The molecular gas properties in local Seyfert 2 galaxies

Salvestrini, Francesco; Gruppioni, C.; Hatziminaoglou, E.; Pozzi, F.; Vignali, C.; Casasola, V.; Paladino, R.; Aalto, S.; Andreani, P.; Marchesi, S.; Stanke, T.

doi:10.1051/0004-6361/202142760

Cited by 13 publications

(8 citation statements)

References 109 publications

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“…The naive expectation that AGN feedback expels and depletes the cold gas reservoir is certainly not borne out by much of the evidence. A variety of observations have demonstrated that active galaxies, covering a wide gamut of accretion power and evolutionary states, are categorically not gas-deficient compared to inactive, star-forming galaxies of similar stellar mass (e.g., Bertram et al 2007;Krips et al 2012;Xia et al 2012;Husemann et al 2017;Shangguan et al 2018Shangguan et al , 2020bShangguan & Ho 2019;Jarvis et al 2020;Yesuf & Ho 2020;Koss et al 2021;Salvestrini et al 2022). The cold gas shows no signs of being substantially disturbed in terms of its global kinematics (e.g., Ho et al 2008;Shangguan et al 2020b;Molina et al 2021), nor does it have any trouble forming stars (e.g., Bernhard et al 2019;Grimmett et al 2020;Jarvis et al 2020;Kirkpatrick et al 2020;Xie et al 2021;Zhuang et al 2021).…”

Section: Summary and Discussionmentioning

confidence: 99%

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Molina

Wang

et al. 2022

ApJ

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We analyze Multi-Unit Spectroscopic Explorer observations of nine low-redshift (z < 0.1) Palomar-Green quasar host galaxies to investigate the spatial distribution and kinematics of the warm, ionized interstellar medium, with the goal of searching for and constraining the efficiency of active galactic nucleus (AGN) feedback. After separating the bright AGN from the starlight and nebular emission, we use pixel-wise, kpc-scale diagnostics to determine the underlying excitation mechanism of the line emission, and we measure the kinematics of the narrow-line region (NLR) to estimate the physical properties of the ionized outflows. The radial size of the NLR correlates with the AGN luminosity, reaching scales of ∼5 kpc and beyond. The geometry of the NLR is well-represented by a projected biconical structure, suggesting that the AGN radiation preferably escapes through the ionization cone. We find enhanced velocity dispersions (≳100 km s−1) traced by the Hα emission line in localized zones within the ionization cones. Interpreting these kinematic features as signatures of interaction between an AGN-driven ionized gas outflow and the host galaxy interstellar medium, we derive mass-outflow rates of ∼0.008–1.6 M ⊙ yr−1 and kinetic injection rates of ∼1039–1042 erg s−1, which yield extremely low coupling efficiencies of ≲10−3. These findings add to the growing body of recent observational evidence that AGN feedback is highly ineffective in the host galaxies of nearby AGNs.

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Section: Summary and Discussionmentioning

confidence: 99%

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Molina

Wang

et al. 2022

ApJ

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“…Ellison et al (2021b) used IFU data from EDGE-CALIFA and found evidence that AGN can deplete molecular gas in the central regions of their host galaxies. Maiolino et al (1997), Koss et al (2021) and Salvestrini et al (2022) found that, on global scales, there is no evidence for depletion of molecular gas mass in AGN compared to star forming galaxies. These works support the idea that AGN can affect the molecular gas content of central regions of the AGN without necessarily affecting the total amount of molecular gas mass of the host galaxy, i.e.…”

Section: The Role Of Agn Feedback In the Local Universementioning

confidence: 99%

“…The properties of molecular gas in AGN has been explored previously in many works on both global and resolved scales (Maiolino et al 1997;Saintonge et al 2017;Ellison et al 2021b;Koss et al 2021;Salvestrini et al 2022). Ellison et al (2021b) used IFU data from EDGE-CALIFA and found evidence that AGN can deplete molecular gas in the central regions of their host galaxies.…”

Section: The Role Of Agn Feedback In the Local Universementioning

confidence: 99%

The molecular gas main sequence and Schmidt–Kennicutt relation are fundamental, the star-forming main sequence is a (useful) byproduct

