GOALS-JWST: Small Neutral Grains and Enhanced 3.3 μm PAH Emission in the Seyfert Galaxy NGC 7469

The strong infrared emission bands at 3.3, 6.2, 7.7, 8.6, 11.3, and 17 μm are detectable in the spectra of a diverse range of astrophysical sources, ranging from photodissociation regions (PDRs) in nebulae (Werner et al. 2004), to nearby star-forming (SF) galaxies (Peeters et al. 2004; Smith et al. 2007) and luminous infrared galaxies (LIRGs; see Armus et al. 2020, for a review), even to distant galaxies at high redshifts (z > 1; Sajina et al. 2009; Pope et al. 2013; Riechers et al. 2014; Spilker et al. 2023). These prominent spectral features are often attributed to polycyclic aromatic hydrocarbon (PAH) molecules (Leger & Puget 1984; Allamandola et al. 1985; Tielens 2008; Li 2020), which can account for up to 15% of the cosmic carbon (Li & Draine 2001; Zubko et al. 2004; Draine & Li 2007; Jones et al. 2017) and contribute up to ∼20% of the total infrared luminosity from a galaxy (Smith et al. 2007).

The 3.3 μm PAH band is the shortest-wavelength feature among all of the PAHs and primarily attributed to the C–H stretching mode. It is known to trace the neutral, smallest PAH population in the interstellar medium (ISM), typically with a radius of ∼5 Å or N_C ∼ 50 carbon atoms (Schutte et al. 1993; Draine & Li 2007). The 3.3 μm PAH has been the least-studied PAH feature due to its inaccessibility from ground-based observations and the lack of spectral coverage of Spitzer/IRS shortward of 5 μm. Nonetheless, observations with the AKARI infrared satellite (Murakami et al. 2007) had previously demonstrated the power of using the 3.3 μm PAH to diagnose star formation and active galactic nuclei (AGN) in (U)LIRGs (Imanishi et al. 2008, 2010; Ichikawa et al. 2014; Inami et al. 2018) and study the photoelectric efficiency that couples the stellar radiation field with gas temperatures (McKinney et al. 2021). Just as importantly, the 3.3 μm band is the only PAH feature that will be accessible to JWST at high redshifts, making detailed studies of this feature at low redshift of paramount importance for understanding dust and metals at early epochs.

In a joint AKARI+Spitzer study, Lai et al. (2020) found that the fractional 3.3 μm PAH power (L_{PAH 3.3}/L_{Σ PAH}) in nearby SF galaxies typically ranges from 1.5% to 3%, a value that is significantly smaller than that for the brightest 7.7 μm PAH complex, which typically reaches L_{PAH 7.7}/L_{Σ PAH} ∼ 40% in nearby SF galaxies (Smith et al. 2007). Despite its faintness, the 3.3 μm PAH feature has been proposed as an accurate tool for measuring the average grain size when paired with the 11.3 and 17 μm PAH bands, which also serve as tracers of neutral grains (e.g., Croiset et al. 2016; Lai et al. 2020; Maragkoudakis et al. 2020, 2022, 2023a, 2023b; Draine et al. 2021; Rigopoulou et al. 2021; Sidhu et al. 2022). The 3.3 μm PAH holds the potential to be a sensitive diagnostic of ISM conditions, as well as an estimator of the star formation rate (SFR; e.g., Peeters et al. 2004; Shipley et al. 2016; Lai et al. 2020) accessible from nearby galaxies to high redshifts with JWST imaging and spectroscopy (Inami et al. 2018; Evans et al. 2022; Leroy et al. 2023; Sandstrom et al. 2023). These applications, however, strongly rely on our understanding of the properties of PAHs and how they depend on metallicity and react to the ambient radiation field, as PAHs can be faint or even absent in low-metallicity environments (Wu et al. 2006; Hao et al. 2009), as well as in galaxies with powerful AGN (O'Dowd et al. 2009; Diamond-Stanic & Rieke 2010; Sajina et al. 2022). Surprisingly, some studies have shown that AGN photons can also be the source of PAH molecule excitation and emission (Howell et al. 2007; Jensen et al. 2017).

