# The Circumnuclear Environment of IRAS 20551-4250: A Case Study of AGN/Starburst Connection forJWST

Authors: E. Sani; E. Nardini
Journal: Advances in Astronomy
 (2012)

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## Abstract

We present a general review of the current knowledge of IRAS 20551-4250 and its circumnuclear environment. This Ultraluminous Infrared Galaxy is one of the most puzzling sources of its class in the nearby Universe: the near-IR spectrum is typical of a galaxy experiencing a very intense starburst, but a highly obscured active nucleus is identified beyond ~5μm and possibly dominates the mid-IR energy output of the system. At longer wavelengths star formation is again the main driver of the global spectral shape and features. We interpret all the available IR diagnostics in the framework of simultaneous black hole growth and star formation and discuss the key properties that make this source an ideal laboratory for the forthcoming James Webb Space Telescope.


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## Body

## 1. Introduction

Two main physical processes characterize the nuclear regions of active galaxies: intense star formation at rates of ~102–103 M⊙ yr−1 (starburst, SB) and accretion on to a supermassive black hole (active galactic nucleus, AGN). The issue of SB and AGN connection in both local and distant galaxies is critical for a proper understanding of galaxy formation and evolution, of star formation history and metal enrichment of the Universe, and of the origin of the extragalactic background at low and high energies. There is indeed increasing evidence of a strong link between the starburst and AGN mechanisms in active systems. The empirical correlation between the mass of black holes (BHs) located at the centre of nearby galaxies (both active and passive/quiescent) and the mass of their spheroids (see [1] and references therein) suggests that the formation of bulges and the growth of the central BHs are tightly connected. Also the presence of circumnuclear star formation in a substantial fraction of local AGN [2–5] hints at the relation between the two phenomena. The overall conclusion of these studies is that in 30–50% of the cases the accreting supermassive BHs are associated with young (i.e., of age less than a few ×100 Myr) star-forming regions, with clear evidence of an enhanced star formation rate (reaching up to starburst intensities) in most AGN. However, this does not necessarily imply any causal connection between the two physical processes. It could be simply the natural consequence of massive gas fuelling into the nuclear regions, due to either interactions/mergers or secular evolution such as bar-driven inflows. Both star formation and nuclear accretion, in fact, are triggered and subsequently fed by this gas reservoir.In the local Universe, the optimal targets to study the AGN/SB interplay are the so-called Ultraluminous Infrared Galaxies (ULIRGs; [6]). These sources are the result of major mergers, during which the redistribution of the gaseous component drives vigorous starburst events and obscured nuclear accretion. It is now well established that ULIRGs are usually powered by a combination of both processes, giving rise to their huge luminosities (Lbol~LIR>1012L⊙). However, since the primary radiation field is reprocessed by dust, the identification of the dominant energy supply is often unclear. The simultaneous presence of star formation and AGN signatures in the mid-IR makes this a really favourable band to disentangle the AGN and SB components and explore their environment. In particular, (i) the available spectra of bona fide starburst-dominated and, respectively, unobscured AGN-dominated sources are widely different, and show little dispersion within the separate classes [7–10]. This allowed us to reproduce the AGN/SB contributions with fixed templates, especially over the the 3–8 μm spectral interval. (ii) For a given bolometric luminosity, the mid-IR AGN emission is higher than that of a starburst by a factor that rapidly declines with wavelength, ranging from ~100 at 3-4 μm [7] to ~25 at 5–8 μm [11]. Such a large difference is due to the key contribution of the hot dust layers directly exposed to the AGN radiation field. Together with the relatively low dust extinction at these wavelengths, this allows the detection of an AGN even when it is heavily obscured and/or its total luminosity is small compared with the SB counterpart. Based on the previous points, we successfully fitted the observed ULIRG spectra with a two-component analytical model, with only two free parameters: the relative AGN/SB contribution and the optical depth of the screen-like obscuration (if any) affecting the compact AGN component.To understand whether the link between star formation and nuclear activity is a matter ofnature (i.e., feedback processes) or nurture (i.e., host environments), here we investigate the circumnuclear structure of IRAS 20551-4250, an ideal laboratory thanks to its unique physical properties (in terms of both relative AGN/SB contribution and AGN obscuration), and to the fairly large multiwavelength dataset available. The paper is organized as follows: in Section 2 we review the present knowledge of the mid-IR properties of IRAS 20551-4250. The dust extinction law and gas column density are dealt with in Section 3. A possible general picture and the feasibility of future observations with James Webb Space Telescope (JWST) are discussed in Section 4. In Section 5 we summarize our findings and draw the conclusions. Throughout this work we adopt a standard cosmology (H0=70 km/s/Mpc, Ωm=0.3, Ωλ=0.7).


## 2. IRAS 20551-4250: General Properties

IRAS 20551-4250 is a nearby (z=0.043) ULIRG lying in the luminosity range of IR quasars, with LIR=4.3×1045 erg/s. It mostly lacks of targeted studies; none the less in literature there are several related measurements among the statistical analyses of the local ULIRG population. IRAS 20551-4250 is a merging system in a fairly advanced state (Figure 1, left panel), characterized by a single nucleus with a prominent tidal tail and a slightly disturbed core, likely caused by a minor merger or strong secular evolution effects. From the high-resolution near-IR data Haan et al. [12] ascribe the large ratio of nuclear excess to bulge luminosity (see also Figure 1, right panel) to the possible presence of an AGN with BH mass ~4.4 × 108 M⊙. The spectral classification changes significantly with the observed waveband. It is optically classified as an H ii region [13], while in the mid-IR it resembles an SB galaxy [2]. However, diagnostic methods exclusively based on emission lines, as the ones mentioned previously, suffer from limited extensibility to faint sources and fail in identifying the heavily absorbed AGN detected in the hard X-rays. Indeed, the hard X-rays emission of IRAS 20551-4250 is clearly dominated by an obscured AGN, with luminosity L2-10keV~7.0×1042 erg s−1 and column density NH~8×1023 cm−2 [14]. According to all these pieces of observational evidence, the relative AGN contribution to the bolometric luminosity is uncertain, but probably highly significant, while the circumnuclear environment is still poorly characterized. The first quantitative determination of the AGN contribution to the mid-IR emission of IRAS 20551-4250 was obtained by Farrah et al. [15] thanks to a series of effective diagnostics based on fine-structure lines. Their analysis of Spitzer/IRS high-resolution spectra suggests a moderate AGN contribution, even though a peculiar geometry and/or extreme optical depth are responsible for the lack of typical AGN tracers (e.g., [Ne v], [O iv]).Figure 1
HST images of IRAS 20551-4250. Left: composite B + I band image obtained with the WFC F435W and F814W filters (PID 10592, PI A. Evans). The white square identifies the nuclear (30′′ × 30′′) region. Right: NICMOS F160W image (PID 11235, PI J. Surace) of the nuclear region. The Spitzer/IRS short-wavelength/low-resolution (SL, 3.6′′ width) and short-wavelength/high-resolution (SH, 4.7′′ width) slits are shown together with the VLT/ISAAC slit (IS, 1′′ width in the L-band). Given a spatial scale of 950 pc/′′, the SL, SH, and IS slits cover regions of 3.4 kpc, 4.5 kpc, and 950 pc, respectively.


