Kinematics and excitation of the molecular hydrogen accretion disc in NGC 1275

Scharwächter, J.; McGregor, Peter; Dopita, Michael A.; Beck, Tracy

doi:10.1093/mnras/sts502

Cited by 89 publications

(108 citation statements)

References 58 publications

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“…Since gas kinematics suggests M• = 8 × 10 8 M⊙ (Scharwächter et al 2013) for NGC 1275, the luminosity is L Edd = 1.0 × 10 47 erg s −1 . In Table 1, we present 2Lj/L Edd .…”

Section: Resultsmentioning

confidence: 99%

The young radio lobe of 3C 84: inferred gas properties in the central 10 pc

Fujita

Kawakatu

Shlosman

et al. 2015

Mon. Not. R. Astron. Soc.

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We analyse the environment of the supermassive black hole (SMBH) in the centre of a massive elliptical galaxy NGC 1275 in the Perseus cluster, hosting the radio source 3C 84. We focus on the young radio lobe observed inside the estimated Bondi accretion radius. We discuss the momentum balance between the jet associated with the lobe and the surrounding gas. The results are compared with the proper motion of the radio lobe obtained with the very long baseline interferometry. We find that under assumption of a high-density environment ( 100 cm −3 ), the jet power must be comparable to the Eddington luminosity -this is clearly inconsistent with the current moderate activity of 3C 84, which indicates instead that the jet is expanding in a very low density region ( 1 cm −3 ), along the rotation axis of the accretion flow. The power required for the jet to expand in the low-density environment is comparable to the past average jet power estimated from the X-ray observations. We estimate the classical Bondi accretion rate, assuming that (1) gas accretion is spherically symmetric, (2) accretion is associated with the jet environment, and (3) the medium surrounding the jet is representative of the properties of the dominant accreting gas. We find that Bondi accretion is inconsistent with the estimated jet power. This means that either accretion of the cold gas in the NGC 1275 is more efficient than that of the hot gas, or the jets are powered by the SMBH spin.

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“…Since gas kinematics suggests M• = 8 × 10 8 M⊙ (Scharwächter et al 2013) for NGC 1275, the luminosity is L Edd = 1.0 × 10 47 erg s −1 . In Table 1, we present 2Lj/L Edd .…”

Section: Resultsmentioning

confidence: 99%

The young radio lobe of 3C 84: inferred gas properties in the central 10 pc

Fujita

Kawakatu

Shlosman

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The total luminosity is 4 × 10 44 erg s −1 (Levinson et al 1995). This luminosity is about 0.4% of the Eddington luminosity for a black hole mass of 8 × 10 8 M (Scharwächter et al 2013). The radio luminosity of this source is 3 × 10 24 W Hz −1 sr −1 at 178 MHz, which is classified as a Fanaroff-Riley I radio source (Fanaroff & Riley 1974).…”

Section: Introductionmentioning

confidence: 90%

“…Previous authors argued that the large-scale gas filaments can be infalling and settling into the CND (e.g. Scharwächter et al 2013). However, these features may not be a representation of a single infalling stream since they are not simply connected to each other in terms of both morphology and kinematics.…”

Section: Filamentsmentioning

confidence: 99%

The ALMA Discovery of the Rotating Disk and Fast Outflow of Cold Molecular Gas in NGC 1275

Nagai

Onishi

Kawakatu

et al. 2019

ApJ

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We present ALMA Band 6 observations of the CO(2-1), HCN(3-2), and HCO + (3-2) lines in the nearby radio galaxy / brightest cluster galaxy (BCG) of NGC 1275 with the spatial resolution of ∼ 20 pc. In the previous observations, CO(2-1) emission was detected as radial filaments lying in the east-west direction. We resolved the inner filament and found that the filament cannot be represented by a simple infalling stream both morphologically and kinematically. The observed complex nature of the filament resembles the cold gas structure predicted by recent numerical simulations of cold chaotic accretion. A crude estimate suggests that the accretion rate of the cold gas can be higher than that of hot gas. Within the central 100 pc, we detected a rotational disk of the molecular gas whose mass is ∼ 10 8 M . This is the first evidence of the presence of massive cold gas disk on this spatial scale for BCGs. The disk rotation axis is approximately consistent with the axis of the radio jet on subpc scales. This probably suggests that the cold gas disk is physically connected to the innermost accretion disk which is responsible for jet launching. We also detected absorption features in the HCN(3-2) and HCO + (3-2) spectra against the radio continuum emission mostly radiated by ∼ 1.2-pc size jet. The absorption features are blue-shifted from the systemic velocity by ∼300-600 km s −1 , which suggests the presence of outflowing gas from the active galactic nucleus (AGN). We discuss the relation of the AGN feeding with cold accretion, the origin of blue-shifted absorption, and estimate of black hole mass using the molecular gas dynamics.

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“…Different line styles correspond to different models. (Scharwächter et al 2013) and the distance to us is D = 78.2 Mpc 3 . For the black hole mass and distance adopted here, 1 mas ≃ 0.38 pc ≃ 5.0 × 10 3 R S .…”

Section: Sed Modeling Of M87mentioning

confidence: 99%

“…b In addition, δ = 0.01, which is the fraction of the turbulent energy that directly heats the electrons as the AD model in Nemmen et al (2014). References: (1) Gebhardt & Thomas (2009); (2) Jordán et al (2005); (3) Scharwächter et al (2013); (4) Strauss et al (1992). lar spatial scales) measured the RM at kpc scale using archival polarimetric VLA data at 8, 15, 22 and 43 GHz, and found that it is on the order of a few ×10 2 rad m −2 .…”

Section: Rotation Measure Of M87mentioning

confidence: 99%

Exploring the Accretion Model of M87 and 3c 84 With the Faraday Rotation Measure Observations

Yuan

Xie

2016

ApJ

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Low-luminosity active galactic nuclei (LLAGNs) are believed to be powered by an accretion-jet model, consisting of an inner advection-dominated accretion flow (ADAF), an outer truncated standard thin disk, and a jet. But model degeneracy still exists in this framework. For example, the X-ray emission can originate from either the ADAF or jet. The aim of the present work is to check these models with the Faraday rotation measure (RM) observations recently detected for two LLAGNs, M87 and 3C 84, in the sub-mm band. For M87, we find that the RM predicted by the model in which the X-ray emission originates from the ADAF is larger than the observed upper limit of RM by over two orders of magnitude, while the model in which the X-ray emission originates from the jet predicts a RM lower than the observed upper limit. For 3C 84, the sub-mm emission is found to be dominated by the jet component, while the Faraday screen is attributed to the ADAFs. This scenario can naturally explain the observed external origin of the RM and why RM is found to be stable during a two-year interval although the sub-mm emission increases at the same period.

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Kinematics and excitation of the molecular hydrogen accretion disc in NGC 1275

Cited by 89 publications

References 58 publications

The young radio lobe of 3C 84: inferred gas properties in the central 10 pc

The young radio lobe of 3C 84: inferred gas properties in the central 10 pc

The ALMA Discovery of the Rotating Disk and Fast Outflow of Cold Molecular Gas in NGC 1275

Exploring the Accretion Model of M87 and 3c 84 With the Faraday Rotation Measure Observations

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