In this paper, we focus on tracing the physical conditions of the neutral dust grains probed by the 3.3 μm PAH in NGC 7469 using the superb spatial and spectral resolution of the JWST Near Infrared Spectrograph (NIRSpec; Jakobsen et al. 2022). As a follow-up study to Lai et al. (2022, hereafter Paper I), the JWST/MIRI results are also included here in a joint analysis to provide a complete view of the aromatic bands in NGC 7469.

NGC 7469 (Arp 298, Mrk 1514, IRAS F23007+0836) is a galaxy located at D_L = 70.6 Mpc and classified as a Seyfert 1.5 (Landt et al. 2008). It is an LIRG (L_{8–1000 μm} = 10^11.6 L_☉) with a supermassive black hole mass of 1.1 × 10⁷ M_☉ (Peterson et al. 2014; Lu et al. 2021) and X-ray luminosity of L_{2–10 keV} = 10^43.19 erg s⁻¹ (Asmus et al. 2015). NGC 7469 contains an accreting black hole and a starburst ring with a radius of ∼500 pc (e.g., Song et al. 2021). Recently, NIRCam imaging data revealed a factor of ∼6 more dusty, young (<5 Myr) clusters compared to the previous identifications made by HST (Bohn et al. 2023). Using JWST integral field spectroscopy, emission lines with ionization potential up to 187 eV are detected within a distance of ∼100 pc from the AGN with an outflowing wind that can reach up to 1700 km s⁻¹ traced by high-ionization lines (Armus et al. 2023), and the ionized coronal wind probed by [Mg v] (IP: 109 eV) extends out to ∼400 pc from the nucleus (Vivian et al. 2022). By studying the PAH ratios in the mid-infrared, Paper I found that feedback from the central black hole mostly impacts the inner ISM region, leading to a larger grain size distribution in the vicinity of the AGN than that in the ring (cf. García-Bernete et al. 2022b).

Throughout this paper, a cosmology with H₀ = 70 km s⁻¹ Mpc⁻¹, Ω_M = 0.30, and Ω_Λ = 0.70 is adopted. The redshift of NGC 7469 (z = 0.01627 ³⁴ ) corresponds to a projected physical scale of 330 pc arcsec^–1.

As part of Director's Discretionary Time Early Release Science program 1328 (Co-PIs: L. Armus and A. Evans), the JWST near-infrared integral field unit (IFU) observations (Böker et al. 2022) of NGC 7469 were taken with NIRSpec on 2022 July 19. The NIRSpec IFU observations were carried out using a set of high-resolution gratings (with a nominal resolving power of R ∼ 2700), namely, G140H/100LP, G235H/170LP, and G395H/290LP, covering a wavelength range of 0.97–5.27 μm. For each grating, the science exposure time was 817 s, and a four-point dither pattern was used to sample the extended SF ring. In this study, we focus on the G395H grating that contains the shortest PAH band at 3.3 μm.

We downloaded the uncalibrated science observations through the MAST portal. The data reduction process was done using the JWST Science Calibration Pipeline version 1.8.3 (Bushouse et al. 2022), with a reference file of jwst_12027.pmap. Three stages of pipeline processing were applied, including Detector1, Spec2, and Spec3. While the dedicated background is not included in the observation strategy, "leakcal" was performed in the observation to mitigate the contamination due to a failed open microshutter assembly. We refer readers to our companion paper (Bianchin et al. 2023) for more details on the data processing.