### 2.1.L- and M-Band Spectroscopy

Risaliti et al. [16] obtained L-band observations of ULIRGs with 8 m class telescopes (VLT and Subaru). The resulting high-quality spectra have revealed the great power of L-band diagnostics in characterizing AGN and SB components inside ULIRGs. The main results of these studies are summarized in the following. (1) A large (~110 nm) equivalent width (EW) of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission feature is typical of SB-dominated sources, while the strong radiation field of an AGN, extending up to the X-ray domain, partially or completely destroys the PAH carriers. (2) A strong (τ3.4>0.2) absorption feature at 3.4 μm due to aliphatic hydrocarbon grains is an indicator of an obscured AGN; indeed, such a deep absorption requires the presence of a bright, point-like source behind a screen of dusty gas. (3) A steep continuum (Γ>3 when describing the flux density as a power law fν∝λΓ) hints at the presence of a highly obscured AGN. Again, a large value of Γ implies the strong dust reddening of a compact source.TheL-band spectrum of IRAS 20551-4250 shows somewhat puzzling properties [7]: a strong 3.3 μm emission feature (EW≃90 nm) suggests a dominant starburst contribution. On the other hand, the steep observed slope (Γ~5) and the detection of the 3.4 μm absorption feature point to the presence of a significant AGN affecting the continuum emission. Sani and coauthors [17] added the M-band (4-5 μm) data to better determine the continuum trend and analyse the broad CO absorption band near 4.65 μm. By combining the L- and M-band data (as shown in Figure 2), we estimated a very large AGN contribution at 3.5 μm, exceeding ~90% once corrected for extinction (see [7] for the analytical details). The observed AGN component, however, is heavily obscured and shows extreme dust reddening. The large optical depth (τL>5, assuming the extinction law of Draine [18]) is necessary to reconcile the apparently contradictory observational results, that is, the high equivalent width of the 3.3 μm PAH feature and the steep, intense continuum. The presence of a dust and gas screen absorbing the AGN emission is also revealed by the deep absorption profiles due to aliphatic hydrocarbons (τ3.4=1.5) and gaseous CO (τ4.6=2.2). This step-wise correlation between continuum reddening and absorption features appears to be a general property of ULIRGs hosting an obscured AGN [11, 17]. Anyhow, this does not hold under a quantitative point of view: no tight correlation is found among the values of the optical depth, not even between the two absorption features themselves. This suggests a nonuniform dust composition among ULIRGs. The implications on the shape of the extinction law are discussed in the following section.Figure 2
L+ M band of IRAS 20551-4250 [17]. The heavily reddened continuum (red curve) is present together with strong CO absorption in the M-band. The regions of bad atmospheric transmission are shaded in yellow. (Note the units on the vertical axis, fλ∝λ-2fν.)


