Dust production in the harsh environment of Sgr A* - MIRI/JWST observation of the O-rich asymptotic giant branch star IRS~3

A. Alonso Herrero; A. Eckart; A. Labiano; D. Dicken; D. Law; D. Rouan; F. Pei{\ss}ker; G. \"Ostlin; G. Wright; J. A. D. L. Blommaert

REVIEW 5 major objections 7 minor 296 references

Dust production in the harsh environment of Sgr A* - MIRI/JWST observation of the O-rich asymptotic giant branch star IRS~3

T0 review · 5 major / 7 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read JWST's MIRI spectra show the AGB star IRS 3, 0.17 pc from Sgr A*, is oxygen-rich, dust-producing, and harbors water in its envelope.

desk verdict New MIRI MRS spectrum makes IRS 3 the clearest O-rich AGB dust producer near Sgr A*, though the water claim and foreground decomposition need tightening. read the letter →

arxiv 2608.09511 v1 pith:A22ZNMJH submitted 2026-08-10 astro-ph.GA astro-ph.SR

F. Pei{ss}ker , M. García Marín , A. Eckart , G. Wright , O. C. Jones , D. Dicken , A. Alonso Herrero , D. Rouan

show 13 more authors

D. Law T. Böker T. Henning M. Baes A. Labiano L. Pantoni L. Hermosa Muñoz P.O. Lagage P. van der Werf G. Östlin J. A. D. L. Blommaert M. Güdel P. Guillard

This is my paper · ORCID

classification astro-ph.GAastro-ph.SR

keywords GalacticcenterAGBstarscircumstellardustsilicatewaterinspaceJWSTMIRIspectroscopymasslossformation

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper claims that IRS 3, the brightest mid-infrared AGB star in the inner parsec of the Milky Way, is an oxygen-rich star whose dusty envelope is actively producing silicates and alumina at a projected distance of only 0.17 pc from Sgr A*. Using new MIRI MRS spectra from JWST spanning 4.9 to 27.9 microns, the authors find deep silicate absorption at 9.7 and 18.5 microns with an optical depth ratio of $\tau_{9.7}/\tau_{18.5} = 3.5 \pm 0.1$, which they argue can only be reproduced by oxygen-rich dust. They report the first detection of water absorption in IRS 3's envelope, and radiative transfer modeling with a multi-shell envelope yields a luminosity near $60000\,L_\odot$ and a mass-loss rate of about $6\times10^{-5}\,M_\odot\,\mathrm{yr}^{-1}$. If correct, this shows that dust formation and the survival of water are not suppressed even in the radiation-dominated environment of a supermassive black hole.

What carries the argument

The load-bearing diagnostics are the two silicate absorption features in the mid-infrared: the 9.7 micron Si-O stretching mode and the 18.5 micron O-Si-O bending mode of amorphous silicates. Their optical depth ratio, measured as $\tau_{9.7}/\tau_{18.5} = 3.5 \pm 0.1$, is the chemical fingerprint that separates oxygen-rich AGB stars (which show both features in this ratio) from carbon-rich ones (which do not show this bending mode). These features are interpreted with the Hyperion Monte-Carlo radiative transfer code, which builds a multi-shell spherically symmetric envelope whose dust components are alumina (Al$_2$O$_3$) in the hot inner region and amorphous silicates in the cooler outer shells, and with HITRAN line lists used to model the H$_2$O absorption bands.

What would settle it

A spatially resolved mid-infrared observation of IRS 3 at roughly 0.1 arcsecond resolution that separates the compact envelope from any foreground clumps, combined with a decomposition of the 9.7 micron feature into interstellar and circumstellar components, would settle the claim: if the entire 9.7 micron feature is accounted for by foreground dust, the ratio $\tau_{9.7}/\tau_{18.5} = 3.5 \pm 0.1$ and the O-rich classification collapse. Alternatively, a detection of the 6.0 micron water band in absorption with a velocity offset matching the stellar wind, rather than at the systemic velocity, would directly confirm the water is in the envelope.

