Circumnuclear Star Formation and AGN Activity: Clues from Surface Brightness Radial Profile of PAHs and [
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Esparza-Arredondo, Donají; González‐Martín, O.; Dultzin, D.; Alonso‐Herrero, A.; Almeida, C. Ramos; Díaz-Santos, T.; García-Bernete, I.; Martínez-Paredes, M.; Rodríguez-Espinosa, J. M.

doi:10.3847/1538-4357/aabcbc

Cited by 27 publications

(25 citation statements)

References 110 publications

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“…We find that the average accretion rate roughly follows a linear proportionality  á ñ µ á ñ M SFR BH for star formation within small radii, but time variability decouples AGN activity and global star formation. These results are consistent with observations in the local universe indicating correlations between nuclear star formation and instantaneous black hole accretion in individual systems but no clear connection to global star formation (Davies et al 2007;Diamond-Stanic & Rieke 2012;LaMassa et al 2013;Esquej et al 2014;Esparza-Arredondo et al 2018).…”

Section: The Sfr-agn Connectionsupporting

confidence: 90%

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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We present cosmological hydrodynamic simulations of a quasar-mass halo (M halo ≈ 10 12.5 M e at z = 2) that for the first time resolve gas transport down to the inner 0.1 pc surrounding the central massive black hole. We model a multiphase interstellar medium including stellar feedback by supernovae, stellar winds, and radiation, and a hyper-Lagrangian refinement technique increasing the resolution dynamically approaching the black hole. We do not include black hole feedback. We show that the subpc inflow rate (1) can reach ∼6 M e yr −1 roughly in steady state during the epoch of peak nuclear gas density (z ∼ 2), sufficient to power a luminous quasar, (2) is highly time variable in the pre-quasar phase, spanning 0.001-10 M e yr −1 on Myr timescales, and (3) is limited to short (∼2 Myr) active phases (0.01-0.1 M e yr −1 ) followed by longer periods of inactivity at lower nuclear gas density and late times (z ∼ 1), owing to the formation of a hot central cavity. Inflowing gas is primarily cool, rotational support dominates over turbulence and thermal pressure, and star formation can consume as much gas as provided by inflows across 1 pc-10 kpc. Gravitational torques from multiscale stellar non-axisymmetries dominate angular momentum transport over gas self-torquing and pressure gradients, with accretion weakly dependent on black hole mass. Subpc inflow rates correlate with nuclear (but decouple from global) star formation and can exceed the Eddington rate by ×10. The black hole can move ∼10 pc from the galaxy center on ∼0.1 Myr. Accreting gas forms pc-scale, rotationally supported, obscuring structures often misaligned with the galaxy-scale disk. These simulations open a new avenue to investigate black hole-galaxy coevolution.

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Section: The Sfr-agn Connectionsupporting

confidence: 90%

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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“…However, PAHs are substantially formed in such environments, and a conclusive solution for this apparent dichotomy is, to the best of our knowledge, still unknown. In fact, observation of PAH emission in the kpc-scaled circumnuclear vicinity of AGNs have been commonly used to track the presence of star forming activity (Peeters et al 2004;Stierwalt et al 2014;Alonso-Herrero et al 2014;Esparza-Arredondo et al 2018). This is due to the fact that the UV radiation emitted from young massive O-and B-stars is able to vibrationally excite PAHs (Peeters et al 2004).…”

Section: Multiple Ionization Of Pahs In Agnsmentioning

confidence: 99%

“…The PAH IR features contribute to about 10% of the ISM luminosity in the 1-1000 µm range, accounting for a large fraction of the elemental C in star-forming galaxies (Lagache et al 2004). In addition, their luminosities are well correlated with star formation rates (Peeters et al 2004;Stierwalt et al 2014;Alonso-Herrero et al 2014;Esparza-Arredondo et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Monfredini