### 2.2.Spitzer/IRS Spectroscopy

In a series of papers [10, 11] we have shown that the high quality of Spitzer-IRS data allows a very effective quantitative determination of the AGN/SB components around 5–8 μm; this method is much more accurate than those possible in other bands in spite of the lower AGN over SB brightness ratio, which rapidly declines with wavelength. Summarizing, once applied to large, virtually complete samples of local ULIRGs, the 5–8 μm analysis yields the main results listed hereinafter. (1) The large variations in the observed spectral shape of ULIRGs can be successfully explained in terms of the relative AGN contribution and its degree of obscuration. (2) Although the larger fraction of ULIRG bolometric energy output is associated with the intense SB events, the AGN contribution is nonnegligible (~25–30%) and increases with both the total IR luminosity of the host galaxy and, possibly, with the merger stage [19]. (3) The apparent lack of continuum reddening and the simultaneous detection of deep absorption troughs in some of the most obscured sources (when a stepwise correlation is generally found, as mentioned earlier) suggests that the extinction of the AGN component in a ULIRG environment is not universal. Both a power-law and a quasigrey behaviour of the optical depth as a function of wavelength are necessary to account for the emission of different objects and seem to be involved among ULIRGs.Consistently with the 3-4μm analysis, also the 5–8 μm spectrum of IRAS 20551-4250 (in Figures 3 and 4) shows remarkable properties: the AGN continuum can be hardly determined due to strong absorption around 6 and 6.85 μm, respectively, attributed to a mixture of ices and hydrogenated amorphous carbons (HACs). The standard spectral decomposition yields again a very bright but strongly reddened AGN, with a mid-IR intrinsic contribution of ~90% and a 6 μm optical depth τ6=1.2 (following the same extinction law introduced before [18]). Although the starburst dominates the bolometric luminosity, the AGN contribution is significant (26 ± 3%). At longer wavelengths (λ>8 μm), the huge silicate absorption troughs at 9.7 and 18 μm require the nuclear source to be deeply embedded in a smooth distribution of dust, both geometrically and optically thick. Ground-based imaging at 18 μm reveals a compact unresolved source (<120 pc) with high surface brightness and large Si optical depth (τ18=0.7), in agreement with a buried AGN interpretation [20]. It is also worth noting that τ9.7 can be combined with the EW of the 6.2 μm PAH feature in a diagnostic diagram that provides not only a direct classification but also possible indications on the evolutionary path of a source, by probing the age of the SB and the geometrical structure of the dust [21]. The location of IRAS 20551-4250 in such a diagram is typical of an intermediate stage between a fully obscured AGN and an unobscured nuclear starburst.Figure 3
Spitzer/IRS 5–20 μm emission. We have already analysed the low-resolution data in a previous work [11], while the high-resolution spectrum (above ~10 μm) has been extracted from the same dataset following Schweitzer et al. [4]. The main features are labelled for ease of identification.Figure 4
VLT/ISAAC L- and M-bands, plus Spitzer/IRS low-resolution spectra of IRAS 20551-4250. The data and best-fit models for each band are plotted in green and black, respectively. The different contributions to the observed spectra (blue for AGN component, red for the SB one) are also shown. Absorption features are fitted separately and then combined with the AGN template. Due to the strong reddening of the AGN continuum, the only AGN signature within the L-band is the shallow, structured 3.4 μm hydrocarbon absorption, highly diluted by the SB emission. The M-band continuum cannot be constrained due to the deep CO features, while the 6.0 μm water ice and 6.85 μm hydrocarbon absorption profiles are detected at 5–8 μm [9, 15].As mentioned before, in IRAS 20551-4250 also fine-structure lines from highly ionized atoms are detected, as well as H2 pure vibrational transitions (Figure 3). Our new measurements of the mid-IR line fluxes are listed in Table 1. Notably, the standard coronal lines produced by the hard AGN photons, such as [Ne v] (14.3 μm) and [O iv] (25.9 μm), are not detected (only upper limits are reported also in [15]); moreover, the [Ne iii]/[Ne ii] line ratio of ~0.2 is well consistent with an SB-dominated radiation field. As a result, taking into account only mid-IR emission lines would lead to a misclassification of IRAS 20551-4250 as a pure SB source. The lack of high-ionization lines and low [Ne iii]/[Ne ii] ratio can be actually reconciled with the presence of a deeply obscured AGN by allowing for a peculiar geometry of the gaseous/dusty absorber. Indeed, a large covering factor of the putative torus predicted by AGN unification models [22] can even prevent the formation of the narrow-line region and the production of high-ionization species. The geometrical properties of the absorber in a ULIRG are likely much more complicated, and a cocoon-like structure can be reasonably expected. Also the other standard diagnostic ratio [S iii](λ18.71)/[S ii](λ33.48) has an intermediate value among ULIRGs (~0.7) and tends to confirm the latter interpretation.Table 1
Properties of the detected mid-IR emission lines. We measured the fluxes with theidl package smart by means of a Gaussian fitting. We use the most recent version of the IRS pipelines; thus our estimates are more reliable than those previously published.
Mid-IR emission linesLineH2S(3)H2S(2)[Ne II][Ne III]H2S(1)[S III]H2S(0)[S III]λrest (μm)9.66212.27512.81415.55517.03018.71328.21933.481Eion (eV)——21.641.0—23.3—23.3Flux (1021 W/cm2)5.36±0.153.06±0.1713.0±0.42.6±0.36.9±0.25.7±0.63.8±0.88.0±0.3Four lines from pure rotational transitions of warm H2 are clearly detected (see Figure 3, Table 1 and [15]): 0-0S(3) 9.67 μm, 0-0S(2) 12.28 μm, 0-0S(1) 17.04 μm and 0-0S(0) 28.22 μm. The upper levels of these transitions are populated via UV pumping, formation of H2 in excited states or collisional excitation; therefore these lines directly probe the warm component of the molecular gas. A standard ortho-to-para ratio of 3 is found for gas with typical temperature T~300 K. The heating mechanisms can be associated to either the SB (e.g., in photodissociation regions (PDRs), shocks/outflows in supernova remnants (SNRs)) or the AGN (due to the X-ray heating). From the line ratios and excitation temperatures measured among ULIRGs (including IRAS 20551-4250) Higdon et al. [23] ascribed the warm H2 component to PDRs associated with massive SB. A more detailed investigation of the physical parameters of the H2 gas is presented in Section 3.2.


## 2.1.L- and M-Band Spectroscopy

Risaliti et al. [16] obtained L-band observations of ULIRGs with 8 m class telescopes (VLT and Subaru). The resulting high-quality spectra have revealed the great power of L-band diagnostics in characterizing AGN and SB components inside ULIRGs. The main results of these studies are summarized in the following. (1) A large (~110 nm) equivalent width (EW) of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission feature is typical of SB-dominated sources, while the strong radiation field of an AGN, extending up to the X-ray domain, partially or completely destroys the PAH carriers. (2) A strong (τ3.4>0.2) absorption feature at 3.4 μm due to aliphatic hydrocarbon grains is an indicator of an obscured AGN; indeed, such a deep absorption requires the presence of a bright, point-like source behind a screen of dusty gas. (3) A steep continuum (Γ>3 when describing the flux density as a power law fν∝λΓ) hints at the presence of a highly obscured AGN. Again, a large value of Γ implies the strong dust reddening of a compact source.TheL-band spectrum of IRAS 20551-4250 shows somewhat puzzling properties [7]: a strong 3.3 μm emission feature (EW≃90 nm) suggests a dominant starburst contribution. On the other hand, the steep observed slope (Γ~5) and the detection of the 3.4 μm absorption feature point to the presence of a significant AGN affecting the continuum emission. Sani and coauthors [17] added the M-band (4-5 μm) data to better determine the continuum trend and analyse the broad CO absorption band near 4.65 μm. By combining the L- and M-band data (as shown in Figure 2), we estimated a very large AGN contribution at 3.5 μm, exceeding ~90% once corrected for extinction (see [7] for the analytical details). The observed AGN component, however, is heavily obscured and shows extreme dust reddening. The large optical depth (τL>5, assuming the extinction law of Draine [18]) is necessary to reconcile the apparently contradictory observational results, that is, the high equivalent width of the 3.3 μm PAH feature and the steep, intense continuum. The presence of a dust and gas screen absorbing the AGN emission is also revealed by the deep absorption profiles due to aliphatic hydrocarbons (τ3.4=1.5) and gaseous CO (τ4.6=2.2). This step-wise correlation between continuum reddening and absorption features appears to be a general property of ULIRGs hosting an obscured AGN [11, 17]. Anyhow, this does not hold under a quantitative point of view: no tight correlation is found among the values of the optical depth, not even between the two absorption features themselves. This suggests a nonuniform dust composition among ULIRGs. The implications on the shape of the extinction law are discussed in the following section.Figure 2
L+ M band of IRAS 20551-4250 [17]. The heavily reddened continuum (red curve) is present together with strong CO absorption in the M-band. The regions of bad atmospheric transmission are shaded in yellow. (Note the units on the vertical axis, fλ∝λ-2fν.)


## 2.2.Spitzer/IRS Spectroscopy

In a series of papers [10, 11] we have shown that the high quality of Spitzer-IRS data allows a very effective quantitative determination of the AGN/SB components around 5–8 μm; this method is much more accurate than those possible in other bands in spite of the lower AGN over SB brightness ratio, which rapidly declines with wavelength. Summarizing, once applied to large, virtually complete samples of local ULIRGs, the 5–8 μm analysis yields the main results listed hereinafter. (1) The large variations in the observed spectral shape of ULIRGs can be successfully explained in terms of the relative AGN contribution and its degree of obscuration. (2) Although the larger fraction of ULIRG bolometric energy output is associated with the intense SB events, the AGN contribution is nonnegligible (~25–30%) and increases with both the total IR luminosity of the host galaxy and, possibly, with the merger stage [19]. (3) The apparent lack of continuum reddening and the simultaneous detection of deep absorption troughs in some of the most obscured sources (when a stepwise correlation is generally found, as mentioned earlier) suggests that the extinction of the AGN component in a ULIRG environment is not universal. Both a power-law and a quasigrey behaviour of the optical depth as a function of wavelength are necessary to account for the emission of different objects and seem to be involved among ULIRGs.Consistently with the 3-4μm analysis, also the 5–8 μm spectrum of IRAS 20551-4250 (in Figures 3 and 4) shows remarkable properties: the AGN continuum can be hardly determined due to strong absorption around 6 and 6.85 μm, respectively, attributed to a mixture of ices and hydrogenated amorphous carbons (HACs). The standard spectral decomposition yields again a very bright but strongly reddened AGN, with a mid-IR intrinsic contribution of ~90% and a 6 μm optical depth τ6=1.2 (following the same extinction law introduced before [18]). Although the starburst dominates the bolometric luminosity, the AGN contribution is significant (26 ± 3%). At longer wavelengths (λ>8 μm), the huge silicate absorption troughs at 9.7 and 18 μm require the nuclear source to be deeply embedded in a smooth distribution of dust, both geometrically and optically thick. Ground-based imaging at 18 μm reveals a compact unresolved source (<120 pc) with high surface brightness and large Si optical depth (τ18=0.7), in agreement with a buried AGN interpretation [20]. It is also worth noting that τ9.7 can be combined with the EW of the 6.2 μm PAH feature in a diagnostic diagram that provides not only a direct classification but also possible indications on the evolutionary path of a source, by probing the age of the SB and the geometrical structure of the dust [21]. The location of IRAS 20551-4250 in such a diagram is typical of an intermediate stage between a fully obscured AGN and an unobscured nuclear starburst.Figure 3
Spitzer/IRS 5–20 μm emission. We have already analysed the low-resolution data in a previous work [11], while the high-resolution spectrum (above ~10 μm) has been extracted from the same dataset following Schweitzer et al. [4]. The main features are labelled for ease of identification.Figure 4
VLT/ISAAC L- and M-bands, plus Spitzer/IRS low-resolution spectra of IRAS 20551-4250. The data and best-fit models for each band are plotted in green and black, respectively. The different contributions to the observed spectra (blue for AGN component, red for the SB one) are also shown. Absorption features are fitted separately and then combined with the AGN template. Due to the strong reddening of the AGN continuum, the only AGN signature within the L-band is the shallow, structured 3.4 μm hydrocarbon absorption, highly diluted by the SB emission. The M-band continuum cannot be constrained due to the deep CO features, while the 6.0 μm water ice and 6.85 μm hydrocarbon absorption profiles are detected at 5–8 μm [9, 15].As mentioned before, in IRAS 20551-4250 also fine-structure lines from highly ionized atoms are detected, as well as H2 pure vibrational transitions (Figure 3). Our new measurements of the mid-IR line fluxes are listed in Table 1. Notably, the standard coronal lines produced by the hard AGN photons, such as [Ne v] (14.3 μm) and [O iv] (25.9 μm), are not detected (only upper limits are reported also in [15]); moreover, the [Ne iii]/[Ne ii] line ratio of ~0.2 is well consistent with an SB-dominated radiation field. As a result, taking into account only mid-IR emission lines would lead to a misclassification of IRAS 20551-4250 as a pure SB source. The lack of high-ionization lines and low [Ne iii]/[Ne ii] ratio can be actually reconciled with the presence of a deeply obscured AGN by allowing for a peculiar geometry of the gaseous/dusty absorber. Indeed, a large covering factor of the putative torus predicted by AGN unification models [22] can even prevent the formation of the narrow-line region and the production of high-ionization species. The geometrical properties of the absorber in a ULIRG are likely much more complicated, and a cocoon-like structure can be reasonably expected. Also the other standard diagnostic ratio [S iii](λ18.71)/[S ii](λ33.48) has an intermediate value among ULIRGs (~0.7) and tends to confirm the latter interpretation.Table 1
Properties of the detected mid-IR emission lines. We measured the fluxes with theidl package smart by means of a Gaussian fitting. We use the most recent version of the IRS pipelines; thus our estimates are more reliable than those previously published.
Mid-IR emission linesLineH2S(3)H2S(2)[Ne II][Ne III]H2S(1)[S III]H2S(0)[S III]λrest (μm)9.66212.27512.81415.55517.03018.71328.21933.481Eion (eV)——21.641.0—23.3—23.3Flux (1021 W/cm2)5.36±0.153.06±0.1713.0±0.42.6±0.36.9±0.25.7±0.63.8±0.88.0±0.3Four lines from pure rotational transitions of warm H2 are clearly detected (see Figure 3, Table 1 and [15]): 0-0S(3) 9.67 μm, 0-0S(2) 12.28 μm, 0-0S(1) 17.04 μm and 0-0S(0) 28.22 μm. The upper levels of these transitions are populated via UV pumping, formation of H2 in excited states or collisional excitation; therefore these lines directly probe the warm component of the molecular gas. A standard ortho-to-para ratio of 3 is found for gas with typical temperature T~300 K. The heating mechanisms can be associated to either the SB (e.g., in photodissociation regions (PDRs), shocks/outflows in supernova remnants (SNRs)) or the AGN (due to the X-ray heating). From the line ratios and excitation temperatures measured among ULIRGs (including IRAS 20551-4250) Higdon et al. [23] ascribed the warm H2 component to PDRs associated with massive SB. A more detailed investigation of the physical parameters of the H2 gas is presented in Section 3.2.


## 3. The Circumnuclear Medium

The combined analysis of 3–8μm data gives the immediate advantage to trace the coexisting AGN and SB environments. Indeed, after the review of all the mid-IR spectral properties, the presence of a heavily absorbed AGN combined with a vigorous SB in IRAS 20551-4250 is well established. None the less, a comprehensive interpretation of all the observables (AGN hot-dust emission, continuum reddening, absorption features, PAH strength) is not straightforward. The general picture is complicated by the different spatial extent of the nuclear region that has been explored in the works mentioned previously. In fact, there can be some aperture effects related to the slit widths, as the nuclear emission is quite diffuse and has a large surface brightness. The slit widths and orientations of the main instruments considered in this work are shown in the right panel of Figure 1. IRAS 20551-4250 presents a very small fraction (<10%) of extended emission in the 13.2 μm continuum, which can be mainly associated with the compact, unresolved hot/warm dust component in proximity of the AGN [24]. Conversely, the extra-nuclear emission is substantial for both the 7.7 μm PAH feature and the [Ne ii] line at 12.8 μm (~40 and 25%, resp.; [25]), which are obviously related to the circumnuclear SB. Here, in order to further investigate the physical conditions responsible for reddening/absorption, we try (i) to fit simultaneously the L-band and 5–8 μm data, and (ii) to measure the column density of the circumnuclear gas for both the atomic and molecular components.


