# The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 µm Imaging Atlas of Active Galactic Nuclei Using SOFIA

Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A Levenson, Masatoshi Imanishi, et al.

► To cite this version:

Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, et al.. The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 µm Imaging Atlas of Active Galactic Nuclei Using SOFIA. The Astrophysical Journal Supplement Series, 2025, 276 (2), pp.64. 10.3847/1538-4365/ad9907. hal-05421774

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# The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 µm Imaging Atlas of Active Galactic Nuclei Using SOFIA

Lindsay Fuller¹, Enrique Lopez-Rodriguez²,³, Ismael García-Bernete⁴, Cristina Ramos Almeida⁵,⁶,⁸, Almudena Alonso-Herrero⁷, Chris Packham¹,⁸, Lulu Zhang¹, Mason Leist¹, Nancy A. Levenson⁹, Masatoshi Imanishi⁸, Sebastian Hoenig¹⁰, Marko Stalevski¹¹,¹², Claudio Ricci¹³,¹⁴, Erin Hicks¹⁵, Enrica Bellocchi¹⁶,¹⁷, Francoise Combes¹⁸, Ric Davies¹⁹, Santiago García Burillo²⁰, Omaira González Martín²¹, Takuma Izumi⁸, Alvaro Labiano²², Miguel Pereira Santaella²³, Dimitra Rigopoulou⁴,²⁴, David Rosario²⁵, Daniel Rouan²⁶, Taro Shimizu¹⁹, and Martin Ward²⁷

¹ University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA

²Department of Physics & Astronomy, University of South Carolina, Columbia, SC 29208, USA

³Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), Stanford University, Stanford, CA 94305, USA

⁴Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK

⁵Instituto de Astrofísica de Canarias, Calle Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain

⁶Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain

⁷Centro de Astrobiología (CAB), CSIC-INTA, Camino Bajo del Castillo s/n, E-28692, Villanueva de la Cañada, Madrid, Spain

⁸National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

⁹Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

¹⁰School of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UK

¹¹Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia

¹²Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281-S9, Gent B-9000, Belgium

¹³Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile

¹⁴Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China

¹⁵Department of Physics and Astronomy, University of Alaska Anchorage, Anchorage, AK 99508-4664, USA

¹⁶Departmento de Física de la Tierra y Astrofísica, Fac. de CC Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain

¹⁷Instituto de Física de Partículas y del Cosmos IPARCOS, Fac. CC Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain

¹⁸LERMA, Observatoire de Paris, Collège de France, PSL University, CNRS, Sorbonne University, Paris, France

¹⁹Max Planck Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching bei München, Germany

²⁰Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, E-28014 Madrid, Spain

²¹Instituto de Radioastronomía y Astrofísica (IRYA), Universidad Nacional Autónoma de México, Antigua Carretera a Pátzcuaro #8701, ExHda. San José de la Huerta, Morelia, Michoacán, C.P. 58089, Mexico

²²Telespazio UK for the European Space Agency, ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Spain

²³Instituto de Física Fundamental, CSIC, Calle Serrano 123, E-28006 Madrid, Spain

²⁴School of Sciences, European University Cyprus, Diogenes Street, Engomi, 1516 Nicosia, Cyprus

²⁵School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne NE1 7RU, UK

²⁶LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Sorbonne Paris Citeé, 5 place Jules Janssen, F-92195 Meudon, France

²⁷Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK

Received 2024 June 11; revised 2024 November 21; accepted 2024 November 21; published 2025 February 3

## Abstract

We present a 19.7–214 µm imaging atlas of local (4–181 Mpc; median 43 Mpc) active galactic nuclei (AGN) observed with FORCAST and HAWC+ on board the SOFIA telescope with angular resolutions ~3′′–20″. This atlas comprises 22 Seyferts (17 Type 2 and five Type 1) with a total of 69 images, 41 of which have not been previously published. The AGN span a range of luminosities of $log_{10}(L_{bol}[erg~s^{-1}]) = [42, 46]$ with a median of $log_{10}(L_{bol}[erg~s^{-1}]) = 44.1 \pm 1.0$. We provide the total fluxes of our sample using aperture photometry for point-source objects and a 2D Gaussian fitting for objects with extended host galaxy emission, which was used to estimate the unresolved nuclear component. Most galaxies in our sample are pointlike sources; however, four sources (Centaurus A, Circinus, NGC 1068, and NGC 4388) show extended emission in all wavelengths. The 30–40 µm extended emission in NGC 4388 is coincident with the narrow-line region at PA ~50°, while the dusty extension at longer wavelengths arises from the host galaxy at PA ~90°. Our new observations allow us to construct the best-sampled parsec-scales (spectral energy distributions, SEDs) available between 30 and 500 µm for a sample of nearby AGN. We estimate that the average peak wavelength of the nuclear SEDs is ~40 µm in $νF_ν$, which we associate with an unresolved extended dusty region heated by the AGN.

*Unified Astronomy Thesaurus concepts: Active galaxies (17); Active galactic nuclei (16); Supermassive black holes (1663)*

## 1. Introduction

There is clear evidence that a considerable amount of dust in the vicinity of supermassive black holes (SMBHs) in active

galaxies obscures the central engine (i.e., accretion disk and SMBH) in some lines of sight. Through spectropolarimetric observations of NGC 1068, R. R. J. Antonucci & J. S. Miller (1985) showed that its optical polarized spectrum contained broad optical polarized emission lines not originally observed by direct total intensity observations. It was subsequently presumed that an optically and geometrically thick dusty structure (“torus”) blocked the central engine in some lines of

<figure><img src="image_3.png" /></figure>

Original content from this work may be used under the terms of the [Creative Commons Attribution 4.0 licence](https://creativecommons.org/licenses/by/4.0/). Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
sight (R. Antonucci 1993; C. M. Urry & P. Padovani 1995). Under this unified scheme, a Type 1 active galactic nucleus (AGN) is seen face-on and shows broadened optical lines, while in Type 2 AGN, the broadened lines are obscured. This model also predicts that broad silicate features at 10 and 18 µm will be seen in emission in Type 1 and in absorption in Type 2. However, silicate emission can be seen in emission in some Type 2 AGN, while absorption can be seen in some Type 1 (e.g., E. Hatziminaoglou et al. 2015). This and other observational features are explained by the inhomogeneous nature of the torus. Clumpy torus models (M. Nenkova et al. 2008a, 2008b) predict shallower silicate features, more similar infrared spectral energy distributions (SEDs) between Type 1 and Type 2 AGN, etc. (see C. Almeida Ramos & C. Ricci 2017 for a review).

A region of narrow forbidden line emission extends above and below the midplane of the dusty torus structure out to several kiloparsec scales. Recent subarcsecond interferometric imaging observations have shown a dust component at parsec scales spatially with the base of the narrow-line region (NLR; S. F. Hönig et al. 2012; L. Burtscher et al. 2013; N. López-Gonzaga et al. 2014, 2016; K. R. W. Tristram et al. 2014; V. Gámez Rosas et al. 2022; J. W. Isbell et al. 2022). This dusty structure is interpreted as part of a dusty wind launched from the inner hot part of the torus driven by radiation pressure at parsec scales (S. F. Hönig 2019), but generated by a magnetohydrodynamical wind at subparsec scales (e.g., R. T. Emmering et al. 1992; E. Lopez-Rodriguez et al. 2015; S. Takasao et al. 2022; E. Lopez-Rodriguez et al. 2023). This extended dusty structure has been resolved in a nearby galaxy, ESO 418-G14, using mid-infrared (MIR) images with JWST/MIRI finding that the dust is primarily heated by the AGN and/or radiative jet-induced shocks in the NLR rather than a wind (H. Haidar et al. 2024).

Atacama Large Millimeter/submillimeter Array (ALMA) observations provide observational support for a dusty torus +outflow scenario. Emission from the nucleus of NGC 1068 was mapped with a resolution of ~4 pc, resolving a 7–10 pc diameter disk interpreted as the submillimeter counterpart of the torus (S. García-Burillo et al. 2016). Rotation of the compact emission was detected in HCN $J=3-2$ and HCO+$J=3-2$ (M. Imanishi et al. 2018; D. D. Nguyen & K. Wada 2020). A molecular outflowing wind spatially with the dusty and molecular torus was also observed (S. García-Burillo et al. 2019). A. Alonso-Herrero et al. (2018) interpreted the measured nuclear (10–20 pc) CO(2–1) emission in NGC 5643 as a nuclear molecular gas component of the torus that is likely collimating the ionization cone. Conditions favorable for launching a cold and molecular wind likely depend on Eddington ratio and nuclear hydrogen column densities (e.g., M. Venanzi et al. 2020; A. Alonso-Herrero et al. 2021; S. García-Burillo et al. 2021; I. García-Bernete et al. 2022a).

This parsec-scale dusty component is possibly associated with larger scale MIR emission detected out to hundreds of parsec scales. In the case of Circinus, high angular resolution MIR imaging, optical polarimetry, and integral field spectra, coupled with state-of-the-art radiative transfer simulations, provide evidence that extended dust emission from parsec to tens of parsec scales in this object is a result of a hollow dusty cone illuminated by a tilted accretion disk (M. Stalevski et al. 2017, 2019; D. Kakkad et al. 2023; M. Stalevski et al. 2023). MIR extended emission out to 1" (~75 pc) was clearly detected

in NGC 1068 by J. J. Bock et al. (2000). Later, 10.8 and 18.2 µm emission extending 3"/5 (~200 pc) across NGC 4151 was also attributed to dust in the NLR heated by the central engine (J. T. Radomski et al. 2003). Likewise, at similar wavelengths, extended emission in 18 AGN at distances out to hundreds of parsecs was detected (D. Asmus et al. 2016; I. García-Bernete et al. 2016; D. Asmus 2019). Using the 37.1 µm filter on SOFIA/FORCAST and thanks to the increase in angular resolution compared with Spitzer, extended dust emission in Mrk 3, NGC 4151, and NGC 4388 was found on approximately hundreds of parsec scales (L. Fuller et al. 2019) coincident with the NLR and radio axis. This emission may be due to dust along the wall of ionization cones (R. E. Mason et al. 2009) or a dusty NLR (R. Mor et al. 2009; R. Mor & H. Netzer 2012).

In this article, we present an imaging atlas of 22 local ($D=4–181$ Mpc; median 42.8 Mpc) AGN obtained using the FORCAST and HAWC+ instruments on the 2.7 m SOFIA telescope in the wavelength range of 20–214 µm. Most of these data sets are unpublished or dispersed throughout the literature. We provide an MIR to far-IR (FIR) imaging atlas at angular scales of ~3"–20". At these scales, contribution from several dust sources is expected and we expect to disentangle the emission sources in a future study. Instead, here we aim to determine whether these objects are extended or not, and at what wavelengths within the resolution of the SOFIA telescope. We also explore the wavelength of turnover in the SED. This atlas is complementary to JWST observations up to ~25 µm and archival Herschel data (70–500 µm).

This article is organized as follows. Section 2 describes the observations and AGN sample definition; Section 3 shows the new IR images; Section 4 contains details of the imaging analysis; and Section 5 shows the resulting SEDs; we present results about the data in Section 6.

## 2. AGN Sample and Observation Data

### 2.1. Sample Selection

This imaging atlas was drawn from the ongoing AGN survey performed by the Galactic Activity, Torus, and Outflow Survey (GATOS; A. Alonso-Herrero et al. 2021; S. García-Burillo et al. 2021; I. García-Bernete et al. 2024). GATOS<fnref n="28" /> aims to characterize the dynamics and composition of the dusty and molecular torus and multi-phase outflows in AGN. The GATOS parent sample is selected from the 70 month Swift Burst Alert Telescope AGN catalog, which is flux limited in the ultrahard 14–195 keV X-ray band (W. H. Baumgartner et al. 2013).

In the initial study of AGN using SOFIA observations (L. Fuller et al. 2016), sources from the GATOS survey were selected based on the criteria that the galaxies had been previously studied using CLUMPY (M. Nenkova et al. 2008a, 2008b) torus models and were well sampled in the 1–18 µm regime (A. Alonso-Herrero et al. 2011; C. Ramos Almeida et al. 2009, 2011). The study of the 11 objects included the 31.5 µm photometry in the SEDs and found that including the 31.5 µm photometry reduces the number of CLUMPY torus models that are compatible with the data and modifies the model output for the torus outer radius. L. Fuller et al. (2019) further extended the wavelength range of a subset of seven

<footnote n="28">²⁸ GATOS website: https://gatos.myportfolio.com/.</footnote>
<table><caption>**Table 1**
SOFIA AGN Sample</caption><thead><tr><th>Object</th><th>Type</th><th>z</th><th>Dist. (Mpc)</th><th>Scale (pc arcsec<sup>-1</sup>)</th><th>logL<sub>bol</sub> (erg s<sup>-1</sup>)</th><th>References</th></tr></thead><tbody><tr><td>Centaurus A</td><td>RLSy2</td><td>0.0018</td><td>3.8</td><td>17</td><td>44.0</td><td>(1)</td></tr><tr><td>Circinus</td><td>Sy2</td><td>0.0014</td><td>4.2</td><td>19</td><td>43.6</td><td>(2)</td></tr><tr><td>MCG-5-23-16</td><td>Sy2</td><td>0.0085</td><td>36.4</td><td>177</td><td>44.4</td><td>(3)</td></tr><tr><td>Mrk 3</td><td>Sy2</td><td>0.0135</td><td>57.9</td><td>280</td><td>45.1</td><td>(4)</td></tr><tr><td>Mrk 231</td><td>ULIRG/Sy1</td><td>0.0422</td><td>181</td><td>877</td><td>45.9</td><td>(5)</td></tr><tr><td>Mrk 573</td><td>Sy2</td><td>0.0172</td><td>73.7</td><td>357</td><td>44.4</td><td>(2)</td></tr><tr><td>NGC 1068</td><td>Sy2</td><td>0.0038</td><td>16.3</td><td>79</td><td>45.0</td><td>(6)</td></tr><tr><td>NGC 1275</td><td>RG/Sy1.5</td><td>0.0176</td><td>75.4</td><td>366</td><td>44.8</td><td>(7)</td></tr><tr><td>NGC 2110</td><td>Sy2</td><td>0.0076</td><td>32.6</td><td>158</td><td>43.9</td><td>(2)</td></tr><tr><td>NGC 2273</td><td>Sy2</td><td>0.0061</td><td>26.1</td><td>127</td><td>43.9</td><td>(2)</td></tr><tr><td>NGC 2992</td><td>Sy1.9</td><td>0.0077</td><td>33.0</td><td>160</td><td>43.5</td><td>(8)</td></tr><tr><td>NGC 3081</td><td>Sy2</td><td>0.0080</td><td>34.2</td><td>166</td><td>44.2</td><td>(2)</td></tr><tr><td>NGC 3227</td><td>Sy1.5</td><td>0.0038</td><td>16.3</td><td>79</td><td>43.3</td><td>(9)</td></tr><tr><td>NGC 3281</td><td>Sy2</td><td>0.0107</td><td>45.9</td><td>222</td><td>43.8</td><td>(2)</td></tr><tr><td>NGC 4151</td><td>Sy1.5</td><td>0.0033</td><td>14.1</td><td>69</td><td>43.9</td><td>(6)</td></tr><tr><td>NGC 4258</td><td>Sy2</td><td>0.0015</td><td>6.4</td><td>31</td><td>42.0</td><td>(10)</td></tr><tr><td>NGC 4388</td><td>Sy2</td><td>0.0047</td><td>20.1</td><td>98</td><td>44.7</td><td>(4)</td></tr><tr><td>NGC 4941</td><td>Sy2</td><td>0.0037</td><td>15.9</td><td>77</td><td>42.2</td><td>(11)</td></tr><tr><td>NGC 5506</td><td>Sy1.9</td><td>0.0062</td><td>26.6</td><td>129</td><td>44.3</td><td>(11)</td></tr><tr><td>NGC 7465</td><td>Sy2/LINER</td><td>0.0066</td><td>28.1</td><td>136</td><td>43.4</td><td>(11)</td></tr><tr><td>NGC 7469</td><td>Sy1</td><td>0.0163</td><td>69.9</td><td>339</td><td>44.6</td><td>(9)</td></tr><tr><td>NGC 7674</td><td>Sy2</td><td>0.0290</td><td>124.3</td><td>603</td><td>45.5</td><td>(2)</td></tr></tbody></table>

**Note.** Redshifts and spectral types were taken from NED. Distances to most sources were obtained using $H_0 = 70$ km s$^{-1}$ Mpc$^{-1}$. Distances to nearby sources Centaurus A and Circinus were taken from G. L. H. Harris et al. (2010) and R. B. Tully et al. (2009), respectively.

**References.** References for log L<sub>bol</sub>: (1) A. Borkar et al. (2021); (2) A. Marinucci et al. (2012); (3) A. Alonso-Herrero et al. (2011); (4) K. Ichikawa et al. (2017); (5) K. M. Leighly et al. (2014); (6) A. Marconi et al. (2004); (7) W. H. Baumgartner et al. (2013); (8) I. Garcia-Bernete et al. (2015); (9) C. Ramos Almeida et al. (2011); (10) F. Yuan et al. (2002); (11) F. Duras et al. (2020).

AGN SEDs to 37.1 µm. They subsequently found extended emission in the point-spread function (PSF)-subtracted images of Mrk 3, NGC 4151, and NGC 4388 that is coincident with the radio axis and NLR. In a separate study, E. Lopez-Rodriguez et al. (2018) modeled the torus of NGC 1068 using ~20–53 µm FORCAST and HAWC+ observations. They showed that the peak wavelength range of emission from the torus is ~30–40 µm with a characteristic temperature 70–100 K. The use of observations >30 µm in that study from SOFIA and ALMA highlights the importance of longer wavelength observations to put constraints on MIR emission sources. Based on these results, we extend the wavelength range in objects previously observed, and also expand the number of AGN observed.

We present the complete imaging atlas of 22 Seyferts observed by SOFIA in the wavelength range of 19.7–214 µm using FORCAST and HAWC+. The final set of observations presented here was part of a multi-year AGN survey over several observing SOFIA cycles (Proposal IDs: 02_0035, 04_0048, 06_0066, 08_0014; PI: Lopez-Rodriguez; 70_0400 PI: Herter). The SOFIA atlas of AGN in the FIR is a flux-limited sample of nearby, bright, and well-studied AGN. All objects have a point source flux of >200 mJy at 31.5 µm, which ensures that each band can be observed within 1 hr of on-source time with a signal-to-noise ratio (SNR) >10 using FORCAST/SOFIA. Although the original AGN sample is larger than that presented here, only 22 AGN were observed in total by SOFIA before the end of operations in 2022. Note that there are gaps in the 20–214 µm wavelength range due to the fact that SOFIA only flies with a single instrument per night. For each SOFIA cycle, we prioritized the objects with

observations acquired in a single instrument from the previous cycle.

The sample properties are given in Table 1. For most objects, we retrieved redshift data from the NASA Extragalactic Database (NED). However, for nearby objects Centaurus A and Circinus, distances were obtained individually (G. L. H. Harris et al. 2010; R. B. Tully et al. 2009). The 22 objects in this atlas cover the luminosity range of log<sub>10</sub>(L<sub>bol</sub>[erg s<sup>-1</sup>]) = [42, 46] with a median of log<sub>10</sub>(L<sub>bol</sub>[erg s<sup>-1</sup>]) = 44.1 ± 1.0, and a distance of 4–181 Mpc with a median of 42.8 Mpc. Figure 1 shows bolometric luminosity plotted against distance, where Seyfert 1 objects are shown as filled red triangles and Seyfert 2 objects are shown as filled purple stars.

## 2.2. SOFIA Observations and Data Reduction

### 2.2.1. FORCAST

FORCAST is an IR camera and spectrograph sensitive in the wavelength range of 5–40 µm with a field of view (FOV) of 3.4 × 3.2 and pixel scale 0.768 pixel$^{-1}$. With one exception (NGC 1068 in the 19.7 µm filter), we only used the Long Wavelength Camera (25–40 µm) due to the abundance of ground-based images at shorter wavelengths for the objects in our sample. FORCAST observations were made in dual-channel mode using the two-position chop-nod method with symmetric nod-match-chop to remove telescope thermal emission and time variable sky background, and to reduce the effect of 1/f noise from the array. Data were reduced by the SOFIA Science Center using the FORCAST_REDX pipeline following the methods described by T. L. Herter et al. (2012). Most of the pipeline changes over the cycles were to refine the
<figure><img src="image_4.png" /><figcaption>**Figure 1.** Luminosity plotted against the distance of the 22 AGN in the atlas. Filled red triangles represent Sy1 and filled purple stars represent Sy2.</figcaption></figure>

spectroscopic mode of FORCAST with little or no change to the image mode presented here.

Observations were flux calibrated using the set of standard stars of the observing run, which provides flux uncertainties of ~10%. The PSF of the 31.5 µm observations from Cycle 2 (see L. Fuller et al. 2016) was the co-average of a set of standard stars from that cycle. Its FWHM was 3.40, in agreement with the SOFIA Observer's Handbook v3.0.0. The PSFs for Cycle 4 in the 30–40 µm wavelength range were determined by using standard star observations from the individual flights (see 2019) and averaged at FWHM ~ 4.33 and 4.58 in the 31.5 and 37.1 µm filters, respectively. The FORCAST PSFs for the observations of NGC 1068 are detailed in E. Lopez-Rodriguez et al. (2018).

### 2.2.2. HAWC+

HAWC+ is an FIR imaging polarimeter designed to allow total and polarized intensity imaging observations in four broad bands centered at 53, 89, 155, and 214 µm, corresponding to bands A, C, D, and E, respectively (see Table 2). On-the-fly mapping observing modes were used for both imaging polarimetry and total intensity imaging. Observing modes for the individual observations are given in Table 3. Data taken in polarization mode was reduced using the HAWC_DPR PIPE-LINE and the reduction steps presented in E. Lopez-Rodriguez et al. (2022). The Comprehensive Reduction Utility for SHARC II (CRUSH; A. Kovács et al. 2006; A. Kovács 2008) was used to obtain the total intensity observations. HAWC+ observations were reduced following the same reduction steps. We quote the pipeline versions or CRUSH versions in Table 3 to differentiate between the observing modes. There are no differences between CRUSH versions to obtain the total intensity images as all the changes in the pipeline were done for the polarimetric mode. Table 3 also shows the pixel scale of each image.

