Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Fazeli, Nastaran; Eckart, A.; Busch, G.; Yttergren, Madeleine; Combes, F.; Misquitta, Persis; Straubmeier, C.

doi:10.1051/0004-6361/201937092

Cited by 5 publications

(4 citation statements)

References 76 publications

(98 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our purely morphological study presented here can be seen complementary to IFU studies in the NIR of other nearby AGN as carried out for example, by Busch et al (2017), Fazeli et al (2020b) and Fazeli et al (2020a). These studies allow to derive a detailed view of the nuclear rings of nearby AGN such as the kinematics of their gas and stars.…”

Section: Discussionsupporting

confidence: 79%

Decomposition of the central structure of NGC 2273 in the NIR: A case study

Schey,

Heidt,

Pramskiy

et al. 2023

Astron Nachr

View full text Add to dashboard Cite

The Seyfert 2 galaxy NGC 2273 is a prime target to explore how active nuclei can be fed. It has a star‐forming innermost nuclear ring with a radius of 0.33kpc from where material may be funneled to the supermassive black hole in its center. In this article, we discuss high‐resolution adaptive optics aided JHKs images of NGC 2273 taken with the Large Binocular Telescope. Using Galfit we decomposed the innermost part of NGC 2273 into a core, a disk, and a ring using 58 parameters, 44 of them were used to describe the ring. The stellar mass of the ring was found to be 12 , a factor of 10 higher than its molecular gas mass. A continuous gas flow via the main stellar bar of NGC 2273 during the lifetime of the bar of up to 10 is required to provide the fuel for the formation of the stars unless the star formation efficiency is on the order of 10%. This does not affect the fueling of the nuclear source as the amount of molecular gas required for this low‐luminosity active galaxy to achieve this is on the order of only.

show abstract

Section: Discussionsupporting

confidence: 79%

Decomposition of the central structure of NGC 2273 in the NIR: A case study

Schey,

Heidt,

Pramskiy

et al. 2023

Astron Nachr

View full text Add to dashboard Cite

show abstract

“…-NGC 1433: Evidence for a central molecular outflow is reported by Combes et al (2013, in CO (3-2) 2019) study the cold molecular gas torus in the central region and do not find evidence for an outflow. Fazeli et al (2020) rules out the presence of an outflow in hot molecular and ionized gas.…”

Section: Individual Galaxiesmentioning

confidence: 99%

Frequency and nature of central molecular outflows in nearby star-forming disk galaxies

Stuber

Saito

Schinnerer

et al. 2021

A&A

View full text Add to dashboard Cite

Central molecular outflows in spiral galaxies are assumed to modulate their host galaxy’s star formation rate (SFR) by removing gas from the inner region of the galaxy. Outflows consisting of different gas phases appear to be a common feature in local galaxies, yet, little is known about the frequency of molecular outflows in main sequence galaxies in the nearby universe. We develop a rigorous set of selection criteria, which allow the reliable identification of outflows in large samples of galaxies. Our criteria make use of central spectra, position-velocity diagrams and velocity-integrated intensity maps (line-wing maps). We use this method on high-angular resolution CO (2–1) observations from the PHANGS-ALMA survey, which provides observations of the molecular gas for a homogeneous sample of 90 nearby main sequence galaxies at a resolution of ∼100 pc. We find correlations between the assigned outflow confidence and stellar mass or global SFR. We determine the frequency of central molecular outflows to be 25 ± 2% considering all outflow candidates, or 20 ± 2% for secure outflows only. Our resulting outflow candidate sample of 16−20 galaxies shows an overall enhanced fraction of active galactic nuclei (AGN) (50%) and bars (89%) compared to the full sample (galaxies with AGN: 24%, with bar: 61%). We extend the trend between mass outflow rates and SFR known for high outflow rates down to lower values (log10 Ṁout [M⊙ yr−1] < 0). Mass loading factors are of order unity, indicating that these outflows are not efficient in quenching the SFR in main sequence galaxies.

show abstract

“…The H2 2.1218 µm/Brγ emission-line ratio is commonly used to investigate the main source of the H2 excitation (Reunanen et al 2002;Rodríguez-Ardila et al 2004Storchi-Bergmann et al 2009;Riffel et al 2010aRiffel et al , 2014Riffel et al , 2013aRiffel 2020b;Colina et al 2015;Schönell et al 2014Schönell et al , 2019Dahmer-Hahn et al 2019b;Fazeli et al 2020). Small values For all galaxies, north is up and east is to the left.…”

Section: Line Ratiosmentioning

confidence: 99%

The AGNIFS survey: distribution and excitation of the hot molecular and ionized gas in the inner kpc of nearby AGN hosts

Riffel

Storchi‐Bergmann

Riffel

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We use the Gemini NIFS instrument to map the H2 2.1218 μm and Brγ flux distributions in the inner 0.04–2 kpc of a sample of 36 nearby active galaxies (0.001 ≲ z ≲ 0.056) at spatial resolutions from 4 to 250 pc. We find extended emission in 34 galaxies. In ∼55 per cent of them, the emission in both lines is most extended along the galaxy major axis, while in the other 45 per cent the extent follows a distinct orientation. The emission of H2 is less concentrated than that of Brγ, presenting a radius that contains half of the flux 60 per cent greater, on average. The H2 emission is driven by thermal processes – X-ray heating and shocks – at most locations for all galaxies, where $0.4<\rm H_2/Br\gamma <6$. For regions where H2/Brγ > 6 (seen in 40 per cent of the galaxies), shocks are the main H2 excitation mechanism, while in regions with H2/Brγ < 0.4 (25 per cent of the sample) the H2 emission is produced by fluorescence. The only difference we found between type 1 and type 2 AGN was in the nuclear emission-line equivalent widths, that are smaller in type 1 than in type 2 due to a larger contribution to the continuum from the hot dusty torus in the former. The gas masses in the inner 125 pc radius are in the range 101 − 104 M⊙ for the hot H2 and 103 − 106 M⊙ for the ionised gas and would be enough to power the AGN in our sample for 105 − 108 yr at their current accretion rates.

show abstract

Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Cited by 5 publications

References 76 publications

Decomposition of the central structure of NGC 2273 in the NIR: A case study

Decomposition of the central structure of NGC 2273 in the NIR: A case study

Frequency and nature of central molecular outflows in nearby star-forming disk galaxies

The AGNIFS survey: distribution and excitation of the hot molecular and ionized gas in the inner kpc of nearby AGN hosts

Contact Info

Product

Resources

About