### 3.1. The Extinction Law

Figure4 shows the observed spectrum of IRAS 20551-4250 between 3 and 8 μm once the ground-based VLT data are combined with the first part of the Short-Low Spitzer/IRS orders. We did not apply any cross-scaling factor, since it would be a very complex task and we are confident about the reliability of the absolute flux calibrations, which are affected only by small relative errors (~10%; [7, 11, 17]). From a visual inspection of the three spectra, it is clear that the observed continuum slope, which is expected to be heavily shaped by the AGN contribution, cannot be reproduced with a single spectral index over the whole range under investigation. In our separate L-band and 5–8 μm studies, we have assumed an intrinsic slope of Γ=1.5 for the AGN hot-dust continuum and then applied a power-law extinction of the form τ(λ)∝λ-1.75 [18]. This screen-like absorption is possibly due to colder dust in the outer layers of the putative torus, or it might be associated with some star-formation region in the circumnuclear environment of the host galaxy. It is now evident that the latter assumptions do not allow us to reproduce simultaneously the AGN emission for the different datasets. In fact, by extending the best-fitting AGN model from the L-band to longer wavelengths, we largely overestimate the 8 μm observed flux. Of course, it is possible that the intrinsic AGN spectrum is more complex than the one adopted in our spectral decomposition. A more detailed analysis should allow for different dust components with individual temperature and emissivity, and also radiative transfer effects need to be taken into account. However, a broken power-law trend seems to describe with fairly good precision the observed spectral curvature. Interestingly, we can try to obtain some empirical (a posteriori) indication about the extinction suffered by the AGN hot-dust emission. Virtually all the available extinction curves in this wavelength range, in fact, are derived from lines of sight within our own Galaxy, while the composition of the interstellar medium (ISM) in active galaxies is expected to be very different, as proved, for example, by the dust-to-gas ratios estimated through a comparison between the mid-IR dust obscuration and the gas column density in the X-rays of these objects  [26, 27].We have therefore fitted all the three bands allowing for different slopes of the observed AGN continuum. TheM-band is clearly poorly constrained and the value of Γ is frozen to give a smooth connection among the spectral intervals for both the AGN and SB templates. We have then computed the trend of the extinction law by making the easiest assumption about the intrinsic shape of the hot-dust emission, that is, the simple power-law dependence of the flux density from wavelength. Figure 5 shows the comparison between two possible extinction laws, corresponding to different values of the intrinsic Γ, and three standard Galactic curves. Although no conclusive indication can be drawn, the similarity is quite remarkable and suggests that the dust extinction law and the AGN intrinsic continuum are partially degenerate. This anyway does not affect the quantitative results of our analysis, as the AGN and SB 6 μm to bolometric corrections are averaged over large samples and this systematic effect is greatly reduced (see also the discussion on the AGN template and dust extinction in [11]).Figure 5
Dust extinction laws obtained by assuming a single power-law form (fν∝λΓ) to reproduce the intrinsic AGN hot-dust emission over the 3–8 μm band. The solid lines correspond to different choices of the spectral index: blue for Γ=2, and red for Γ=3. The dashed lines are standard Galactic extinction curves for comparison: cyan for [18], orange for Chiar and Tielens [28], and green for Nishiyama et al. [29, 30]. The relation with the extinction in visual magnitudes plotted on the vertical axis is based on the latter works, and all the curves are normalized in order to have the same value at 3 μm. While the exact extinction shape is not so important in the L-band, at 5–8 μm (and most likely beyond, with the presence of the silicate absorption feature) the difference in terms of optical depth in the different cases can be as large as a factor of 3. However, it seems quite hard to obtain such a large dust extinction around 6 μm to be consistent with the gas column density of nearly ~1024 cm−2 measured in the X-rays.


### 3.2. Gas and Dust Content

To further constrain the absorbing/emitting medium in IRAS 20551-4250, we attempted at estimating the gas column density by means of a multiwavelength approach. We start by assuming a Galactic gas-to-dust ratio [31]:(1)NHAV=1.9×1021mag-1cm-2
with AL~0.04AV and A6~0.012AV. We then employ the following estimates: (a) the column density of the gas absorbing the X-ray radiation directly measured in the 2–10 keV energy range [14], (b) the L-band and 6 μm optical depth assessed through the continuum reddening in our decomposition method [11], and (c) the optical depth of the 3.4 μm hydrocarbon feature [7]. The corresponding visual extinction values are listed in Table 2.Table 2
Extinction obtained by assuming a gas-to-dust ratio as in (1). Columns: (1) observational band used for the direct measurement with the relative reference. (2) and (3) L-band and 6 μm optical depth for the AGN continuum as obtained with our spectral decomposition model. (4) Optical depth of the aliphatic hydrocarbon feature once corrected for the SB dilution. (5) Gas column density measured from the X-ray spectrum. (6) Optical extinction predicted by Galactic relations (see text for details).
Extinction estimatesBandτLτ6τ3.4NH cm−2ExpectedAV mag3μm [9]82206μm [15]1.21103.4μm [9]1.54502–10 keV [11]8×1023420From a comparison among these independentAV predictions, we can draw four main considerations. (1) Independently from the adopted proxy, we infer a huge extinction in the visual band, which naturally explains the optical misclassification of IRAS 20551-4250. (2) As discussed in the previous section, a flatter extinction law over the 3–8 μm range with respect to a steep power-law trend [18] seems to be more appropriate to reproduce the observed AGN emission. Otherwise, the values of AV derived from the 3 μm and 6 μm reddening differ by a factor of two. (3) By using the depth of the hydrocarbon feature to deabsorb the continuum, following the Galactic relation AL=(12±4)τ3.4 [32], the resulting AGN intrinsic luminosity would exceed the source bolometric emission. The abundance of hydrocarbons dust grains is therefore higher in IRAS 20551-4250 than in the Galactic ISM. (4) The X-ray column density corresponds to an AV(X) at least a factor of two larger than that expected from our mid-IR modelling (τL,τ6). Irrespectively of the actual dust extinction law, any reasonable value of the mid-IR optical depth implies a lower dust-to-gas ratio than in the Milky Way ISM. As a ULIRG is by definition a dust-rich system, this apparent inconsistency can be explained in two ways, which are in part complementary. (i) Due to orientation effects, our line of sight pierces through the regions of highest column density in the circumnuclear absorber. (ii) There is little coupling between the dust and gas components because the bulk of X-ray absorption occurs close to the central engine, in a region comparable in size with the dust sublimation radius.Another line of investigation into the physical properties of the circumnuclear medium relies on the rotation diagram of the warm molecular hydrogen, from which we can derive the temperature, column density, and mass of the gas. To this purpose, the observed fluxes listed in Table1 are converted into column densities of the Jth state (Nj) assuming the LTE regime, an ortho-to-para ratio of 3, a point-like source, and no extinction [23] (see also [33]). While Higdon and collaborators [23] construct the rotation diagram for IRAS 20551-4250 using only the H2 S(1) and S(3) transitions detected in the low-resolution mode, here we make use of high-resolution detections and add the S(0) and S(2) lines. In this way, the parameters derived from the linear fitting in Figure 6 are more reliable and accurate. Clearly a single temperature model applies to the S(1), S(2), and S(3) transitions, with the excitation temperature (Tex) given by minus the reciprocal of the slope, while the total H2 column density (NH2) depends on the fit normalization and the partition functions of the populations. We thus obtain Tex=347-6+5 K, NH2=(2.7×1020) cm−2 and a corresponding H2 mass of MH2=6.8×108M⊙. (Uncertainties on Tex and NH2 are estimated by refitting the data while varying the S(1) and S(3) fluxes within their errors.) Our estimate gives a higher temperature (~8%) and correspondingly lower gas mass with respect to [23]. The inclusion of the S(0) line requires some caution, as it is detected with the IRS-LH slit, much larger (11.1′′) than the SH one (4.7′′) that samples the previous fluxes. For completeness, we plot in Figure 6 the observed S(0) value as a cross and the value corrected for the relative slit apertures SH/LH as a green point. Including also the corrected S(0) significantly steepens the linear regression and leads to a lower temperature Tex=303 K, hence doubling the column density and mass. As a matter of fact, a single-temperature component is not suitable to properly reproduce complex systems such as IRAS 20551-4250, and a multitemperature model should be adopted [23, 33]. Unfortunately the nondetection of higher level transitions (e.g., from S(4) to S(7)), or their blending with PAH features, prevents us from modelling a hot (T≃1000 K) H2 component. None the less, as an exercise, we can exclude the S(3) point and adopt the corrected S(0) in the linear regression. We now trace a colder H2 component with Tex=265 K, characterized by a huge, likely unphysical (A mass for the molecular hydrogen larger than ~109M⊙ would correspond to enormous star formation rates, with an IR radiation even greater than IRAS 20551-4250 bolometric luminosity.) gas mass (MH2~2×109M⊙). We remind that ortho-H2 exists only in states of odd rotational quantum number, while para-H2 is represented only by states of even J; therefore the S(1)/S(3) line ratio is independent from the ortho-to-para ratio. The measured S(1)/S(3) is 1.29±0.07, in agreement with the theoretical value of 1.23 computed for no extinction and Tex=350 K. From this, we conclude that the obscuring material along the line of sight producing the continuum reddening, deep features, and X-ray absorption lies in between the AGN and molecular H2 clouds and is possibly associated with the SB region.Figure 6
H2 rotation diagram: for each transition the column density Nj normalized to the statistical weight of the state (gj) is plotted as a function of the upper level energy [34]. The dashed line represents the best LTE fit obtained for S(1), S(2), and S(3) transitions (black points). For completeness we plot also the S(0) observation (black cross) and the measurement corrected for aperture effects (green point).


## 3.1. The Extinction Law

Figure4 shows the observed spectrum of IRAS 20551-4250 between 3 and 8 μm once the ground-based VLT data are combined with the first part of the Short-Low Spitzer/IRS orders. We did not apply any cross-scaling factor, since it would be a very complex task and we are confident about the reliability of the absolute flux calibrations, which are affected only by small relative errors (~10%; [7, 11, 17]). From a visual inspection of the three spectra, it is clear that the observed continuum slope, which is expected to be heavily shaped by the AGN contribution, cannot be reproduced with a single spectral index over the whole range under investigation. In our separate L-band and 5–8 μm studies, we have assumed an intrinsic slope of Γ=1.5 for the AGN hot-dust continuum and then applied a power-law extinction of the form τ(λ)∝λ-1.75 [18]. This screen-like absorption is possibly due to colder dust in the outer layers of the putative torus, or it might be associated with some star-formation region in the circumnuclear environment of the host galaxy. It is now evident that the latter assumptions do not allow us to reproduce simultaneously the AGN emission for the different datasets. In fact, by extending the best-fitting AGN model from the L-band to longer wavelengths, we largely overestimate the 8 μm observed flux. Of course, it is possible that the intrinsic AGN spectrum is more complex than the one adopted in our spectral decomposition. A more detailed analysis should allow for different dust components with individual temperature and emissivity, and also radiative transfer effects need to be taken into account. However, a broken power-law trend seems to describe with fairly good precision the observed spectral curvature. Interestingly, we can try to obtain some empirical (a posteriori) indication about the extinction suffered by the AGN hot-dust emission. Virtually all the available extinction curves in this wavelength range, in fact, are derived from lines of sight within our own Galaxy, while the composition of the interstellar medium (ISM) in active galaxies is expected to be very different, as proved, for example, by the dust-to-gas ratios estimated through a comparison between the mid-IR dust obscuration and the gas column density in the X-rays of these objects  [26, 27].We have therefore fitted all the three bands allowing for different slopes of the observed AGN continuum. TheM-band is clearly poorly constrained and the value of Γ is frozen to give a smooth connection among the spectral intervals for both the AGN and SB templates. We have then computed the trend of the extinction law by making the easiest assumption about the intrinsic shape of the hot-dust emission, that is, the simple power-law dependence of the flux density from wavelength. Figure 5 shows the comparison between two possible extinction laws, corresponding to different values of the intrinsic Γ, and three standard Galactic curves. Although no conclusive indication can be drawn, the similarity is quite remarkable and suggests that the dust extinction law and the AGN intrinsic continuum are partially degenerate. This anyway does not affect the quantitative results of our analysis, as the AGN and SB 6 μm to bolometric corrections are averaged over large samples and this systematic effect is greatly reduced (see also the discussion on the AGN template and dust extinction in [11]).Figure 5
Dust extinction laws obtained by assuming a single power-law form (fν∝λΓ) to reproduce the intrinsic AGN hot-dust emission over the 3–8 μm band. The solid lines correspond to different choices of the spectral index: blue for Γ=2, and red for Γ=3. The dashed lines are standard Galactic extinction curves for comparison: cyan for [18], orange for Chiar and Tielens [28], and green for Nishiyama et al. [29, 30]. The relation with the extinction in visual magnitudes plotted on the vertical axis is based on the latter works, and all the curves are normalized in order to have the same value at 3 μm. While the exact extinction shape is not so important in the L-band, at 5–8 μm (and most likely beyond, with the presence of the silicate absorption feature) the difference in terms of optical depth in the different cases can be as large as a factor of 3. However, it seems quite hard to obtain such a large dust extinction around 6 μm to be consistent with the gas column density of nearly ~1024 cm−2 measured in the X-rays.