As in FORCAST observations, the source of uncertainty in the photometry for HAWC+ results from calibration factors of the standard stars associated with the observation, giving an uncertainty of ~10% (E. Lopez-Rodriguez et al. 2022). HAWC+ PSFs were estimated using standard star observations in 2017. Pallas was observed in bands A and C on 2017 November 7, while Neptune was observed in bands D and E on 2017 October 19. The FWHM of these standards are 5.25,

<table><caption>**Table 2**
HAWC+ Filter Suite</caption><thead><tr><th>Filter</th><th>λ<sub>central</sub><br>(μm)</th><th>Δλ<br>(μm)</th><th>FWHM<br>(arcsec)</th></tr></thead><tbody><tr><td>Band A</td><td>53</td><td>8.7</td><td>4.85</td></tr><tr><td>Band C</td><td>89</td><td>17</td><td>7.8</td></tr><tr><td>Band D</td><td>154</td><td>34</td><td>13.6</td></tr><tr><td>Band E</td><td>214</td><td>44</td><td>18.2</td></tr></tbody></table>

8.26, 14.74, and 19.65 in bands A, C, D, and E, respectively. The FWHMs from the Observer's Handbook<fnref n="29" /> are given in Table 2.

### 2.3. Observing Data

Table 3 provides the final AGN sample with information about the wavelength, observing mode, observation and mission details, versions of the separate pipelines, and also the FOV of the individual images.

## 3. Images

Images of the 22 AGN in the 19.7–214 µm wavelength range are presented in Figures 2, 3, 4, and 5. The orange scale on the bottom left of the images indicates a scale of 500 pc. The beam size is depicted in white in the top right of the images. In all images, north is up and east is to the left. Complementary Herschel 70–500 µm images are shown in Appendix A (Figures 10, 11) and Appendix C (Figures 12, 13). These fully reduced images were obtained through the Herschel Science Archive.<fnref n="30" /> All objects are presented and analyzed individually.

**Centaurus A.** The host galaxy of Centaurus A is clearly visible in the 53 µm image with a bright compact center. However, the host galaxy becomes more dominant in the 89 µm image (see a detailed analysis of host galaxy dust emission at 89 µm in E. Lopez-Rodriguez 2021). The kiloparsec-scale warped dust and gas lane was first observed with Spitzer imaging using IRAC and MIPS (A. C. Quillen et al. 2006). On subarcsecond scales, J. T. Radomski et al. (2008) observed the nucleus of Centaurus A using the 8.8, 10.4, and 18.3 µm filters on T-ReCS at Gemini South. They concluded that the most likely sources of nuclear MIR emission are an unresolved clumpy dusty torus in the core, and a dusty NLR for the arcsecond-scale extended emission (see also I. Garcia-Bernete et al. 2016).

**Circinus Galaxy.** HAWC+ 53 and 89 µm images of the Circinus Galaxy show a very bright FIR core with extended emission at a PA ~ 30°, whereas the 215 µm image shows a slightly different PA ~ 55°. We estimate the FWHM of the extended FIR nuclear emission to be ~6" × 6", 13.5 × 11.5, and 22.3 × 25.6 at 53, 89, and 214 µm, respectively. These are larger than the PSF FWHMs given in Section 2.2.2, which indicates extended emission along the axis of the inner bar of the galaxy. MIR emission was resolved at 8.7 and 18.3 µm out to 2" in an approximate east-west direction, coincident with the ionization cones at PA ~ 100° (C. Packham et al. 2005; M. Stalevski et al. 2017). However, the elongation seen in the SOFIA images (and in Herschel images in Appendix A) seems to be arising from dust in the host galaxy.

<footnote n="29">²⁹ https://irsa.ipac.caltech.edu/data/SOFIA/docs/sites/default/files/Other/Documents/OH-Cycle7.pdf</footnote>

<footnote n="30">³⁰ The Herschel archive can be found at http://herschel.esac.esa.int/Science_Archive.shtml.</footnote>
<table><caption>Table 3
Observation Data</caption><thead><tr><th>Object<br>(1)</th><th>Wavelength<br>(μm)<br>(2)</th><th>Instrument<br>(3)</th><th>Date<br>YYYY-MM-DD<br>(4)</th><th>Observing Mode<br>(5)</th><th>Pipeline/CRUSH Version<br>(6)</th><th>On-source Time<br>(s)<br>(7)</th><th>Altitude<br>(feet)<br>(8)</th><th>Mission ID<br>(9)</th><th>Program ID<br>(10)</th><th>Image FOV<br>(arcsec²)<br>(11)</th><th>Pixel Scale<br>(arcsec)<br>(12)</th></tr></thead><tbody><tr><td rowspan="2">Centaurus A</td><td>53</td><td>HAWC+</td><td>2019-07-17</td><td>Polarization</td><td>2.3.2</td><td>428</td><td>39,022</td><td>HA_F597</td><td>07_0032</td><td>75" × 75"</td><td>1.29</td></tr><tr><td>89</td><td>HAWC+</td><td>2019-07-17</td><td>Polarization</td><td>2.3.2</td><td>856</td><td>39,020</td><td>HA_F597</td><td>07_0032</td><td>130" × 130"</td><td>2.02</td></tr><tr><td rowspan="3">Circinus</td><td>53</td><td>HAWC+</td><td>2019-07-16</td><td>Polarization</td><td>2.3.2</td><td>107</td><td>42,014</td><td>HA_F596</td><td>07_0032</td><td>70" × 70"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2019-07-16</td><td>Polarization</td><td>2.3.2</td><td>856</td><td>40,994</td><td>HA_F596</td><td>07_0032</td><td>105" × 105"</td><td>2.00</td></tr><tr><td>215</td><td>HAWC+</td><td>2019-07-16</td><td>Polarization</td><td>2.3.2</td><td>281</td><td>43,011</td><td>HA_F596</td><td>07_0032</td><td>140" × 140"</td><td>4.72</td></tr><tr><td rowspan="4">MCG-5-23-16</td><td>31.5</td><td>FORCAST</td><td>2014-05-03</td><td>Imaging</td><td>1.0.1Beta</td><td>324</td><td>38,076</td><td>FO_F167</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2018-07-04</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>39,996</td><td>HA_F480</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2018-07-04</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>40,003</td><td>HA_F480</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td>155</td><td>HAWC+</td><td>2018-07-04</td><td>Total intensity</td><td>CSH 2.41-3</td><td>642</td><td>39,991</td><td>HA_F480</td><td>06_0066</td><td>90" × 90"</td><td>2.75</td></tr><tr><td rowspan="4">Mrk 3</td><td>31.5</td><td>FORCAST</td><td>2016-09-27</td><td>Imaging</td><td>1.1.3</td><td>35</td><td>42,994</td><td>FO_F133</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2016-09-27</td><td>Imaging</td><td>1.1.3</td><td>43</td><td>43,002</td><td>FO_F133</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2018-09-21</td><td>Total intensity</td><td>CSH 2.41-3</td><td>1926</td><td>43,002</td><td>HA_F508</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2019-02-13</td><td>Total intensity</td><td>CSH 2.41-3</td><td>1277</td><td>43,015</td><td>HA_F546</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td rowspan="2">Mrk 231</td><td>89</td><td>HAWC+</td><td>2019-09-18</td><td>Polarization</td><td>2.3.2</td><td>749</td><td>40,010</td><td>HA_F611</td><td>07_0032</td><td>75" × 75"</td><td>2.00</td></tr><tr><td>31.5</td><td>FOR</td><td>2015-02-05</td><td>Imaging</td><td>1.0.3</td><td>384</td><td>40,008</td><td>FO_F192</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="2">Mrk 573</td><td>37.1</td><td>FOR</td><td>2018-09-08</td><td>Imaging</td><td>1.3.2</td><td>31</td><td>43,006</td><td>FO_F502</td><td>06_0066</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>19.7</td><td>HAWC+</td><td>2016-09-17</td><td>Imaging</td><td>1.1.3</td><td>427</td><td>42,980</td><td>FO_F329</td><td>70_0400</td><td>30" × 30"</td><td>0.77</td></tr><tr><td rowspan="2">NGC 1068</td><td>31.5</td><td>HAWC+</td><td>2016-09-17</td><td>Imaging</td><td>1.1.3</td><td>471</td><td>42,980</td><td>FO_F329</td><td>70_0400</td><td>40" × 40"</td><td>0.77</td></tr><tr><td>37.1</td><td>HAWC+</td><td>2016-09-17</td><td>Imaging</td><td>1.1.3</td><td>343</td><td>42,980</td><td>FO_F329</td><td>70_0400</td><td>40" × 40"</td><td>0.77</td></tr><tr><td rowspan="2">Mrk 231</td><td>53</td><td>HAWC+</td><td>2016-12-08</td><td>Total intensity</td><td>CSH 2.41-3</td><td>455</td><td>40,012</td><td>HA_F356</td><td>70_0409</td><td>60" × 60"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2017-10-20</td><td>Polarization</td><td>2.7.0</td><td>1364</td><td>40,018</td><td>HA_F443</td><td>08_0012</td><td>10" × 60"</td><td>4.02</td></tr><tr><td rowspan="2">NGC 1275</td><td>31.5</td><td>FORCAST</td><td>2016-09-21</td><td>Imaging</td><td>1.1.3</td><td>48</td><td>41,103</td><td>FO_F274</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2016-09-21</td><td>Imaging</td><td>1.1.3</td><td>56</td><td>41,094</td><td>FO_F274</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="2">NGC 2110</td><td>89</td><td>HAWC+</td><td>2019-09-05</td><td>Polarization</td><td>2.3.2</td><td>7680</td><td>40,021</td><td>HA_F606</td><td>07_0032</td><td>50" × 50"</td><td>1.55</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2015-02-05</td><td>Imaging</td><td>1.0.3</td><td>768</td><td>38,001</td><td>FO_F192</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="5">NGC 2273</td><td>53</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>642</td><td>42,984</td><td>HA_F512</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>320</td><td>42,945</td><td>HA_F512</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td>155</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>320</td><td>42,955</td><td>HA_F512</td><td>06_0066</td><td>90" × 90"</td><td>2.75</td></tr><tr><td>215</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>320</td><td>42,945</td><td>HA_F512</td><td>06_0066</td><td>90" × 90"</td><td>3.70</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2016-09-27</td><td>Imaging</td><td>1.1.3</td><td>34</td><td>42,998</td><td>FO_F333</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="5">NGC 2992</td><td>37.1</td><td>FORCAST</td><td>2016-09-27</td><td>Imaging</td><td>1.1.3</td><td>41</td><td>42,996</td><td>FO_F333</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>428</td><td>38,987</td><td>HA_F512</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>534</td><td>38,949</td><td>HA_F512</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td>155</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>38,956</td><td>HA_F512</td><td>06_0066</td><td>90" × 90"</td><td>2.75</td></tr><tr><td>215</td><td>HAWC+</td><td>2018-09-28</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>38,960</td><td>HA_F512</td><td>06_0066</td><td>90" × 90"</td><td>3.70</td></tr><tr><td rowspan="2">NGC 3081</td><td>31.5</td><td>FORCAST</td><td>2014-05-02</td><td>Imaging</td><td>1.0.1Beta</td><td>232</td><td>39,026</td><td>FO_F166</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2014-05-02</td><td>Imaging</td><td>1.0.1Beta</td><td>480</td><td>39,021</td><td>FO_F166</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="2">NGC 3227</td><td>37.1</td><td>FORCAST</td><td>2016-02-17</td><td>Imaging</td><td>1.0.1Beta</td><td>63</td><td>43,004</td><td>FO_F278</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2014-05-06</td><td>Imaging</td><td>1.0.1Beta</td><td>152</td><td>37,990</td><td>FO_F168</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="2">NGC 3281</td><td>37.1</td><td>FORCAST</td><td>2016-02-17</td><td>Imaging</td><td>1.1.0</td><td>35</td><td>43,002</td><td>FO_F278</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2014-05-02</td><td>Imaging</td><td>1.0.1Beta</td><td>300</td><td>39,033</td><td>FO_F166</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="2">NGC 2992</td><td>53</td><td>HAWC+</td><td>2018-07-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>37,036</td><td>HA_F485</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2018-07-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>320</td><td>37,025</td><td>HA_F485</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td rowspan="2">NGC 3081</td><td>155</td><td>HAWC+</td><td>2018-07-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>320</td><td>37,043</td><td>HA_F485</td><td>06_0066</td><td>90" × 90"</td><td>2.75</td></tr><tr><td>215</td><td>HAWC+</td><td>2018-07-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>534</td><td>37,049</td><td>HA_F485</td><td>06_0066</td><td>90" × 90"</td><td>3.70</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>Object<br>(1)</th><th>Wavelength<br>(μm)<br>(2)</th><th>Instrument<br>(3)</th><th>Date<br>YYYY-MM-DD<br>(4)</th><th>Observing Mode<br>(5)</th><th>Pipeline/CRUSH Version<br>(6)</th><th>On-source Time<br>(s)<br>(7)</th><th>Altitude<br>(feet)<br>(8)</th><th>Mission ID<br>(9)</th><th>Program ID<br>(10)</th><th>Image FOV<br>(arcsec<sup>2</sup>)<br>(11)</th><th>Pixel Scale<br>(arcsec)<br>(12)</th></tr></thead><tbody><tr><td rowspan="5">NGC 4151</td><td>31.5</td><td>FORCAST</td><td>2014-05-08</td><td>Imaging</td><td>1.0.1Beta</td><td>153</td><td>40,042</td><td>FO_F170</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2016-02-17</td><td>Imaging</td><td>1.0.1Beta</td><td>41</td><td>36,996</td><td>FO_F278</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2019-02-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>1069</td><td>39,777</td><td>HA_F545</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2019-02-12</td><td>Polarization</td><td>2.3.2</td><td>891</td><td>40,034</td><td>HA_F545</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2016-02-17</td><td>Imaging</td><td>1.1.0</td><td>156</td><td>39,002</td><td>FO_F278</td><td>04_0048</td><td>30" × 30"</td><td>0.77</td></tr><tr><td rowspan="5">NGC 4258</td><td>37.1</td><td>FORCAST</td><td>2016-02-17</td><td>Imaging</td><td>1.1.0</td><td>446</td><td>38,999</td><td>FO_F278</td><td>04_0048</td><td>30" × 30"</td><td>0.77</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2014-05-02</td><td>Imaging</td><td>1.0.1Beta</td><td>162</td><td>37,982</td><td>HA_F545</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2016-02-06</td><td>Imaging</td><td>1.1.0</td><td>63</td><td>42,372</td><td>FO_F274</td><td>04_0048</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2019-02-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>932</td><td>42,045</td><td>HA_F545</td><td>06_0066</td><td>50" × 50"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2019-02-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>534</td><td>42,035</td><td>HA_F545</td><td>06_0066</td><td>75" × 75"</td><td>1.55</td></tr><tr><td rowspan="5">NGC 4388</td><td>155</td><td>HAWC+</td><td>2019-02-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>321</td><td>42,021</td><td>HA_F545</td><td>06_0066</td><td>90" × 90"</td><td>2.00</td></tr><tr><td>215</td><td>HAWC+</td><td>2019-02-12</td><td>Total intensity</td><td>CSH 2.41-3</td><td>213</td><td>42,037</td><td>HA_F545</td><td>06_0066</td><td>90" × 90"</td><td>3.70</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2021-04-09</td><td>Imaging</td><td>2.2.1</td><td>154</td><td>38,992</td><td>FO_F715</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2021-04-09</td><td>Imaging</td><td>2.2.1</td><td>313</td><td>38,986</td><td>FO_F715</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2014-05-02</td><td>Imaging</td><td>1.0.1Beta</td><td>261</td><td>37,982</td><td>FO_F166</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td rowspan="5">NGC 4941</td><td>37.1</td><td>FORCAST</td><td>2021-06-30</td><td>Imaging</td><td>2.3.0</td><td>427</td><td>39,005</td><td>FO_F752</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>89</td><td>HAWC+</td><td>2020-01-31</td><td>Polarization</td><td>2.3.2</td><td>779</td><td>43,009</td><td>HA_F657</td><td>07_0032</td><td>75" × 75"</td><td>1.55</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2022-09-17</td><td>Imaging</td><td>2.6.0</td><td>427</td><td>41,017</td><td>FO_F915</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2022-09-17</td><td>Imaging</td><td>2.6.0</td><td>222</td><td>41,009</td><td>FO_F915</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2021-09-14</td><td>Total intensity</td><td>CSH 2.42-1</td><td>641</td><td>38,008</td><td>HA_F783</td><td>08_0014</td><td>20" × 20"</td><td>1.00</td></tr><tr><td rowspan="5">NGC 5506</td><td>89</td><td>HAWC+</td><td>2021-09-14</td><td>Total intensity</td><td>CSH 2.42-1</td><td>426</td><td>39,004</td><td>HA_F783</td><td>08_0014</td><td>20" × 20"</td><td>1.55</td></tr><tr><td>31.5</td><td>FORCAST</td><td>2022-09-17</td><td>Imaging</td><td>1.0.1Beta</td><td>231</td><td>43,005</td><td>FO_F176</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>37.1</td><td>FORCAST</td><td>2022-09-17</td><td>Imaging</td><td>2.6.0</td><td>222</td><td>41,009</td><td>FO_F915</td><td>08_0014</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>53</td><td>HAWC+</td><td>2021-09-14</td><td>Total intensity</td><td>CSH 2.42-1</td><td>641</td><td>38,008</td><td>HA_F783</td><td>08_0014</td><td>20" × 20"</td><td>1.00</td></tr><tr><td>89</td><td>HAWC+</td><td>2021-09-14</td><td>Total intensity</td><td>CSH 2.42-1</td><td>426</td><td>39,004</td><td>HA_F783</td><td>08_0014</td><td>20" × 20"</td><td>1.55</td></tr><tr><td>NGC 7469</td><td>31.5</td><td>FORCAST</td><td>2014-06-04</td><td>Imaging</td><td>1.0.1Beta</td><td>165</td><td>43,005</td><td>FO_F176</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr><tr><td>NGC 7674</td><td>31.5</td><td>FORCAST</td><td>2014-06-04</td><td>Imaging</td><td>1.0.1Beta</td><td>165</td><td>43,005</td><td>FO_F176</td><td>02_0035</td><td>20" × 20"</td><td>0.77</td></tr></tbody></table>