Baker

Maiolino

Belfiore

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We investigate the relationship between the star formation rate (SFR), stellar mass (M*) and molecular gas mass ($M_{H_2}$) for local star-forming galaxies. We further investigate these relationships for high-z (z=1-3) galaxies and for the hosts of a local sample of Active Galactic Nuclei (AGN). We explore which of these dependencies are intrinsic and which are an indirect by-product by employing partial correlation coefficients and random forest regression. We find that for local star-forming galaxies, high-z galaxies, and AGN host galaxies, the Schmidt-Kennicutt relation (SK, between $M_{H_2}$ and SFR), and the Molecular Gas Main Sequence (MGMS, between $M_{H_2}$ and M*) are intrinsic primary relations, while the relationship between M* and SFR, i.e. the Star-Forming Main Sequence (SFMS), is an indirect by-product of the former two. Hence the Star-Forming Main Sequence is not a fundamental scaling relation for local or high-redshift galaxies. We find evidence for both the evolution of the MGMS and SK relation over cosmic time, where, at a given stellar mass, the higher the redshift, the greater the molecular gas mass and the star formation efficiency. We offer a parameterisation of both the MGMS and SK relation’s evolution with redshift, showing how they combine to form the observed evolution of the SFMS. In addition, we find that the local AGN host galaxies follow an AGN-MGMS relation (as well as a AGN-SK relation), where the MGMS is offset to lower $M_{H_2}$ for a given M* compared to local SF galaxies.

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“…Conversely, local Seyferts often show ongoing or recent star formation (e.g., Davies et al 2007;Esquej et al 2014), and compelling evidence indicates that the more luminous AGNs are commonly hosted in galaxies with star formation rates (SFRs) similar to those reported in typical inactive spirals (Harrison et al 2012;Rosario et al 2012Rosario et al , 2013Husemann et al 2014;Zhang et al 2016;Stanley et al 2017;Bernhard et al 2019;Schulze et al 2019;Grimmett et al 2020;Koss et al 2021;Vietri et al 2022), or even comparable to those of starbursts (Young et al 2014;Bernhard et al 2016;Pitchford et al 2016;Shangguan et al 2020a;Kirkpatrick et al 2020;Xie et al 2021). The increasing availability of cold-gas observations targeting the carbon monoxide (CO) and neutral atomic hydrogen (H I) emission lines (e.g., Evans et al 2001Evans et al , 2006Scoville et al 2003;Ho et al 2008;Xia et al 2012;Brusa et al 2015;Husemann et al 2017;Kakkad et al 2017;Husemann et al 2019a;Shangguan et al 2020b;Salvestrini et al 2022) or measurements from indirect tracers based on dust absorption and emission (e.g., Lutz et al 2018;Shangguan et al 2018;Yesuf & Ho 2019Zhuang & Ho 2020) support the view that AGNs are preferentially observed in gas-rich and highly star-forming systems (Florez et al 2020;Jarvis et al 2020;…”

Section: Introductionmentioning

confidence: 99%

Enhanced Star Formation Efficiency in the Central Regions of Nearby Quasar Hosts

Molina

Wang

et al. 2023

ApJ

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We combine Atacama Large Millimeter/submillimeter Array and Multi Unit Spectroscopic Explorer observations tracing the molecular gas, millimeter continuum, and ionized gas emission in six low-redshift (z ≲ 0.06) Palomar–Green (PG) quasar host galaxies to investigate their ongoing star formation at roughly kiloparsec-scale resolution. The AGN contribution to the cold dust emission and the optical emission-line flux is carefully removed to derive spatial distributions of the star formation rate (SFR), which, complemented with the molecular gas data, enables the mapping of the depletion time (t dep). We report ubiquitous star formation activity within the quasar host galaxies, with the majority of the ongoing star formation occurring in the galactic center. The rise of the SFR surface density (ΣSFR) toward the nucleus is steeper than that observed for the cold molecular gas surface density, reaching values up to ΣSFR ≈ 0.15–0.80 M ⊙ yr−1 kpc−2. The gas in the nuclear regions is converted into stars at a shortened depletion time (t dep ≈ 0.2–2.0 Gyr), suggesting that those zones can be deemed as starbursts. At large galactocentric radius, we find that the ongoing star formation takes place within spiral arms or H ii region complexes, with an efficiency comparable to that reported for nearby inactive spirals (t dep ≈ 1.8 Gyr). We find no evidence of star formation activity shutoff in the PG quasar host galaxies. On the contrary, these observations shed light on how the central environments of galaxies hosting actively accreting supermassive black holes build up stellar mass.

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The molecular gas properties in local Seyfert 2 galaxies

Cited by 13 publications

References 109 publications

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

The molecular gas main sequence and Schmidt–Kennicutt relation are fundamental, the star-forming main sequence is a (useful) byproduct

Enhanced Star Formation Efficiency in the Central Regions of Nearby Quasar Hosts

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