The obscured nucleus of NGC3256 S. I. Anisotropic AGN near-IR radiation field traced by CO v=1-0 with JWST/NIRSpec

abstract · abstract

The southern nucleus of NGC3256, a nearby luminous infrared (IR) interacting system (d=40 Mpc; L(IR)=10^11.6 Lsun), hosts a deeply obscured low-luminosity active galactic nucleus (AGN) associated with a massive and fast bipolar collimated molecular outflow. JWST/NIRSpec observations revealed bright spatially resolved ro-vibrational CO v=1-0 4.67um emission at the base of this molecular outflow extending out to ~300pc, which is excited by the ~4.7um IR radiation from the southern dusty core. Using Monte Carlo radiative transfer (MCRT) models, we analyzed the CO v=1-0 band emission to determine the intensity of the ~4.7um IR radiation field across the outflow base. We find that the core spectral luminosity density at ~4.7um, as seen by the material in the outflow base, is ~2-4 times higher than that inferred along our line of sight, indicating an anisotropic near-IR radiation field. Moreover, the slower than d^-2 decrease of the near-IR flux density across the outflow base suggests a collimated radiation field, for which we estimate a small half-opening angle (15-20deg) and a diameter of the collimating structure of 15 +- 5 pc. This is slightly smaller than the diameter of the obscuring envelope (25 +- 5 pc). Combined with the expansion of this obscuring envelope, traced by the blueshifted CO v=1-0 absorption toward the nucleus, this suggests that the AGN is beginning to clear its environment. We estimate N_H~10^22-23 cm^-2 for NGC 3256 S, which is similar to that of Type 2 AGN. However, in contrast to Type 2 AGN, a high covering factor of the obscuring material, possibly sustained by inflows linked to the galaxy merger, and similar to that expected in deeply obscured compact obscured nuclei (CONs), is needed to explain the absence of extended high-ionization emission. Therefore, NGC 3256 S shares properties with CONs and Type 2 AGN.

S3.SS2: 3.2 Best-fit parameters / block 1 · html

The results from this fit are shown in Figs. 3 and 6 and are summarized in Table 1 . The predicted and observed CO band fluxes for all regions agree very well (left panels of Figs. 3 and 6 ). The probability distributions obtained for T kin T_{\rm kin} and ⟨ N CO ⟩ / Δ ​ v \langle N_{\rm CO}\rangle/\penalty\Delta{\rm v} are also shown in the middle panels of Fig. 3 and 6 . T kin T_{\rm kin} follows the same trend as reported in 44 with decreasing temperatures, from 40 K to 20 K, for increasing nuclear distances between 70 and 300 pc (see Fig. 12 of 44 ) . No clear trend is observed for ⟨ N CO ⟩ / Δ ​ v \langle N_{\rm CO}\rangle/\penalty\Delta{\rm v} , which varies between 10 18.0 and 10 18.5 cm -2 /(km s -1 ), although the values in the southern regions are higher by ∼ \sim 0.3 dex. The obtained ⟨ N CO ⟩ / Δ ​ v \langle N_{\rm CO}\rangle/\penalty\Delta{\rm v} are consistent within the uncertainties with those estimated using the two-temperature model in 44 . n H 2 n_{\rm H_{2}} it not shown since it is not well constrained by these data and its distribution is almost flat.

S5: 5 Conclusions / block 1 · html

The southern nucleus of the interacting luminous IR system NGC 3256 ( d d =40 Mpc; L IR L_{\rm IR} =4 × \times 10 11 L ⊙ L_{\rm\odot} ) hosts a deeply obscured low-luminosity AGN ( L 2 − 10 ​ keV ∼ 10 40 L_{\rm 2-10\,keV}\sim 10^{40} erg s -1 ) and a massive bipolar collimated molecular outflow ( mass outflow rate > 50 >50 M ⊙ M_{\rm\odot} yr -1 ), oriented nearly in the plane of the sky (e.g., Sakamoto et al. 2014 ; Emonts et al. 2014 ; Ohyama et al. 2015 ). We used JWST/NIRSpec data to study the spatially resolved CO v v =1–0 4.67 μ \upmu m ro-vibrational band emission mostly detected along the base of the bipolar molecular outflow. We extended the analysis of this band presented in 44 by using MC RT models and a non-LTE treatment of the CO excitation. With this new models, we investigated the angular anisotropy of the near-IR radiation field produced by the obscured AGN core that excites the CO v v =1–0 band. The main results from this work are listed below.