## 3.2. Gas and Dust Content

To further constrain the absorbing/emitting medium in IRAS 20551-4250, we attempted at estimating the gas column density by means of a multiwavelength approach. We start by assuming a Galactic gas-to-dust ratio [31]:(1)NHAV=1.9×1021mag-1cm-2
with AL~0.04AV and A6~0.012AV. We then employ the following estimates: (a) the column density of the gas absorbing the X-ray radiation directly measured in the 2–10 keV energy range [14], (b) the L-band and 6 μm optical depth assessed through the continuum reddening in our decomposition method [11], and (c) the optical depth of the 3.4 μm hydrocarbon feature [7]. The corresponding visual extinction values are listed in Table 2.Table 2
Extinction obtained by assuming a gas-to-dust ratio as in (1). Columns: (1) observational band used for the direct measurement with the relative reference. (2) and (3) L-band and 6 μm optical depth for the AGN continuum as obtained with our spectral decomposition model. (4) Optical depth of the aliphatic hydrocarbon feature once corrected for the SB dilution. (5) Gas column density measured from the X-ray spectrum. (6) Optical extinction predicted by Galactic relations (see text for details).
Extinction estimatesBandτLτ6τ3.4NH cm−2ExpectedAV mag3μm [9]82206μm [15]1.21103.4μm [9]1.54502–10 keV [11]8×1023420From a comparison among these independentAV predictions, we can draw four main considerations. (1) Independently from the adopted proxy, we infer a huge extinction in the visual band, which naturally explains the optical misclassification of IRAS 20551-4250. (2) As discussed in the previous section, a flatter extinction law over the 3–8 μm range with respect to a steep power-law trend [18] seems to be more appropriate to reproduce the observed AGN emission. Otherwise, the values of AV derived from the 3 μm and 6 μm reddening differ by a factor of two. (3) By using the depth of the hydrocarbon feature to deabsorb the continuum, following the Galactic relation AL=(12±4)τ3.4 [32], the resulting AGN intrinsic luminosity would exceed the source bolometric emission. The abundance of hydrocarbons dust grains is therefore higher in IRAS 20551-4250 than in the Galactic ISM. (4) The X-ray column density corresponds to an AV(X) at least a factor of two larger than that expected from our mid-IR modelling (τL,τ6). Irrespectively of the actual dust extinction law, any reasonable value of the mid-IR optical depth implies a lower dust-to-gas ratio than in the Milky Way ISM. As a ULIRG is by definition a dust-rich system, this apparent inconsistency can be explained in two ways, which are in part complementary. (i) Due to orientation effects, our line of sight pierces through the regions of highest column density in the circumnuclear absorber. (ii) There is little coupling between the dust and gas components because the bulk of X-ray absorption occurs close to the central engine, in a region comparable in size with the dust sublimation radius.Another line of investigation into the physical properties of the circumnuclear medium relies on the rotation diagram of the warm molecular hydrogen, from which we can derive the temperature, column density, and mass of the gas. To this purpose, the observed fluxes listed in Table1 are converted into column densities of the Jth state (Nj) assuming the LTE regime, an ortho-to-para ratio of 3, a point-like source, and no extinction [23] (see also [33]). While Higdon and collaborators [23] construct the rotation diagram for IRAS 20551-4250 using only the H2 S(1) and S(3) transitions detected in the low-resolution mode, here we make use of high-resolution detections and add the S(0) and S(2) lines. In this way, the parameters derived from the linear fitting in Figure 6 are more reliable and accurate. Clearly a single temperature model applies to the S(1), S(2), and S(3) transitions, with the excitation temperature (Tex) given by minus the reciprocal of the slope, while the total H2 column density (NH2) depends on the fit normalization and the partition functions of the populations. We thus obtain Tex=347-6+5 K, NH2=(2.7×1020) cm−2 and a corresponding H2 mass of MH2=6.8×108M⊙. (Uncertainties on Tex and NH2 are estimated by refitting the data while varying the S(1) and S(3) fluxes within their errors.) Our estimate gives a higher temperature (~8%) and correspondingly lower gas mass with respect to [23]. The inclusion of the S(0) line requires some caution, as it is detected with the IRS-LH slit, much larger (11.1′′) than the SH one (4.7′′) that samples the previous fluxes. For completeness, we plot in Figure 6 the observed S(0) value as a cross and the value corrected for the relative slit apertures SH/LH as a green point. Including also the corrected S(0) significantly steepens the linear regression and leads to a lower temperature Tex=303 K, hence doubling the column density and mass. As a matter of fact, a single-temperature component is not suitable to properly reproduce complex systems such as IRAS 20551-4250, and a multitemperature model should be adopted [23, 33]. Unfortunately the nondetection of higher level transitions (e.g., from S(4) to S(7)), or their blending with PAH features, prevents us from modelling a hot (T≃1000 K) H2 component. None the less, as an exercise, we can exclude the S(3) point and adopt the corrected S(0) in the linear regression. We now trace a colder H2 component with Tex=265 K, characterized by a huge, likely unphysical (A mass for the molecular hydrogen larger than ~109M⊙ would correspond to enormous star formation rates, with an IR radiation even greater than IRAS 20551-4250 bolometric luminosity.) gas mass (MH2~2×109M⊙). We remind that ortho-H2 exists only in states of odd rotational quantum number, while para-H2 is represented only by states of even J; therefore the S(1)/S(3) line ratio is independent from the ortho-to-para ratio. The measured S(1)/S(3) is 1.29±0.07, in agreement with the theoretical value of 1.23 computed for no extinction and Tex=350 K. From this, we conclude that the obscuring material along the line of sight producing the continuum reddening, deep features, and X-ray absorption lies in between the AGN and molecular H2 clouds and is possibly associated with the SB region.Figure 6
H2 rotation diagram: for each transition the column density Nj normalized to the statistical weight of the state (gj) is plotted as a function of the upper level energy [34]. The dashed line represents the best LTE fit obtained for S(1), S(2), and S(3) transitions (black points). For completeness we plot also the S(0) observation (black cross) and the measurement corrected for aperture effects (green point).