To obtain a complete spectroscopic view of NGC 7469, we combined the NIRSpec IFU data with the MIRI IFU data presented in Paper I, allowing us to study all of the PAH features from 3 to 20 μm. To properly compare the NIRSpec and MIRI data, two modifications to the NIRSpec cube had to be made. First, a spatial offset of ∼024 between the NIRSpec and MIRI IFUs was found, so we combined the two IFUs by shifting the WCS of NIRSpec to match with that of MIRI, whose astrometry has been verified with the MIRI imaging. This offset was measured by comparing the collapsed images from the spectral overlap region between 5.0 and 5.1 μm in both IFUs. Second, in order to combine the IFUs while matching their spatial resolution, we smoothed the NIRSpec G395H/290LP cube and MIRI channels 1 and 2 by convolving them with wavelength-dependent Gaussian convolution kernels to match with the FWHM measured at 11.5 μm (FWHM ∼ 046), where the longest-wavelength PAH feature (PAH 11.3 μm in MIRI channel 2) studied in this paper is located. The convolution was performed as in Zhang & Ho (2023) and based on the Gaussian2DKernel function in astropy.convolution. The convolution kernel is calculated using the NIRSpec-observed standard star P330E (PID: 1538; PI: K. Gordon) and the MIRI observed star HD 159222 (PID: 1050; PI: B. Vandenbussche).

Many studies have found that the hardness of the radiation field probed by [Ne iii]/[Ne ii] plays an important role in regulating PAH ratios in AGN and SF galaxies (e.g., Smith et al. 2007; Sales et al. 2010; García-Bernete et al. 2022a). Particularly, in Paper I, we have shown that the main driver of grain size variation in this galaxy is [Ne iii]/[Ne ii], which will also be used here to understand the properties of the 3.3 μm PAH. In Figure 1, we present the PAH and [Ne ii] maps, along with a [Ne iii]/[Ne ii] emission line flux ratio map. The SF ring is dominated by bright PAH emission, which provides a dust map with the highest available spatial resolution of FWHM ∼ 019 using the NIRSpec IFU data compared to the MIRI channel 3 [Ne ii] map, which has an FWHM ∼ 048. In general, the PAH 3.3 and [Ne ii] emission show similar morphology, having four clumps along the ring, but the relative intensities differ. For example, the neon emission is brighter in the southern clump (4-1), whereas PAH 3.3 is brighter in the northern clump (4-5).

Zoom In Zoom Out Reset image size

In Paper I, the study of the MIR dust and gas properties in NGC 7469 was carried out on an aperture-based analysis of the MIRI IFU data. In the study presented here, we maximize the full potential of an IFU observation by applying a grid extraction to both the NIRSpec and MIRI IFUs. This allows us to obtain spectra across a wide wavelength range from 3 to 28 μm in a systematic approach. The grid extraction was performed on the smoothed NIRSpec and MIRI cubes using the spectral extraction tool included in the most recent version of the Continuum And Feature Extraction (CAFE) software. This software was initially developed by Marshall et al. (2007) for Spitzer/IRS and has recently been updated for JWST (see T. Díaz-Santos et al. 2023, in preparation), which includes the capability of handling both spectral extraction of the IFU cube and spectral decomposition of the extracted spectra.

For the grid extraction, we initially set the center of the grid at the nucleus (23:03:15.6139, +8:52:26.266 J2000) and used 7 × 7 grid cells, each 06 wide, to extract spectra across the full field of view (FoV) from both the smoothed NIRSpec and MIRI cubes. The grid presented in Figure 1 shows the positions of our extracted spectra. No extraction is done if the grid cell exceeds the coverage of the IFU FoV, so the total number of extractions is 38 instead of 49, including the 30 cells (white) having full G395H and MIRI coverage and eight cells (dark blue) having complete NIRSpec coverage but incomplete MIRI coverage (missing some PAH emission). Of the eight cells, five (2-0, 3-6, 4-5, 5-5, and 6-0) exhibit the 3.3 μm PAH, the 3.4 μm aliphatic feature, and the [Ne ii] and [Ne iii] lines, even in the absence of MIRI coverage. These cells will be discussed in the analysis focusing on the aliphatic-to-aromatic ratio (see Figure 3, left panel). This partial coverage of MIRI is due to the slight spatial mismatch between each MIRI subchannel. To obtain the full spectral coverage of 3–28 μm, we stitched the spectrum of NIRSpec to MIRI.