S3: 3 Analysis and results / block 1 · html

The stellar disk of NGC 3256 S is seen almost edge-on from our line of sight, while the molecular outflow lies approximately in the plane of the sky (e.g., Sakamoto et al. 2014 ). This orientation is ideal for the study of the CO v v =1–0 emission at base of the outflow, since it limits the contribution of the disk to the spectra of the outflow (see Fig. 1 ). The CO v v =1–0 band is excited by the bright near-IR continuum emission produced by the warm dust ( T d ∼ 600 T_{\rm d}\sim 600 K; Ohyama et al. 2015 ) in the dust-embedded nucleus of NGC 3256 S. This near-IR continuum illuminates the molecular gas in the outflow base, exciting the v v =1 vibrational levels of the CO molecules, which subsequently decay through the observed v v =1–0 emission (see Fig. 6 of 44 ).

S3: 3 Analysis and results / block 1 · html

In 44 , we showed that the low- J J lines of the band (up to J lo ∼ J_{\rm lo}\sim 3–4) are optically thick. To model the observed intensities of all the lines of band, a detailed radiative transfer treatment is therefore required. To achieve this, we developed an MC RT model (Sect. 3.1 ) that is sensitive to the different optical depths of the lines in the band and can predict the expected luminosity of each line. We used the MC RT model predictions to fit the observed band emission and constrain the physical conditions of the outflowing gas and the near-IR radiation field (Sect. 3.2 ).

S3.SS1: 3.1 MC RT model for the CO v v =1–0 band / block 1 · html

From the MC RT models, we obtained the ratio, r i r_{i} , of the continuum power density integrated over a velocity bin, Δ ​ v ​ P ν \Delta{\rm v}P_{\nu} , and the line luminosity, r i = Δ ​ v ​ P ν / L line , i r_{i}=\Delta{\rm v}P_{\nu}/\penalty L_{{\rm line},i} . When this result is combined with Eqs. 1 and 3 , the near-IR flux density exciting the CO v v = 1–0 band is

S3.SS1: 3.1 MC RT model for the CO v v =1–0 band / block 1 · html

Figure 3: MC RT fitting results for each region. The name of the region is indicated in the top-left panel. Top left: Continuum-subtracted JWST/NIRSpec spectrum (solid black line). The red line is the best-fit CO v v =1–0 model plus the contribution from the other species, indicated as a solid green line (see Sect. 3.2 ). Bottom left; Observed fluxes of the CO v v =1–0 lines (black diamonds) as a function of the wavelength. The flux of the best-fit model is represented by the red circles and downward arrows for the upper limits. The dashed blue line shows the fitted optical depth for CO ice band at 4.67 μ \upmu m (right axis). Middle panels: Probability density distributions for log ⁡ T kin \log T_{\rm kin} (top panel in orange) and log ⁡ ⟨ N CO ⟩ / Δ ​ v \log\langle N_{\rm CO}\rangle/\penalty\Delta{\rm v} (bottom panel in black). The median value is indicated in the top right corner of the panel and shown with a vertical dotted line. Right panel: Hypothetical core flux derived from the MC RT model for each CO v v =1–0 line assuming that the core emission is isotropic (red circles). The dashed red line represents the scaled emission of blackbody at 400 K. For reference, the nuclear spectrum of NGC 3256 S measured with JWST/NIRSpec is shown in blue. The discrepancy between the observed nuclear flux (blue line) and that derived from the MC RT model (red points) suggests that the core does not emit isotropically (see Sect. 4.1 ).

