[C II]-deficit caused by self-absorption in an ionized carbon-filled bubble in RCW79

Eduard Keilmann, Simon Dannhauer, Slawa Kabanovic, Nicola Schneider, Volker Ossenkopf-Okada, Robert Simon, Lars Bonne, Paul F Goldsmith, Rolf Güsten, Annie Zavagno, et al.

► To cite this version:

Eduard Keilmann, Simon Dannhauer, Slawa Kabanovic, Nicola Schneider, Volker Ossenkopf-Okada, et al.. [C II]-deficit caused by self-absorption in an ionized carbon-filled bubble in RCW79. Astronomy & Astrophysics - A&A, 2025, 697, pp.L2. 10.1051/0004-6361/202453445. hal-05097039

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<figure><img src="image_1.png" /></figure>

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LETTER TO THE EDITOR

[CII]-deficit caused by self-absorption in an ionized carbon-filled
bubble in RCW79

E. Keilmann<fnref n="1" />,*, S. Dannhauer<fnref n="1" />, S. Kabanovic<fnref n="1" />, N. Schneider<fnref n="1" />, V. Ossenkopf-Okada<fnref n="1" />, R. Simon<fnref n="1" />,
L. Bonne<fnref n="2" />, P. F. Goldsmith<fnref n="3" />, R. Güsten<fnref n="4" />, A. Zavagno<fnref n="5" />,<fnref n="6" />, J. Stutzki<fnref n="1" />, D. Riechers<fnref n="1" />, M. Röllig<fnref n="7" />,<fnref n="1" />,⁰
J. L. Verbena<fnref n="1" />, and A. G. G. M. Tielens<fnref n="8" />,<fnref n="9" />

Received 13 December 2024 / Accepted 8 April 2025

ABSTRACT

Recent spectroscopic observations of the [C II] 158 µm fine-structure line of ionized carbon (C+), using the Stratospheric Observatory for Infrared Astronomy (SOFIA), have revealed expanding [C II] shells in Galactic H II regions. We report the discovery of a bubble-shaped source (S144 in RCW79 in the GLIMPSE survey), associated with a compact H II region, excited by a single O7.5–9.5V/III star, which is consistent with a scenario that the bubble is still mostly “filled” with C+. This indicates most likely a very early evolutionary state, in which the stellar wind has not yet blown material away as it has in more evolved H II regions. Using the SimLine non-local thermodynamic equilibrium radiative transfer code, the [C II] emission can be modeled to originate from three regions: first, a central H II region with little C+ in the fully ionized phase, followed by two layers with a gas density around 2500 cm⁻<fnref n="3" /> of partially photodissociated gas. From these two layers, the second layer is a slowly expanding [C II] shell with an expansion velocity of ~2.6 km s⁻<fnref n="1" /> that corresponds approximately to a bright ring at 8 µm. The outermost layer exhibits a temperature and velocity gradient that produces the observed self-absorption features in the optically thick [C II] line (τ ~ 4), leading to an apparent deficit in [C II] emission and a low ratio of [C II] to total far-infrared (FIR) emission. We developed a procedure to reconstruct the missing [C II] flux and find a linear correlation between [C II] and FIR without a [C II]-deficit after incorporating the missing [C II] flux. This example demonstrates that at least some of the [C II]-deficit found in Galactic H II bubbles can be attributed to self-absorption, although a broader sample of these objects needs to be studied to fully constrain the range of conditions in which [C II]-deficits can be explained by this process.

**Key words.** ISM: bubbles – evolution – HII regions – ISM: kinematics and dynamics – photon-dominated region (PDR) – infrared: ISM

**1. Introduction**

Recent spectroscopic studies of Galactic H II regions in the 158 µm line of ionized carbon ([C II]) have confirmed that this far-infrared (FIR) fine-structure line is a key tracer for the cooling processes and the dynamics of gas in photodissocia- tion regions (PDRs). Exploratory observations have discovered expanding [C II] shells, e.g. in Orion (Pabst et al. 2019) and in FEEDBACK (Schneider et al. 2020) galactic H II region bub- bles such as RCW120 (Luisi et al. 2021), using large maps of [C II] obtained with the Stratospheric Observatory for Infrared Astronomy (SOFIA). With velocities of up to 15 km s⁻<fnref n="1" />, the shell expansion is mostly attributed to be driven by stellar winds of massive stars and not to the thermal expansion of the H II region.

These examples underline the potential of [C II] to trace the evolution of an H II region and its related molecular cloud. In this study, we report the detection of a C⁺ bubble in a very early evo- lutionary phase, designated as S144, in the *Spitzer*/GLIMPSE survey (Churchwell et al. 2006). The 8 µm emission (Fig. 1) exhibits a bright infrared (IR) ring with an opening in the north- east (NE) and moderate emission inside the ring, except for a concentrated peak around the exciting O7.5–9.5V/III star. S144 is embedded in the southeastern (SE) PDR ring outside of the larger H II region RCW79. Figure 2 (top) presents the [C II] emis- sion from the PDR ring of RCW79 and the associated molecu- lar cloud fragments (Bonne et al. 2023). The bottom panel illus- trates that the [C II] (as the 8 µm) emission from S144 does not exhibit a central void.

The diameter of S144 (Fig. 2) is about 1.5', corresponding to 1.7 pc at a distance of 3.9 kpc (Bonne et al. 2023). S144 is

<footnote n="1">1. I. Physikalisches Institut, Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany</footnote>

<footnote n="2">2 SOFIA Science Center, USRA, NASA Ames Research Center, Moffett Field, CA 94 045, USA</footnote>

<footnote n="3">³ Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099, USA</footnote>

<footnote n="4">⁴ Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</footnote>

<footnote n="5">⁵ Aix Marseille Univ., CNRS, CNES, LAM, Marseille, France</footnote>

<footnote n="6">⁶ Institut Universitaire de France, 1 Rue Descartes, Paris, France</footnote>

<footnote n="7">⁷ Physikalischer Verein, Gesellschaft für Bildung und Wissenschaft, Robert-Mayer-Str. 2, 60325 Frankfurt, Germany</footnote>

<footnote n="8">⁸ University of Maryland, Department of Astronomy, College Park, MD 20742-2421, USA</footnote>

<footnote n="9">⁹ Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands</footnote>

