Absence of nuclear polycyclic aromatic hydrocarbon emission from a compact starburst: The case of the type-2 quasar Mrk 477

Almeida, C. Ramos; D., Esparza-Arredondo,; González‐Martín, O.; García-Bernete, I.; Pereira-Santaella, M.; Alonso‐Herrero, A.; Acosta–Pulido, J. A.; Bessiere, P. S.; Levenson, N. A.; Tadhunter, C. N.; Rigopoulou, D.; Martínez-Paredes, M.; Cazzoli, S.; García-Lorenzo, B.

doi:10.1051/0004-6361/202245409

Cited by 5 publications

(3 citation statements)

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“…After experimenting with different values for the PAH mass fraction, we used in our final modelling the minimal value 𝑞 PAH ∼ 0.45% (Draine & Li 2007). Indeed, even with high SFR in the QSO hosts, the PAH features should not play a great role due to the dominant AGN component (e.g., Marshall et al 2018); the fine dust producing PAH emission can also be destroyed by the intense AGN luminosity (Ramos Almeida et al 2023).…”

Section: Methods Of Analysismentioning

confidence: 99%

Probing the rapid formation of black holes and their galaxy hosts in QSOs

Cutiva-Alvarez¹,

Coziol²,

Torres‐Papaqui³

2023

Preprint

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Using the modelling code X-CIGALE, we reproduced the SEDs of 1,359 SDSS QSOs within the redshift range 0 < 𝑧 < 4, for which we have NIR/MIR fluxes with the highest quality and spectral data characterizing their SMBHs. Consistent with a rapid formation of the host galaxies, the star formation histories (SFHs) have small e-folding, at most 750 Myrs using an SFH function for Spiral or 1000 Myrs using one for Elliptical. Above 𝑧 ∼ 1.6, the two solutions are degenerate, the SEDs being dominated by the AGN continuum and high star formation rates (SFRs), typical of starburst galaxies, while at lower redshifts the starburst nature of the host, independent from its morphology, is better reproduced by an Spiral SFH. In general, the SFR increases with the redshift, the mass of the bulge, the AGN luminosity and Eddington ratio, suggesting there is no evidence of AGN quenching of star formation. Comparing the specific BHAR with specific SFR, all the QSOs at any redshift trace a linear sequence below the Eddington luminosity, in parallel and above the one-to-one relation, implying that QSOs are in a special phase of evolution during which the growth in mass of their SMBH is more rapid than the growth in mass of their galaxy hosts. This particular phase is consistent with a scenario where the galaxy hosts of QSOs in the past grew in mass more rapidly than their SMBHs, suggesting that a high star formation efficiency during their formation was responsible in limiting their masses.

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Section: Methods Of Analysismentioning

confidence: 99%

Probing the rapid formation of black holes and their galaxy hosts in QSOs

Cutiva-Alvarez¹,

Coziol²,

Torres‐Papaqui³

2023

Preprint

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“…Considering that the QSO2 outflows have dynamical timescales of ∼1-10 Myr (Bessiere & Ramos Almeida 2022;Ramos Almeida et al 2022), their properties should be compared with recent star formation. This can be probed using resolved stellar population analyses (Bessiere & Ramos Almeida 2022) or the polycyclic aromatic hydrocarbon (PAH) features detected in the mid-infrared, which are good probes of young and massive stars, but whose properties vary with distance from the AGN (García-Bernete et al 2022;Ramos Almeida et al 2023). These types of studies can reveal whether recent star formation is prevented or triggered by the outflows, or if both can simultaneously happen (Cresci et al 2015;Carniani et al 2016;Bessiere & Ramos Almeida 2022).…”

Section: A Multiphase View Of Outflowsmentioning

confidence: 99%

Multiphase characterization of AGN winds in five local type-2 quasars

Speranza,

Ramos Almeida,

Acosta-Pulido

et al. 2024

A&A

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We present MEGARA integral field unit (IFU) observations of five local type-2 quasars (QSO2s, z $ 0.1$) from the Quasar Feedback (QSOFEED) sample. These active galactic nuclei (AGN) have bolometric luminosities of $ erg s$^ $ and stellar masses of sim 1011 M$_ sun $. The LR-V grating of MEGARA allows us to explore the kinematics of the ionized gas through the O III lambda 5007 AA emission line. The nuclear spectra of the five QSO2s, extracted in a circular aperture of $ (sim 2.2 kpc) in diameter, matching the resolution of these seeing-limited observations, show signatures of high velocity winds in the form of broad (full width at half maximum, 1300leq FWHMleq 2240 and blueshifted components. We found that four out of the five QSO2s present outflows that we can resolve with our seeing-limited data, and they have radii ranging from 3.1 to 12.6 kpc. In the case of the two QSO2s with extended radio emission, we found that it is well aligned with the outflows, suggesting that low-power jets might be compressing and accelerating the ionized gas in these radio-quiet QSO2s. In the four QSO2s with spatially resolved outflows, we measured ionized mass outflow rates of 3.3-6.5 M$_ $ when we used S II -based densities, and of 0.7-1.6 M$_ $ when trans-auroral line-based densities were considered instead. We compared them with the corresponding molecular mass outflow rates (8 - 16 M$_ $), derived from CO(2-1) ALMA observations at 0.2 resolution. The cold molecular outflows carry more mass than their ionized counterparts. However, both phases show lower outflow mass rates than those expected from observational scaling relations where uniform assumptions on the outflow properties were adopted. This might be indicating that the AGN luminosity is not the only driver of massive outflows and/or that these relations need to be rescaled using accurate outflow properties (i.e., electron density and radius). We did not find a significant impact of the outflows on the global star formation rates when considering the energy budget of the molecular and ionized outflows together. However, spatially resolved measurements of recent star formation in these targets are needed in order to evaluate this fairly, considering the dynamical timescales of the outflows, of 3-20 Myr for the ionized gas and 1-10 Myr for the molecular gas.

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“…Luckily, the larger and neutral molecules that produce the 11.3 and 17 µm features are more resilient and they have been found to be enhanced in AGN relative to the short-wavelength PAHs, at least in Seyfert galaxies [253]. At higher AGN luminosities, it is not clear whether even the largest PAH molecules can survive the AGN radiation field [254][255][256], but upcoming JWST datasets will be crucial to study the viability of PAH features as the tracers of star formation in AGN of different luminosities, at different distances from the AGN, and in and out of the outflow/jet regions [257][258][259].…”

Section: Localised and Transient Impact On Gas And Star Formationmentioning

confidence: 99%

Observational Tests of Active Galactic Nuclei Feedback: An Overview of Approaches and Interpretation

Harrison,

Ramos Almeida

2024

Galaxies

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Growing supermassive black holes (Active Galactic Nuclei; AGN) release energy with the potential to alter their host galaxies and larger-scale environment; a process named “AGN feedback”. Feedback is a required component of galaxy formation models and simulations to explain the observed properties of galaxy populations. We provide a broad overview of observational approaches that are designed to establish the physical processes that couple AGN energy to the multi-phase gas, or to find evidence that AGN impact upon galaxy evolution. The orders-of-magnitude range in spatial, temporal, and temperature scales, requires a diverse set of observational studies. For example, studying individual targets in detail sheds light on coupling mechanisms; however, evidence for the long-term impact of AGN is better established within galaxy populations that are not necessarily currently active. We emphasise how modern surveys have revealed the importance of radio emission for identifying and characterising feedback mechanisms. At the achieved sensitivities, the detected radio emission can trace a range of processes, including a shocked interstellar medium caused by AGN outflows (driven by various mechanisms including radiation pressure, accretion disc winds, and jets). We also describe how interpreting observations in the context of theoretical work can be challenging, in part, due to some of the adopted terminology.

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Absence of nuclear polycyclic aromatic hydrocarbon emission from a compact starburst: The case of the type-2 quasar Mrk 477

Cited by 5 publications

References 50 publications

Probing the rapid formation of black holes and their galaxy hosts in QSOs

Probing the rapid formation of black holes and their galaxy hosts in QSOs

Multiphase characterization of AGN winds in five local type-2 quasars

Observational Tests of Active Galactic Nuclei Feedback: An Overview of Approaches and Interpretation

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