Excitation of the molecular gas in the nuclear region of M 82

Loenen, A. F.; Guêsten, R.; Meijerink, R.; Israel, F.P.; Requeña-Torres, M. A.; García‐Burillo, S.; Harris, A. I.; Klein, Thomas; Krämer, C.; Lord, S. D.; Martı́n-Pintado, J.; Roellig, M.; Stützki, J.; Szczerba, R.; Weiß, A.; Philipp-May, Sabine; Yorke, H. W.; Caux, E.; Delforge, B.; Helmich, Frank; Lorenzani, A.; Morris, P.; Philips, T. G.; Risacher, C.; Tielens, A. G. G. M.; Werf, P. P. van der

doi:10.1051/0004-6361/201015114

Cited by 21 publications

(31 citation statements)

References 15 publications

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“…The latter indicate typical densities of 10 3 cm −3 and temperatures of ∼100 K, comparable to the conditions in starburst galaxies (Wild et al 1992;Aalto et al 1995;Loenen et al 2010). Indeed, more recent studies by Hsieh et al (2011) have for the first time resolved individual giant molecular cloud complexes, allowing to test the correlation between molecular gas and star formation on more local scales.…”

Section: Introductionmentioning

confidence: 62%

Star formation and accretion in the circumnuclear disks of active galaxies

Wutschik

Schleicher

Palmer

2013

A&A

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Aims. We explore the evolution of supermassive black holes (SMBH) centered in a circumnuclear disk (CND) as a function of the mass supply from the host galaxy and considering different star formation laws, which may give rise to a self-regulation via the injection of supernova-driven turbulence. Methods. A system of equations describing star formation, black hole accretion and angular momentum transport in the disk was solved self-consistently for an axisymmetric disk in which the gravitational potential includes contributions from the black hole, the disk and the hosting galaxy. Our model extends the framework provided by Kawakatu & Wada (2008, ApJ, 681, 73), by separately considering the inner and outer part of the disk, and by introducing a potentially non-linear dependence of the star formation rate on the gas surface density and the turbulent velocity. The star formation recipes are calibrated using observational data for NGC 1097, while the accretion model is based on turbulent viscosity as a source of angular momentum transport in a thin viscous accretion disk. Results. We find that current data provide no strong constraint on the star formation recipe, and can in particular not distinguish between models entirely regulated by the surface density, and models including a dependence on the turbulent velocity. The evolution of the black hole mass, on the other hand, strongly depends on the applied star formation law, as well as the mass supply from the host galaxy. We suggest to explore the star formation process in local AGN with high-resolution ALMA observations to break the degeneracy between different star formation models.

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Section: Introductionmentioning

confidence: 62%

Star formation and accretion in the circumnuclear disks of active galaxies

Wutschik

Schleicher

Palmer

2013

A&A

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“…The J up =4-13 CO line intensities (CO SLED) have been extracted from archival SPIRE/FTS observations (Panuzzo et al 2010;Rangwala et al 2011;Spinoglio et al 2012;Meijerink et al 2013;Papadopoulos et al 2014;Rosenberg et al 2014). For some sources (e.g., M82, NGC 253, and Cen A) high-J ( = J 5 up to 13) CO lines observed with HIFI have also been collected (see, e.g., Loenen et al 2010;Israel et al 2014 An updated version of the non-LTE 3D radiative transfer code "β3D" is used to calculate the excitation and radiative transfer of the molecular gas species (H 2 O and CO in our work). β3D was first developed by Poelman & Spaans (2005.…”

Section: Co Datamentioning

confidence: 99%

HIFI Spectroscopy of H₂O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies

Liu

Weiß

Pérez-Beaupuits

et al. 2017

ApJ

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We present a systematic survey of multiple velocity-resolved H 2 O spectra using Herschel/Heterodyne Instrument for the Far Infrared (HIFI) toward nine nearby actively star-forming galaxies. The ground-state and low-excitation lines (E up 130 K) show profiles with emission and absorption blended together, while absorption-free mediumexcitation lines (130 K E up 350 K) typically display line shapes similar to CO. We analyze the HIFI observation together with archival SPIRE/PACS H 2 O data using a state-of-the-art 3D radiative transfer code that includes the interaction between continuum and line emission. The water excitation models are combined with information on the dust and CO spectral line energy distribution to determine the physical structure of the interstellar medium (ISM). We identify two ISM components that are common to all galaxies: a warm10 10 cm 3 ), more extended phase is present. It outputs the emission in the low-excitation H 2 O lines and typically also produces the prominent line absorption features. For the two ULIRGs in our sample (Arp 220 and Mrk 231) an even hotter and more compact (R s 100 pc) region is present, which is possibly linked to AGN activity. We find that collisions dominate the water excitation in the cold gas and for lines with  E 300 up K and  E 800 up K in the warm and hot component, respectively. Higher-energy levels are mainly excited by IR pumping.

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“…HIFI found ionized water absorption from diffuse gas (Weiß et al 2010) and high-J transitions of the CO ladder. These CO transitions indicated a combination of one low and two high density gas components via comparison to PDR models (Loenen et al 2010).…”

Section: Introductionmentioning

confidence: 95%

HERSCHEL-SPIRE IMAGING SPECTROSCOPY OF MOLECULAR GAS IN M82

Kamenetzky

Glenn

Rangwala

et al. 2012

ApJ

100

157

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We present new Herschel-SPIRE imaging spectroscopy (194-671 µm) of the bright starburst galaxy M82. Covering the CO ladder from J = 4 → 3 to J = 13 → 12, spectra were obtained at multiple positions for a fully sampled ∼ 3 x 3 arcminute map, including a longer exposure at the central position. We present measurements of 12 CO, 13 CO, [C I], [N ii], HCN, and HCO + in emission, along with OH + , H 2 O + and HF in absorption and H 2 O in both emission and absorption, with discussion. We use a radiative transfer code and Bayesian likelihood analysis to model the temperature, density, column density, and filling factor of multiple components of molecular gas traced by 12 CO and 13 CO, adding further evidence to the high-J lines tracing a much warmer (∼ 500 K), less massive component than the low-J lines. The addition of 13 CO (and [C I]) is new and indicates that [C I] may be tracing different gas than 12 CO. No temperature/density gradients can be inferred from the map, indicating that the single-pointing spectrum is descriptive of the bulk properties of the galaxy. At such a high temperature, cooling is dominated by molecular hydrogen. Photon-dominated region (PDR) models require higher densities than those indicated by our Bayesian likelihood analysis in order to explain the high-J CO line ratios, though cosmic-ray enhanced PDR models can do a better job reproducing the emission at lower densities. Shocks and turbulent heating are likely required to explain the bright high-J emission.

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Excitation of the molecular gas in the nuclear region of M 82

Cited by 21 publications

References 15 publications

Star formation and accretion in the circumnuclear disks of active galaxies

Star formation and accretion in the circumnuclear disks of active galaxies

HIFI Spectroscopy of H₂O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies

HERSCHEL-SPIRE IMAGING SPECTROSCOPY OF MOLECULAR GAS IN M82

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Excitation of the molecular gas in the nuclear region of M 82

Cited by 21 publications

References 15 publications

Star formation and accretion in the circumnuclear disks of active galaxies

Star formation and accretion in the circumnuclear disks of active galaxies

HIFI Spectroscopy of H2O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies

HERSCHEL-SPIRE IMAGING SPECTROSCOPY OF MOLECULAR GAS IN M82

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HIFI Spectroscopy of H₂O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies