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

Riffel, Rogemar A.; Storchi‐Bergmann, Thaisa; Riffel, Rogério; Zakamska, Nadia L.; Ruschel-Dutra, D.; Schönell, Astor J.; Rosario, D. J.; Rodríguez-Ardila, A.; Fischer, Travis C.; Davies, R. I.; Dametto, N. Z.; Dahmer-Hahn, L G; Crenshaw, D. M.; Burtscher, L.; Bentz, Misty C.

doi:10.1093/mnras/stab998

Cited by 23 publications

(44 citation statements)

References 117 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…As reported previously, radio and nearinfrared (e.g. Rodríguez-Ardila et al 2004;Storchi-Bergmann et al 2009;Riffel et al 2010Riffel et al , 2021cMezcua et al 2015;Schönell et al 2017;Bianchin et al 2022, among others) observations have shown that AGNs harbor a neutral and warm (1000-3000 K) molecular gas reservoir. Therefore, a substantial proportion of neutral helium is expected in Seyfert nuclei.…”

Section: Ionization Correction Factorsupporting

confidence: 51%

“…In fact, Méndez-Delgado et al (2022) found that only 9/42 Galactic H regions have negligible contributions of 𝑦 0 (see also Delgado-Inglada et al 2014). Since AGNs present a large amount of molecular gas (e.g., Rodríguez-Ardila et al 2004;Davies et al 2005;Rodríguez-Ardila et al 2005;Mazzalay et al 2013;Riffel et al 2013Riffel et al , 2018Riffel et al , 2021cRamakrishnan et al 2019;Riffel et al 2019;Jarvis et al 2020;Alonso-Herrero et al 2020) and have similar ionization parameter (𝑈) other than SFs (Pérez-Montero et al 2019), a higher abundance of neutral and molecular gas are expected in AGNs as compared to H regions, which favors the presence of larger contribution of 𝑦 0 in the total helium abundance. In fact, radio observations have shown the existence of a gas neutral reservoir in the central parts of galaxies containing AGNs (e.g.…”

Section: Helium Abundancementioning

confidence: 98%

See 1 more Smart Citation

Chemical abundances in Seyfert galaxies -IX. Helium abundance estimates

Dors,

Valerdi,

Freitas-Lemes

et al. 2022

Preprint

View full text Add to dashboard Cite

For the first time, the helium abundance relative to hydrogen (He/H), which relied on direct measurements of the electron temperature, has been derived in the narrow line regions (NLRs) from a local sample of Seyfert 2 nuclei. In view of this, optical emission line intensities [3000 < 𝜆(Å) < 7000] of 65 local Seyfert 2 nuclei (𝑧 < 0.2), taken from Sloan Digital Sky Survey Data Release 15 and additional compilation from the literature, were considered. We used photoionization model grid to derive an Ionization Correction Factor (ICF) for the neutral helium. The application of this ICF indicates that the NLRs of Seyfert 2 present a neutral helium fraction of ∼ 50 per cent in relation to the total helium abundance. We find that Seyfert 2 nuclei present helium abundance ranging from 0.60 to 2.50 times the solar value, while ∼ 85 per cent of the sample present over-solar abundance values. The derived (He/H)-(O/H) abundance relation from the Seyfert 2 is stepper than that of star-forming regions (SFs) and this difference could be due to excess of helium injected into the Interstellar Medium by the winds of Wolf Rayet stars. From a regression to zero metallicity, by using Seyfert 2 estimates combined with SFs estimates, we obtained a primordial helium mass fraction 𝑌 p = 0.2441 ± 0.0037, a value in good agreement with the one inferred from the temperature fluctuations of the cosmic microwave background by the Planck Collaboration, i.e. 𝑌 𝑃𝑙𝑎𝑛𝑐𝑘 p = 0.2471 ± 0.0003.

show abstract

Section: Ionization Correction Factorsupporting

confidence: 51%

Section: Helium Abundancementioning

confidence: 98%

Chemical abundances in Seyfert galaxies -IX. Helium abundance estimates

Dors,

Valerdi,

Freitas-Lemes

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…This value is much larger than the nuclear gas masses of between 4 and 74 M measured by Mazzalay et al (2013) for a sample of six nearby low-luminosity AGN using data from VLT/SINFONI. A larger average gas mass, of 850 M , was reported by Riffel et al (2021) for a larger sample of nearby Seyfert 2 galaxies observed with Gemini/NIFS as part of the AGNIFS survey. Finally, our mass is similar to those measured for other QSO2s in the QSOFEED sample.…”