Note. Column (1): object; column (2): wavelength; column (3): instrument; column (4): observation date; column (5): observing mode; column (6): pipeline/CRUSH version; column (7): on-source time; column (8): aircraft starting altitude; column (9): mission ID; column (10): program ID; column (11): FOV of images in Section 3; column (12): pixel scale.
<figure><img src="image_5.png" /><figcaption>**Figure 2.** FORCAST 31.5 and 37.1 µm images, and HAWC+ 53, 89, 155, and 215 µm images. Each image has a differing FOV, which can be found in Table 3. For bright objects (Centaurus A, Circinus, and Mrk 231), contours start at $3\sigma$, then follow log(maximum) from [−1.2 to 0.8], [−1.8 to 0.8], [−1.4, 0.8] in steps of 0.2. For MCG-5-23-16 and Mrk 3, the lowest contours are $3\sigma$ and increase in steps of $5\sigma$. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.</figcaption></figure>

MCG-5-23-16. MCG-5-23-16 appears as a pointlike source in the 31.5–155 µm wavelength range whose brightness decreases with increasing wavelength. However, this galaxy appears as an extended source in the MIR using high angular resolution data from the Very Large Telescope (VLT; I. García-Bernete et al. 2016). Likewise, P. Ferruit et al. (2000) found that this nucleus has an extended optical NLR at a PA of 40°. They found a dust lane extending 2" on either side of the nucleus, parallel to the axis of the galaxy. Their extended dusty emission at 40° was detected at a $3\sigma$ level up to ~4" from the core. This extended structure has no thermal emission counterpart within the 31.5–155 µm wavelength range.

Mrk 3. Although the FORCAST and HAWC+ images generally appear to be pointlike sources, L. Fuller et al. (2019) found extended emission in the PSF-subtracted 37.1 µm image of Mrk 3 in the direction of the radio axis (84°) (M. J. Kukula et al. 1993) and the NLR (~70°) (A. Capetti et al. 1995). D. Asmus et al.<fnref n="31" /> found an elongated nucleus out to ~170 pc with PA ~70° in the Si-5 (11.6 µm) filter using Gemini/

MICHELLE. However, the Si-2 (8.7 µm) image from GTC/Canaricam appears pointlike (A. Alonso-Herrero et al. 2016). The large-scale east-west structure in the 53 µm image here is a background artifact produced by the data reduction due to the small spatial coverage and short integration time of the observation.

Mrk 231. The 89 µm image shown here is pointlike with an FWHM of ~8.5, similar to the standard FWHM of 8"/26 (see Section 2.2.2). Mrk 231 is a Type 1 ultraluminous infrared galaxy and is the nearest known quasar at a distance of 181 Mpc. It is known for its multiphase and multiscale outflows (see D. S. N. Rupke & S. Veilleux 2011), with a neutral outflow up to 3 kpc in radius (D. S. Rupke et al. 2005).

Mrk 573. Although the SNR is very low ($3\sigma$–4$\sigma$), both 31.5 and 37.1 µm images of Mrk 573 show marginally resolved ~4.5" elongation in the east-west direction at PA ~110°. Mrk 573 was previously shown to have a biconical NLR coincident with radio emission 3"–4" from the nucleus at a PA ~125° (J. S. Ulvestad & A. S. Wilson 1984; R. W. Pogge & M. M. De Robertis 1995). The marginal detection here may be cold extended dust in the outer layers of the NLR.