<footnote>* Corresponding author: keilmann@ph1.uni-koeln.de</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Spitzer 8 µm image of the bubble at ~2'' angular resolution from the GLIMPSE survey (Churchwell et al. 2006). The blue star is the O7.5–9.5V/III star and the small black stars are members of the associated IR clusters. The green circle is a by-eye approximation of the bright IR ring. The contour lines show [CII] emission from 50 to 250 K km s⁻¹ in steps of 50 K km s⁻¹.</figcaption></figure>

deeply embedded in a massive molecular clump (“condensation 2”, Zavagno et al. 2006) with a mass of ~5000 M⊙ (Liu et al. 2017), excited by an O7.5–9.5V/III star (Martins et al. 2010). The molecular gas bulk emission velocity ranges between −50 and −44 km s⁻¹. The region is undergoing massive star formation, witnessed by a small cluster of IR sources (Zavagno et al. 2006). The source is classified as a compact H II region (cH II R) with a determined 5 GHz total flux of 1 Jy (Zavagno et al. 2006), corresponding to an ionizing flux of 1.9 × 10⁴⁸ photons s⁻¹, typical of an O8 star. Assuming spherical symmetry for the cH II R region, the authors calculated a dynamical age of 0.13 Myr.

We have studied the gas dynamics and excitation conditions of photodissociated gas in the S144 bubble to understand the evolution of H II regions and their molecular cloud. We show that the low observed ratio of [C II] to the total FIR luminosity, the so-called [C II]-deficit (Smith et al. 2017; Pabst et al. 2021), can be explained by [C II] self-absorption.

## 2. Observations

### 2.1. SOFIA

The [¹²C II] line at 157.74 µm was mapped across RCW79 (~470 arcmin²) in the on-the-fly (OTF) mode, using the upgraded German REceiver for Astronomy at Terahertz frequencies (upGREAT; Risacher et al. 2018) on board SOFIA. A forward efficiency of η<sub>f</sub> = 0.97 and main beam efficiencies, η<sub>mb</sub>, between 0.63 and 0.69 were applied to obtain main beam temperatures (for further observational information and details on the SOFIA legacy program FEEDBACK, see Schneider et al. 2020; Bonne et al. 2023). The generic angular resolution is 14.1'' and the velocity resolution was binned to 0.3 km s⁻¹ wide channels.

### 2.2. APEX

The ¹²CO and ¹³CO 3 → 2 transitions at 345.80 GHz and 330.59 GHz were mapped in OTF mode with the LAsMA receiver on the APEX telescope and presented in Bonne et al. (2023). The data, in main beam temperature units using η<sub>mb</sub> = 0.68 with a velocity resolution of 0.3 km s⁻¹, had a first-order baseline removed from the spectra at 18'' resolution. In May 2024, a 180'' × 180'' ¹²CO 6 → 5 (ν = 691.47 GHz) map cen-

<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Line-integrated (−70 to −20 km s⁻¹) [C II] intensity maps of RCW79 and S144. Top: RCW79 with an overlay of ¹³CO 3 → 2 emission with contours from 7 to 52 K km s⁻¹ in steps of 9 K km s⁻¹ (~5σ). The green stellar symbols indicate the central cluster of O-type stars (Martins et al. 2010), the blue stellar symbol the exciting O7.5–9.5V/III star of the cH II R within S144 in the southeast, and the small black stellar symbols members of the IR clusters (Zavagno et al. 2006). The dashed black rectangle outlines the area shown in the bottom panel. Bottom: S144 with an overlay of ¹³CO 3 → 2 at the same levels as in the upper panel. The dashed green circle (50'' radius) indicates the bright IR ring seen in the Spitzer 8 µm map (see Fig. 1). The region taken into account to compute the average [C II] spectrum is indicated by a black contour. The black line corresponds to the PV cut shown in Fig. 3. Both maps have an angular resolution of 20'', indicated by gray disks in the lower right corner of the panels.</figcaption></figure>

tered on S144 was observed in OTF mode with the SEPIA660 receiver (Belitsky et al. 2018). The data have an angular resolution of 9'' and a velocity resolution of 0.25 km s⁻¹, leading to a root-mean-square noise level of 0.59 K. Spectra were processed by removing a third-order spectral baseline and applying a main beam efficiency of η<sub>mb</sub> = 0.6.

## 3. Results

### 3.1. Spatial and kinematic distribution of [C II] emission

We observe centrally concentrated [C II] emission with a peak slightly to the west of the exciting O star; the bottom panel of Fig. 2 displays the [C II] line-integrated intensity in S144. The 8 µm image (Fig. 1) shows a more complex emission distribution with a small, circular emission peak just around the O star (radius ~15''), followed by low-surface-brightness emission and a bright dust ring, which most likely represent a
<figure><img src="image_4.png" /></figure>

**Fig. 3.** Position-velocity cut in [C II] at 20'' angular resolution. The cut is outlined in the lower panel in Fig. 2. Offset 0 arcmin marks the lower declination. The dashed ellipse results from fitting the emission in various PV cuts. Movies are available online. In these PV diagrams, the dotted black line marks the cloud bulk velocity at −46.5 km s⁻<fnref n="1" />, the vertical gray line the position of the O star, and the green lines the extent of the IR ring.

swept-up gas shell, as has been proposed for other H II regions (Deharveng et al. 2010). The 8 µm emission is dominated by the 7.7 and 8.6 µm features of polycyclic aromatic hydrocarbons (PAHs) that are easily destroyed by the hard radiation field of the central star or blown out by stellar winds (Churchwell et al. 2006). The absence of a central void in the 8 µm emission suggests that the cH II R region is in an early evolutionary stage in which the gas dynamics are not yet dominated by stellar winds. Additionally, the UV radiation is attenuated by gas and dust, creating conditions that allow PAHs to survive.

Lastly, we have a scenario in which the central O star has created a cH II R but no wind-blown cavity, and in which the star is enveloped by an extended PDR seen in the (F)IR and in [C II]. The whole region is embedded in a larger molecular cloud that extends mostly to the SE, containing a few dense clumps with ongoing star formation. Figure A.1 presents overlays of [C II] with several other tracers (Herschel 70 µm, 843 MHz continuum, etc.), a [C II] and $^{12}$CO 3 → 2 channel map (Fig. A.2), and an overlay between [C II] and $^{12}$CO 6 → 5 emission (Fig. A.3). The online material includes movies that further detail the bubble's characteristics.