Section: The Warm Molecular Gasmentioning

confidence: 71%

Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

Speranza

Almeida

Acosta–Pulido

et al. 2022

A&A

View full text Add to dashboard Cite

We analyze Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 10 45.7 erg s −1 and a redshift of z = 0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 µm where low-ionization (Paα and Brδ), high ionization ([S XI]λ1.920 µm and [Si VI]λ1.963 µm) and warm molecular lines (from H 2 1-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low-and high-ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.3 (686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM)= 350-400 km s −1 , while Paα, Brδ, and [Si VI] are best fitted with two blue-shifted Gaussian components of FWHM∼800 and 1700 km s −1 , in addition to a narrow component of ∼300 km s −1 . We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to −840 km s −1 , in the south-east direction (PA∼125 • ), extending up to a distance of ∼3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of Ṁout, max =42-51 M yr −1 , and its kinetic power represents 0.1% of the quasar bolometric luminosity. VLA data of J0945 show extended radio emission (PA∼100 • ) that is aligned with the clumpy emission traced by the narrow component of the ionized lines up to scales of several kpc, and with the innermost part of the outflow (central ∼0.4 = 915 pc). Beyond that radius, at the edge of the radio jet, the high-velocity gas shows a different PA, of ∼125 • . This might be indicating that the line-emitting gas is being compressed and accelerated by the shocks generated by the radio jet.

show abstract

“…Higher resolution CO(2-1) (beam size of 0.214 × 0.161 arcsec 2 ) ALMA observations unravelled the structure of the ring: several star-forming clumps associated with star formation events (Alonso-Herrero et al 2019 ). The presence of a ring of star-forming regions is also supported by the low H 2 /Br γ ratios (Sch önell et al 2019 ;Riffel et al 2021c ), higher Br γ equi v alent width (Rif fel et al 2021c ), lo w gas ( ∼50 km s −1 -Fig. 4 ), and stellar velocity dispersion (Barbosa et al 2006 ;Riffel et al 2017 ) values.…”

Section: B4 Ngc 3227mentioning

confidence: 87%

Gemini NIFS survey of feeding and feedback in nearby active galaxies – V. Molecular and ionized gas kinematics

Riffel

Storchi‐Bergmann

Riffel

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We study the gas distribution and kinematics of the inner kpc of six moderately luminous (43.43 ≤ log Lbol ≤ 44.83) nearby (0.004 ≤ z ≤ 0.014) Seyfert galaxies observed with the Near-infrared Integral Field Spectrograph (NIFS) in the J(1.25μm) and K(2.2μm) bands. We analyse the most intense emission lines detected on these spectral wavebands: [Fe ii] 1.2570 μm and Paβ, which trace the ionised gas in the partially and fully ionised regions, and H2 2.1218 μm, that traces the hot (∼2000 K) molecular gas. The dominant kinematic component is rotation in the disc of the galaxies, except for the ionised gas in NGC 5899 which shows only weak signatures of a disc component. We find ionised gas outflow in four galaxies, while signatures of H2 outflows are seen in three galaxies. The ionised gas outflows display velocities of a few hundred km s−1, and their mass-outflow rates are in the range 0.005 − 12.49 M⊙yr−1. Their kinetic powers correspond to 0.005 − 0.7 per cent of the AGN bolometric luminosities. Besides rotation and outflows signatures in some cases, the H2 kinematics reveals also inflows in three galaxies. The inflow velocities are 50 − 80 km s−1and the mass inflow rates are in the range 1 − 9 × 10−4 M⊙yr−1 for hot molecular gas. These inflows might be only the hot skin of the total inflowing gas, which is expected to be dominated by colder gas. The mass inflow rates are lower than the current accretion rates to the AGN, and the ionised outflows are apparently disturbing the gas in the inner kpc.

show abstract

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

Cited by 23 publications

References 117 publications

Chemical abundances in Seyfert galaxies -IX. Helium abundance estimates

Chemical abundances in Seyfert galaxies -IX. Helium abundance estimates

Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

Gemini NIFS survey of feeding and feedback in nearby active galaxies – V. Molecular and ionized gas kinematics

Contact Info

Product

Resources

About