The 35 cells with 3.3, 3.4, [Ne ii], and [Ne iii] are divided into three groups: SF, gap, and nucleus. Most of the extracted spectra belong to the SF ring, except for the five cells 2-3, 2-4, 3-4, 4-3, and 4-4, which are designated as gap region cells, and the nuclear extraction (3-3). Note that the nuclear spectrum presented here differs from the AGN spectrum analyzed in Armus et al. (2023), which was extracted using an expanding cone with a small inner diameter of 03 at 5.5 μm to isolate the central source and the base of the outflow.

The FoV of the dithered JWST NIRSpec IFU observations (42 × 48) provides complete coverage of the NGC 7469 circumnuclear ring and inner ISM, allowing for high spatial and spectral resolution in the study of dust and star formation properties in the near-infrared. To demonstrate the variation of the spectra across the IFU, we summed the individual grid spectra to create three NGC 7469 spectra: nuclear, ring, and gap (see Figure 2(a)). The low-resolution (R ∼ 100) AKARI+Spitzer spectrum taken from the AKARI–Spitzer Extragalactic Spectral Survey (ASESS; Lai et al. 2020) is also presented for comparison. Clearly, PAHs are heavily suppressed in the nuclear spectrum, while the high-ionization fine-structure lines are noticeably strong. For example, the nuclear spectrum has the highest [Ne iii]/[Ne ii] and [S iv]/[Ne ii] line flux ratios among the region spectra.

Zoom In Zoom Out Reset image size

To fit and analyze the NIRSpec spectra, we use CAFE, a spectral decomposition tool that is able to simultaneously fit the PAH features, dust continuum, absorbed ice and gas features, and narrow fine-structure atomic and molecular gas emission lines. The stacked SF ring spectrum, together with its spectral fit, is presented in Figure 2(b), and a zoom-in view at the 3 μm region is presented in Figure 2(c). In this regime, the spectrum is dominated by the 3.3 μm PAH band and 3.4 μm aliphatic feature, sitting on top of a broad plateau that can extend up to ∼3.8 μm. In addition, absorption features due to water ice at 3.05 μm, CO₂ ice at 4.27 μm, and CO ice at 4.67 μm can also be seen. We report the central wavelengths and widths of the three dust components seen in the stacked ring spectrum in Table 1. We find the 3.3 and 3.4 μm features to be narrower, while the plateau is broader than previous measurements made with AKARI (Lai et al. 2020). This is undoubtedly due to the substantially higher spectral resolution of NIRSpec, enabling an accurate and detailed deblending of the dust components in the 3 μm complex for the first time. The measurements of the extinction-corrected PAH and neon fluxes in each cell, as derived from the 9.7 μm silicate absorption depth and fit with CAFE, are presented in Table 2.

4.1. Aliphatic versus Aromatic Emission in NGC 7469

The abundance ratios of different types of carbonaceous dust can provide insights into their formation mechanisms and histories. The 3.4 μm emission feature is often attributed to the vibrations of –CH₃ (methyl) and –CH₂ (methylene) groups in aliphatic hydrocarbons (Joblin et al. 1996; Yang et al. 2016), and it can also be seen in absorption along sight lines with large extinction (Pendleton & Allamandola 2002; Chiar et al. 2013; Hensley & Draine 2020). The variation of the ratio between this 3.4 μm aliphatic feature and the 3.3 μm aromatic feature is indicative of the processing of dust particles in the ISM, as the chainlike aliphatic bonds are more fragile compared to the ringlike aromatic bonds.

The 3.4 μm aliphatic feature was detected in all of the grid cells of NGC 7469 except for the nucleus. The 3.4/3.3 ratio varies by about a factor of 2 across the IFU FoV. Regions with a harder radiation field, as measured by the [Ne iii]/[Ne ii] line flux ratio, tend to have a lower average 3.4/3.3 ratio and a larger scatter. The 3.4/3.3 ratio is lower in cells between the ring and the nucleus, decreasing by about 20% compared to those in the SF ring, suggesting that the aliphatic bonds are more susceptible to photodestruction than the aromatic bonds (Figure 3, left panel). There is no detection of the 3.4 μm emission at the nucleus, and the range in 3.4/3.3 ratio values is largest in the cells with [Ne iii]/[Ne ii] > 0.5. While visible, the variation of the 3.4/3.3 ratio in the SF ring of NGC 7469 is relatively small, ranging only from 5% to 8%, compared to Galactic regions that can range widely from ∼1% to 17% in PDRs (Pilleri et al. 2015, see Figure 7(c)), suggesting that the photoenergy density in the ring is high, with log(G₀) > 3 in units of the Habing field (Habing 1968).

Zoom In Zoom Out Reset image size

4.2. PAH Size Distribution

4.3. Enhancement of the 3.3 μm PAH

In Paper I, it was shown that the hardness of the radiation field was correlated with the PAH size variations seen in NGC 7469. Here we expand that analysis using the 3.3 μm PAH feature. Figure 4(a) shows the variation of the total PAH-to-[Ne ii]+[Ne iii] ratio as a function of the [Ne iii]/[Ne ii] line flux ratio, color-coded by the total ionized PAH surface density, which traces the amount of photoelectric heating in the ISM. Here the total PAH (ΣPAH) refers to the sum of the 3.3, 6.2, 7.7, 8.6, 11.3, and 17 μm PAH features, while the total ionized PAH surface density is derived from only the 6.2, 7.7, and 8.6 μm PAH features. In cells with large [Ne iii]/[Ne ii] line flux ratios (>0.25), the ΣPAH-to-Ne ratio drops, resulting in a downward trend of ΣPAH to Ne with increasing radiation hardness. Their low ΣPAH-to-Ne ratios may be due to excess emission from AGN, together with a possible deficit of total PAH emission in highly ionized regions, similar to what has recently been observed in four nearby SF galaxies with JWST and MUSE (Egorov et al. 2023).

Zoom In Zoom Out Reset image size

Besides the grid cell spectral extractions, we include two additional points to Figure 4. The diamond represents the total extraction of the IFU using a radius of 16 that covers the AGN and the entire ring, while the triangle represents the integrated light obtained from the combined AKARI+Spitzer NGC 7469 spectrum in the ASESS sample (Lai et al. 2020). The AKARI+Spitzer measurement probes an area that is three times wider than the coverage provided by the IFU, with a measured ΣPAH-to-Ne ratio that is larger than all of the individual JWST points. This is consistent with Díaz-Santos et al. (2011), who showed that PAHs are more extended, on average, than the [Ne ii] emission in the GOALS galaxies. The two sets of contours indicate the distributions based on 244 galaxies within GOALS (red; Stierwalt et al. 2014) and 62 galaxies that are in both GOALS and the bright PAH samples in ASESS (blue; Lai et al. 2020) but refitted with CAFE to rule out the potential discrepancy caused by the use of different spectral decomposition tools. The GOALS sample includes LIRGs powered by starbursts and/or AGN, while the bright PAH sample consists only of SF galaxies. The NGC 7469 data points overlap with the two sets of contours but lie at the lower envelope of both distributions, suggesting slightly weaker overall PAH emission (with respect to the fine-structure line emission) in NGC 7469 compared to global measurements of other LIRGs and SF galaxies. We note that only PAHs at wavelengths >5 μm are considered in Stierwalt et al. (2014), so there is no inclusion of the 3.3 μm PAH, which typically contributes less than 3% of the total PAH emission in SF galaxies (Lai et al. 2020) but would nevertheless raise the GOALS points even further.