<footnote n="31">³¹ http://dc.zah.uni-heidelberg.de/sasmirala/q/im/info</footnote>
<figure><img src="image_6.png" /><figcaption>**Figure 3.** FORCAST 31.5 and 37.1 µm images, and HAWC+ 53, 89, 155, and 215 µm images. Note that the wavelength range for NGC 1068 starts at 19.7 µm, so its range is shifted. Each image has a differing FOV, which can be found in Table 3. For NGC 1068 FORCAST images, contours begin at 3σ and follow log(maximum) from [−2.0, 0.8] in steps of 0.2, while the HAWC+ images follow the same steps but log (max) ranges [−1.6, 0.8]. For all other images, the lowest contours are 3σ and increase in steps of 5σ. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.</figcaption></figure>

NGC 1068. The 19–53 µm images of NGC 1068 were published previously in E. Lopez-Rodriguez et al. (2018), where it was shown that the peak emission from the torus occurs between 30 and 40 µm with a corresponding temperature of 70–100 K. The 89 µm image was published as a polarimetric observation (E. Lopez-Rodriguez et al. 2020). Within a scale of about 1 kpc, NGC 1068 shows extended emission in the northeast (NE) to southwest (SW) direction at a PA ~ 45°, similar to MIR observations using VISIR/VLT (D. Asmus et al. 2014). Their observations revealed a nuclear structure in the north–south direction and extended structures to the NE and SW. From the N-band spectrum, R. E. Mason et al. (2006) concluded that while torus emission dominates NIR wavelengths, large-scale MIR emission is dominated by diffuse dust within the ionization cones.

NGC 1275. All 30–53 µm images are dominated by a pointlike source. However, the 31.5 µm image (L. Fuller et al. 2019) shows 3σ extended emission along the PA ~ 140°. This AGN is known to have a network of Hα filaments extending out to ~100'' (see C. J. Conselice et al. 2001) and is possibly

the result of a merger (J. A. Holtzman et al. 1992). The MIR core shows silicate dust emission in both the 10 and 18 µm bands (see L. Fuller et al. 2019). Hence, both dust and gas are extended, covering several kiloparsecs around the core. In the HAWC+ 89 µm filter, E. Lopez-Rodriguez et al. (2023) found extended dust emission at a PA ~ 125° out to a 12 kpc radius potentially associated with a magnetized dusty filament along the NW direction (A. C. Fabian et al. 2008).

NGC 2110. The 30–215 µm images of NGC 2110 are all pointlike. The north–south pattern in the 53 µm image is due to background noise and does not represent extended dust. NGC 2110 is a Type 2 AGN that shows silicate emission at 10 and 18 µm that is interpreted as a result of a clumpy torus, or as dust within the ionization cones (PA ~ 160°) (J. S. Mulchaey et al. 1994) in the inner 32 pc of the AGN (R. E. Mason et al. 2009). This galaxy appears as an extended source in Gemini/MICHELLE high-resolution N-band observations (I. Garcia-Bernete et al. 2016). However, any structure within the NLR or ionization cones is not resolved by our observations.
<figure><img src="image_7.png" /><figcaption>**Figure 4.** FORCAST 31.5 and 37.1 µm images, and HAWC+ 53, 89, 155, and 215 µm images. Each image has a differing FOV, which can be found in Table 3. The lowest contours are 3σ and increase in steps of 5σ. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.</figcaption></figure>

NGC 2273. The full set of 30–215 µm images of NGC 2273 show a pointlike source. The north–south pattern in the 53 µm image is due to background noise and does not represent extended dust. Within the FWHM of these images (see Sections 2.2.1, 2.2.2), there is a known star-forming ring within ~2" of the nucleus (P. Ferruit et al. 2000; P. Martini et al. 2003; E. Sani et al. 2012). GTC/Canaricam observations (A. Alonso-Herrero et al. 2014, 2016) at 8.7 µm show elongation from the NE to the SW, likely with contribution from PAH. This structure is consistent with extension seen in the PSF-subtracted 37.1 µm SOFIA image (L. Fuller et al. 2019).

NGC 2992. The image of NGC 2992 in the 31.5 µm filter is published in L. Fuller et al. (2016) and appears as a pointlike

source. Subarcsecond N-band imaging (I. García-Bernete et al. 2015) reveals extended emission along PA ~30° out to ~3 kpc, which is attributed to dust heated by star formation based on corresponding N-band spectroscopy. The FWHM of the SOFIA image is ~3.5 × 3.5 (560 × 560 pc²) so the extension should be resolvable within the SOFIA image. Since we do not see the extension in the image here, we conclude that either the extended dust emission tapers at wavelengths >20 µm or SOFIA does not have enough sensitivity to detect it.

NGC 3081. The 31.5 µm image of NGC 3081 was published in L. Fuller et al. (2016), while the 37.1 µm image was published in L. Fuller et al. (2019). The nucleus is known to harbor a region of strong optical emission ~1" from the AGN (P. Ferruit et al. 2000) likely due to dust or gas heated by the
<figure><img src="image_8.png" /><figcaption>**Figure 5.** FORCAST 31.5 and 37.1 µm images, and HAWC+ 53, 89, 155, and 215 µm images. Each image has a differing FOV, which can be found in Table 3. The white transparent circle on the top right indicates the telescope beam size. The orange bar on the bottom left of the images is scaled to 500 pc. For all images, north is up and east is to the left.</figcaption></figure>

AGN. L. Fuller et al. (2019) estimated that ~35% of the MIR emission within the central few arcseconds (few hundred parsecs) of the AGN originates in the NLR. High angular resolution N- and Q-band observations show extension toward the north, extending out to ~450 pc from the southeast to the NW (PA ~ 160°) (I. García-Bernete et al. 2016). On larger scales, optical and NIR observations reveal a series of star-forming resonance rings at distances of 2.3, 11.0, 26.9 kpc, and 33.1 kpc (R. Buta 1990, 1998; R. J. Buta et al. 2004). At longer wavelengths (>200 µm), C. Ramos Almeida et al. (2011) concluded that FIR emission is contaminated by the star-forming ring 2.3 kpc in diameter.

NGC 3227. The 31.5 µm image was published in L. Fuller et al. (2016), while the 37.1 µm image was published in

L. Fuller et al. (2019). These images show a pointlike source, although NGC 3227 is known to harbor a nuclear star-forming region (E. Schinnerer et al. 2001; R. I. Davies et al. 2006) with a nuclear cluster within ~70 pc (~1") from the core. The 8.7 µm image from A. Alonso-Herrero et al. (2016) shows a slight north-south elongation and the corresponding spectrum shows clear PAH in the nucleus (see also I. García-Bernete et al. 2016). These star-forming regions likely contaminate the nuclear MIR emission within the FWHM of our images.

NGC 3281. While the 31.5 m FORCAST image is published in L. Fuller et al. (2016), the HAWC+ images at 53, 89, 154, and 214 µm are presented here for the first time and appear pointlike in all filters. The images taken at 53 and 89 µm appear to have significant noise in their backgrounds. The
subarcsecond (0.35) N-band spectrum in O. González-Martín et al. (2013) shows a deep 10 µm silicate absorption feature, which originates in the inner ~80 pc of the AGN.

**NGC 4151.** The SOFIA images of NGC 4151 appear as a pointlike source, with a potential detection of extended emission at PA ~120° at a $3\sigma$ level at 37.1 µm. L. Fuller et al. (2019) confirmed this elongation in the PSF-subtracted 37.1 µm image coincident with the NLR and radio axes. J. T. Radomski et al. (2003) show extended emission in 10.8 and 18.2 µm images that coincides with the NLR axis at PA ~-60°. For $\ge$37.1 µm, we conclude that any extended emission due to NLR dust is within the FWHM of the SOFIA instruments.

**NGC 4258.** NGC 4258 was not detected but we include the data here since it is part of the sample. It has been observed and analyzed in the N band with Gemini/MICHELLE by R. E. Mason et al. (2012). These authors found a compact nucleus that is marginally resolved at 10 µm (FWHM ~0.5).

**NGC 4388.** NGC 4388 is an edge-on spiral that shows the most interesting MIR to FIR morphology in this study. Notably, in the 30–40 µm FORCAST images of NGC 4388, extension can be seen in the NE to SW direction at PA ~40° (see also L. Fuller et al. 2019), coincident with the NLR. This emission is seen on smaller scales at shorter wavelengths (D. Asmus et al. 2016; I. García-Bernete et al. 2016). The 53 µm image decreases in intensity and does not show a strong central core of emission as in the 31.5–37.1 wavelength range. However, at longer wavelengths (89–214 µm), host galaxy emission clearly dominates the images in the east-west direction at PA ~ 90°.

**NGC 4941.** NGC 4941 is a low-luminosity AGN that appears here as a faint pointlike source in the 31.5 and 37.1 µm images, but brighter at 53 and 89 µm. Subarcsecond resolution N-band imaging on VLT/VISIR (D. Asmus et al. 2011) showed no significant extended MIR sources outside of the nucleus.

**NGC 5506.** NGC 5506 appears as a bright point source in both the 31.5 and 37.1 µm filters. While the nucleus is unresolved, extended MIR emission has been detected up to a few arcseconds to the NE at 11.9 µm (D. Raban et al. 2008). Extended emission in the north-south direction was detected in the N band out to ~560 pc, while faint extended emission toward the east in the Q band was also detected (I. García-Bernete et al. 2016). However, the PSF-subtracted 12.27 µm $2'' \times 2''$ VLT/VISIR image of A. Alonso-Herrero et al. (2021) show that the PA of extended emission varies from 30° in the central ~0.5 to nearly 90° in the outer regions.

**NGC 7465.** The 31.5 µm FORCAST image appears faint with a $3\sigma$ upper-limit in the 37.1 µm image. The 53 and 89 µm HAWC+ images here appear increasingly brighter, albeit as pointlike sources. Cold molecular gas observations (L. M. Young et al. 2021) reveal that NGC 7465 is quite gas-rich, possibly from a recent merger.

**NGC 7469.** NGC 7469 appears as a very bright source in the 31.5 µm image with FWHM ~4.3. After PSF subtraction, L. Fuller et al. (2016) found extended emission in the north-south direction. This AGN is known to have a circumnuclear ring of star formation at a radius of ~480 pc (~1.4) (C. Ramos Almeida et al. 2011) in 8.7 and 18.3 µm images taken on Gemini/T-ReCS. Recent JWST observations reveal prominent PAH emission, indicative of star formation, in the circumnuclear ring (I. García-Bernete et al. 2022b; L. Zhang & L. C. Ho 2023).

**NGC 7674.** The previously published (L. Fuller et al. 2016) FORCAST 31.5 µm image appears as a pointlike source. D. Asmus et al.<fnref n="32" /> found that the nucleus of NGC 7674 is extended at PA ~ 125° at subarcsecond-scale resolution, where the extension roughly aligns with the ionization cone.

# 4. Nuclear Flux Extraction

We aim to construct well-sampled MIR to FIR SEDs of the nuclear emission of AGN at scales of several arcseconds, depending on the PSF of the observation and possible extended emission. On these scales, we expect multiple dust sources (i.e., torus, star-forming regions, dusty outflow); however, disentangling these sources is beyond the scope of this imaging atlas. Because the images span a range of observing cycles, instruments, and observing modes, we analyzed each image individually. Of our sample, 17 objects appear visually as point sources. For these sources, we performed aperture photometry where the aperture size was set to be $2 \times$ the FWHM at a given band. For objects that show host galaxy emission, we extract the central PSF to construct the SEDs as described below. We complement our SOFIA data with Herschel imaging data (see Appendix A) and use a similar analysis method to construct the full IR SEDs.

## 4.1. Extended Sources: 2D Gaussian Fitting

For sources with extended dust emission, we performed a two-component simultaneous fit to accurately model both the central source based on the PSF, and the host galaxy whose fit assumes an elongated 2D Gaussian profile. In order to supplement the SOFIA data for the full MIR to FIR SEDs, we used a similar methodology with Herschel images.

For the SOFIA images, the PSF used was based on the standard stars of the observing runs for each cycle as explained in Section 2.2. However, the same analysis could not be performed on Herschel images due to the threefold lobes associated with the instrument PSFs. To accommodate this, we compared three different PSF models to reproduce and fit the central source. Two of the PSFs were point source images, while the third was an approximation of the theoretical instrumental PSF using a Gaussian profile. The fitting routine used four free parameters for the Gaussian profile: (1, 2) the position in x and y of the PSF center according to the image center, (3) the amplitude of the PSF, (4) the fourth parameter was dependent on the PSF type used. For archival PSFs, this parameter represents the rotation angle that needs to be applied to the PSF to match the orientation of the image. For the Gaussian PSFs, this fourth parameter represents a scaling factor to the width of the Gaussian compared to its ideal value for a perfect instrument ($1.22 \times \lambda/D$).

The galaxy background is defined by seven parameters: (1, 2) the 2D Gaussian's center position ($x_0$ and $y_0$), (3, 4) its width ($\sigma_x$ and $\sigma_y$) in both directions, (5) its amplitude, and (6) its orientation on the image ($\theta$). To these six parameters, we added a constant background as a seventh free parameter. We combined these components and fit this simulated intensity map to the observed map using the 11 total free parameters (four from the PSF and seven from the 2D Gaussian). We thus derived the parameters describing the best central source for our intensity maps, and then studied the properties extracted for

<footnote n="32">³² http://dc.zah.uni-heidelberg.de/sasmirala/q/im/info</footnote>
<figure><img src="image_9.png" /><figcaption>Figure 6. PSF-subtracted images of host galaxy backgrounds</figcaption></figure>

the central source and removed it from the initial map to study the host galaxy itself. An example of this procedure is given in Appendix C (Figure 14).

## 4.2. AGN and Host Galaxy Contribution

While most SOFIA images were treated as point sources, Centaurus A, Circinus, NGC 1068, and NGC 4388 all had significant host galaxy contamination that needed to be subtracted from at least some of the images. Figure 6 shows the PSF-subtracted images of these sources and Table 4 gives the percentage of the contribution of the PSF to the total flux of the object. In several other objects, the shorter wavelength (~30–100 µm) images did not show host galaxy contamination, but longer wavelength Herschel images show the colder extended dust. Because this is an atlas of SOFIA images, we include objects with host galaxy contamination only in Herschel images in Appendix C for completeness (see Figure 15).

The 53 µm image of Centaurus A contains (<5%) emission from extended sources, so we performed aperture photometry to account for the central emission. At wavelengths $\gtrsim$70 µm, the host galaxy substantially (~56%–70%) contributes to the central AGN emission, so the extended emission was subtracted. The PSF of Centaurus A at these wavelengths contributes ~35%. This can be interpreted as the nucleus having a relatively constant IR contribution, so the brightness of the nucleus coincides with the IR brightness of the host galaxy.

The PSF contribution of the Circinus Galaxy decreases between 53 and 160 µm from 58% to 35%. At longer FIR wavelengths, the contribution of the PSF appears to be from the host galaxy and the fitting no longer provides information about the AGN. We interpret this as a decreasing IR contribution from the nucleus compared to the extended emission.

For the completeness of the SOFIA Atlas presented here, we used the 19–53 µm images of NGC 1068 from E. Lopez-Rodriguez et al. (2018). These data sets were

analyzed as described in that study and here we only present the results and images in that wavelength range. The study showed that the fractional contribution from star formation increases from 20 to 50 µm, while extended emission from 200 K dust decreases. Emission from the torus peaks in this range, a result which is in agreement with L. Fuller et al. (2016), who found that the turnover in torus emission occurs at wavelengths $>31.5$ µm. Extended emission is observed here at all wavelengths $\gtrsim$70 µm arising from dust in the host galaxy and star formation regions.

For NGC 4388, we show the results of PSF subtraction at all wavelengths, but only use the results in wavelengths $>40$ µm for the SED. In the 30–40 µm range, the NE to SW extension is clear in the PSF-subtracted images. However, almost all of the extended emission lies within the FWHM of the observation; the FWHM of these images is only ~10% greater than the FWHM of the PSF. Thus, while we show the PSF-subtracted images of NGC 4388 here, for the SED, we use the total 30–40 µm fluxes, which encompass the apparent extended emission due to the NLR. The change in the extended emission source and morphology between 40 and 70 µm is clear in the PSF-subtracted images (Figure 6). The host galaxy clearly dominates the extended emission in the FIR, while the NLR region dominates the extended emission in MIR wavelengths. The 53 µm HAWC+ image appears to show the transition between dominant extended sources. The contribution of the PSF in the images of NGC 4388 is ~60% in the 30–40 µm range, where the extended emission is in the NE to SW direction. The contribution then decreases drastically to ~20%. This reflects the turnover in extended emission seen in the images in Figure 5. The contribution of the PSF returns to ~70% between 70 and 100 µm, which suggests two separate but significant IR emission sources.

# 5. SEDs

Tables 5 (SOFIA) and 6 (Herschel) give the nuclear fluxes of the AGN in our sample along with their associated errors in units of jansky. The sources of uncertainty here are the
<table><caption>**Table 4**
Contribution of the PSF to the Host Galaxy Extended Emission</caption><thead><tr><th rowspan="3">Object</th><th colspan="12">Wavelength (μm)</th></tr><tr><th>19.7</th><th>31.5</th><th>37.1</th><th>53</th><th>70</th><th>89</th><th>100</th><th>155</th><th>160</th><th>215</th><th>250</th><th>350</th><th>500</th></tr><tr><th colspan="12">Unresolved Emission Contribution (%)</th></tr></thead><tbody><tr><td>Centaurus A</td><td>...</td><td>...</td><td>...</td><td>...</td><td>30 ± 1</td><td>34 ± 1</td><td>...</td><td>...</td><td>31 ± 1</td><td>...</td><td>36 ± 2</td><td>37 ± 2</td><td>44 ± 2</td></tr><tr><td>Circinus</td><td>...</td><td>...</td><td>...</td><td>58 ± 0.2</td><td>48 ± 1</td><td>35 ± 0.3</td><td>40 ± 1</td><td>...</td><td>33 ± 1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>NGC 1068</td><td>36 ± 4</td><td>49 ± 5</td><td>51 ± 8</td><td>33 ± 15</td><td>56 ± 2</td><td>...</td><td>...</td><td>...</td><td>13 ± 2</td><td>...</td><td>13 ± 1</td><td>35 ± 1</td><td>54 ± 1</td></tr><tr><td>NGC 4388</td><td>...</td><td>62 ± 16</td><td>56 ± 12</td><td>19 ± 2</td><td>64 ± 1</td><td>71 ± 2</td><td>...</td><td>47 ± 2</td><td>29 ± 1</td><td>38 ± 3</td><td>31 ± 4</td><td>38 ± 6</td><td>44 ± 5</td></tr></tbody></table>
<table><caption>**Table 5**
Nuclear Fluxes for SOFIA/FORCAST and HAWC+ Images</caption><thead><tr><th rowspan="2">Object</th><th colspan="6">Wavelength (μm)</th><th rowspan="2">References</th></tr><tr><th>31.5</th><th>37.1</th><th>53<br>Flux (Jy)</th><th>89</th><th>155</th><th>215</th></tr></thead><tbody><tr><td>Centaurus A</td><td>...</td><td>...</td><td>10.7 ± 1.1</td><td>18.2 ± 2.1</td><td>...</td><td>...</td><td>(This work)</td></tr><tr><td>Circinus</td><td>...</td><td>...</td><td>85.8 ± 8.7</td><td>84.7 ± 8.52</td><td>...</td><td>51.5 ± 5.2</td><td>(This work)</td></tr><tr><td>MCG-5-23-16</td><td>1.8 ± 0.2</td><td>...</td><td>1.7 ± 0.2</td><td>0.7 ± 0.1</td><td>0.5 ± 0.1</td><td>...</td><td>(1, this work)</td></tr><tr><td>Mrk 3</td><td>2.9 ± 0.3</td><td>3.0 ± 0.3</td><td>3.1 ± 0.4</td><td>2.7 ± 0.3</td><td>2.1 ± 0.2</td><td>...</td><td>(2, this work)</td></tr><tr><td>Mrk 231</td><td>...</td><td>...</td><td>...</td><td>22.9 ± 2.3</td><td>...</td><td>...</td><td>(This work)</td></tr><tr><td>Mrk 573</td><td>0.7 ± 0.1</td><td>0.8 ± 0.1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(2, this work)</td></tr><tr><td>NGC 1068<sup>a</sup></td><td>28.8 ± 1.8</td><td>29.7 ± 2.5</td><td>23.8 ± 4.8</td><td>...</td><td>...</td><td>...</td><td>(3, 4)</td></tr><tr><td>NGC 1275</td><td>4.0 ± 0.4</td><td>5.0 ± 0.8</td><td>...</td><td>5.3 ± 0.2</td><td>...</td><td>...</td><td>(2, this work)</td></tr><tr><td>NGC 2110</td><td>1.3 ± 0.2</td><td>...</td><td>3.7 ± 0.5</td><td>4.4 ± 0.5</td><td>4.5 ± 0.5</td><td>2.2 ± 0.2</td><td>(1, this work)</td></tr><tr><td>NGC 2273</td><td>1.9 ± 0.2</td><td>2.7 ± 0.3</td><td>4.3 ± 0.5</td><td>6.5 ± 0.7</td><td>5.4 ± 0.6</td><td>3.8 ± 0.4</td><td>(1, this work)</td></tr><tr><td>NGC 2992</td><td>0.9 ± 0.1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(1)</td></tr><tr><td>NGC 3081</td><td>1.0 ± 0.1</td><td>1.4 ± 0.2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(1, 2)</td></tr><tr><td>NGC 3227</td><td>2.3 ± 0.3</td><td>2.8 ± 0.3</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(1, 2)</td></tr><tr><td>NGC 3281</td><td>2.7 ± 0.3</td><td>...</td><td>5.3 ± 0.6</td><td>6.4 ± 0.7</td><td>4.6 ± 0.5</td><td>2.5 ± 0.3</td><td>(1, this work)</td></tr><tr><td>NGC 4151</td><td>3.9 ± 0.4</td><td>4.5 ± 0.3</td><td>4.9 ± 0.5</td><td>4.1 ± 0.4</td><td>...</td><td>...</td><td>(1, this work)</td></tr><tr><td>NGC 4258</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(This work)</td></tr><tr><td>NGC 4388</td><td>3.0 ± 0.4</td><td>3.2 ± 0.3</td><td>0.7 ± 0.1</td><td>3.3 ± 0.4</td><td>3.4 ± 0.4</td><td>2.7 ± 0.3</td><td>(1, 2, this work)</td></tr><tr><td>NGC 4941</td><td>0.29 ± 0.04</td><td>0.5 ± 0.1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(This work)</td></tr><tr><td>NGC 5506</td><td>4.1 ± 0.5</td><td>5.2 ± 0.5</td><td>...</td><td>7.0 ± 0.2</td><td>...</td><td>...</td><td>(1, this work, 5)</td></tr><tr><td>NGC 7465</td><td>...</td><td>...</td><td>1.8 ± 0.2</td><td>4.9 ± 0.5</td><td>...</td><td>...</td><td>(This work)</td></tr><tr><td>NGC 7469</td><td>9.4 ± 1.1</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(1)</td></tr><tr><td>NGC 7674</td><td>1.8 ± 0.2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>(1)</td></tr></tbody></table>

**Note.**

a E. Lopez-Rodriguez et al. (2018) measured the flux of NGC 1068 at 19.7 µm to be 22.0 ± 1.4.