Figure 3 presents a position-velocity (PV) cut of the [C II] emission showing the characteristic emission distribution of an expanding shell, with both blueshifted and redshifted parts. The latter is sometimes missing in other sources. The expansion speed is low, around 2.6 km s⁻<fnref n="1" />, and was derived by fitting an ellipse to the emission distributions for all PV cuts and taking the overall average. The shell most likely corresponds to the bright IR ring (Fig. 1); whether it is driven by wind or thermal pressure will be discussed in another study. The central dip in the profiles may reflect the effects of absorption by a colder foreground gas. The emission within the dip reaches 10–15 K, which is above the 3σ noise (~7.5 K in a 0.5 km s⁻<fnref n="1" /> channel), indicating significant [C II] emission at the center of the bubble. In the next section, we show that optical depth effects and self-absorption lead to the apparent depression in the emission line profile.

## 3.2. Self-absorption of the [12C II] line

S144 has a complex spatial and velocity structure, which is also reflected in the spectra of [C II] and CO 6 → 5 emission (Fig. A.3). The [C II] and CO spectra often reveal two veloc-

<figure><img src="image_5.png" /></figure>

**Fig. 4.** Spatially averaged [12C II] and [13C II] spectra. Top: Averaged spectrum of the [13C II] HFS *F* = 1–0 component. The spatial region over which the averaging was carried out is defined by the black dendrogram contour in Fig. 2. Gaussian fit parameters are included. Bottom: Averaged [12C II] line (red) and the [13C II] HFS *F* = 1–0 component (light blue histogram) with its Gaussian fit (dark blue curve), scaled by the 12C/13C ratio of 59±10 (Milam et al. 2005) and considering the fractional weight (0.25) of the 1–0 HFS. Black dots indicate optical depth.

ity components and a dip at ~−46 km s⁻<fnref n="1" />. In the SE region, the CO line consists of only one component at the bulk emission of ~46.5 km s⁻<fnref n="1" />. In the northwestern (NW) region, CO emission decreases, while the [C II] line is strong and shows two velocity components. In addition, the [C II] spectrum displays in all spectra high-velocity gas from the large expanding [C II] shell of RCW79 (Bonne et al. 2023), which is lacking in the CO line. There is also [C II] emission arising from the slowly expanding shell of the bubble and from the bulk emission of the PDR gas, in which the bubble is embedded.

To answer the main question – whether the [C II] intensity dip is due to the kinematics of the expanding [C II] shell of the bubble or due to self-absorption effects in an optically thick [C II] line, as is seen in other C⁺ bubbles (Bonne et al. 2022; Kabanovic et al. 2022) – we need an observation of at least one hyperfine-structure (HFS) component of the optically thin [13C II] line (Ossenkopf et al. 2013). For S144, we do not observe this line in individual spectra. We detect the [13C II] *F* = 1–0 component<fnref n="1" /> only in the averaged spectrum. Figure 4 shows the line together with the [C II] optical depth derived from the observed [12C II]/[13C II]-ratio in each velocity channel within the single-layer model using Eq. B.6 (Guevara et al. 2020; Kabanovic et al. 2022, and Appendix B). We find that the [13C II] line, scaled by the local carbon abundance ratio, overshoots the [12C II] line, resulting in a velocity-resolved optical depth between 1 and 5. The peak optical depth is shifted relative to the [C II] peak emission, which cannot be explained if the optical depth arises purely from a gas column with a single temperature. Thus, a more sophisticated calculation is needed to properly explain the observations, separating the gas into a warm emitting layer and a colder absorbing foreground gas. The two-layer model and its results are discussed in Appendix B. In

<footnote n="1">¹ The strongest [13C II] *F* = 2–1 component is not accessible, as it is contaminated by the redshifted wing of the [C II] line.</footnote>
the following, we assume that the [¹²C II] line is optically thick throughout the map, which is a presumption because we do not have measurements of the [¹³C II] line at each position. However, all observed [¹²C II] lines show a dip or sometimes a flat-top profile (Fig. A.3) and considering the small extent of the region (diameter ~2 pc), we do not expect a large variation in the bulk emission of the gas, which would shift the [¹²C II] dip and the [¹³C II] line center position.

To verify our finding of partly self-absorbed [C II] profiles, we used the 1D non-local thermodynamic equilibrium radiative transfer code SimLine (Ossenkopf et al. 2001). This evaluation is not intended to provide a fully quantitative reproduction of the bubble parameters, as the angular resolution of the [C II] data imposes certain limitations.<fnref n="2" /> Our goal is to demonstrate that even a simple model can satisfactorily reproduce the observations. The model consists of a central, fully ionized H II region (with a radius of r = 0.5 pc, electron density of $n_e = 100 \text{ cm}^{-3}$, temperature of T = 8000 K), followed by a dense ($n = 2500 \text{ cm}^{-3}$) PDR layer ($r = 0.95$ pc) with T = 100 K, surrounded by a layer in which the parameters drop to the environmental conditions reached at r = 1.5 pc using a power law with an exponent of -2. The PDR layer exhibits a radial velocity of 2.6 km s⁻¹ and a turbulent velocity of 2.2 km s⁻¹, consistent with observational constraints. A detailed description of the model parameters and their values is provided in Appendix C.

The radius and width of the shells, the expansion velocity, and the steep outer temperature gradient are well constrained. Conversely, the local density and temperature are uncertain. A lower density can always be compensated for by a higher temperature and vice versa. The 8 µm ring likely traces a compressed shell that is somewhat thinner than the modeled PDR layer. This indicates that C⁺ can be extended more than the PAHs in S144. However, these structural differences do not impact our key conclusion: the observed [C II] line can be self-absorbed due to temperature and velocity gradients. The exact amount of C⁺ contained in the H II region remains currently unclear. Modeling the H II region with the assumed parameters from SimLine using the CLOUDY spectral synthesis code (Ferland et al. 2017) yields very small quantities of C⁺ (less than 1%), although up to 20% of the observed [C II] can stem from the H II regions in other sources (RCW120, Luisi et al. 2021). Observations of carbon recombination lines could probably settle this issue and help investigate the dynamics of the expanding [C II] shell.