In Figure 4(b), the PAH 3.3–to–Ne ratios do not show a trend when [Ne iii]/[Ne ii] < 0.25, but as the [Ne iii]/[Ne ii] ratio becomes larger (>0.25), the PAH 3.3/neon ratio drops by at least 50%, most clearly seen in the gap cells between the nucleus and the ring. The relative enhancement of the 3.3 μm PAH emission compared to other PAH features is evident in Figure 4(c). Here a striking picture emerges when we zoom in on the scale of the SF ring, with each cell having a width of ∼200 pc, and find PAH 3.3/ΣPAH ratios that can be up to 4× higher than the global measurements seen in other starburst galaxies. This excess 3.3 μm PAH persists compared to most starburst galaxies even in cells close to the nucleus, suggesting that the regions viewed by the IFU in NGC 7469 have a smaller grain size distribution than those measured in starburst galaxies on kiloparsec scales. A detailed discussion of this excess can be found in Section 5.2. Another PAH band exhibiting a noteworthy enhancement is the 6.2 μm feature; however, its maximum increase is limited to 30%, a magnitude that falls significantly short of the enhancement observed in the 3.3 μm PAH band.

5.1. Photodestruction of PAH

5.2. The Excess of PAH 3.3

5.3. PAH 3.3 as an SFR Indicator

JWST has opened up the possibility of spectroscopically detecting PAH emission in large numbers of high-z galaxies (Spilker et al. 2023) and, in particular, using this feature as an SFR indicator. The 3.3 μm PAH is the last band to shift beyond the long-wavelength coverage of MIRI, making it a prime tool to probe star formation out to redshifts of z ∼ 6. At low redshifts, it has been shown that there is a tight correlation between the SFR probed by PAH 3.3 and [Ne ii]+[Ne iii] emission in metal-rich SF galaxies; metal-poor galaxies, on the other hand, exhibit peculiar behavior that may lead to an underestimation of the SFR via the use of PAHs by nearly an order of magnitude in some cases (Lai et al. 2020).

Figure 5 shows the comparison between the SFR derived from the 3.3 μm PAH (Lai et al. 2020), which can be written as

$$\begin{eqnarray}&&\mathrm{log}\left(\displaystyle \frac{\mathrm{SFR}}{{M}_{\odot }\,{\mathrm{yr}}^{-1}}\right)=-(6.80\pm 0.18)+\mathrm{log}\left(\displaystyle \frac{{L}_{\mathrm{PAH}\ 3.3}}{{L}_{\odot }}\right),\end{eqnarray} \tag{ 1 }$$

and that from the neon lines, which is based on Equation (13) in Ho & Keto (2007), with the fraction of ionized neon emission derived from Equation (5) in Zhuang et al. (2019). An independent test has also been conducted by comparing our PAH-derived SFR to the PAH 6.2–to–IR luminosity relation reported in Table 4 of Gruppioni et al. (2016). By assuming the median 6.2/3.3 PAH ratio of 3.08 found in our SF cells, the SFRs provided in Gruppioni et al. (2016) and Lai et al. (2020) are consistent at the 10% level.

Zoom In Zoom Out Reset image size

In Figure 5, on average, the measurements in the SF ring follow the 1:1 line, showing slightly higher (27%) SFR_PAH3.3 than SFR_Ne with a small spread of 0.09 dex. However, the gap region cells and the nucleus show substantial deviations from the correlation due to the suppressed PAH emission in and around the AGN. An observation of a galaxy like NGC 7469 at high redshift, where the AGN and ring were spatially unresolved, would result in an underestimate of the SFR by at least 50% if measured from PAH 3.3 alone due to the mixing of the AGN and starburst emission in the beam.

With the advent of JWST, we can now probe the ISM in the vicinity of a powerful AGN on scales of a few hundred parsecs. In this paper, we present observations of the ISM in the nearby Seyfert galaxy NGC 7469 using NIRSpec IFU, supported by MIRI observations first reported in Lai et al. (2022). In particular, we focus on the properties of small and neutral aromatic grains traced by the 3.3 μm PAH band, together with a nearby aliphatic feature at 3.4 μm. Our findings can be summarized as follows.