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Anisotropic radiation field . Using a grid of non-LTE MC RT models, we successfully fitted the fluxes of all the ro-vibrational lines of the CO v v =1–0 band in 13 apertures ( r r =0 . ′′ \aas@@fstack{\prime\prime} 2; ∼ \sim 40 pc) where this band is detected in emission. From this fit, the ∼ \sim 4.7 μ \upmu m spectral luminosity density, L ν L_{\nu} , from the NGC 3256 S core, as seen by the material at the base of the bipolar outflow, is approximately two to four times higher than that inferred from the core spectrum along our line of sight. This indicates that the near-IR radiation field in this object is anisotropic.

S5: 5 Conclusions / block 1 · html

Collimated radiation field. In addition, the radiation field exciting the CO v v =1–0 band at the base of the outflow does not decrease with distance according to the expected d − 2 d^{-2} law. Instead, the observed intensity scaling can be explained if the radiation from the core is collimated into a relatively narrow solid angle. Assuming a collimated beam, with a half-opening angle α \alpha of 15–20 ∘ based on the extent of the bipolar molecular outflow base, we found that the diameter of the structure collimating the radiation is 15 ± \pm 5 pc. This is slightly smaller than but comparable to the diameter of the obscuring envelope ( ∼ \sim 25 ± \pm 5 pc). The estimated about three times higher L ν L_{\nu} at 4.7 μ \upmu m toward the outflow base indicates that it is either illuminated by dust hotter than that observed along our line of sight or that the intrinsic core emission is anisotropic at smaller scales.

S5: 5 Conclusions / block 1 · html

Expanding optically and geometrically thick envelope. To date, no high-ionization lines have been detected in NGC 3256 S, including in its mid-IR spectrum. This indicates that the AGN is surrounded by optically thick material even in the mid-IR ( N H N_{\rm H} >10 23 cm -2 ) with a high covering factor. The bipolar outflow and the increased IR radiation field along the outflow direction suggest that the geometry of the obscuring material resembles a torus that is seen almost edge-on in our line of sight. The bipolar outflow and the blueshifted CO v v =1–0 absorption toward the nucleus suggests that the obscuring envelope is currently expanding.

S4.SS1: IV.1 Gas extinction / block 1 · html

The galaxy 3C 293 exhibits a complex dust morphology, characterized by five interlaced dust lanes extending over a scale of approximately 10 kpc. This structure likely results from the merger event that occurred around 1 Gyr ago, as the dust orbits have not yet fully settled [ 33 , 93 ] . To study the spatial distribution of extinction in 3C 293, we derived the visual extinction ( A V A_{V} ) using the Br ​ β / Pa ​ α \rm Br\beta/Pa\alpha emission line ratio for each of the three kinematic components. The A V A_{V} is given by

S4.SS3: IV.3 Molecular gas inflows / block 1 · html

Adopting r d ≈ r_{d}\approx 1.5 arcsec ≈ \approx 1.5 kpc, a region that encompasses most of the H 2 emission, we obtain F H 2 ​ 2.12 = 1.11 × 10 − 14 ​ erg ​ s − 1 F_{\rm H_{2}2.12}=1.11\times 10^{-14}\,\rm erg\,s^{-1} , resulting in M H 2 = 2.3 × 10 4 ​ M ⊙ M_{\rm H_{2}}=2.3\times 10^{4}\,{\rm M_{\odot}} . Then, using the inclination angle θ = 53 ∘ \theta=53^{\circ} determined by our rotational model (Sec. IV.2 ), we convert our observed velocity v obs ≈ v_{\rm obs}\approx 100 km s -1 (from Fig. 9 ) to an intrinsic inflow velocity v = 100 / sin ⁡ ( 53 ∘ ) ≈ 125 v=100/\sin(53^{\circ})\approx 125 km s -1 . Combining this with the typical molecular disk height for active galaxies h = 30 h=30 pc [ 61 , e.g.] , the estimated mass-inflow rate is M ˙ i ​ n ≈ 8 × 10 − 3 ​ M ⊙ ​ yr − 1 \dot{M}_{in}\approx 8\times 10^{-3}\rm~M_{\odot}\,yr^{-1} .