### 3.3. [C II]-deficit

The self-absorption seen in the [C II] line leads to a deficiency in the line-integrated emission. Thus, the ratio of [C II] to total FIR continuum is lower than the nominal value, assuming that the FIR emission is optically thin, an assumption that is reasonable given the density (a few 1000 cm⁻<fnref n="3" />, Sect. 3.2) and the radiation field regime (up to a few 1000 $G_0$; Appendix A) present in S144 (Goldsmith et al. 2012).

To correct for the missing emission, we fit the [C II] line and the [¹³C II] HFS to the outer wings of the double-peak spectra using radiative transfer equations, where the optical thickness, peak position, and width were free fit parameters. We first detected the peaks and then subtracted the blueshifted and redshifted components of the large shell of RCW79 that were fit with Gaussians. For each position, we calculated the area between the spectra and the fit line, denoted as the “correction”;

<figure><img src="image_6.png" /><figcaption>**Fig. 5.** Example of the fitting procedure for one spectrum toward the O star with fixed $T_{ex} = 80$ K. Vertical dotted lines signify the outer wings of the double-peak spectrum. The gray area indicates the missing [C II] emission. The large blueshifted and redshifted expanding shell of RCW79 is fit and indicated.</figcaption></figure>

we show an example spectrum in Fig. 5. We performed calculations for an excitation temperature, $T_{ex}$, between 54 to 80 K in steps of 1 K, but kept each $T_{ex}$ fixed during the fitting process. As a lower limit, 54 K is derived from the two-layer model (Appendix B) and 80 K is an upper limit, since the mean correction factor becomes insensitive to $T_{ex} \ge 80$ K (see Fig. B.2). The correction factor is shown in Fig. B.3 and varies from ~1.1 to ~1.4.

Figure 6 compares the correlations of the [C II] intensity with the FIR intensity for both the “uncorrected” (top panel) and corrected [C II] values (bottom panel) reconstructed in the manner described above.<fnref n="3" /> The total FIR intensity was determined from a spectral energy distribution fit to the Herschel fluxes (Appendix D). First, the distribution is bimodal for log(FIR) $\lesssim -0.9$ and log([C II]) $\lesssim -3.1$ due to environmental effects. The corresponding pixels originate from the map edges in the NW and SE, where PDR gas emits at similar [C II] levels but exhibits weaker FIR emission in the NW. Consequently, the [C II]/FIR ratio is higher in the NW, resulting in the observed bimodality.

Second, the upper panel shows that the highest [C II] intensities depend less than linearly on the FIR. This so-called [C II]-deficit is sometimes observed in Galactic and extragalactic star-forming regions. For ultraluminous IR galaxies, it is often a high dust optical depth, a high ionization parameter (when carbon can become doubly ionized to C<fnref n="2" />⁺ and higher states), metallicity variations, and very strong and hard radiation fields that can cause the [C II]-deficit (Lagache et al. 2018; Luhman et al. 2003, and references therein). In less extreme environments in Galactic PDRs, other processes are proposed. In very dense regions, an increased heating efficiency caused by dust grains and collisional de-excitation of [C II] can take place and in environments with high values of $G_0 T^{0.5}/n_e$, photoelectric heating efficiency may drop, reducing overall gas cooling (Hollenbach & Tielens 1999; Goicoechea et al. 2015; Pabst et al. 2021). Saturation<fnref n="4" /> of the [C II] line can occur under specific conditions, and [O I] cooling (Hollenbach & Tielens 1999) can dominate in very dense and warm PDRs. Self-absorption of the [C II] line is another viable mechanism for reducing the integrated [C II] line emission. This has not yet been discussed for [C II] in the literature;

<footnote n="3">³ A linear relation, $\eta = \alpha + \beta\xi + \epsilon$, in log-log space was fit to the samples using Bayesian Interference with linmix (Kelly 2007). $\alpha$ and $\beta$ correspond to the intercept and slope, while $\epsilon$ is the intrinsic scatter of the relation. The absolute values, however, are not relevant here and will be discussed in another study.</footnote>

<footnote n="4">⁴ The [C II] emissivity ceases to increase, even with a stronger radiation field. In this case, the fraction of ions in the upper excited state of the two-level system of the [C II] 158 µm line reaches a threshold.</footnote>

<footnote n="2">² Note, however, that the angular resolution is handled fully self-consistently within SimLine.</footnote>
<figure><img src="image_7.png" /><figcaption>**Fig. 6.** [C II]/FIR correlation for both uncorrected (top) and corrected (bottom) [C II] emission. Pixels (derived from maps at 36" resolution) are color-coded based on their proximity to the O star; their density is reflected in the shaded blue areas. A dashed red line represents a linear fit intended to guide the eye for a linear [C II]/FIR correlation. Corrected pixels near the O star with high [C II] and FIR values $log(FIR) > -0.6$ are shifted upward in the lower panel (indicated by a dashed red ellipse).</figcaption></figure>

however, Goldsmith et al. (2021) propose this mechanism for a low [O I]/FIR ratio in W3.

For S144, we can exclude processes requiring extremely high density and UV radiation fields, as the conditions are moderate ($n \sim$ a few 1000 cm⁻³, $G_0 \sim$ a few 1000). Saturation is also unlikely, as it typically becomes significant for dust temperatures exceeding 40 K (Fig. 16 of Ebagezio et al. 2024). However, the dust temperatures in S144 are below 30 K (Fig. 2a in Liu et al. 2017). A high ionization parameter is also not expected to be a significant issue. The [C II] emission predominantly originates in the PDR, where carbon remains in a C⁺ state. While the C⁺ to C²⁺ transition may occur within the H II region, Ebagezio et al. (2024) indicate that this process is more relevant for evolved H II regions, which is not the case for our cH II R. Gerin et al. (2015) propose that the [C II]-deficit toward nuclear regions in luminous IR galaxies is caused by absorption on kiloparsec scales from diffuse gas in the foreground. This is not what we suggest, because in our case the absorption takes place very close to the source and is mostly due to a temperature and velocity gradient in the PDR.

Our straightforward approach of correcting for self-absorption shows that the [C II] to FIR correlation becomes linear again for high [C II] and FIR values, as shown in Fig. 6, in which the [C II] values shift upward. This finding does not exclude the possibility that other mechanisms are also at work, but demonstrates that in this PDR region with not-so-extreme radiation fields and densities the [C II]-deficit can indeed be mainly caused

by self-absorption effects in the [C II] line. This view will be further investigated by studying the [C II]/FIR ratio and the [C II] line properties in other FEEDBACK sources and carrying out a comparison with simulations of H II regions including stellar winds and radiation.

