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Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster

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Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster. / Schartmann, M.; Burkert, A.; Krause, Martin; Camenzind, M.; Meisenheimer, K.; Davies, R.~I.

In: Monthly Notices of the Royal Astronomical Society, Vol. 403, No. 4, 21.04.2010, p. 1801-1811.

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Schartmann, M. ; Burkert, A. ; Krause, Martin ; Camenzind, M. ; Meisenheimer, K. ; Davies, R.~I. / Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster. In: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 403, No. 4. pp. 1801-1811.

Bibtex

@article{e4332248cf8a4c2489220f3d3547bbfd,
title = "Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster",
abstract = "Recently, high-resolution observations with the help of the near-infrared adaptive optics integral field spectrograph Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI) at the Very Large Telescope proved the existence of massive and young nuclear star clusters in the centres of a sample of Seyfert galaxies. With the help of three-dimensional high-resolution hydrodynamical simulations with the PLUTO code, we follow the evolution of such clusters, especially focusing on stellar mass loss feeding gas into the ambient interstellar medium and driving turbulence. This leads to a vertically wide distributed clumpy or filamentary inflow of gas on large scales (tens of parsec), whereas a turbulent and very dense disc builds up on the parsec scale. In order to capture the relevant physics in the inner region, we treat this disc separately by viscously evolving the radial surface density distribution. This enables us to link the tens of parsec-scale region (accessible via SINFONI observations) to the (sub-)parsec-scale region (observable with the mid-infrared interferometer instrument and via water maser emission). Thereby, this procedure provides us with an ideal testbed for data comparison. In this work, we concentrate on the effects of a parametrized turbulent viscosity to generate angular momentum and mass transfer in the disc and additionally take star formation into account. Most of the input parameters are constrained by available observations of the nearby Seyfert 2 galaxy NGC 1068, and we discuss parameter studies for the free parameters. At the current age of its nuclear starburst of 250Myr, our simulations yield disc sizes of the order of 0.8-0.9pc, gas masses of 106Msolar and mass transfer rates of 0.025Msolaryr-1 through the inner rim of the disc. This shows that our large-scale torus model is able to approximately account for the disc size as inferred from interferometric observations in the mid-infrared and compares well to the extent and mass of a rotating disc structure as inferred from water maser observations. Several other observational constraints are discussed as well.",
keywords = "accretion, accretion discs, hydrodynamics, ISM: evolution, galaxies: nuclei, galaxies: Seyfert, galaxies: structure",
author = "M. Schartmann and A. Burkert and Martin Krause and M. Camenzind and K. Meisenheimer and R.~I. Davies",
note = "M. Schartmann; Burkert; M. Krause; M. Camenzind; K. Meisenheimer; and R. I. Davies, 'Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster', Monthly Notices of the Royal Astronomical Society, Vol. 40 (3): 1801-1811, first published online 6 April 2010. The version of record is available online at doi: :10.1111/j.1365-2966.2010.16250.x. Published by Oxford University Press on behalf of the Royal Astronomical Society. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.",
year = "2010",
month = apr,
day = "21",
doi = "10.1111/j.1365-2966.2010.16250.x",
language = "English",
volume = "403",
pages = "1801--1811",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster

AU - Schartmann, M.

AU - Burkert, A.

AU - Krause, Martin

AU - Camenzind, M.

AU - Meisenheimer, K.

AU - Davies, R.~I.

N1 - M. Schartmann; Burkert; M. Krause; M. Camenzind; K. Meisenheimer; and R. I. Davies, 'Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster', Monthly Notices of the Royal Astronomical Society, Vol. 40 (3): 1801-1811, first published online 6 April 2010. The version of record is available online at doi: :10.1111/j.1365-2966.2010.16250.x. Published by Oxford University Press on behalf of the Royal Astronomical Society. © 2010 The Authors. Journal compilation © 2010 RAS.

PY - 2010/4/21

Y1 - 2010/4/21

N2 - Recently, high-resolution observations with the help of the near-infrared adaptive optics integral field spectrograph Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI) at the Very Large Telescope proved the existence of massive and young nuclear star clusters in the centres of a sample of Seyfert galaxies. With the help of three-dimensional high-resolution hydrodynamical simulations with the PLUTO code, we follow the evolution of such clusters, especially focusing on stellar mass loss feeding gas into the ambient interstellar medium and driving turbulence. This leads to a vertically wide distributed clumpy or filamentary inflow of gas on large scales (tens of parsec), whereas a turbulent and very dense disc builds up on the parsec scale. In order to capture the relevant physics in the inner region, we treat this disc separately by viscously evolving the radial surface density distribution. This enables us to link the tens of parsec-scale region (accessible via SINFONI observations) to the (sub-)parsec-scale region (observable with the mid-infrared interferometer instrument and via water maser emission). Thereby, this procedure provides us with an ideal testbed for data comparison. In this work, we concentrate on the effects of a parametrized turbulent viscosity to generate angular momentum and mass transfer in the disc and additionally take star formation into account. Most of the input parameters are constrained by available observations of the nearby Seyfert 2 galaxy NGC 1068, and we discuss parameter studies for the free parameters. At the current age of its nuclear starburst of 250Myr, our simulations yield disc sizes of the order of 0.8-0.9pc, gas masses of 106Msolar and mass transfer rates of 0.025Msolaryr-1 through the inner rim of the disc. This shows that our large-scale torus model is able to approximately account for the disc size as inferred from interferometric observations in the mid-infrared and compares well to the extent and mass of a rotating disc structure as inferred from water maser observations. Several other observational constraints are discussed as well.

AB - Recently, high-resolution observations with the help of the near-infrared adaptive optics integral field spectrograph Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI) at the Very Large Telescope proved the existence of massive and young nuclear star clusters in the centres of a sample of Seyfert galaxies. With the help of three-dimensional high-resolution hydrodynamical simulations with the PLUTO code, we follow the evolution of such clusters, especially focusing on stellar mass loss feeding gas into the ambient interstellar medium and driving turbulence. This leads to a vertically wide distributed clumpy or filamentary inflow of gas on large scales (tens of parsec), whereas a turbulent and very dense disc builds up on the parsec scale. In order to capture the relevant physics in the inner region, we treat this disc separately by viscously evolving the radial surface density distribution. This enables us to link the tens of parsec-scale region (accessible via SINFONI observations) to the (sub-)parsec-scale region (observable with the mid-infrared interferometer instrument and via water maser emission). Thereby, this procedure provides us with an ideal testbed for data comparison. In this work, we concentrate on the effects of a parametrized turbulent viscosity to generate angular momentum and mass transfer in the disc and additionally take star formation into account. Most of the input parameters are constrained by available observations of the nearby Seyfert 2 galaxy NGC 1068, and we discuss parameter studies for the free parameters. At the current age of its nuclear starburst of 250Myr, our simulations yield disc sizes of the order of 0.8-0.9pc, gas masses of 106Msolar and mass transfer rates of 0.025Msolaryr-1 through the inner rim of the disc. This shows that our large-scale torus model is able to approximately account for the disc size as inferred from interferometric observations in the mid-infrared and compares well to the extent and mass of a rotating disc structure as inferred from water maser observations. Several other observational constraints are discussed as well.

KW - accretion, accretion discs, hydrodynamics, ISM: evolution, galaxies: nuclei, galaxies: Seyfert, galaxies: structure

U2 - 10.1111/j.1365-2966.2010.16250.x

DO - 10.1111/j.1365-2966.2010.16250.x

M3 - Article

VL - 403

SP - 1801

EP - 1811

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -