Stellar and Molecular Gas Kinematics of NGC 1097: Inflow Driven by a Nuclear Spiral

Davies, R. I.; Maciejewski, Witold; Hicks, E. K. S.; Tacconi, L. J.; Genzel, R.; Engel, H.

doi:10.1088/0004-637x/702/1/114

Cited by 124 publications

(154 citation statements)

References 66 publications

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“…With JWST and an AO-fed GSMT/E-ELT, we will just be able access this regime and map the emission of hot dust (Tristram et al 2007) and hot molecular hydrogen (Davies et al 2006;Hicks & Malkan 2008). On larger spatial scales, JWST, GSMT/E-ELT, and ALMA could be used to map out the distribution and kinematics of ionized and molecular gas for a large and complete sample of AGN and suitable control sample (e.g., Fathi et al 2006;Storchi-Bergmann et al 2007;Riffel et al 2008;Davies et al 2009a;Lindt-Krieg et al 2008;Schinnerer et al 2000). A complementary approach could be provided by mapping of the stellar population and star-formation history in these regions (e.g., Gonzalez Delgado et al 2004;Davies et al 2007).…”

Section: Fueling the Black Holementioning

confidence: 99%

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Heckman

2009

Proc. IAU

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Abstract. I begin by summarizing the evidence that there is a close relationship between the evolution of galaxies and supermassive black holes. They evidently share a common fuel source, and feedback from the black hole may be needed to suppress over-cooling in massive galaxies.I then review what we know about the co-evolution of galaxies and black holes in the modern universe (z < 1). We now have a good documentation of which black holes are growing (the lower mass ones), where they are growing (in the less massive early-type galaxies), and how this growth is related in a statistical sense to star formation in the central region of the galaxy. The opportunity in the next decade will be to use the new observatories to undertake ambitious programs of 3-D imaging spectroscopy of the stars and gas in order to understand the actual astrophysical processes that produce the demographics we observe. At high redshift (z > 2), the most massive black holes and the progenitors of the most massive galaxies are forming. Here, we currently have a tantalizing but fragmented view of their co-evolution. In the next decade, the huge increase in sensitivity and discovery power of our observatories will enable us to analyze the large, complete samples we need to achieve robust and clear results.

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Section: Fueling the Black Holementioning

confidence: 99%

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Heckman

2009

Proc. IAU

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“…Gas inflows have also been observed by other groups. Near-infrared integral field spectroscopic observations revealed inflows along nuclear spiral arms in NGC 1097 (Davies et al 2009), NGC 5643 (Davies et al 2014) and NGC 7743 (Davies et al 2014), and gas inflow along a bar in NGC 3227 (Davies et al 2014). Recent ALMA observations releaved streaming motions along nuclear spirals in NGC 1433 (Combes et al 2013) and NGC 1566 (Combes et al 2014).…”

Section: Introductionmentioning

confidence: 98%

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

Schnorr-Müller

Storchi‐Bergmann

Ferrari

et al. 2017

Mon. Not. R. Astron. Soc.

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We use optical spectra from the inner 2 × 3 kpc 2 of the Seyfert 2 galaxy NGC 1667, obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈ 240 pc, to assess the feeding and feedback processes in this nearby AGN. We have identified two gaseous kinematical components in the emission line profiles: a broader component (σ ≈ 400 km s −1 ) which is observed in the inner 1-2 ′′ and a narrower component (σ ≈ 200 km s −1 ) which is present over the entire field-ofview. We identify the broader component as due to an unresolved nuclear outflow. The narrower component velocity field shows strong isovelocity twists relative to a rotation pattern, implying the presence of strong non-circular motions. The subtraction of a rotational model reveals that these twists are caused by outflowing gas in the inner ≈ 1 ′′ , and by inflows associated with two spiral arms at larger radii. We calculate an ionized gas mass outflow rate ofṀ out ≈ 0.16 M ⊙ yr −1 . We calculate the net gas mass flow rate across a series of concentric rings, obtaining a maximum mass inflow rate in ionized gas of ≈ 2.8 M ⊙ year −1 at 800 pc from the nucleus, which is two orders of magnitude larger than the accretion rate necessary to power this AGN. However, as the mass inflow rate decreases at smaller radii, most of the gas probably will not reach the AGN, but accumulate in the inner few hundred parsecs. This will create a reservoir of gas that can trigger the formation of new stars.

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“…This bar may be responsible for driving gas into the central region of the galaxy, forming a ring of gas near the Inner Lindblad Resonance, triggering the formation of massive star clusters (e.g., Athanassoula 1992). There is also gas inflow inside the ring possibly fueling the central supermassive black hole (Prieto et al 2005;Fathi et al 2006;Davies et al 2009), triggering the formation of a compact star cluster seen near the nucleus. The star-forming ring and the nucleus of NGC 1097 are prominent in CO 1-0 (Kohno et al 2003) as well as rovibrational H 2 and hydrogen recombination lines (Reunanen et al 2002;Kotilainen et al 2000).…”

Section: Introductionmentioning

confidence: 99%

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

Beirão

Armus

Hélou

et al. 2012

ApJ

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NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar, and an active nucleus. We present a detailed study of the spatial variation of the far-infrared (FIR) [C ii]158 μm and [O i]63 μm lines and mid-infrared H 2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star-forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([C ii]158 μm+[O i]63 μm)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7 μm PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [C ii]158 μm/PAH(5.5-14 μm) is found. PAHs in the ring are responsible for a factor of two more [C ii]158 μm and [O i]63 μm emission per unit mass than PAHs in the Enuc S. spectral energy distribution (SED) modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high-intensity photodissociation regions (PDRs), in which case G 0 ∼ 10 2.3 and n H ∼ 10 3.5 cm −3 in the ring. For these values of G 0 and n H , PDR models cannot reproduce the observed H 2 emission. Much of the H 2 emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.

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Stellar and Molecular Gas Kinematics of NGC 1097: Inflow Driven by a Nuclear Spiral

Cited by 124 publications

References 66 publications

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC 1667

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

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