S3.SS1: III.1 Emission Line Profiles and Kinematics / block 1 · html

Figure 3: Diagnostic diagrams of ionized emission line ratios: (a) [Ne V ]/[Ne III ] versus [O IV ]/[Ne III ], and (b) [Ne V ]/[Fe II ] versus [O IV ]/[Fe II ]. The reddish and greenish contours show the distributions of model results computed by [ 165 ] for AGN and fast radiative shocks (including the shock precursor), respectively, with each contour enclosing 30%, 60%, and 90% of the model results from inside to outside. The colored and gray data points represent measurements for the nuclear regions of the four low-luminosity AGN studied here and the six higher-luminosity Seyferts studied by [ 164 ] , respectively. The line ratios of NGC 1266 are marked as upper limits because [Ne V ] and [O IV ] flux measurements of this galaxy are below three times of the standard deviation noise of local continuum.

S3.SS4: III.4 Warm Molecular Gas Excitation / block 1 · html

Figure 5 also shows that the warm H 2 gas, mostly traced by low-J pure-rotational transitions, in the nuclear regions of the four low-luminosity AGN does not reach particularly high temperatures. This result is consistent with a higher fraction of the H 2 gas distributed toward the lower-temperature end in these nuclear regions, as indicated by their higher power-law temperature distribution index β \beta ( ∼ 5.0 − 5.5 \sim 5.0-5.5 ; see Section B ), particularly when compared to the nuclear apertures of higher-luminosity Seyferts ( β ≈ 4.0 − 5.0 \beta\approx 4.0-5.0 ; Davies et al. 23 , Zhang et al. 163 , Delaney et al. 25 ). This result further implies that non-thermal heating contributes to the warm H 2 excitation in the nuclear regions of the four low-luminosity AGN. As discussed above, slow molecular shocks are the most likely source of this non-thermal heating, and neither UV heating in PDRs nor X-ray heating from XDRs can account for the observed H 2 emission strength. Cosmic rays could be another heating source for the warm H 2 ( Ferland et al. 38 , Ogle et al. 119 ). However, even only for the warm H 2 content in these nuclear regions ( ∼ 10 4.2 − 10 6.4 ​ M ⊙ \sim 10^{4.2}-10^{6.4}\,{\rm M_{\odot}} ; see Appendix B ), reproducing the observed H 2 fluxes through cosmic-ray heating alone would require cosmic-ray excitation rates of order ∼ 10 − 11 ​ s − 1 \sim 10^{-11}\,{\rm s^{-1}} , assuming an energy deposition of 20 eV per excitation event and ∼ \sim 5% of this energy ultimately going to H 2 rotational emission (i.e., L H 2 L_{\rm H_{2}} is of N H 2 × 20 ​ eV × 0.05 × 10 − 11 ​ s − 1 N_{\rm H_{2}}\times\rm 20\,eV\times 0.05\times 10^{-11}\,s^{-1} ). The implied cosmic-ray excitation rates are much higher than those expected for low-luminosity AGN ( ∼ 10 − 12 ​ s − 1 \sim 10^{-12}\,{\rm s^{-1}} ; Koutsoumpou et al. 90 , Koutsoumpou et al. 91 ), indicating that cosmic-ray heating can only play a secondary role in powering the H 2 rotational emission in these nuclear regions.

S3.SS2: 3.2 Relation between H 2 /PAH and jet orientation / block 1 · html

Figure 3: Results of the Spearman correlation tests between H 2 S(3)/PAH 11.3 versus T H2 ​ ( 3 , 1 ) T_{\rm H2}{\rm(3,1)} (H 2 temp.), [Fe ii ]/PAH 11.3 (Shocks), and [Ne iii ]/[Ne ii ] (AGN ion.), measured both along and perpendicular to the radio axis. The numbers in each cell correspond to the measured R S R_{\rm S} coefficients. Only correlations with statistical significance, defined by p < 0.05 p<0.05 (95% confidence level), are shown; cases that do not satisfy this criterion are marked as NC.