## Data availability

Movies associated to Figs. 3 and A.3 are available at https://www.aanda.org

**Acknowledgements.** This study was based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association Inc. (USRA), under NASA contract NNA17BF53C and the Deutsches SOFIA Institut (DSI), under DLR contract 50 OK 0901 to the University of Stuttgart. upGREAT is a development by the MPIfR and the KOSMA/University Cologne, in cooperation with the DLR Institut für Optische Sensorsysteme. This work was carried out in part at the JPL, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Financial support for FEEDBACK at the University of Maryland was provided by NASA through award SOF070077 issued by USRA. The FEEDBACK project was supported by the BMWI via DLR, project number 50OR2217. S.D. acknowledges support from the IMPRS at the Universities of Bonn and Cologne. S.K. acknowledges support by the BMWI via DLR, project number 50OR2311. This work was supported by the CRC 1601 (SFB 1601 sub-projects B2, C1, C2, C3, C6) funded by the DFG – 500700252.

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## Appendix A: Multiwavelength plots and channel maps in [C II] and $^{12}$CO 3 → 2 emission

Figure A.1 presents a Herschel 70 µm map, our computed UV field map, and a 843 MHz emission and Herschel column density map. The 843 MHz map outlines the approximate extent of the H II region, though it suffers from beam dilution due to its 45" beam size. The dust ring, seen in both the Herschel 70 µm and the Spitzer 8 µm maps (Fig. 1), probably indicates compressed gas, predominantly to the west. The FUV map of the total RCW79 region was generated following the procedure outlined in Schneider et al. (2023), using the spectral classification of all O stars as detailed in Martins et al. (2010). The features in these maps partly motivated the modeling of the two outer shells using SimLine (Sect. C).

The Herschel dust column density map (Liu et al. 2017) illustrates the dense gas distribution, highlighting a SE region comprising multiple high-density clumps, one reaching up to $6 \times 10^{22} \text{ cm}^{-2}$ NE of the O star. Identified as a cluster-forming star-formation site (Zavagno et al. 2006), this molecular clump shields the H II region and PDR gas. The movie overlays with [C II] and CO alongside the column density nicely show the gas flow around this clump.

Figure A.2 displays a [C II] channel map with superimposed contours of $^{12}$CO 3 → 2 emission. The purple areas represent [C II] emission of low surface brightness, primarily originating from the large expanding [C II] shells spanning the RCW79 region and the disorganized [C II] flows that are eroding the molecular cloud (Bonne et al. 2023). Within the velocity range of -54 km s$^{-1}$ to -40 km s$^{-1}$ (indicated in blue), we detect the shell/bubble of [C II] exclusively associated with the cH II R. The “filled C$^+$ bubble” geometry is disturbed by the prominent CO clump, which becomes visible around -59 km s$^{-1}$ to the west. Furthermore, near a velocity of ~ -47 km s$^{-1}$, a [C II]-deficit is detected due to self-absorption.

Figure A.3 displays a map of the line-integrated [C II] and $^{12}$CO 6 → 5 emission, together with spectra overlays selected for two representative positions. The NW spectrum (left) is an example of a self-absorbed [C II] line, also showing prominent wings from the expanding [C II] shell. The right panel is a position from the SE where the PDR emission from the surface of the molecular clump dominates the [C II] and CO emission. The high-velocity [C II] wings are, however, well visible.

## Appendix B: The two-layer radiative transfer model

The two-layer multicomponent model (Guevara et al. 2020; Kabanovic et al. 2022) solves the radiative transfer equation for multiple velocity components distributed between two layers with different excitation temperatures along the line-of-sight. While the model itself has no restriction on the excitation temperature, we choose the excitation temperature $T_{ex,bg}$ of the background layer (bg) to be higher than the temperature $T_{ex,fg}$ of the foreground layer (fg), considering the geometry of the region with the exciting O star in the center and cooler PDR shells around. Thus, we account for self-absorption due to a column of gas along the line-of-sight in a single layer (which results in flat top spectra for high optical depth $\tau$) as well as the foreground absorption by a colder foreground layer (which produces absorption dips in the spectrum). The absorption can originate from a spatially separated, cold foreground cloud, which is located between the warm emitting gas and the observer, or from a temperature gradient along the line-of-sight of the same cloud. Following the model presented in Kabanovic et al. (2022), we solve

the following equation:

$$T_{mb}(v) = \left[ \mathcal{J}_v(T_{ex,bg}) (1 - e^{-\sum_{bg} \tau_{bg}(v)}) \right] e^{-\sum_{fg} \tau_{fg}(v)} + \mathcal{J}_v(T_{ex,fg}) (1 - e^{-\sum_{fg} \tau_{fg}(v)}). \quad (B.1)$$

The equivalent brightness temperature of a black body emission at a temperature $T_{ex}$ is

$$\mathcal{J}_v(T_{ex,i}) = \frac{T_0}{e^{T_0/T_{ex}} - 1}, \quad (B.2)$$

with the equivalent temperature of the transition $T_0 = h\nu/k_B$ and $\nu$ the transition frequency. The optical depth of each Gaussian component is given by

$$\tau(v) = \tau_0 e^{-4 \ln 2 \left( \frac{v-l_0}{w} \right)^2}, \quad (B.3)$$

with the central local standard of rest (LSR) velocity $v_0$ of each component. The line width $w$ is expressed as the full width at half maximum (FWHM) of the component. For a simple two-level system, we can express the peak optical depth $\tau_0$ of each Gaussian component as a function of the excitation temperature $T_{ex}$ and column density $N$ by

$$\tau_0 = N \frac{c^3}{8\pi v^3} \frac{g_u}{g_l} A_{ul} \frac{1 - e^{-T_0/T_{ex}}}{1 + \frac{g_u}{g_l} e^{-T_0/T_{ex}}} \frac{2\sqrt{2\ln 2}}{w\sqrt{2\pi}}. \quad (B.4)$$

For the [C II] fine-structure transition, the rest frequency is $\nu = 1900.5369$ GHz, the Einstein coefficient for spontaneous emission $A_{ul} = 2.29 \cdot 10^{-6} \text{ s}^{-1}$, the equivalent temperature of the upper level $T_0 = h\nu/k_B = 91.25$ K, and the statistical weights of the transition energy levels are $g_u = 4$ and $g_l = 2$.

