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

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...

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Veröffentlicht in:	Monthly notices of the Royal Astronomical Society Jg. 403; H. 4; S. 1801 - 1811
Hauptverfasser:	Schartmann, M., Burkert, A., Krause, M., Camenzind, M., Meisenheimer, K., Davies, R. I.
Format:	Journal Article
Sprache:	Englisch
Veröffentlicht:	Oxford, UK Blackwell Publishing Ltd 21.04.2010 Wiley-Blackwell Oxford University Press
Schlagworte:	accretion accretion discs accretion, accretion discs Astronomy Astrophysics Earth, ocean, space Exact sciences and technology galaxies: nuclei galaxies: Seyfert galaxies: structure hydrodynamics ISM: evolution Simulation Spectrum analysis Stars & galaxies galaxies: structure galaxies: Seyfert hydrodynamics galaxies: nuclei ISM: evolution accretion, accretion discs Young cluster Seyfert 2 galaxies Accretion disks Interferometric observation Young stars Seyfert galaxies Momentum transfer Star formation Galaxy nuclei Turbulent viscosity Observables Age Pluto planet Nuclear cluster model Turbulence Radial distribution Gas dynamics Digital simulation Mass loss Star clusters Density distribution Mass transfer Stellar mass Galaxy structure Tori Rotating disk Masers Angular momentum Hydrodynamic model Adaptive optics Interstellar matter
ISSN:	0035-8711, 1365-2966
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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 250 Myr, our simulations yield disc sizes of the order of 0.8–0.9 pc, gas masses of 106 M⊙ and mass transfer rates of 0.025 M⊙ yr−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.
AbstractList	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 250 Myr, our simulations yield disc sizes of the order of 0.8–0.9 pc, gas masses of 106 M⊙ and mass transfer rates of 0.025 M⊙ yr−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. 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 250 Myr, our simulations yield disc sizes of the order of 0.8–0.9 pc, gas masses of 106 M⊙ and mass transfer rates of 0.025 M⊙ yr−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. 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 250 Myr, our simulations yield disc sizes of the order of 0.8-0.9 pc, gas masses of 106 M[odot] and mass transfer rates of 0.025 M[odot] yr-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. 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 250 Myr, our simulations yield disc sizes of the order of 0.8-0.9 pc, gas masses of 106 M[dotcircle] and mass transfer rates of 0.025 M[dotcircle] yr-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. [PUBLICATION ABSTRACT]
Author	Davies, R. I. Krause, M. Meisenheimer, K. Schartmann, M. Camenzind, M. Burkert, A.
Author_xml	– sequence: 1 givenname: M. surname: Schartmann fullname: Schartmann, M. email: schartmann@mpe.mpg.de, * schartmann@mpe.mpg.de organization: Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany – sequence: 2 givenname: A. surname: Burkert fullname: Burkert, A. organization: Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany – sequence: 3 givenname: M. surname: Krause fullname: Krause, M. organization: Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany – sequence: 4 givenname: M. surname: Camenzind fullname: Camenzind, M. organization: ZAH, Landessternwarte Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany – sequence: 5 givenname: K. surname: Meisenheimer fullname: Meisenheimer, K. organization: Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany – sequence: 6 givenname: R. I. surname: Davies fullname: Davies, R. I. organization: Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany
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Keywords	galaxies: structure galaxies: Seyfert hydrodynamics galaxies: nuclei ISM: evolution accretion, accretion discs Young cluster Seyfert 2 galaxies Accretion disks Interferometric observation Young stars Seyfert galaxies Momentum transfer Star formation Galaxy nuclei Turbulent viscosity Observables Age Pluto planet Nuclear cluster model Turbulence Radial distribution Gas dynamics Digital simulation Mass loss Star clusters Density distribution Mass transfer Stellar mass Galaxy structure Tori Rotating disk Masers Angular momentum Hydrodynamic model Adaptive optics Interstellar matter
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Snippet	Recently, high-resolution observations with the help of the near-infrared adaptive optics integral field spectrograph Spectrograph for INtegral Field... ABSTRACT Recently, high‐resolution observations with the help of the near‐infrared adaptive optics integral field spectrograph Spectrograph for INtegral Field...
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SubjectTerms	accretion accretion discs accretion, accretion discs Astronomy Astrophysics Earth, ocean, space Exact sciences and technology galaxies: nuclei galaxies: Seyfert galaxies: structure hydrodynamics ISM: evolution Simulation Spectrum analysis Stars & galaxies
Title	Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster
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