> 40 K) molecular gas located at
A_ V ∼ 1-5 mag from the ionization front. Moreover, the intensity
of the [S l] 25.249 μm line is only accounted for if we assume the presence
of undepleted sulfur.
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