Quitián-Lara

Fantuzzi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The infrared signatures of polycyclic aromatic hydrocarbons (PAHs) are observed in a variety of astrophysical objects, including the circumnuclear medium of active galactic nuclei (AGNs). These are sources of highly energetic photons (0.2 to 10 keV), exposing the PAHs to a harsh environment. In this work, we examined experimentally the photoionization and photostability of naphthalene (C 10 H 8 ), anthracene (C 14 H 10 ), 2methyl-anthracene (C 14 H 9 CH 3 ) and pyrene (C 16 H 10 ) upon interaction with photons of 275, 310 and 2500 eV. The measurements were performed at the Brazilian Synchrotron Light Laboratory using time-of-flight mass-spectrometry (TOF-MS). We determined the absolute photoionization and photodissociation cross sections as a function of the incident photon energy; the production rates of singly, doubly and triply charged ions; and the molecular half-lives in regions surrounding AGNs. Even considering moderate X-ray optical depth values (τ = 4.45) due to attenuation by the dusty torus, the halflives are not long enough to account for PAH detection. Our results suggest that a more sophisticated interplay between PAHs and dust grains should be present in order to circumvent molecular destruction. We could not see any significant difference in the half-life values by increasing the size of the PAH carbon backbone, N C , from 10 to 16. However, we show that the multiple photoionization rates are significantly greater than the single ones, irrespective of the AGN source. We suggest that an enrichment of multiply charged ions caused by X-rays can occur in AGNs.

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“…Their IR light consists of several components, including continuum emission dominated by the re-processed radiation arising from the dusty torus, heated by the central AGN (Efstathiou & Rowan-Robinson 1995;Tristram et al 2007;Nenkova et al 2008;Mor et al 2009;Alonso-Herrero et al 2011;Siebenmorgen et al 2015;González-Martín et al 2019). In addition, their IR emission also show (i) a contribution due to star formation (Cid Fernandes et al 2001;Davies et al 2007;LaMassa et al 2012;Diamond-Stanic & Rieke 2012;García-Bernete et al 2016;Ruschel-Dutra et al 2017;Esparza-Arredondo et al 2018); (ii) polycyclic aromatic hydrocarbons, again related with star formation (Peeters et al 2004;Sani et al 2010;Gallimore et al 2010;Calzetti 2011;Jensen et al 2017); (iii) emission lines from fine structure ionic species (e.g., [Ne II] 12.8 µm, [Ne III] 15.5 µm, [Ne V] 14.5 µm, [S IV] 10.5 µm) (Ruschel-Dutra et al 2014), and silicate emissions or other molecular emission (Sturm et al 2005;Hao et al 2007;Roche et al 2007;Mason et al 2009;Gallimore et al 2010;Xie et al 2017;Menezes et al 2018), often associated with outflows (see, e.g., García-Burillo et al 2014;Morganti et al 2015;Alonso-Herrero et al 2019;Feruglio et al 2020).…”

Section: A Brief Historical Introductionmentioning

confidence: 99%

Turin-SyCAT: A multifrequency catalog of Seyfert galaxies

Peña-Herazo

Massaro

Chavushyan

et al. 2022

A&A

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Aims. We present the first release of Turin-SyCAT, a multifrequency catalog of Seyfert galaxies. Methods. We selected Seyfert galaxies considering criteria based on radio, infrared, and optical properties and starting from sources belonging to hard X-ray catalogs and surveys. We visually inspected optical spectra available for all selected sources. We adopted homogeneous and stringent criteria in the source selection aiming at reducing the possible contamination from other source classes. Results. Our final catalog includes 351 Seyfert galaxies distinguished in 233 type 1 and 118 type 2. Type 1 Seyfert galaxies appear to have mid-IR colors similar to blazars, but are distinguished from them by their radio-loudness. Additionally, Seyfert 2 galaxies have mid-IR colors more similar to quasars than BL Lac objects. As expected from their spectral properties, type 1 and 2 Seyfert galaxies show a clear distinction when using the u − r color. Finally, we found a tight correlation between the mid-IR fluxes at both 12 and 22 µm (i.e., F 12 and F 22 , respectively) and hard X-ray fluxes between 15 and 150 keV. Both Seyfert types appear to follow the same trend and share similar values of the ratios of F 12 and F 22 to F HX in agreement with expectations of the AGN unification scenario. Conclusions. As future perspectives, the Turin-SyCAT will then be used to search for heavily obscured Seyfert galaxies among unidentified hard X-ray sources, given the correlation between mid-IR and hard X-rays, and to investigate their large-scale environments.

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Circumnuclear Star Formation and AGN Activity: Clues from Surface Brightness Radial Profile of PAHs and [ S IV ]

Cited by 27 publications

References 110 publications

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Turin-SyCAT: A multifrequency catalog of Seyfert galaxies

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