Watch

Extended reading notes

Core claim

The central discovery is that IRS 3 is an oxygen-rich (M-type) asymptotic giant branch star, not the carbon-rich star previously proposed, and that its extended envelope is a working dust factory. After correcting for foreground extinction with the stellar-based Kemper et al. (2004) law, the MIRI MRS spectrum shows the 9.7 micron Si-O stretching and 18.5 micron O-Si-O bending modes of amorphous silicates, with an optical depth ratio of $3.5 \pm 0.1$, a diagnostic of oxygen-rich chemistry. The same spectrum shows clear H$_2$O absorption bands between 6.0 and 7.0 microns, attributed to water in the envelope rather than the foreground. Hyperion radiative transfer models reproduce the observed spectral energy distribution with a multi-shell envelope containing alumina near the star and amorphous silicates further out, with a temperature gradient from roughly 1200 K to 80-100 K. The paper concludes that the harsh environment of Sgr A* does not inhibit dust formation or the survival of molecular species such as H$_2$O, and that IRS 3 is enriching the interstellar medium close to the black hole.

Load-bearing premise

The load-bearing premise is that the foreground extinction toward IRS 3 is accurately described by the Kemper et al. (2004) stellar-based law scaled with $A_{\mathrm{fg}} = 0.3\,\mathrm{mag}$, so that the residual 9.7 and 18.5 micron absorption features are intrinsic to the envelope of IRS 3 rather than an artifact of that correction.

Editorial extensions

If this is right

IRS 3 should be reclassified from a carbon-rich to an oxygen-rich AGB star, changing the census of evolved stars in the Galactic center.
The estimated mass-loss rate of about $6\times10^{-5}\,M_\odot\,\mathrm{yr}^{-1}$ implies that IRS 3 is a significant local source of newly formed dust in the immediate vicinity of Sgr A*.
The multi-shell envelope, with expansion ages of roughly 300 to 3200 years for the MIRI-visible shells, traces recent episodic mass-loss events of the star.
Water vapor can survive in the envelope at roughly 900 AU from the star despite the harsh radiation field, so molecular survival near a supermassive black hole is possible.
If IRS 3 is representative, dust observed in the inner parsec may be partly produced in situ by AGB stars rather than fully advected from larger radii.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

One implication the authors do not develop is that the bow-shock stand-off distance and the inferred low ambient density (about $10^2\,\mathrm{cm}^{-3}$) could be tested by future 3D hydrodynamical simulations of the wind-ISM interaction, which would also clarify whether shell 2 is genuinely bow-shock-compressed material.
A testable extension is to search for maser or rotational line emission of H$_2$O with ALMA at the roughly 900 AU location where the model places the water; a detection would confirm that the water is circumstellar rather than a foreground artifact.
If the local dust-production picture is correct, other luminous AGB stars in the inner parsec should show similar silicate features with mass-loss rates above a threshold; a systematic MIRI survey of the nuclear cluster could quantify how many faint envelopes are being stripped away.
The inferred young age of about 72 Myr and mass around $6\,M_\odot$, if confirmed by astrometry, would tie IRS 3's birthplace to the young stellar population of the Nuclear Stellar Cluster, with consequences for the 'missing red giants' debate.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

IRS 3 is now the best case for an O-rich AGB star actively making dust 0.17 pc from Sgr A*. The MIRI MRS spectrum is genuinely new, the 18.5 µm bending mode clinches the O-rich classification against Pott's C-rich suggestion, and the robustness check across three extinction laws is the right instinct. The paper deserves a serious referee and likely publication after revision.

What is new: first MIRI MRS spectrum of IRS 3 from 4.9–27.9 µm; first extinction-corrected MIR spectrum; the O-rich classification; the H2O claim. The custom saturation recovery is careful, and the paper honestly notes the ambiguities in the 6 µm water band and the Yusef-Zadeh multi-shell work.