**References.** (1) L. Fuller et al. (2016); (2) (2019); (3) E. Lopez-Rodriguez et al. (2018); (4) E. Lopez-Rodriguez et al. (2020); (5) E. Lopez-Rodriguez et al. (2022).

<table><caption>**Table 6**
Nuclear Fluxes for Herschel/PACS and SPIRE Images</caption><thead><tr><th rowspan="2">Object</th><th colspan="6">Wavelength (μm)</th></tr><tr><th>70</th><th>100</th><th>160<br>Flux (Jy)</th><th>250</th><th>350</th><th>500</th></tr></thead><tbody><tr><td>Centaurus A</td><td>15.6 ± 1.0</td><td>...</td><td>19.9 ± 2.0</td><td>9.9 ± 1.0</td><td>6.9 ± 0.5</td><td>5.8 ± 0.4</td></tr><tr><td>Circinus</td><td>99.0 ± 5.3</td><td>63.5 ± 3.3</td><td>47.2 ± 2.4</td><td>20.1 ± 1.1</td><td>18.9 ± 1.2</td><td>6.5 ± 0.4</td></tr><tr><td>MCG-5-23-16</td><td>1.1 ± 0.1</td><td>...</td><td>0.34 ± 0.05</td><td>0.11 ± 0.02</td><td>0.05 ± 0.01</td><td>0.02 ± 0.005</td></tr><tr><td>Mrk 3</td><td>2.9 ± 0.2</td><td>2.6 ± 0.1</td><td>1.9 ± 0.1</td><td>0.9 ± 0.1</td><td>0.6 ± 0.1</td><td>0.34 ± 0.09</td></tr><tr><td>Mrk 231</td><td>31.2 ± 1.6</td><td>26.4 ± 1.4</td><td>13.9 ± 0.7</td><td>5.2 ± 0.3</td><td>1.8 ± 0.1</td><td>0.49 ± 0.03</td></tr><tr><td>Mrk 573</td><td>1.02 ± 0.05</td><td>1.05 ± 0.61</td><td>0.94 ± 0.06</td><td>0.44 ± 0.03</td><td>0.23 ± 0.02</td><td>0.08 ± 0.02</td></tr><tr><td>NGC 1068</td><td>101.7 ± 2.2</td><td>...</td><td>142.2 ± 0.5</td><td>69.7 ± 0.5</td><td>27.4 ± 0.4</td><td>8.8 ± 0.3</td></tr><tr><td>NGC 1275</td><td>6.8 ± 0.4</td><td>6.7 ± 0.4</td><td>5.5 ± 0.3</td><td>3.2 ± 0.2</td><td>2.7 ± 0.2</td><td>2.4 ± 0.1</td></tr><tr><td>NGC 2110</td><td>4.3 ± 0.2</td><td>5.0 ± 0.3</td><td>4.2 ± 0.2</td><td>1.7 ± 0.1</td><td>0.57 ± 0.09</td><td>0.20 ± 0.05</td></tr><tr><td>NGC 2273</td><td>5.2 ± 0.3</td><td>6.0 ± 0.3</td><td>5.8 ± 0.3</td><td>2.3 ± 0.1</td><td>0.93 ± 0.06</td><td>0.19 ± 0.02</td></tr><tr><td>NGC 2992</td><td>2.4 ± 0.1</td><td>3.3 ± 0.2</td><td>3.5 ± 0.2</td><td>1.9 ± 0.1</td><td>0.74 ± 0.04</td><td>0.54 ± 0.04</td></tr><tr><td>NGC 3081</td><td>1.9 ± 0.1</td><td>2.1 ± 0.1</td><td>1.6 ± 0.1</td><td>0.67 ± 0.04</td><td>0.24 ± 0.02</td><td>0.11 ± 0.02</td></tr><tr><td>NGC 3227</td><td>6.3 ± 0.3</td><td>8.3 ± 0.4</td><td>4.8 ± 0.3</td><td>2.1 ± 0.1</td><td>0.68 ± 0.04</td><td>0.16 ± 0.01</td></tr><tr><td>NGC 3281</td><td>6.4 ± 0.3</td><td>6.3 ± 0.3</td><td>4.5 ± 0.2</td><td>1.3 ± 0.1</td><td>0.38 ± 0.03</td><td>0.25 ± 0.03</td></tr><tr><td>NGC 4151</td><td>4.4 ± 0.2</td><td>3.1 ± 0.2</td><td>1.5 ± 0.1</td><td>0.40 ± 0.02</td><td>0.06 ± 0.005</td><td>0.0007 ± 7e-5</td></tr><tr><td>NGC 4258</td><td>1.1 ± 0.2</td><td>4.1 ± 0.3</td><td>4.7 ± 0.5</td><td>3.3 ± 0.3</td><td>2.5 ± 0.3</td><td>0.9 ± 0.1</td></tr><tr><td>NGC 4388</td><td>2.9 ± 0.2</td><td>...</td><td>3.5 ± 0.2</td><td>1.1 ± 0.1</td><td>0.91 ± 0.08</td><td>0.49 ± 0.04</td></tr><tr><td>NGC 4941</td><td>0.80 ± 0.04</td><td>...</td><td>0.70 ± 0.08</td><td>0.12 ± 0.01</td><td>0.015 ± 0.001</td><td>0.05 ± 0.006</td></tr><tr><td>NGC 5506</td><td>6.8 ± 0.4</td><td>6.4 ± 0.3</td><td>3.9 ± 0.2</td><td>1.2 ± 0.1</td><td>0.53 ± 0.03</td><td>0.26 ± 0.03</td></tr><tr><td>NGC 7465</td><td>3.6 ± 0.2</td><td>4.9 ± 0.3</td><td>4.1 ± 0.2</td><td>1.8 ± 0.1</td><td>0.89 ± 0.07</td><td>0.42 ± 0.04</td></tr><tr><td>NGC 7469</td><td>22.8 ± 1.2</td><td>25.9 ± 1.3</td><td>18.3 ± 0.9</td><td>7.5 ± 0.4</td><td>2.9 ± 0.2</td><td>0.79 ± 0.05</td></tr><tr><td>NGC 7674</td><td>3.9 ± 0.2</td><td>4.5 ± 0.2</td><td>4.9 ± 0.3</td><td>2.7 ± 0.2</td><td>1.2 ± 0.1</td><td>0.44 ± 0.04</td></tr></tbody></table>
<figure><img src="image_10.png" /><figcaption>**Figure 7.** MIR to FIR SEDs of the several arcsecond-scale nuclear fluxes in our sample of AGN. Filled pink diamonds represent SOFIA observations, while black dots represent complementary Herschel observations. The solid black lines correspond to Spitzer spectra.</figcaption></figure>

instrument calibration, sky background, and the 2D Gaussian fitting, where applicable. We estimate FORCAST and HAWC + errors at ~10%. We use PACS instrument errors at 5%<fnref n="33" /> and SPIRE instrument errors as 5.5%.<fnref n="34" /> The uncertainty due to sky background is determined on an individual basis, but averages ~5%. The average uncertainty due to the 2D Gaussian fitting is ~1.5%. We add these uncertainties in quadrature for the error bar estimation.

The nuclear SEDs are shown in Figure 7 in $\nu F_\nu$. The filled pink diamonds represent SOFIA observations, while the filled black circles represent the complementary Herschel data. We obtained Spitzer/IRS spectra from the Spitzer/CASSIS database (V. Lebouteiller et al. 2011) for 21 of the 22 objects in our sample (solid black line). There was no spectrum available for NGC 7465. Low-resolution spectra ($R \sim 100$) were obtained for 18 of the objects, while moderate-resolution spectra ($R \sim 600$) were available for Circinus, NGC 1068, and NGC 7674. This data set provides the most completed SED coverage available between 30 and 500 µm. Decomposing the SEDs in this sample is outside the scope of this article, as we are presenting an imaging atlas. Here, we provide the main results and features of the SEDs of these objects.

The morphological changes seen in the extended emission source in Figure 5 for NGC 4388 are reflected in the SED at 53 µm, where there is a marked decline in the SED. The drastic decrease seems to be due to the change in dominant emitting sources. The extended emission at wavelengths $\lesssim 40$ µm is due to dust in the direction of the radio axis, and the extended emission at wavelengths $\gtrsim 50$ µm is due to the host galaxy.

The wavelength of peak emission can give insight into the primary processes that drive MIR emission. The peak wavelength, determined by the highest flux from photometry and spectroscopy, ranges from 18 to 100 µm in $\nu F_\nu$, with an average of ~40 µm. This average only includes the peak in continuum values and does not take into account fine structure lines. Most (73%; 11 out of 15) Seyfert 2 have a peak emission at wavelengths $\lesssim 40$ µm. The SEDs of MCG-5-23-16, Mrk 3, Mrk 573, NGC 1068, NGC 3081, and NGC 4151 peak at ~18–20 µm. This is in agreement with the correlation peak between the hard X-rays and the MIR for Type 1 AGN in I. García-Bernete et al. (2017). The peak wavelengths in the $F_\nu$ (Jy) range of ~20–160 µm, with an average of ~93 µm. NGC 1068 is the only AGN to peak at the same wavelength in both sets of units.

The Spitzer spectrum for NGC 1068 does not align with the SOFIA photometry because of the extensive PSF subtraction that we performed in the photometry that was not accounted for in the spectroscopy. This is the only object that not only has

<footnote n="33">³³ PACS: https://www.cosmos.esa.int/web/herschel/pacs-overview.</footnote>

<footnote n="34">³⁴ SPIRE: https://www.cosmos.esa.int/web/herschel/spire-overview.</footnote>
<figure><img src="image_11.png" /><figcaption>**Figure 8.** Bolometric luminosity vs. the peak wavelength of the SED for both Sy1 (filled red triangles) and Sy2 (filled purple stars).</figcaption></figure>

overlapping 20–40 µm Spitzer and SOFIA data, but also that has had the background emission subtracted at these wavelengths.

## 5.1. Luminosity and Peak Wavelength

To test whether the peak wavelength is a function of luminosity, we plot $L_{bol}$ versus $\lambda_{peak}$. Figure 8 shows the bolometric luminosities of the AGN plotted against the peak wavelength in the SEDs for both Sy1s, shown as filled red triangles, and Sy2s, shown as filled purple stars. The correlation coefficient between the luminosity and peak wavelength is $|R| \sim 0.63$ with statistical significance $p = 0.0015$. While it is argued that $|R|$ of 0.6–0.7 may show moderate to strong correlation (see Section 3.2 in S. J. Messenger et al. 2013), a $p$-value $\le 0.05$ is generally accepted as statistically significant. The data suggests that higher luminosity objects have SEDs that peak at shorter wavelengths, which indicates the presence of a hot dust component in the vicinity of the AGN.