## 4. Discussion

We can now compile all the different aspects of the previous analysis in order to construct a comprehensive picture of the absorbing/emitting medium in IRAS 20551-4250. A stratified structure of the circumnuclear material, involving the different spatial scales (see Figure1), can well explain all the observational evidence. The basic ingredients are summarized as follows: (i) the hot dust component, where the grains are transiently heated to temperatures close to the sublimation limit, can be associated with both the inner surface of the AGN torus and the starburst environment; however, due to the different spatial concentration of the hot dust in the two cases, the resulting nearly power-law continuum is much more intense for an AGN. (ii) A cold dust component and a large amount of gas are required to produce the continuum reddening, the deep absorption features (aliphatic hydrocarbon, CO, HAC, silicates), as well as the X-ray absorption. Consequently, the inferred properties of the circumnuclear absorber point to an optically thick screen along the line of sight towards a point-like source such as a bright AGN, rather than to a diffuse dust distribution spatially mixed with the energy source (as in a starburst). Moreover, this dust screen must be geometrically thick, since a large covering factor would be consistent with the absence of high-ionization coronal lines (e.g., [Ne v], [O iv]). These properties are typical of the AGN putative torus, which is located at the spatial scales ranging from a few pc to several tens of pc from the central engine. The obscuring medium is also expected to be sufficiently close to the central AGN (i.e., with the inner edge of the torus falling within the dust sublimation radius) to allow for the observed gas over-abundance. On farther scales (several hundreds to a few thousands pc), molecular clouds are associated with the starburst event. Here, in addition to warm thermal dust, the PAH grains can survive and give rise to the typical set of emission features usually employed as SF tracers. Furthermore, with the increasing optical depth within the individual star-forming clouds, photodissociation becomes eventually slow and inefficient, so that hydrogen also appears in the molecular state. This explains the unextincted H2 pure rotational lines detected in the mid-IR. A cartoon of the circumnuclear environment is shown in Figure 7.Figure 7
Schematic view of the possible spatial distribution of the absorbing/emitting medium in IRAS 20551-4250. The X-ray absorbing gas (in light yellow) is located within the dust sublimation radius and represents the inner edge of the axisymmetric (toroidal) absorber. The dusty regions emitting the thermal radiation are in orange (for both AGN torus and SB clouds). A compact, dense screen of cold dusty gas (in blue) forms the outer layer of the AGN absorber and is responsible for both continuum reddening and deep absorption troughs. PAH features and H2 lines come from diffuse material spatially mixed with young stars (yellow/orange clouds). Due to the large spatial extent, only moderate internal obscuration is affecting the SB environment.Of course, the qualitative considerations driven by the mid-IR spectral properties are not sufficient to fully understand the multiple physical conditions characterizing such an extreme source. In order to probe the nuclear environment and its surroundings, a detailed spectral analysis at different wavelengths is needed, possibly resolving and disentangling the different spatial scale. This would make it possible to address the problems connected to the uncertain shape of both the intrinsic and the observed AGN continuum, and therefore to better constrain the actual extinction law. At present, even the joint modelling of the ~2–20μm spectral energy distribution (SED) is frustrated by the spread of the signal-to-noise ratio (S/N) and the relative flux calibration among ground-based and space facilities involved in the observations. The forthcoming James Webb Space Telescope (JWST) is the ideal instrument to probe the mid-IR SED of local ULIRGs, offering the opportunity of high-quality data obtained with relatively short exposures. For example, a high-resolution (R~2700) observation of IRAS 20551-4250 with NIRspec [35] centred at 3.5 μm requires only ~300 sec of exposure time (We used the exposure time calculator available at http://jwstetc.stsci.edu/etc/input/nirspec/spectroscopic/ with the following settings: G395H grating plus F290LP filter, average thermal background, and zodiacal light.) to reach a S/N~150 per resolution element. At longer wavelengths, the medium-resolution spectrometer MIRI [36] will ensure similarly high performances. Besides the unique settings available (among which integral field unit and multi-shutter array), JWST will fully cover the ~1–25 μm range, allowing us to detect and resolve even faint and/or blended features. In this context, the separation of highly excited rotational levels of the CO ν=1-0 band would be particularly suitable to constrain the dense gas temperature, density, and kinematics within the circumnuclear environment (see, e.g., [37]).


## 5. Conclusions and Remarks

In the present work we have first reviewed the properties of IRAS 20551-4250, a prototypical local ULIRG observed by our group in theL- and M-band with ISAAC at the VLT. The spectral analysis also includes the 5–8 μm spectrum obtained by Spitzer/IRS. According to the AGN/SB decomposition method we have developed in several previous papers [7, 10, 17], IRAS 20551-4250 turns out to be a composite source, dominated in the mid-IR by hot dust emission associated with deeply embedded BH accretion and characterized by a vigorous circumnuclear starburst which provides the main power supply to the whole system. We have then interpreted the key spectral properties of the source over the ~3–20 μm wavelength range (e.g., the reddening of the continuum, the presence of deep absorption features, the lack of high-ionization coronal lines, and the detection of H2 rotational transitions) in the framework of dust and gas spatial distribution and physical conditions. Our main results are the following. (i) The shape of the AGN intrinsic continuum is partly degenerate with the form of the extinction law. This is mainly evident beyond 5 μm. (ii) Given the gas amount inferred from X-ray observations, the central regions of IRAS 20551-4250 seem to have a dust-to-gas ratio much lower than the Galactic interstellar medium. (iii) Aliphatic hydrocarbon and HAC grains are over-abundant with respect to the local molecular clouds. (iv) A large covering of the nuclear engine likely prevents the ionization of the AGN narrow-line region and the excitation of fine-structure lines. Therefore, a screen of cold, dusty gas lies along the line of sight to the AGN, heavily extinguishing its spatially compact primary emission. (v) A large amount (MH2=6.8×108M⊙) of warm (Tex=347 K) molecular hydrogen and PAH grains are associated with the starburst environment on typical scales of a few kpc. The findings have been qualitatively interpreted by means of a simple geometrical configuration as the one sketched in Figure 7. We have finally described the great improvement in terms of sensitivity, spectral coverage, and resolution that will be achieved in the near future with the advent of JWST. This will also allow us to separate the different spatial scales and explore in larger detail the connection between the AGN and SB environments and the mutual feedback between the two physical processes.



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*Source: 783451-2012-02-22.xml*