Soft spots: (1) The foreground extinction decomposition. A_fg=0.3 is hand-set and the statement that 'the majority of the silicate absorption is intrinsic' is asserted, not demonstrated. The stress-test is right: all three extinction laws have similar 9.7 µm silicate features, so the robustness check shows the dereddened morphology is insensitive to the choice of law, not that the residual tau ratio is intrinsic. A joint fit that includes foreground plus envelope, or a decomposition plot showing the observed optical depth before dereddening, would settle this. Still, the 18.5 µm bending mode is present after dereddening, and C-rich AGB stars do not show it, so I would be surprised if the classification flips. (2) The water claim: the abstract says 'clear signs', the body says the broad component is ambiguous. That should be aligned in revision. (3) The circularity: shell temperatures are set by Eq. 3 and then reported as a measured gradient; the luminosity is saturated in RMSE between 5e4 and 6e4 L_sun, yet the derived mass, age, and mass-loss rate carry small formal errors from the tracks. These should be labeled as model-dependent.

None of this is fatal. The O-rich classification is probably right, and the paper is an honest observational study. I would send it to review, with a request to tone down the abstract and add a foreground–envelope decomposition.

Referee Report

5 major / 7 minor

Summary. The paper presents JWST/MIRI MRS spectroscopy (4.9–27.9 µm) of the Galactic Center AGB star IRS 3. After dereddening with a foreground extinction law scaled by a hand-set factor A_fg = 0.3 mag, the authors measure τ9.7/τ18.5 = 3.5 ± 0.1 and classify IRS 3 as an O-rich AGB star with an envelope containing amorphous silicates, alumina, and water. Radiative transfer modeling with Hyperion is used to infer a multi-shell envelope with a ~1000 K temperature gradient, a best-fit luminosity of 60000 L_sun, a mass-loss rate of about 6e-5 M_sun/yr, and a stellar mass of about 6 M_sun with an age of about 72 Myr. The paper claims the first detection of H2O in the envelope of IRS 3 and argues that dust production and molecular survival occur at 0.17 pc from Sgr A*.

Significance. If the central claims hold, the paper provides a valuable new view of dust and molecule production in an extreme Galactic Center environment, using a uniquely suited JWST dataset and a custom reduction that recovers saturated MRS data. The comparison of three extinction laws and the explicit radiative-transfer grid are strengths, as is the engagement with earlier VLTI and ALMA work. However, the load-bearing conclusions—the O-rich classification, the water detection, and the derived stellar parameters—depend on assumptions that are currently not quantitatively separated from model inputs. The dataset itself is important, but the analysis needs to be tightened before the claims can be accepted.

major comments (5)