S3: 3 Results / block 1 · html

Detailed studies of individual sources based on MIRI/MRS have already been conducted for most objects in our sample ( Costa-Souza et al., 2024 ; Dasyra et al., 2024 ; Goold et al., 2024 ; Alonso-Herrero et al., 2025 ; Ogle et al., 2025 ; Riffel et al., 2025 ; Evangelista et al., 2026 ) . Here, we focus our analysis on the H 2 / PAH \mathrm{H_{2}/PAH} ratio and on the relation between the jet orientation and the gas kinematics.

S3: 3 Results / block 1 · html

JWST probes the inner kiloparsecs of M58 with unprecedented detail ( Fig. 1 ). PAH 7.7 μ \mu m emission traces the dusty spiral arms and the inner dust disk. NIRCam F200W imaging maps the old stellar population as a smooth continuum aligned with a ∼ \sim 8 kpc bar and decoupled from the inner dust disk. The F212N narrowband show the H 2 1–0 S(1) rovibrational emission confined to the inner 2.6 kpc and consistent with 70 . The IFU data cover the central 0.7–1.2 kpc and trace the molecular phase of the ISM around the AGN. Two main dust lanes to the north and south dominate the H 2 emission, converging toward the nucleus, in agreement with absorption seen in HST optical images and the CO morphology ( 70 ) . Closer to the AGN, two regions show enhanced H 2 emission: one in the northeast (NE) at ∼ \sim 100 pc and another in the southwest (SW), partially overlapping the nucleus.

S3: 3 Results / block 1 · html

Moment maps ( Fig. 3 ) show that H 2 emission follows the dust lanes, except for very high-excitation transitions (e.g., ν \nu = = 2 2 ). The low-ionization line [Ar ii ] is extended within the inner 200 pc and peaks at the AGN. The high-ionization line [Ne v ] is confined to ∼ \sim 100 pc and display distinct kinematics. The enhanced mid- J J H 2 emission (e.g., S(5)) relative to lower- J J lines (e.g., S(1)) are consistent with 70 . However, the presence of higher vibrational levels within ≲ \lesssim 100 pc of the AGN suggests that additional excitation sources may contribute (see Section 4 ). The velocity fields of low-ionization lines and H 2 appear broadly consistent, with a ± \pm 200 km s -1 difference between the northern and southern lanes. While this may suggest rotation, caution is advised due to non-circular motions driven by the stellar bar ( 28 ) . Nevertheless, the lanes show low velocity dispersion as expected for rotation, whereas the nucleus reaches several hundred km s -1 . Ionized and high-excitation H 2 lines show elevated dispersions in the nucleus and NE.

S5: V Discussion and Summary / block 1 · html

The central engine of LRD-204851 has already been characterized in detail elsewhere, as reviewed in Section I . The combined picture is broadly consistent with recent models invoking dense neutral gas clumps around AGNs or “black-hole-star”-like configurations for the broad-line emission of LRDs [ 34 , 64 , 16 , e.g.,] , in which the central black hole is enshrouded by a dense, partially ionized gas envelope of substantial column density. In LRD-204851 itself, spectroscopic evidence for slow outward motion of such a central envelope, of order 100 km s -1 , is provided by the P-Cygni Balmer absorber identified in a very recent NIRSpec R2700 spectrum by Matthee et al. [59] . Adopting this picture, we focus here on the question that the present study uniquely constrains: the origin of the remarkable ∼ \sim kpc-scale elongated structure of LRD-204851, made visible in detail by the combination of MUSE rest-frame UV spectroscopy and JWST/NIRCam optical emission-line mapping.