<table><caption>Table B.1. Two-layer multicomponent model results.</caption><thead><tr><th rowspan="2">Components</th><th colspan="4">Model I: T<sub>ex,bg</sub> = 54 K, T<sub>ex,fg</sub> = 20 K</th></tr><tr><th>N<sub>[C II]</sub><br>[10<sup>18</sup> cm<sup>-2</sup>]</th><th>τ<sub>0</sub></th><th>ν<sub>0</sub><br>[km s<sup>-1</sup>]</th><th>w<br>[km s<sup>-1</sup>]</th></tr></thead><tbody><tr><td>Backg. Comp. 1</td><td>4.77</td><td>4.26</td><td>-47.06</td><td>4.48</td></tr><tr><td>Backg. Comp. 2</td><td>1.37</td><td>0.27</td><td>-48.88</td><td>20.02</td></tr><tr><td>Backg. Comp. 3</td><td>0.54</td><td>0.32</td><td>-44.29</td><td>6.67</td></tr><tr><td>Foreg. Comp. 1</td><td>0.17</td><td>0.28</td><td>-44.96</td><td>2.36</td></tr><tr><td>Foreg. Comp. 2</td><td>0.64</td><td>0.89</td><td>-50.88</td><td>2.90</td></tr></tbody><tbody><tr><th colspan="5">Model II: T<sub>ex,bg</sub> = 80 K, T<sub>ex,fg</sub> = 20 K</th></tr><tr><td>Backg. Comp. 1</td><td>3.29</td><td>1.81</td><td>-46.81</td><td>5.07</td></tr><tr><td>Backg. Comp. 2</td><td>0.16</td><td>0.04</td><td>-59.13</td><td>10.50</td></tr><tr><td>Backg. Comp. 3</td><td>0.88</td><td>0.15</td><td>-46.26</td><td>15.95</td></tr><tr><td>Foreg. Comp. 1</td><td>1.28</td><td>0.81</td><td>-45.33</td><td>4.43</td></tr><tr><td>Foreg. Comp. 2</td><td>1.52</td><td>1.07</td><td>-50.69</td><td>3.95</td></tr></tbody></table>

The physical properties of the background layer can be derived from an optically thin line, which is not affected by self-absorption. In case of [C II], we can utilize the much weaker $^{13}$C II hyperfine transition lines, see Guevara et al. (2020) for a more detailed description. Model fit parameters such as LSR velocity, line width, and number of components can be simply derived from the observed line. However, the optical depth and the excitation temperature are not independent of each other. We therefore need to first derive the excitation temperature from the observed data, which leaves the optical depth as the free model fit parameter. Assuming that the warm emitting background can
<figure><img src="image_8.png" /><figcaption>Fig. A.1. Complementary plots for the S144 C⁺ bubble in RCW79. The upper left panel illustrates the 70 µm emission from Herschel at ~6" resolution. This emission resembles the Spitzer 8 µm image (as seen in Fig. 1), though it highlights more clearly the NE clump containing the embedded IR cluster in the 70 µm map. The upper right panel presents the UV field, which is derived from the spectral type of the O star (indicated by a blue star) and the central O-cluster from RCW79, located farther to the west. The lower left panel displays the 843 MHz emission with a 45" angular resolution, outlining the H II region (Cohen et al. 2002). In the lower right panel, the Herschel dust column density map (Liu et al. 2017) at 18" angular resolution reveals the clumpy structure of condensation 2. Each panel includes [C II] contours in increments of 50 K km s⁻¹ from 50 to 250 K km s⁻¹, while the 843 MHz map also depicts 843 MHz contours at 0.1 and 0.2 Jy/Beam in purple. The small black stars are members of the IR clusters.</figcaption></figure>

partly shine through the cold absorbing layer (Kabanovic et al. 2022), we can determine the excitation temperature via

$$T_{\text{ex}} = \frac{T_0}{\ln\left(\frac{T_0}{T_{\text{[C II],peak}}} (1 - e^{-\tau_{\text{[C II],peak}}}) + 1\right)} \quad (\text{B.5})$$

The optical depth is then calculated from the observed [¹²C II]/[¹³C II] ratio at the peak of the [¹²C II] emission

$$\frac{T_{[^{12}\text{C II}]}(v)}{T_{[^{13}\text{C II}]}(v)} = \frac{1 - e^{-\tau(v)}}{\tau(v)/\alpha} = \frac{1 - e^{\tau(v)}}{\tau(v)}\alpha, \quad (\text{B.6})$$

with the local carbon abundance ratio α that we take as 59 ± 10 (Milam et al. 2005). The resulting velocity-resolved optical depth is shown in Fig. 4. For the calculation, only the second strongest [¹³C II] F = 1 − 0 line is used, since the strongest F = 2 − 1 HFS line is covered by the redshifted [C II] wing and the weakest HFS F = 1 − 1 line is detected only marginally. The resulting lower limit for the [C II] excitation temperature is Tex = 54 K. For the upper limit, we derive an excitation temperature of Tex = 80 K, see Fig. B.2.

The resulting model fit of the two-layer model is shown in Fig. B.1 for a background excitation temperature of Texbg = 80 K, which is the derived upper limit, indicating an optically thick [C II] line. However, the background (see Table B.1) derived from the [¹³C II] line still overshoots the observed line, which requires additional cold foreground material. Although

we do not have observational constraints on the excitation temperature in the foreground, multiple studies (Kabanovic et al. 2022; Schneider et al. 2023) have shown that a temperature of Texbg = 20 K is reasonable for [C II]. We find that the observed foreground material is either blueshifted or redshifted from the systemic velocity. The blueshifted component can be explained due to the expanding bubble, which pushes the cold material in front of it toward the observer. However, the redshifted component cannot be attributed to the opposite hemisphere, since it is only visible in absorption. Decreasing the background excitation temperature results in a higher background column density and therefore higher optical depth; see Table B.1. Note, however, that we derived a temperature of ~100 K from the SimLine modeling, so that low excitation temperatures are unlikely.

As a final note, we show in Fig. B.3 a map of the correction factor that was applied to the spectra showing self-absorption effects. Obviously, the spectra with the highest [C II] brightness are the most affected.