[Sec. 2.2 and Sec. 3.2] The classification ratio τ9.7/τ18.5 = 3.5 ± 0.1 is measured on a spectrum dereddened with the Kemper et al. (2004) law normalized by a hand-set foreground factor A_fg = 0.3 mag. Section 4.2 states that 'the majority of the silicate absorption is intrinsic' but provides no quantitative decomposition of the foreground contribution; since the adopted law itself has A_9.7 = 1.44 mag, the residual envelope optical depths and their ratio could be dominated by the foreground normalization. Please provide a decomposition, for example by varying A_fg over a plausible range and reporting τ9.7, τ18.5, and their ratio, or by fitting a foreground-only model anchored to a truly continuum region. The stated anchor region 5.0–7.7 µm is not continuum-dominated because Sec. 3.1 identifies H2O absorption in exactly this range, which can bias the scaling.
[Table 1, Eq. (3), Sec. 3.3, Secs. 4.3–4.5] The shell temperatures listed in Table 1 are inputs used to define characteristic radii via Eq. (3); the same temperatures are then reported as a discovered 'temperature gradient of about 1000 K' in Sec. 3.3 and Sec. 4.3. Likewise, the stellar luminosity is selected as the best RMSE model in Sec. 2.3 and Fig. 5, then used in Sec. 4.5 to derive stellar mass and age, and in Sec. 4.4 to derive the mass-loss rate. These derived quantities are therefore not independent constraints but propagation of model inputs. Please state explicitly which parameters are fitted, which are assumed, and which are derived, and explore degeneracies (e.g., between temperature, density exponent, and dust density).
[Sec. 4.1] The statement that the spectrum 'can naturally only be reproduced by an oxygen-rich dust model' is not supported by the model grid: Sec. 2.3 states that only O-rich dust species (silicates and alumina) were included in Hyperion. No C-rich (e.g., SiC, amorphous carbon) or mixed-chemistry models were run. The absence of an 11.3 µm SiC feature is consistent with O-rich chemistry but does not establish uniqueness. Please either run alternative chemistry models or rephrase the claim as 'consistent with' rather than 'only'.
[Sec. 3.4 and Abstract] The abstract claims 'clear signs of H2O', but Sec. 3.4 describes the 6.12–6.25 µm feature as ambiguous, with the Gaussian components G0–G4 approximating unknown species and possible contributions from ice, PAHs, or residual extinction correction. To support the H2O claim, the fit should be compared against a model without H2O lines and with alternative species; otherwise the claim should be downgraded to 'tentative' or made explicitly conditional on the extinction-correction assumptions.
[Sec. 4.4, Eqs. (12)–(14)] The mass-loss rate and the ambient density are coupled within the same formalism: Eq. (12) gives Mdot from L and T_eff, and Eq. (14) uses that same Mdot to infer n_H. Thus the bow-shock calculation does not provide an independent check of Mdot. Please clarify which quantities are assumed and which are constrained, and propagate uncertainties from v_w and v_star through Eq. (14).

minor comments (7)

[Throughout] The word 'derreddened' appears in Sec. 4.1 and elsewhere; it should be 'dereddened'.
[Fig. 4] The label 'inlet' for the smaller optical-depth panels should be 'inset'.
[Sec. 4.5] The phrase 'inspect its the possible age' should read 'inspect its possible age'.
[Table 4] The column header 'Std' should specify that the quoted uncertainties are 3σ standard deviations, as stated in the notes; giving 1σ values would aid comparison with other work.
[Sec. 2.3] The notation '105 models' would read more clearly as '10^5 models'.
[Appendix A] The term 'third-rate file' is confusing; consider renaming it to something like 'third rate file (jump step skipped)' to avoid the unintended connotation.
[Sec. 3.2] The uncertainty estimate for τ uses Gaussian noise around the anchor points, but the number of realizations and the adopted anchor-point uncertainty are not stated; please add this information.

Circularity Check

2 steps flagged · score 6.0 of 10

Partial circularity: the reported shell temperature gradient is the assumed input grid restated as a result, and the O-rich-only model claim reuses the O-rich dust species put into the model; the central 9.7/18.5 micron classification itself is not circular.

self definitional [Abstract; Sec. 2.3, Table 1; Sec. 3.3]
""we find a multi-shell configuration that shows a significant temperature gradient between the inner and outer layers of the envelope" (Abstract); Table 1: "Temperature T[K] 1200 280–300 180 80–100"; Sec. 3.3: "Consequently, the temperature gradient ranges from 1200 K for the inner regions to 80-100 K for the outer dust components.""

The shell temperatures in Table 1 are input parameters, not quantities inferred from the MIRI spectrum: the characteristic radii are computed from the stellar luminosity and the chosen temperatures via Eq. (3). The paper then reports the difference between these same input temperatures (1200 K down to 80-100 K) as a discovered 'temperature gradient of about 1000 K' and lists it among the main results. This is a restatement of the model setup, not an output of the fit, so the claimed finding reduces by construction to the assumed parameter grid.
other [Sec. 2.3 and Sec. 4.1]
""For the dust composition of the models displayed in Fig. 5, a mixture of Al2O3 and silicates for an O-rich late-type star are used (Begemann et al. 1997; Karovicova et al. 2013; Gobrecht et al. 2016). ... Consequently, our analysis demonstrates that the spectral shape of IRS 3 and its deep silicate absorption can naturally only be reproduced by an oxygen-rich dust model (Ossenkopf et al. 1992).""

