A correlation between the stellar and [Fe ii] velocity dispersions in active galaxies

Riffel, Rogemar A.; Storchi‐Bergmann, Thaisa; Riffel, Rogério; Pastoriza, M. G.; Rodríguez-Ardila, A.; Dors, O. L.; Fuchs, Jaciara; Diniz, Marlon Rodrigo; Schönell, Astor J.; Hennig, Moiré Gonçalves; Brum, Carine

doi:10.1093/mnras/sts536

Cited by 13 publications

(23 citation statements)

References 44 publications

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“…While previous work (Riffel et al 2013a and references therein) gave the flux-weighted emission line ratios and corresponding limits for Seyferts, starbursts, and LINERs as above, we identify new limits and relations for the different excitation mechanism as a function of location within the galaxy (Fig. 5 for the prototypes, and Fig.…”

Section: Lirgs and Seyferts Defining New Near-ir Line Ratio Limits Amentioning

confidence: 65%

“…The overall distribution of the line ratios in the [FeII]1.64 µm/Brγ-H 2 2.12 µm/Brγ plane (Fig. 2, lower left panel) is such that the mode of the line ratios is outside the previously identified region for star-forming galaxies (Riffel et al 2013a) but with a long tail towards low The line ratios are well separated from that of the young starforming regions with [FeII]/Brγ and H 2 /Brγ ratios about six times higher than that of young star-forming clumps, respectively. The diffuse, line-emitting gas (white points/region in Fig.…”

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 68%

“…For these two galaxies, the H 2 /Brγ ratio in the [SiVI] emitting regions is about 1.5−2 times higher than in the [SiVI] non-emitting regions. Detailed studies of the near-IR H 2 line ratios in Seyferts, star-forming galaxies (Riffel et al 2013a), LIRGs (Bedregal et al 2009;Emonts et al 2014), and nearby spirals (Mazzalay et al 2013) indicate that the hot molecular gas is close to thermally excited because of a combination of X-ray radiation and shocks. On the other hand, the Brγ line is a direct tracer of the UV-ionizing radiation and therefore the H 2 /Brγ ratio gives an empirical first indication of the relative importance of each mechanism (UV radiation versus X-ray radiation or shocks).…”

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 99%

“…LINERs according to the classification scheme proposed by Riffel and collaborators (Riffel et al 2013a). These results come as a surprise as all LIRGs but two (NGC 5135 and NGC 7130) In addition, according to the optical emission line diagnostics, the excitation of the extended emission is characteristic of star formation and LINERs (Monreal-Ibero et al 2006.…”

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 99%

“…close to a factor 2 higher than that of the young star-forming clumps. (Riffel et al 2013a) based on 1D spectroscopy. Contours contain 25%, 50%, 75%, and 90% of the points for each class.…”

Section: Ngc 5135: Prototype Of Composite Lirgmentioning

confidence: 99%

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Understanding the two-dimensional ionization structure in luminous infrared galaxies

Colina

López

Arribas

et al. 2015

A&A

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We investigate the two-dimensional excitation structure of the interstellar medium (ISM) in a sample of luminous infrared galaxies (LIRGs) and Seyferts using near-IR integral field spectroscopy. This study extends to the near infrared the well-known optical and mid-IR emission line diagnostics used to classify activity in galaxies. Based on the spatially resolved spectroscopy of prototypes, we identify in the [FeII]1.64 µm/Brγ − H 2 2.12 µm/Brγ plane regions dominated by the different heating sources, i.e. active galactic nuclei (AGNs), young main-sequence massive stars, and evolved stars i.e. supernovae. The ISM in LIRGs occupy a wide region in the near-IR diagnostic plane from −0.6 to +1.5 and from −1.2 to +0.8 (in log units) for the [FeII]/Brγ and H 2 /Brγ line ratios, respectively. The corresponding median(mode) ratios are +0.18(0.16) and +0.02(−0.04). Seyferts show on average larger values by factors ∼2.5 and ∼1.4 for the [FeII]/Brγ and H 2 /Brγ ratios, respectively. New areas and relations in the near-IR diagnostic plane are defined for the compact, high surface brightness regions dominated by AGN, young ionizing stars, and supernovae explosions, respectively. In addition to these high surface brightness regions, the diffuse regions affected by the AGN radiation field cover an area similar to that of Seyferts, but with high values in [FeII]/Brγ that are not as extreme. The extended, non-AGN diffuse regions cover a wide area in the near-IR diagnostic diagram that overlaps that of individual excitation mechanisms (i.e. AGN, young stars, and supernovae), but with its mode value to that of the young star-forming clumps. This indicates that the excitation conditions of the extended, diffuse ISM are likely due to a mixture of the different ionization sources, weighted by their spatial distribution and relative flux contribution. The integrated line ratios in LIRGs show higher excitation conditions i.e. towards AGNs, than those measured by the spatially resolved spectroscopy. If this behaviour is representative, it would have clear consequences when classifying high-z, star-forming galaxies based on their near-infrared integrated spectra.