## Appendix C: SimLine modeling of a C⁺ filled bubble

We use the 1D radiative transfer code SimLine (Ossenkopf et al. 2001) to model the observed [C II] emission from a symmetric spherical geometry. SimLine self-consistently solves the excitation problem of any species by taking into account the collisional excitation from the surrounding gas and the radiative
<figure><img src="image_9.png" /><figcaption>**Fig. A.2.** Channel map showing [C II] and $^{12}$CO 3 → 2 emissions of the C$^+$ bubble. CO contours range from 0.67 to 32 K km s$^{-1}$ in steps of 2.4 K km s$^{-1}$. The prominent blue star marks the position of the exciting O star, while smaller black stars denote IR cluster members. The green dotted circle indicates the approximate extent of the IR shell as observed in the *Spitzer* 8 µm image.</figcaption></figure>

<table><caption>**Table C.1.** Parameters of SimLine modeling.</caption><thead><tr><th></th><th>shell 1</th><th>shell 2</th><th>shell 3</th></tr></thead><tbody><tr><td>outer radius [pc]</td><td>0.5</td><td>0.95</td><td>1.5</td></tr><tr><td>density [cm<sup>-3</sup>]</td><td>100</td><td>2500</td><td>2500</td></tr><tr><td>density profile (α<sub>s</sub>)</td><td>-</td><td>-</td><td>-2</td></tr><tr><td>temperature [K]</td><td>8000</td><td>100</td><td>100</td></tr><tr><td>temperature profile (α<sub>s</sub>)</td><td>-</td><td>-</td><td>-2</td></tr><tr><td>turbulent velocity [km s<sup>-1</sup>]</td><td>3.7</td><td>2.2</td><td>2.2</td></tr><tr><td>turbulent velocity profile (α<sub>s</sub>)</td><td>-</td><td>-</td><td>-1</td></tr><tr><td>radial velocity [km s<sup>-1</sup>]</td><td>-</td><td>2.6</td><td>2.6</td></tr><tr><td>radial velocity profile (α<sub>s</sub>)</td><td>-</td><td>-</td><td>-2</td></tr><tr><td>X([C II]) [10<sup>-4</sup>]</td><td>1.2</td><td>1.2</td><td>1.2</td></tr></tbody></table>

interaction throughout the cloud. After solving the excitation problem through an accelerated Λ-iteration, the line profiles are computed at any desired velocity and spatial resolution. We simulate the properties of the observed [C II] data at 15" resolution. Collisional excitation in the H II region is assumed to come from electrons in a fully ionized medium. In the outer shells, we assume that collisions are dominated by H$_2$, although a contribution of atomic hydrogen is also possible.

Due to the one-dimensional nature of the model, it can only reproduce angular-invariant properties, ignoring variations in different directions. Therefore, we ignore the SE direction which is heavily affected by the foreground molecular cloud and reproduce the observed radial profiles seen in the NW direction indicated by blue squares in Fig. C.1, which shows the general

shell-setup of the model. We do not perform an accurate $\chi^2$-fit to the data. This would fail due to the radial asymmetry given by the overabundance of foreground material from the molecular cloud at the peak position relative to the background material and the contribution of the high-velocity wing material that we ignored as discussed in Sect. 3.2. Instead, we performed a qualitative fit to all significant features by eye, ignoring the wings below -55 km s$^{-1}$ and above -40 km s$^{-1}$ and the blueshifted material close to the O star position.

The model consists of a central, fully ionized H II region, followed by a dense layer with high temperature and outer region providing a steep gradient in density, temperature, and expansion velocity ($\propto r^{-\alpha_s}$) to the surrounding ambient medium.

We estimated the approximate extent of the H II region using the 843 MHz emission map at 45" angular resolution (lower left panel in Fig. A.1). First, the H II region must be smaller than the area enclosed by the 8 µm ring-like feature, represented by the green dashed circle with a radius of 50". Second, the contour at 0.2 Jy/beam delineates the level, at which the emission drops to ~50% of its maximum value corresponding to an observed radius of approximately 34". Using this value and a beam of 45", we derive a de-convolved radius of the H II region of ~0.5 pc. We note that this is only an approximation, particularly as we see clear deviations from a circular symmetry. The H II region may be slightly smaller, suggested by the *Spitzer* 8 µm image, as a small circular feature is visible in Fig. 1, located directly around the exciting O star. Higher angular resolution cm observations are necessary to resolve this uncertainty. Beyond the H II region, the model assumes a PDR with a transition from atomic to molecular gas, where the outermost layer provides the transition to the gas from the surrounding ambient molecular cloud.
<figure><img src="image_10.png" /><figcaption>**Fig. A.3.** Example spectra of $[^{12}\text{CO}\text{II}]$ and $[^{12}\text{CO}\text{6}] \rightarrow 5$ lines with a fit to the HFS F = 1 – 0 component of the average $[^{13}\text{CO}\text{II}]$ line. The upper panels show the spectra/fit in a smoothed 30′′ beam at the positions marked by a black circle in the lower panel of line-integrated [CII] emission and $[^{12}\text{CO}\text{6}] \rightarrow 5$ emission contours (10 to 130 by 10 K km s$^{-1}$). The two pairs of gray lines mark the blue and red velocity ranges of the large expanding [CII] shell over the whole RCW79 region (Bonne et al. 2023). The two pairs of black lines outline approximately the velocity range of the expanding [CII] shell. The black star in the lower panels indicates the position of the O-star and the green dashed circle the 8 µm ring. A movie showing all spectra is available online.</figcaption></figure>

We setup the shells in the following way (all parameters are summarized in Table C.1): In the inner H II region (up to 0.5 pc), we assume that carbon is singly ionized. We cannot exclude that some of the C$^+$ is photo-ionized to C$^{2+}$ caused by the stellar radiation (Eagezio et al. 2023, 2024), but this effect should be more prominent in more evolved H II regions (Eagezio et al. 2024). We take a typical temperature of 8000 K for the H II region. The density has no impact on the model result as long as it is below a few hundred cm$^{-3}$. We choose 100 cm$^{-3}$ as a typical value.