• 1.  
  With the NIRSpec IFU, we are able for the first time to confidently separate the dust features at 3 μm in a resolved extragalactic source. In NGC 7469, the aliphatic (3.4 μm) to aromatic (3.3 μm) ratio varies by a factor of 2 across the IFU FoV, and this ratio is slightly lower near the AGN. This low 3.4/3.3 flux ratio, although with scatter, is most visible in the region between the Seyfert nucleus and the starburst ring, where the [Ne iii]/[Ne ii] line flux ratio reaches values of 0.5–1.0. The 3.4/3.3 ratio at the nucleus is very low compared to all other regions, suggesting extreme photodestruction of the grains by the AGN.
• 2.  
  The 11.3/3.3 PAH ratio, which is a measure of the average grain size, is significantly larger (>2×) in the vicinity of the AGN than it is in the starburst ring, suggesting a destruction of small grains within 300 pc of the nucleus, consistent with the results of Paper I. The nuclear spectrum displays a seemingly low 11.3/3.3 ratio, although with a large uncertainty, as all of the PAH fluxes are suppressed in this region.
• 3.  
  The total PAH-to-Ne ratio throughout the NIRSpec field is low in NGC 7469 compared to most local LIRGs and star-forming galaxies. However, the 3.3-to-Ne ratio and the fractional 3.3 μm PAH power (3.3/ΣPAH) in the starburst ring of NGC 7469 are high compared to most LIRGs, which may be due to recurrent fluorescence of small grains or multiple photon absorption by large grains on 100 pc scales.
• 4.  
  An unresolved measurement of the PAH and Ne line emission in the central region of NGC 7469 that includes both the AGN and the star-forming ring, such as might be observed with JWST at high redshift, would lead to an underestimation of its PAH-derived star formation rate (SFR) by at least 50%. Thus, caution should be exercised when using PAHs to measure SFR in high-z AGN hosts or galaxies where AGN cannot be safely ruled out.

Here we have shown that the 3.3 μm PAH feature varies on subkiloparsec scales in NGC 7469, and that these variations can reveal changes in the grain populations as they react to changes in the ISM properties around an AGN and an intense starburst in this composite galaxy. Further observations of other nearby sources like NGC 7469 will be critical to fully understand, from a statistical standpoint, the expected variations in the PAH-band fluxes and ratios that we can expect to see at high redshift with JWST in the coming years.

The authors thank A. Witt and E. Peeters for helpful discussions. This work is based on observations made with the NASA/ESA/CSA JWST. T.S.-Y.L. acknowledges funding support from NASA grant JWST-ERS-01328. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program No. 1328 and can be accessed via doi:10.17909/vq6q-sd19. Research at UCI by M.B. and V.U. was supported by funding from program No. JWST-GO-01717, which was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. V.U. further acknowledges partial funding support from NASA Astrophysics Data Analysis Program (ADAP) grant Nos. 80NSSC20K0450 and 80NSSC23K0750 and HST grant Nos. HST-AR-17063.005-A and HST-GO-17285.001. The Flatiron Institute is supported by the Simons Foundation. H.I. and T.B. acknowledge support from JSPS KAKENHI grant No. JP21H01129 and the Ito Foundation for Promotion of Science. A.M.M. acknowledges support from the National Science Foundation under grant No. 2009416. A.S.E. and S.L. acknowledge support from NASA grants HST-GO15472 and HST-GO16914. S.A. gratefully acknowledges support from ERC Advanced grant 789410, the Swedish Research Council, and the Knut and Alice Wallenberg (KAW) Foundation. K.I. acknowledges support by the Spanish MCIN under grant PID2019-105510GB-C33/AEI/10.13039/501100011033. F.M.-S. acknowledges support from NASA through ADAP award 80NSSC19K1096. Finally, this research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

Facilities: JWST (NIRSpec & MIRI) - , MAST - , NED - .

Software: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), CAFE (Marshall et al. 2007), JWST Science Calibration Pipeline (Bushouse et al. 2022), lmfit (Newville et al. 2014), Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2011; Harris et al. 2020), QFitsView (Ott 2012), SciPy (Virtanen et al. 2020).