S5: V Discussion and Summary / block 1 · html

The kinematic constraints on this outflow remain modest. Our Ly α \alpha modeling yields a bulk expansion velocity V exp ≃ 110 V_{\rm exp}\!\simeq\!110 km s -1 in the favored biconical geometry (Section III.2 ), in agreement with the P-Cygni H α \alpha absorber at Δ ​ v ≈ − 80 \Delta v\approx-80 km s -1 [ 59 ] . We emphasize that this outflow is geometrically anisotropic and biconical, distinct from the spherically symmetric Galactic_Wind configuration that our zELDA model comparison decisively disfavors (Appendix B ); the disfavored Galactic_Wind model reflects a geometric mismatch with the observed two-peak Ly α \alpha profile rather than the absence of outflow. Combining the intrinsic Ly α \alpha emission velocity offset ( Δ ​ v ≈ − 130 \Delta v\approx-130 km s -1 relative to systemic) with V exp V_{\rm exp} , the bulk near-side cone gas reaches a systemic-frame velocity of approximately − 240 -240 km s -1 , which sits at the lower edge of the v s ≳ 200 v_{\rm s}\!\gtrsim\!200 – 300 300 km s -1 threshold required for collisional shock ionization of high-ionization species such as N v [ 18 , 3 , 82 , e.g.,] . Both photoionization by hard radiation escaping the central engine along the low- N HI N_{\rm HI} channels and modest shock ionization in the bulk outflow are therefore plausible mechanisms for the high-ionization line emission at the south-eastern clump. If the tentative N v λ ​ 1238 \lambda 1238 detection is confirmed at higher S/N, its central velocity ( Δ ​ v ≈ − 467 \Delta v\approx-467 km s -1 relative to systemic) would lie above the shock-ionization threshold, and both production channels would remain viable. We further note that, if confirmed, this N v velocity exceeds the bulk cone-gas value implied by combining z Ly ​ α z_{\rm Ly\alpha} and V exp V_{\rm exp} . This difference can be accommodated by the resonant nature of Ly α \alpha , whose observed peak positions are a non-trivial function of V exp V_{\rm exp} , N HI N_{\rm HI} , geometry, and the intrinsic line profile, and can be reproduced by a range of bulk velocities once these parameters are varied [ 91 , 90 , e.g.,] .

abstract / block 1 · abstract

We present JWST observations of the radio galaxy TGSSJ1530+1049, spectroscopically confirmed at $z=4.0$. NIRCam images and NIRSpec/IFU spectroscopy (R=2700) show that TGSSJ1530+1049 is part of one of the densest-known structures of continuum and line-emitting objects found at these redshifts. NIRCam images show a number of distinct continuum objects and evidence of interactions traced by diffuse emission, and the NIRSpec IFU cube reveals further strong line emitting regions. We identify six continuum and four additional strong H$α$ emitting sources with weaker or no underlying continuum within the 3x3 arcsec IFU field. From spatial alignment with high-resolution radio data and emission line profiles, the radio AGN host galaxy is clearly identified. The bright H$α$ emission (but not the optical components) is distributed remarkably linearly along the radio axis, suggestive of a biconical illumination zone by a central obscured AGN. The emission line kinematics indicate jet-gas interactions on scales of a few kpc. However, due to large relative velocities and presence of underlying continuum, the alignment with the radio structure appears to be, at least partly, caused by a particular configuration of interacting galaxies. At least four objects within a 10x10 (projected) kpc$^2$ area which includes the radio source have high stellar masses ($\log(M_\star/M_\odot)>10.3$) and star formation rates in the range $70-163\,M_\odot$ yr$^{-1}$. Using a stellar mass-based analysis, we predict a total dark matter halo mass of $\approx10^{13} M_\odot$. Based on the physical separations and velocity differences between the galaxies, it is expected that these galaxies will merge to form a massive galaxy within a few Gyr. The system qualitatively resembles the forming brightest cluster galaxies in cosmological simulations that form early through a rapid succession of mergers.

A5: Appendix E Kinematic modelling of the central molecular gas disk with 3D Barolo / block 1 · html

Figure 19 : Modelling results of the central kpc of the CO (J = 2 - 1) emission from 3D Barolo. The left and middle panels show the PV diagrams of the fitted model of the nuclear rotating molecular disk (in red contours), along the major ( ϕ = 256 ∘ \phi=256^{\circ} ) and minor axis ( ϕ = 345 ∘ \phi=345^{\circ} ) previously determined by Agostino et al. (2026) . The observed emission are shown in grey scales, and area covered by region C is indicated with vertical dashed cyan lines. The right panel compares the observed and modeled CO ( J = 2 - 1) line profile extracted from region C, shown in grey and red, respectively. The modeled nuclear disk contributes 60% of the total flux contained within region C.

article / block 1 · html

Results. We confirm the presence of a multi-phase galactic biconical outflow along the minor axis of a highly inclined rotating disk, based on the multi-phase gas morphology and prominent line broadening (FWHM > 500 >500 km s -1 ) in the ionized gas tracers detected out to ∼ \sim 5 kpc from the nucleus. The molecular gas tracers are detected out to ∼ \sim 2 kpc, and exhibit a distinct “X”-shaped morphology and different velocity fields from the ionized gas, which we attribute to the higher concentration of molecular gas near the disk. We adopt a simple model to interpret the observed multiphase gas kinematics and infer an outflow velocity of ∼ \sim\, 500 - 600 km s -1 ∼ \sim\, 350 km s -1 , and ∼ \sim\, 200 - 300 km s -1 , in the ionized, warm and cold molecular phase, respectively, with corresponding mass outflow rates of ∼ 0.3 − 2.3 \sim 0.3-2.3 , ∼ 31 \sim 31 , and ∼ 38 − 240 \sim 38-240 M ⊙ {}_{\odot}\, yr -1 . The cold molecular phase dominates both the total mass outflow rate and the associated kinetic energy ( ∼ 2 − 8 × 10 42 \sim\,2-8\times 10^{42} erg s -1 ). Via JWST/MIRI-MRS detection of the [Ne V] 14.3 μ \mu m line, we identify, for the first time, a dust-obscured AGN in IRAS F01364-1042. The low inferred AGN bolometric luminosity ( 1.2 − 1.8 × 10 43 1.2-1.8\times 10^{43} erg s -1 ) suggests that the nuclear starburst alone, with a star formation rate of ∼ 40 − 60 \sim 40-60 M ⊙ yr -1 , can account for the energy required to drive the outflow, though a more active AGN phase in the recent past may have also played a role.

S5: 5 Summary and conclusion / block 1 · html

The spectrum of the host galaxy exhibits an extreme ionised outflow, mainly observed in [O iii ] λ ​ λ \lambda\lambda 4960,5008, H α \alpha and H β \beta . This outflow is modelled with two components with maximal outflowing velocities of v out ∼ 425 v_{\rm out}\sim 425 km s -1 and v out ∼ 3263 v_{\rm out}\sim 3263 km s -1 respectfully. The first outflow is observed at approximately the same redshift as the narrow component, but the second outflow is blueshifted by Δ ​ z ∼ 0.01 \Delta z\sim 0.01 . The narrow component is compatible with no dust attenuation, while the two outflowing components are compatible with some attenuation, hinting for expulsion of dust with the outflow. Despite the high velocity of one outflowing component, the observed outflows are not significant for the galaxy, as the mass loading factors reach ∼ 7 % \sim 7\% and > 10 % >10\% and the inferred kinetic energy is rather low compared to similar velocities AGN-driven outflows ( Bertola et al., 2025 ) . The gas in the host component shows a relatively low oxygen abundance of 12 + log ⁡ ( O / H ) ∼ 7.95 12+\log(O/H)\sim 7.95 and slight nitrogen enhancements log ⁡ ( N / O ) ∼ − 0.75 \log(N/O)\sim-0.75 . Using a mass-metallicity relationship ( Chemerynska et al., 2024 ) , we estimate a de-lensed stellar mass of log ⁡ ( M ⋆ / M ⊙ ) ∼ 8.2 \log(M_{\star}/M_{\odot})\sim 8.2 .

S4.SS2: 4.2 Nature of the ionised outflow in GLIMPSED-329380 / block 1 · html

In conclusion, we found strong evidence that the observed fast ionised outflow in GLIMPSED-329380 is driven by AGN activity. The similarities between this object and the diverse class of LRDs, including spectral features, emission line profiles, and continuum shape, suggest that this LRD hosts an active AGN. To date, most LRD studies have relied on low-resolution PRISM data, which may limit the detection of outflows. Future medium- or high-resolution spectroscopic observations of LRDs will be important to determine whether such extreme outflows are a common feature of these systems.