The following two shells constitute the PDR, in which carbon collides with atomic and molecular hydrogen. For these shells, we adopt an abundance of X(C$^{+}$/H) = 1.2 × 10$^{-4}$ (Simón-Díaz & Stasińska 2011). The first shell (up to 0.95 pc) has no velocity, density, or temperature gradient. It expands with the velocity of 2.6 km s$^{-1}$ as determined in Sect. 3.1 and has a turbulent velocity dispersion of $v_{\text{turb}} = 2.2$ km s$^{-1}$ to match the [CII] line width, a temperature of T = 100 K reflecting typical PDR conditions, in which the [CII] line cools efficiently, and a density of $n_{\text{H}_2} = 2500$ cm$^{-3}$.

This matches the density from the Herschel column density map at 18" resolution from the HOBYS keyprogram (Motte et al. 2010) presented in Liu et al. (2017). The cutout for the bubble is shown in Fig. A.1. Since RCW79 is embedded in the Galactic plane, the column density is overestimated. Following the procedure presented in Schneider et al. (2015), that estimates the line-of-sight contamination directly from the Herschel maps, we derived a value of 4–6 × 10$^{21}$ cm$^{-2}$ for the contaminating column density. This is a typical value for massive star-forming regions (Schneider et al. 2022). After subtracting a

value of 4 × 10$^{21}$ cm$^{-2}$, we calculated densities between 2.3 and 2.9 × 10$^{3}$ cm$^{-3}$ in an 18" beam for the outermost points of shell 2 and 3, which fits our fit value of 2500 cm$^{-3}$.

The outer region (up to 1.5 pc), representing the transition to the pre-shock material in front of the expanding first shell, is simulated through a power-law decay of all parameters, with a steep exponent of $\alpha_s = 2$ for density, temperature, and expansion velocity; and a shallower exponent of $\alpha_s = 1$ for the turbulent velocity, reflecting the indirect driving of turbulence through the expansion. This description should roughly mimic the gas properties and condition in front of a C-shock, where the temperature and density rise steeply.

The result is shown in Fig. C.2 comparing the PV cut through the model and selected spectra with the correspondingly observed data at the same scale. Our SimLine setup with an absorbing layer, including temperature, radial, and turbulent velocity gradients, shows a good agreement to our observed spectra in terms of intensity and line profiles and PV cut. The most evident difference is the reversion of the blue and red peaks for positions Δr = 0 and 21. In an ideal bubble scenario including absorption, a higher redshifted line is expected since the blueshifted gas experiences more absorption along the sightline. However, the geometry of the C$^+$ bubble is more complex, as seen in Fig. C.1. The spherical symmetry of the H II region and the expanding C$^+$ bubble is disturbed by the molecular gas distribution located SE of the O star, which is slightly more blueshifted with respect to the [CII] emission. Therefore, the PDR surfaces of the molecular clumps emit [CII] efficiently and the increased gas density results in stronger [CII] emission.
<figure><img src="image_11.png" /><figcaption>**Fig. B.1.** Two-layer model results for the average [C II] spectrum. The average spectrum corresponds to the area defined with dendrograms (refer to Fig. 2, right). The spectrum, shown in red, has a velocity resolution of 1 km s⁻¹. The model’s background and foreground layer temperatures are T<sub>ex,bg</sub> = 80 K and T<sub>ex,fg</sub> = 20 K respectively. The upper left panel illustrates the observed spectrum in red beside its two-layer model fit in blue. The left central panel replicates the top panel’s data but expands the intensity axis for clearer viewing of the three [¹³C II] lines. The bottom left panel shows the residuals of the fit, with two horizontal black lines denoting the 3σ threshold. The top right panel focuses on individual background elements in red and the total background in violet. Meanwhile, the dashed blue curve represents velocity-resolved optical depth. The bottom right panel illustrates individual foreground elements in pink, alongside the overall foreground in red, again accompanying the dashed blue curve for optical depth representation.</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Fig. B.2.** Mean correction factor versus T<sub>ex</sub>. The mean correction factor rises up to ~ 80 K, beyond which it becomes independent of T<sub>ex</sub>.</figcaption></figure>

<figure><img src="image_13.png" /><figcaption>**Fig. B.3.** [C II] correction factor map (at an angular resolution of 36'' and 8'' grid) with fixed T<sub>ex</sub> = 80 K.</figcaption></figure>

## Appendix D: Determination of the total far-infrared flux

In order to determine a total FIR flux, we create dust spectral energy distributions (SEDs) using the Herschel PACS 70 µm and 160 µm and SPIRE 250 to 500 µm bands. All maps are convolved and re-gridded to the largest common angular resolution of 36'' with an 8'' pixel size. Following Pabst et al. (2022), we fit a gray

body given by

$$I_{\lambda} = B(\lambda, T_{d}) \left[ 1 - \exp\left(-\tau_{160} \left(\frac{160 \mu m}{\lambda}\right)^{\beta}\right) \right], \quad (D.1)$$
<figure><img src="image_14.png" /><figcaption>**Fig. C.1.** SimLine modeling setup of the C⁺ bubble overlaid on the observed <sup>12</sup>CO 6 → 5 and [C II] intensities. The panels (<sup>12</sup>CO 6 → 5 on the left and [C II] on the right) show a sketch of the setup for an ideal 3D bubble (note that the calculations are in 1D) in which the different shell regions are indicated. The positions of observed and modeled spectra, shown in Fig. C.2, are indicated by blue squares. The red star marks the exciting O star of the cH IIR.</figcaption></figure>

<figure><img src="image_15.png" /><figcaption>**Fig. C.2.** Observations versus results of the SimLine modeling. The left panel shows a PV cut from the center position along the positions of the observed and modeled spectra, indicated in Fig. C.1, together with the observed spectra. Δr = 21, etc. corresponds to an offset of (−15”, 15”) etc. The right panel displays the modeled PV cut and spectra from SimLine.</figcaption></figure>

with a fixed emissivity index $\beta = 2$ and an optical depth specified at 160 µm. A total FIR flux is then determined by integration between 40 to 500 µm. The choice of fixing $\beta$ biases the SED fit toward shorter wavelengths and warmer dust, but allows comparison with above mentioned studies. We note that the overall effect on the determined total FIR intensity is not strong, and the discussed correlations remain insensitive to this choice. The dominant error in the SED fit is the individual flux uncertainties in the *Herschel* PACS and SPIRE bands, which we assume to be 20% and 10%, respectively.