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Section: Lirgs and Seyferts Defining New Near-ir Line Ratio Limits Amentioning

confidence: 65%

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 68%

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 99%

Section: The Characterization Of the Ism In Lirgs According To The H mentioning

confidence: 99%

“…close to a factor 2 higher than that of the young star-forming clumps. (Riffel et al 2013a) based on 1D spectroscopy. Contours contain 25%, 50%, 75%, and 90% of the points for each class.…”

Section: Ngc 5135: Prototype Of Composite Lirgmentioning

confidence: 99%

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Understanding the two-dimensional ionization structure in luminous infrared galaxies

Colina

López

Arribas

et al. 2015

A&A

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Limited impact of jet-induced feedback in the multi-phase nuclear interstellar medium of 4C12.50

Villar-Martı́n¹,

Castro-Rodríguez²,

Santaella³

et al. 2023

A&A

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Context. 4C12.50 (IRAS 13451+1232) at z = 0.122 is an ultraluminous infared radio galaxy that has often been proposed as a prime candidate for the link between ultraluminous infared galaxies and young radio galaxies. It is also an interesting target to investigate whether and how radio-induced feedback affects the evolution of galaxies in the early phases of radio activity. Aims. We study, in detail for the first time, the hot (≥1500 K) molecular gas in 4C12.50. The potential impact of the radio jet on this gas phase, as well as on the star formation activity, are investigated. We also study the ionised (including coronal) gas as traced by the near-infrared lines. Methods. Using near-infrared long slit spectroscopy obtained with EMIR on GTC and X-shooter on VLT, we analyse the emission line spectrum of the ionised, coronal, and, specially, the hot molecular gas in the western nucleus hosting the compact radio jet. Based on high spatial resolution ALMA CO(2–1) data, we also revise the location of 4C12.50 in the Kennicutt-Schmidt diagram in order to investigate whether star formation is suppressed. Results. 4C12.50 hosts (2.1 ± 0.4) × 104 M⊙ of hot molecular gas. An unusually high rotational temperature Trot = 3020 ± 160 K is inferred. The molecular gas mass obeys a power-law temperature distribution, dMH2/dT ∝ T−5, from T ∼ 300 K and up to ∼3000 K. Both results support the idea that shocks (probably induced by the radio jet) contribute to the heating and excitation of the hot molecular gas. A molecular outflow is not detected. The coupling of the outflowing ionised and neutral outflows with the hot molecular gas is poor. Contrary to other studies, we claim that there is no evidence for star formation suppression in this object. Conclusions. If radio-induced feedback can regulate the star formation activity in galaxies, 4C12.50 is a promising candidate to reveal this phenomenon in action. However, we find no solid evidence for a current or past impact of this mechanism on the evolution of this system, neither by clearing out the dusty central cocoon efficiently, nor by suppressing the star formation activity.

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Young Star Clusters in the Circumnuclear Region of NGC 2110

Durré

Mould

2014

ApJ

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High-resolution observations in the near infrared show star clusters around the active galactic nucleus (AGN) of the Seyfert 1 NGC2110, along with a 90 x 35 pc bar of shocked gas material around its nucleus. These are seen for the first time in our imaging and gas kinematics of the central 100pc with the Keck OSIRIS instrument with adaptive optics. Each of these clusters is 2-3 times brighter than the Arches cluster close to the centre of the Milky Way. The core star formation rate (SFR) is 0.3 M⊙ yr -1 . The photoionized gas (He I) dynamics imply an enclosed mass of 3-4x10 8 M⊙. These observations demonstrate the physical linkage between AGN feedback, which triggers star formation in massive clusters, and the resulting stellar (and SNe) winds, which cause the observed [Fe II] emission and feed the black hole.

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A correlation between the stellar and [Fe ii] velocity dispersions in active galaxies

Cited by 13 publications

References 44 publications

Understanding the two-dimensional ionization structure in luminous infrared galaxies

Understanding the two-dimensional ionization structure in luminous infrared galaxies

Limited impact of jet-induced feedback in the multi-phase nuclear interstellar medium of 4C12.50

Young Star Clusters in the Circumnuclear Region of NGC 2110

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