The Hyperion grid was constructed using only O-rich dust species (alumina and amorphous silicates), so the statement that the spectrum 'can naturally only be reproduced by an oxygen-rich dust model' is partly the premise of the model rather than a test outcome. No carbon-rich dust model was run in this comparison, so the model-based part of the 'only' conclusion is circular. The observed 9.7/18.5 micron ratio provides independent support for O-rich chemistry, which prevents this from being the sole basis of the classification, but the model demonstration as phrased reuses its own input as its conclusion.

full rationale

The central classification claim is not itself circular: IRS 3 is classified as O-rich from the residual 9.7 and 18.5 micron silicate absorption features and their optical-depth ratio tau_9.7/tau_18.5 = 3.5 +/- 0.1, and the paper explicitly checks that the overall morphology survives dereddening with three independent Galactic Center extinction laws (Fig. 7). That is an external robustness test, and the C-rich/stellar-vs-YSO arguments rest on published spectra and an earlier VLTI classification, not on the present model assumptions. The foreground scaling A_fg = 0.3 mag is hand-set and the claim that 'the majority of the silicate absorption is intrinsic' is not quantitatively decomposed, but this is a systematic uncertainty in the foreground subtraction rather than a self-definitional reduction, because the measured ratio is still a residual quantity that could in principle fail the adopted correction. The HITRAN-based H2O identification is a standard line-fitting exercise: the line positions come from an external database, so calling the fit a detection is not circular, although the residual Gaussian components are fitted to the same band. The genuine circular steps are secondary but public: the 'temperature gradient of about 1000 K' is exactly the range of shell temperatures adopted as input in Table 1, and the claim that the model demonstrates O-rich uniqueness reuses the O-rich dust species that were loaded into Hyperion. These are prominent conclusions, so they raise the score, but the independent spectroscopic ratio and the extinction-law comparison keep the central classification from reducing entirely to the model inputs.

Assumptions & free parameters 9 free parameters · 8 assumptions · 0 invented entities

The central claims rest on a set of modeling choices: a chosen foreground extinction normalization (A_fg=0.3), a luminosity that is an RMSE fit saturated at the top of the scanned range, shell temperatures and densities that are inputs to the radiative transfer model, and fitted H2O line parameters. The molecular line identification and the optical depth ratio give independent grounding to the O-rich classification, but the quantitative parameters (M, age, Mdot, n_H) are only as strong as these fitted inputs. No new physical entities are introduced.

free parameters (9)

Foreground extinction factor A_fg = 0.3 mag
Chosen to align the Kemper et al. (2004) extinction law with the 5-7.7 micron continuum and to match Fritz et al. (2011) and von Fellenberg et al. (2025) multiplicative factors; higher values are rejected as yielding inconsistent 9.7 micron levels. It sets the absolute scale of the dereddened spectrum and thus the depth of the intrinsic 9.7 micron silicate feature.
Stellar luminosity L = 60000 L_sun
RMSE best fit over a 6000-60000 L_sun scan; authors note no substantial difference between 50000 and 60000 L_sun models, so the value is a saturated upper bound. Drives stellar mass, age, and mass-loss rate.
Shell temperatures (inner, S1-S3) = 1200, 280-300, 180, 80-100 K
Inputs in Table 1 and Eq. (3), presented as the discovered 'temperature gradient of about 1000 K'; they are modeling inputs, not outputs of an independent derivation.
Density exponents p and dust densities = p=2.0/1.2 inner, 0.1-0.2 S1, 2.0 S2, 2.5-3.0 S3; rho0=4e-15 to 3e-22 g/cm3
Adopted to reproduce the SED; shell 1's near-flat density is interpreted as swept-up material.
H2O model parameters = T=700 K, N=1.5e17 cm^-2, p=1e-6 atm, vmac=4 km/s, vturb=1 km/s
Fitted to the 6.0-6.25 micron absorption band using HITRAN line lists plus Gaussian residuals.
Gaussian residual components G0-G4 = See Table 3 (tau0=0.02-0.15, widths 0.0008-0.036 micron)
Added to match residuals in the water band; G4, the broad 6.12-6.25 micron feature, is freely scanned and its origin is left ambiguous.
Assumed wind velocity v_w = 15 km/s
Taken as 'typical' from Vassiliadis and Wood (1993); used to convert shell radii to expansion times and in the bow-shock density estimate. Other groups used 20-30 km/s.
Space velocity v_star = 100 km/s
Adopted from Pott et al. (2008) for the bow-shock pressure balance.
Metallicity [M/H] = +0.35 dex
Assumed from Nuclear Stellar Cluster literature for PARSEC-COLIBRI tracks; affects the derived mass and age.

assumptions (8)

domain assumption IRS 3 lies at the Galactic center distance (about 8 kpc), so angular sizes convert to AU scales linearly.
Used throughout to turn the measured 0.1 pc envelope and 4316 AU stand-off distance into physical quantities; a different distance would rescale radii, densities, and mass-loss estimates.
domain assumption The Kemper et al. (2004) stellar-based extinction law, derived toward the inner parsec using the WR star IRS 1W, is representative of the foreground extinction toward IRS 3.
Sec. 2.2 and Appendix B: the dereddened spectrum and all derived optical depths rest on this. Robustness checks with Fritz et al. (2011) and von Fellenberg et al. (2025) laws are shown, but the foreground/source decomposition is not independently measured.
domain assumption The residual 9.7 and 18.5 micron absorption after dereddening is intrinsic to IRS 3's envelope.
Sec. 4.2 states 'the majority of the silicate absorption is intrinsic'; this is load-bearing for the O-rich classification and is entangled with the choice of A_fg and the shape of the extinction law.
standard math Hyperion Monte Carlo radiative transfer with spherical shells, a blackbody central source, and the adopted dust opacities (Ossenkopf et al. 1992 silicates, Begemann et al. 1997 alumina) adequately represents the source.
Sec. 2.3: the model grid assumes spherical symmetry and does not include the bow shock, which the authors note may explain the 5-9 micron excess and luminosity saturation.
standard math HITRAN line lists and the Voigt profile parameters provide a valid template for identifying H2O in the 6.0-6.25 micron band.
Sec. 2.4: the identification rests on the match of narrow features; the broad residual is not uniquely attributed.
domain assumption The empirical van Loon et al. (2005) mass-loss scaling applies to IRS 3.
Sec. 4.4, Eq. (12): used to estimate 6e-5 M_sun/yr; the authors call it an order-of-magnitude estimate.
domain assumption PARSEC-COLIBRI stellar tracks with super-solar metallicity (+0.35 dex) constrain the stellar mass and age from L and Teff.
Sec. 4.5: assumes IRS 3 formed in the Nuclear Stellar Cluster with mean cluster metallicity; different metallicity or migration history would shift the mass/age.
ad hoc to paper The three-shell envelope structure is a legitimate description rather than a numerical artifact of the chosen grid.
Sec. 3.3: the shells are adopted to reproduce the SED; the paper notes two outer shells were already reported by Yusef-Zadeh et al. (2017) from ALMA, and the origin of the inner shells remains ambiguous.

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Cite this review

Pith. "Pith review of Dust production in the harsh environment of Sgr A* - MIRI/JWST observation of the O-rich asymptotic giant branch star IRS~3." pith.science (2026). https://pith.science/paper/A22ZNMJH

@misc{pith2026260809511,
  author       = {Pith},
  title        = {Pith review of: Dust production in the harsh environment of Sgr A* - MIRI/JWST observation of the O-rich asymptotic giant branch star IRS~3},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/A22ZNMJH}},
  note         = {Machine review of arXiv:2608.09511}
}

abstract

Studies of the interstellar medium (ISM) have frequently revealed signatures of the dust produced in the envelopes of asymptotic giant branch (AGB) stars, demonstrating a connection between the dust composition of the ISM and that of AGB stellar envelopes. Investigating this relationship in the extreme, radiation-dominated environment surrounding Sgr A*, the center of our own galaxy, reveals how such conditions might influence dust composition and the recycling of material in galactic centers. IRS 3, the brightest L band source in the Galactic center and most prominent AGB star within the inner parsec of the Milky Way, is embedded in a dusty envelope with an estimated radius of $\sim$10000 AU. We aim to conduct a comprehensive spectral analysis to more tightly constrain the dust composition and line-emitting species within the envelope of IRS 3 in the immediate vicinity of Sgr A*. In 2025, we observed the inner parsec of the Milky Way with the Mid-Infrared Instrument (MIRI) on board the James Webb Space Telescope (JWST) as part of the guaranteed time observations (GTO) program Mid-Infrared Characterisation of Nearby Iconic galaxy Centres (MICONIC). We used the MIRI Medium Resolution Spectrometer (MRS) to study the spectroscopic characteristics of the AGB star IRS 3, located about 0.17 parsecs in projection from Sgr A*.

Figures

Figures reproduced from arXiv: 2608.09511 by the authors.

**Figure 1.** Mid-infrared image of the IRS 3 environment, observed with NACO (VLT) and MIRI/MRS (JWST). The background image is observed in the L-band (3.6 µm), the yellow inset shows a slice from the Channel 3 Long data cube, which covers (15.41–17.98 µm). The light blue boxes highlight an area of 1.6"×1.6". The SMBH Sgr A* is marked with a yellow ×, located at R.A. 17h45m40.05s and DEC -29:00:28.120. The projected distance be… view at source ↗

**Figure 2.** Comparison of available extinction laws for the inner parsec of the Galactic Center. Here, we plot the factor 100.4·Aλ against the wavelength. The observed flux is multiplied by this factor to achieve the dereddened spectrum (see text for details). infrared extinction laws is around 9.7 µm, explained by a different optical depth of the used objects/regions to construct the models. Regardless of the difference in o… view at source ↗

**Figure 4.** Optical depth estimates of the 9.7 µm and 18.5 µm absorption feature. The upper plot shows the 9.7 µm-, the lower the 18.5 µm-silicate absorption. Both plots exhibit an inlet that displays the related fit of the optical depth. The anchor points of the fit are shaded in gray, whereas the spectral range of the peak of the optical depth is indicated in light blue. Ultimately, we compare the observed and dereddened spec… view at source ↗

Figures from the paper (5 more)

**Figure 5.** Figure 5: Comparison of the dereddened spectrum and the results of the radiative transfer modeling. For all models, we use the same parameter range as listed in [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]

**Figure 6.** Figure 6: Synthetic spectrum based on HITRAN line list of H2O overlaid on the observed spectrum of IRS 3 between 6.00-6.25 µm. The 0.1 µm wide absorption feature between 6.12-6.25 µm represents an additional water component at 6.19 µm coupled with an unidentified species. absorp…

**Figure 7.** Figure 7: Resulting dereddened spectrum of IRS 3 using three different extinction laws. For all three final spectra, the classification of IRS 3 as an O-rich AGB star holds. there are deviations between 12.5-15.0 µm and 20.0-25.0 µm, the overall morphology is robust against the …

**Figure 8.** Figure 8: Projected stand-off distance estimate of the bow shock of IRS 3. The stand-off distance is a measure of the ambient ISM and the ram pressure of the star. Here, the green x marks the position of IRS 3 and the green circle the apex of the bow shock. stand-off distance, t…

**Figure 9.** Figure 9: Hertzsprung-Russel-Diagram with isochrones showing the main-sequence (central diagonal line) and post-main-sequence (upper horizontal line) stellar tracks for low, intermediate, and massive stars with a super-solar metallicity of ≈+0.35. The cold and luminous AGB star …

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Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.

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