## 5.2. MIR to FIR Colors

The ratio of $F_{\nu}(70)/F_{\nu}(160)$ has been used as a proxy for dust temperature (M. Meléndez et al. 2014; J. García-González et al. 2016), where the ratio is higher for dust heated by the AGN and lower for dust heated by star formation. Here, we perform this analysis using the ratio $F_{\nu}(31)/F_{\nu}(70)$ by using the 31.5 µm SOFIA data in our atlas. For objects that do not have data in the 31.5 µm filter, we supplement that with data from the Spitzer/IRS continuum. NGC 7465 did not have 31.5 µm flux data, nor did it have Spitzer data so we leave that object out of this analysis. Using the fluxes in Table 5, we plot a color–color diagram in $F_{\nu}$ in Figure 9. This figure also visually shows the peak wavelength from the SEDs (in $\nu F_{\nu}$). Longer peak wavelengths tend to cluster at $F_{\nu}(70)/F_{\nu}(160) \sim 1$ and $F_{\nu}(31)/F_{\nu}(70)$ between 0.25 and 0.5.

In this sample, we find an average $F_{\nu}(70)/F_{\nu}(160)$ ratio of $1.4 \pm 0.7$. Previous studies (M. Meléndez et al. 2014; J. García-González et al. 2016) with larger sample sizes (313 and 33, respectively) have found an average ratio of $\sim 0.8$, albeit the data was analyzed using independent methods. This suggests a higher amount of AGN-heated dust in our sample.

<figure><img src="image_12.png" /><figcaption>**Figure 9.** Color diagram of 21 of the 22 AGN in our sample. Sy1s are represented by filled triangles, while Sy2 are filled stars. The scale on the right shows peak wavelength by color.</figcaption></figure>

We find that 18 objects have $F_{\nu}(31)/F_{\nu}(70) < 1$, with an average $F_{\nu}(31)/F_{\nu}(70)$ of $0.6 \pm 0.3$. The only object with both $F_{\nu}(70)/F_{\nu}(160)$ and $F_{\nu}(31)/F_{\nu}(70) > 1$ is MCG-5-23-16, and an SED that peaks $\sim 20$ µm. This object may be the most AGN-dominated source in our sample. The other objects that show a peak at $\sim 20$ µm in $\nu F_{\nu}$ still show $F_{\nu}(31)/F_{\nu}(70) < 1$. Only one object, NGC 4388, shows $F_{\nu}(31)/F_{\nu}(70) > 1$ while $F_{\nu}(70)/F_{\nu}(160) < 1$. This reflects the change in extended emission seen in Figure 5.

Half (11) of the objects in the sample show ratios $F_{\nu}(31)/F_{\nu}(70) < 1$ while $F_{\nu}(70)/F_{\nu}(160) > 1$. These objects (Circinus, Mrk 231, Mrk 573, NGC 1275, NGC 2110, NGC 3081, NGC 3227, NGC 3281, NGC 4151, NGC 4941, NGC 5506, NGC 7469) are likely AGN dominated. Six objects show $F_{\nu}(31)/F_{\nu}(70) < 1$ and $F_{\nu}(70)/F_{\nu}(160) < 1$, meaning that their SEDs peak at longer wavelengths. The emission from these objects (Centaurus A, NGC 1068, NGC 2273, NGC 2992, NGC 4258, NGC 7674) are likely dominated by star formation.

# 6. Conclusions

We have presented a SOFIA atlas of nearby AGN in the 20–215 µm wavelength range using FORCAST and HAWC+. We have released 69 observations, of which 41 are newly published and 28 have been previously published (L. Fuller et al. 2016, 2019, E. Lopez-Rodriguez et al. 2018, 2023). From these observations, NGC 4388 shows the most dramatic visual change in emission morphology. The 30–40 µm images show an NE to SW dusty extension associated with the NLR, while the $>50$ µm images show an east to west dusty emission associated with the plane of the host galaxy. Our observations show that $<10''$ resolution 30–70 µm observations are crucial to disentangle the emitting contribution from AGN and the host galaxy.

We measured arcsecond-scale unresolved nuclear fluxes in order to construct SEDs of the objects in our sample. We included complementary Herschel data to cover up to 500 µm. For point sources, we used aperture photometry to determine the flux. For extended sources, we used a 2D Gaussian fitting method to extract the central unresolved source(s) of emission from the galaxy background. For this method, the PSF is scaled
to represent the central emission, while a 2D Gaussian
represents a host galaxy or background emission. Based on
the SEDs, we make the following conclusions:

1. There is a sharp drop in the SED of NGC 4388 that corresponds to the wavelength where the angle of extended emission transitions from NE–SW (NLR) to east–west (host galaxy).

2. The average peak of the SEDs is 40 µm in $νF_ν$, spanning a range of [20, 100] µm.

3. The peak wavelength of the SED appears to be a function of AGN luminosity, where higher luminosity objects peak at shorter wavelengths.

4. MCG-5-23-16 is the only object whose color diagram shows both $F_ν(31)/F_ν(70)$ and $F_ν(70)/F_ν(160) > 1$, which may indicate an AGN-dominated source.

5. Half of the objects in the sample have flux ratios, which suggests that the SED is dominated by AGN-heated dust, while six objects show ratios consistent with heating by SF.

6. In future studies, we will combine data from this atlas with incoming data from JWST to update our IR data sets with the latest and highest resolution data available. Newly obtained JWST/MIRI observations will provide new higher angular resolution data for some of the sources in the wavelength range of 5–28 µm.

Acknowledgments

We acknowledge Dr. Lucas Grosset for his effort in
subtracting the image backgrounds. E.L.-R. is supported by
the NASA/DLR Stratospheric Observatory for Infrared

Astronomy (SOFIA) under the 08_0012 Program. 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 50OK0901 to the University of Stuttgart. E.L.-R. is supported by the NASA Astrophysics Decadal Survey Precursor Science (ADSPS) Program (NNH22ZDA001N-ADSPS) with ID 22-ADSPS22-0009 and agreement number 80NSSC23K1585. I.G. B. acknowledges support from STFC through grants ST/S000488/1 and ST/W000903/1. C.R. acknowledges support from Fondecyt Regular grant 1230345 and ANID BASAL project FB210003. E.B. acknowledges support from the Spanish grants PID2022-138621NB-I00 and PID2021-123417OB-I00, funded by MCIN/AEI/10.13039/501100011033/FEDER, EU.

*Software:* Astropy (Astropy Collaboration et al. 2022; Astropy Collaboration 2018; Astropy Collaboration et al. 2013); SciPy.

**Appendix A**

Herschel Images

We used images from the Herschel Archive to supplement SOFIA data in FIR wavelengths. Images from the PACS and SPIRE instruments covering the wavelength range 70–500 µm are shown in this appendix (Figures 10–13). The white circle in the upper right indicates the beam size, while the pink scale in the bottom left indicates a distance of 1 kpc. To extract nuclear fluxes on scales of several arcseconds, we use the methods described in Section 4. For point sources, we performed aperture photometry. For extended sources, we used the 2D Gaussian routine outlined in Section 4.1.
<figure><img src="image_13.png" /><figcaption>**Figure 10.** Herschel PACS and SPIRE FIR images. The white circle in the top right indicates the beam size of the observation, while the pink line in the bottom left indicates a distance of 1 kpc.</figcaption></figure>
<figure><img src="image_14.png" /><figcaption>**Figure 11.** Herschel PACS and SPIRE FIR images. The white circle in the top right indicates the beam size of the observation, while the pink line in the bottom left indicates a distance of 1 kpc.</figcaption></figure>
<figure><img src="image_15.png" /><figcaption>**Figure 12.** Herschel PACS and SPIRE FIR images. The white circle in the top right indicates the beam size of the observation, while the pink line in the bottom left indicates a distance of 1 kpc.</figcaption></figure>
<figure><img src="image_16.png" /><figcaption>**Figure 13.** Herschel PACS and SPIRE FIR images. The white circle in the top right indicates the beam size of the observation, while the pink line in the bottom left indicates a distance of 1 kpc.</figcaption></figure>
## Appendix B
### Background Fitting

Figure 14 shows an example of the 2D Gaussian fitting we used to extract the central flux from the background of the host galaxy in wavelengths 30–500 µm. The object used here is NGC 4388. In the first column, the original observation image is shown. The second column shows a model of the image using a PSF (column 3) combined with the model background. Column 4 shows a PSF-subtracted image

(columns 1–3) used to make the model background (column 5). Column 6 shows the PSF- and background-subtracted images of the residuals.

## Appendix C
### Host Galaxy Backgrounds—Herschel

Figure 15 shows the results of PSF-subtracted images for objects in which only Herschel data showed host galaxy contamination.

<figure><img src="image_17.png" /><figcaption>Figure 14. Example of the 2D Gaussian fitting routine explained in Section 4.1.</figcaption></figure>
<figure><img src="image_18.png" /><figcaption>**Figure 15.** PSF-subtracted host galaxy images from archive Herschel data.</figcaption></figure>

ORCID iDs

Lindsay Fuller Ⓒ https://orcid.org/0000-0003-4809-6147

Enrique Lopez-Rodriguez Ⓒ https://orcid.org/0000-0001-5357-6538

Ismael García-Bernete Ⓒ https://orcid.org/0000-0002-9627-5281

Cristina Ramos Almeida Ⓒ https://orcid.org/0000-0001-8353-649X

Almudena Alonso-Herrero Ⓒ https://orcid.org/0000-0001-6794-2519

Chris Packham Ⓒ https://orcid.org/0000-0001-7827-5758

Lulu Zhang Ⓒ https://orcid.org/0000-0003-4937-9077

Mason Leist Ⓒ https://orcid.org/0000-0003-4975-2046

Nancy A. Levenson Ⓒ https://orcid.org/0000-0003-4209-639X

Masatoshi Imanishi Ⓒ https://orcid.org/0000-0001-6186-8792

Sebastian Hoenig Ⓒ https://orcid.org/0000-0002-6353-1111

Marko Stalevski Ⓒ https://orcid.org/0000-0001-5146-8330

Claudio Ricci Ⓒ https://orcid.org/0000-0001-5231-2645

Erin Hicks Ⓒ https://orcid.org/0000-0002-4457-5733

Enrica Bellocchi Ⓒ https://orcid.org/0000-0001-9791-4228

Françoise Combes Ⓒ https://orcid.org/0000-0003-2658-7893

Ric Davies Ⓒ https://orcid.org/0000-0003-4949-7217

Santiago García Burillo Ⓒ https://orcid.org/0000-0003-0444-6897

Omaira González Martín Ⓒ https://orcid.org/0000-0002-2356-8358

Takuma Izumi Ⓒ https://orcid.org/0000-0001-9452-0813

Alvaro Labiano Ⓒ https://orcid.org/0000-0002-0690-8824

Miguel Pereira Santaella Ⓒ https://orcid.org/0000-0002-4005-9619

Dimitra Rigopoulou Ⓒ https://orcid.org/0000-0001-6854-7545

David Rosario Ⓒ https://orcid.org/0000-0002-0001-3587

Taro Shimizu Ⓒ https://orcid.org/0000-0002-2125-4670
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