The Ubiquity of AGN Winds in Seyfert 1 Galaxies at Low Redshift

Torres‐Papaqui, J. P.; Coziol, R.; Romero-Cruz, F. J.; Robleto-Orús, A. C.; Escobar-Vásquez, Gabriela; Morales-Vargas, A.; Trejo-Alonso, J. J.; Chow-Martínez, M.; Cutiva-Alvarez, Karla Alejandra

doi:10.3847/1538-3881/abae5a

Cited by 8 publications

(22 citation statements)

References 63 publications

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“…However, the shift in colour happening at high redshift contradicts this explanation, since Sy1s (mostly spiral galaxies) appear only at low redshifts (cf. Torres-Papaqui et al 2020). Also, the fact that the W2 fluxes show no evidence of a similar shift in W2-W3 at this redshift suggests this particularity of the W1-W2 colour must be related to a change in the SED of the QSOs.…”

Section: Sample and Datamentioning

confidence: 82%

“…However, this would be difficult to explain, considering the spectral similarities and metallicities of QSOs at any redshift. Related topics consist in searching for correlations between the BH accretion rate (BHAR) and star formation rate (SFR) in AGNs at different redshifts (e.g., McDonald et al 2021) and determining what role (if any; e.g., Peng 2007; Jahnke & Macciò 2011) AGN feedback (outflows or winds) play in establishing the 𝑀 BH − 𝜎 relation (e.g., Harrison et al 2018;Torres-Papaqui et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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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: Sample and Datamentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

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

Cutiva-Alvarez¹,

Coziol²,

Torres‐Papaqui³

2023

Preprint

View full text Add to dashboard Cite

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“…The other possible connection between GV galaxies and AGNs is that both of the two populations may be experiencing "morphological compaction" (e.g., Barro et al 2013Barro et al , 2015Kocevski et al 2017;Lu et al 2021). But till now, there has been little direct evidence about AGN activities inevitably suppressing the global galaxy star formation, especially at high redshifts (e.g., Torres-Papaqui et al 2020). There are indeed some studies about AGN-driven star-formation quenching in the local universe.…”

Section: Agn Lifetimes In Galaxies Of Different Extinction-corrected ...mentioning

confidence: 99%

AGN lifetimes in UV-selected galaxies: a clue to supermassive black hole-host galaxy coevolution

Lin,

Xue,

Fang

et al. 2021

Preprint

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The coevolution between supermassive black holes (SMBHs) and their host galaxies has been proposed for more than a decade, albeit with little direct evidence about black hole accretion activities regulating galaxy star formation at z > 1. In this paper, we study the lifetimes of X-ray active galactic nuclei (AGNs) in U V -selected red sequence (RS), blue cloud (BC) and green valley (GV) galaxies, finding that AGN accretion activities are most prominent in GV galaxies at z ∼ 1.5 − 2, compared with RS and BC galaxies. We also compare AGN accretion timescales with typical color transition timescales of U V -selected galaxies. We find that the lifetime of GV galaxies at z ∼ 1.5 − 2 is very close to the typical timescale when the AGNs residing in them stay in the high-accretionrate mode at these redshifts; for BC galaxies, the consistency between the color transition timescale and the black hole strong accretion lifetime is more likely to happen at lower redshifts (z < 1). Our results support the scenario where AGN accretion activities govern U V color transitions of host galaxies, making galaxies and their central SMBHs coevolve with each other.

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“…In order to study the possible relation between [OIII] profile wings and the central engine, we first need to estimate the black hole masses for the galaxies of our sample. Despite broad Hβ being the most commonly used for black hole mass estimate in AGNs (e.g., Greene & Ho 2005;Torres-Papaqui et al 2020), the 6dF survey lacks absolute flux calibration (e.g., Chen et al 2018). In addition, some galaxies present broad components of Hβ buried in the data noise, with certain objects exhibiting very irregular profiles (see Fig.…”

Section: Black Hole Massesmentioning

confidence: 99%

Spectroscopic study of the [OIII]$λ$5007 profile in Seyfert 1 galaxies

Schmidt,

Baravalle,

Rodríguez-Kamenetzky

2021

Preprint

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The spectra of active galactic nuclei usually exhibit wings in some emission lines, such as [OIII]λ λ 5007,4959, with these wings generally being blueshifted and related to strong winds and outflows. The aim of this work was to analyse the [OIII] emission lines in broad line Seyfert 1 (BLS1) galaxies in order to detect the presence of wings, and to study the [OIII] line properties and their possible connection with the central engine. In addition, we attempted to compare the black hole mass distribution in both BLS1 galaxies with symmetric and blue-asymmetric [OIII] profiles. For this purpose, we carried out a spectroscopic study of a sample of 45 nearby southern BLS1 galaxies from the 6 Degree Field Galaxy survey. The [OIII] emission lines were well fitted using a single Gaussian function in 23 galaxies, while 22 objects presented a wing component and required a double-Gaussian decomposition. By computing the radial velocity difference between the wing and core centroids (i.e. ∆v), we found 18 galaxies exhibiting blueshifted wings, 2 objects presenting red wings and 2 galaxies showing symmetric wings (∆v= 0). Moreover, ∆v was slightly correlated with the black hole mass. In addition, we computed the radial velocity difference of the blue-side full extension of the wing relative to the centroid of the core component through the blue emission parameter, which revealed a correlation with black hole mass, in agreement with previous results reported for narrow line galaxies. Finally, in our sample, similar black hole mass distributions were observed in both BLS1 galaxies with symmetric and blueshifted asymmetric [OIII] profiles.

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The Ubiquity of AGN Winds in Seyfert 1 Galaxies at Low Redshift

Cited by 8 publications

References 63 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

AGN lifetimes in UV-selected galaxies: a clue to supermassive black hole-host galaxy coevolution

Spectroscopic study of the [OIII]$λ$5007 profile in Seyfert 1 galaxies

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