The Impact of Nuclear Star Formation on Gas Inflow to AGN

Davies, R. I.; Hicks, E. K. S.; Schartmann, M.; Genzel, R.; Tacconi, L. J.; Engel, H.; Burkert, Andreas; Krause, Martin; Sternberg, A.; Sánchez, Francisco; Maciejewski, Witold

doi:10.1017/s1743921310006496

Cited by 6 publications

(6 citation statements)

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“…This CN excess questions the suitability of the bipolar outflow template in NGC 1068. The age dating of the most recent star-formation episode of the CND (>2−3 × 10 8 yrs old, Davies et al 2010) also questions the hypothesis that shocks in NGC 1068 can be interpreted as stemming from an embedded population of young stellar objects.…”

Section: Tracers Of Shocks In Ngc 1068mentioning

confidence: 99%

“…; Boger & Sternberg 2005;Fuente et al 1993Fuente et al , 2008Janssen et al 1995). However, based on the age estimated for the most recent star formation episode taking place in the CND(>2−3 × 10 8 yrs old, Davies et al 2010), and considering that the UV radiation from young massive stars should dominate the feedback in a starburst, we can safely discard PDR chemistry as the origin for the high abundances of CN in the CND of NGC 1068. As argued in Sect.…”

Section: X-ray Chemistry In Ngc 1068mentioning

confidence: 99%

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Molecular gas chemistry in AGN

García‐Burillo

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et al. 2010

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Context. This paper is part of a multi-species survey of line emission from the molecular gas in the circum-nuclear disk (CND) of the Seyfert 2 galaxy NGC 1068. Unlike in other active galaxies, the intensely star-forming regions in NGC 1068 and the CND can be resolved with current instrumentation. This makes this galaxy an optimal test-bed to probe the effects of AGN on the molecular medium at ∼100 pc scales. Aims. Single-dish observations have provided evidence that the abundance of silicon monoxide (SiO) in the CND of NGC 1068 is enhanced by 3-4 orders of magnitude with respect to the values typically measured in quiescent molecular gas in the Galaxy. We aim at unveiling the mechanism(s) underlying the SiO enhancement. Methods. We have imaged the emission of the SiO(2−1) (86.8 GHz) and CN(2−1) (226.8 GHz) lines in NGC 1068 at ∼150 pc and 60 pc spatial resolution with the IRAM Plateau de Bure interferometer (PdBI). We have also obtained complementary IRAM 30 m observations of HNCO and methanol (CH 3 OH) lines. These species are known as tracers of shocks in the Galaxy. Results. SiO is detected in a disk of ∼400 pc size around the AGN. SiO abundances in the CND of ∼(1−5)×10 −9 are about 1−2 orders of magnitude above those measured in the starburst ring. The overall abundance of CN in the CND is high: ∼(0.2−1) × 10 −7 . The abundances of SiO and CN are enhanced at the extreme velocities of gas associated with non-circular motions close to the AGN (r < 70 pc). On average, HNCO/SiO and CH 3 OH/SiO line ratios in the CND are similar to those measured in prototypical shocked regions in our Galaxy. Yet the strength and abundance of CN in NGC 1068 can be explained neither by shocks nor by photondominated region (PDR) chemistry. Abundances measured for CN and SiO and the correlation of CN/CO and SiO/CO ratios with hard X-ray irradiation suggest that the CND of NGC 1068 has become a giant X-ray-dominated region (XDR). Conclusions. The extreme properties of molecular gas in the circum-nuclear molecular disk of NGC 1068 result from the interplay between different processes directly linked to nuclear activity. The results presented here highlight in particular the footprint of shocks and X-ray irradiation on the properties of molecular gas in this Seyfert. Whereas XDR chemistry offers a simple explanation for CN and SiO in NGC 1068, the relevance of shocks deserves further scrutiny. The inclusion of dust grain chemistry would help solve the controversy regarding the abundances of other molecular species, like HCN, which are under-predicted by XDR models.

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Section: Tracers Of Shocks In Ngc 1068mentioning

confidence: 99%

Section: X-ray Chemistry In Ngc 1068mentioning

confidence: 99%

Molecular gas chemistry in AGN

García‐Burillo

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et al. 2010

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“…This is equivalent to ∼1% of the rest-mass energy of the black hole, and is sufficient (in principle) to expel the entire ISM of such a galaxy. This feedback may play a major role in regulating the growth of the black hole (Davies et al 2007(Davies et al , 2009bWild et al 2010). …”

Section: T M Heckmanmentioning

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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“…Clever techniques are being used to study not only the most luminous quasars but also less luminous sources (Treister et al 2011, Mullaney et al 2012. Ongoing work using integral-field spectroscopy (Davies et al 2010, Storchi-Bergmann 2010, Müller-Sánchez et al 2011, Riffel & Storchi-Bergmann 2011 on nearby Seyfert galaxies is revealing spatially resolved distributions and kinematics of the gas that feeds the MBH and fuels star formation. The James Webb Space Telescope and Euclid, successors of the Hubble Space Telescope, and the Atacama Large Millimeter Array will zoom in on the highest quasars, and may eventually bring us to the edge of the Dark Ages when the first MBHs and galaxies formed.…”

Section: Outstanding Questions and Future Developmentsmentioning

confidence: 99%

Black holes in the early Universe

Volonteri¹,

Bellovary²

2012

Rep. Prog. Phys.

104

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Abstract.The existence of massive black holes was postulated in the sixties, when the first quasars were discovered. In the late nineties their reality was proven beyond doubt, in the Milky way and a handful nearby galaxies. Since then, enormous theoretical and observational efforts have been made to understand the astrophysics of massive black holes. We have discovered that some of the most massive black holes known, weighing billions of solar masses, powered luminous quasars within the first billion years of the Universe. The first massive black holes must therefore have formed around the time the first stars and galaxies formed. Dynamical evidence also indicates that black holes with masses of millions to billions of solar masses ordinarily dwell in the centers of today's galaxies. Massive black holes populate galaxy centers today, and shone as quasars in the past; the quiescent black holes that we detect now in nearby bulges are the dormant remnants of this fiery past. In this review we report on basic, but critical, questions regarding the cosmological significance of massive black holes. What physical mechanisms lead to the formation of the first massive black holes? How massive were the initial massive black hole seeds? When and where did they form? How is the growth of black holes linked to that of their host galaxy? Answers to most of these questions are work in progress, in the spirit of these Reports on Progress in Physics.

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The Impact of Nuclear Star Formation on Gas Inflow to AGN

Cited by 6 publications

References 30 publications

Molecular gas chemistry in AGN

Molecular gas chemistry in AGN

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

Black holes in the early Universe

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