Evidence for the connection between star formation rate and the evolutionary phases of quasars

Chen, Zhi-Fu; He, Zhicheng; Ho, Luis C.; Gu, Qiusheng; Wang, Tinggui; Zhuang, Ming-Yang; Liu, Guilin; Wang, Zhiwen

doi:10.1038/s41550-021-01561-3

Cited by 39 publications

(24 citation statements)

References 50 publications

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“…Outflows or jets driven by accreting supermassive black holes (active galactic nuclei; AGNs) are considered to play a crucial role in regulating star formation in massive galaxies, and thus, determine the evolution of galaxies in the universe (e.g., Scannapieco & Oh 2004;Förster Schreiber & Wuyts 2020). In particular, outflows are considered to be capable of quenching star formation activity by heating and/or sweeping dense and cold molecular regions in the interstellar medium (ISM), where stars form (negative AGN feedback; e.g., Sturm et al 2011;Chen et al 2022). Thus, galactic cold (neutral atomic and molecular) outflows are important phenomena in galaxy evolution (Veilleux et al 2020).…”

Section: Introductionmentioning

confidence: 99%

AGN-driven Cold Gas Outflow of NGC 1068 Characterized by Dissociation-sensitive Molecules

Tosaki

Takano

Harada

et al. 2022

ApJ

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Recent developments in (sub)millimeter facilities have drastically changed the amount of information obtained from extragalactic spectral scans. In this paper, we present a feature extraction technique using principal component analysis (PCA) applied to arcsecond-resolution (1.″0–2.″0 = 72–144 pc) spectral scan data sets for the nearby type-2 Seyfert galaxy NGC 1068, using Band 3 of the Atacama Large Millimeter/submillimeter Array. We apply PCA to 16 well-detected molecular line intensity maps convolved to a common 150 pc resolution. In addition, we include the [S iii]/[S ii] line ratio and [C i] 3 P 1–3 P 0 maps in the literature, both of whose distributions show a remarkable resemblance to that of a kiloparsec-scale biconical outflow from the central active galactic nucleus. We identify two prominent features: (1) central concentration at the circumnuclear disk (CND) and (2) two peaks across the center that coincide with the biconical outflow peaks. The concentrated molecular lines in the CND are mostly high-dipole molecules (e.g., H13CN, HC3N, and HCN). Line emissions from molecules known to be enhanced in an irradiated interstellar medium, CN, C2H, and HNC, show similar concentrations and extended components along the bicone, suggesting that molecule dissociation is a dominant chemical effect of the cold molecular outflow of this galaxy. Although further investigation should be made, this scenario is consistent with the faintness or absence of emission lines from CO isotopologues, CH3OH, and N2H+ in the outflow, which are easily destroyed by dissociating photons and electrons.

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Section: Introductionmentioning

confidence: 99%

AGN-driven Cold Gas Outflow of NGC 1068 Characterized by Dissociation-sensitive Molecules

Tosaki

Takano

Harada

et al. 2022

ApJ

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“…AGNs usually play an important role in forming and driving outflows which might further affect the star formation of their host galaxies (He et al 2019;Chen et al 2022;King & Pounds 2015, for a review). These outflows might interact with the ACM.…”

Section: Introductionmentioning

confidence: 99%

Density profile of ambient circumnuclear medium in Seyfert 1 galaxies

Wang,

He,

Mao

et al. 2022

Preprint

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The shape of the ambient circumnuclear medium (ACM) density profile can probe the history of accretion onto the central supermassive black hole in galaxies and the circumnuclear environment. However, due to the limitation of the instrument resolution, the density profiles of the ACM for most of galaxies remain largely unknown. In this work, we propose a novel method to measure the ACM density profile of active galactic nucleus (AGN) by the equilibrium between the radiation pressure on the warm absorbers (WAs, a type of AGN outflows) and the drag pressure from the ACM. We study the correlation between the outflow velocity and ionization parameter of WAs in each of the five Seyfert 1 galaxies (NGC 3227, NGC 3783, NGC 4051, NGC 4593, and NGC 5548), inferring that the density profile of the ACM is between n ∝ r −1.7 and n ∝ r −2.15 (n is number density and r is distance) from 0.01 pc to pc scales in these five AGNs. Our results indicate that the ACM density profile in Seyfert 1 galaxies is steeper than the prediction by the spherically symmetric Bondi accretion model and the simulated results of the hot accretion flow, but more in line with the prediction by the standard thin disk model.

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“…At this stage, an extreme starburst approaches its ends and the surrounding dust cocoon are being blown away. Indeed, a significant fraction of them are dust-reddened quasars (Farrah et al 2007;Urrutia et al 2009) and star formation rate depends on the existence of (Lo)BALs (Chen et al 2022). Prochaska et al (2013) and Jalan et al (2019) excluded BAL quasars from their samples.…”

Section: Introductionmentioning

confidence: 99%

Exploratory Study of the Transverse Proximity Effect around BAL Quasars

Misawa

Ishimoto

Kobu

et al. 2022

ApJ

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We aim to determine why there exists anisotropic H i absorption around quasars; i.e., the environments around quasars are highly biased toward producing strong H i absorption in the transverse direction while there exists a significant deficit of H i absorption within a few megaparsecs of quasars along the line of sight. The most plausible explanation for this opposite trend is that the transverse direction is shielded from quasar UV radiation by dust torus. However, a critical weakness of this explanation is that we do not have any information on the inclination angle of our sightline relative to the torus. In this study, we examine environments of quasars with broad-absorption troughs in their spectra (i.e., BAL quasars) because it is widely believed that BAL troughs are observed if the central continuum is viewed from the side through their powerful outflows near the dust torus. With closely separated 12 projected quasar pairs at different redshifts with a separation angle of θ < 120″, we examine H i absorption at foreground BAL quasars in the spectra of background quasars. We confirm that there exists optically thick gas around two of 12 BAL quasars, and that the mean H i absorption strength is EWrest ∼ 1 Å. This is consistent with past results of studies of non-BAL quasars, although not statistically significant. The origins of optically thick H i absorbers around BAL and non-BAL quasars could be different since their column densities are different by ∼3 orders of magnitude. A larger sample is required to narrow down possible scenarios explaining the anisotropic H i absorption around quasars.

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Evidence for the connection between star formation rate and the evolutionary phases of quasars

Cited by 39 publications

References 50 publications

AGN-driven Cold Gas Outflow of NGC 1068 Characterized by Dissociation-sensitive Molecules

AGN-driven Cold Gas Outflow of NGC 1068 Characterized by Dissociation-sensitive Molecules

Density profile of ambient circumnuclear medium in Seyfert 1 galaxies

Exploratory Study of the Transverse Proximity Effect around BAL Quasars

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