TWO-DIMENSIONAL MAPPING OF YOUNG STARS IN THE INNER 180 pc OF NGC 1068: CORRELATION WITH MOLECULAR GAS RING AND STELLAR KINEMATICS

Storchi‐Bergmann, Thaisa; Riffel, Rogemar A.; Riffel, Rogério; Diniz, Marlon Rodrigo; Vale, Tibério Borges; McGregor, Peter

doi:10.1088/0004-637x/755/2/87

Cited by 68 publications

(89 citation statements)

References 46 publications

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“…Paα line emission can be interpreted as a tracer of young (<30 Myr) star formation or gas emission. Storchi-Bergmann et al (2012) found an episode of young (30 Myr) stellar population in a ring-like structure at ∼100 pc from the nucleus, coincident with the ring of molecular gas detected in the 2.12 µm warm molecular hydrogen line and in cold molecular gas detected by ALMA (García-Burillo et al 2014). We found that the morphology of this young stellar population and cold molecular gas resembles neither the Paα line emission nor the MIR features in the northern ionization cone.…”

Section: The Northern Ionization Conementioning

confidence: 77%

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

López-Rodríguez

Packham

Roche

et al. 2016

Mon. Not. R. Astron. Soc.

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We present sub-arcsecond 7.5−13 µm imaging-and spectro-polarimetric observations of NGC 1068 using CanariCam on the 10.4-m Gran Telescopio CANARIAS. At all wavelengths, we find: (1) A 90 × 60 pc extended polarized feature in the northern ionization cone, with a uniform ∼44 • polarization angle. Its polarization arises from dust and gas emission in the ionization cone, heated by the active nucleus and jet, and further extinguished by aligned dust grains in the host galaxy. The polarization spectrum of the jet-molecular cloud interaction at ∼24 pc from the core is highly polarized, and does not show a silicate feature, suggesting that the dust grains are different from those in the interstellar medium. (2) A southern polarized feature at ∼9.6 pc from the core. Its polarization arises from a dust emission component extinguished by a large concentration of dust in the galaxy disc. We cannot distinguish between dust emission from magnetically aligned dust grains directly heated by the jet close to the core, and aligned dust grains in the dusty obscuring material surrounding the central engine. Silicate-like grains reproduce the polarized dust emission in this feature, suggesting different dust compositions in both ionization cones. (3) An upper limit of polarization degree of 0.3 per cent in the core. Based on our polarization model, the expected polarization of the obscuring dusty material is 0.1 per cent in the 8−13 µm wavelength range. This low polarization may be arising from the passage of radiation through aligned dust grains in the shielded edges of the clumps.

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Section: The Northern Ionization Conementioning

confidence: 77%

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

López-Rodríguez

Packham

Roche

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Regions of low stellar velocity dispersion have been observed in the inner ≈ 200 pc of nearby Seyferts (Emsellem 2008;Comerón et al 2008) and young to intermediate (10 6 -10 8 yrs old) stellar population have been observed associated to these regions (Riffel et al 2010Storchi-Bergmann et al 2012;Hicks et al 2013). These low velocity dispersion regions have been interpreted as due to a stellar component in the vicinity of the nucleus of Seyfert galaxies that is dynamically colder in comparison to the stars that dominate the detected stellar light in quiescent galaxies (Hicks et al 2013).…”

Section: Estimating the Mass Inflow Ratementioning

confidence: 96%

“…The rotational model we obtained for the stellar velocity field in Sec. 4.1 is not an adequate description of the gaseous velocity field, as the stellar component usually rotates more slowly than the gas (van der Kruit & Freeman 1986;Bottema et al 1987;Noordermeer et al 2008). To acccount for this difference, we fitted the model described in Sect.…”

Section: The Narrower Componentmentioning

confidence: 99%

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 torus/reservoir, with size ranging from a few to several tens of parsecs, has been studied in detail only in nearby AGNs. High spatial resolution observations reveal that molecular gas and dust is largely present (e.g., Muller-Sanchez et al 2009;Krips et al 2011;Diamond-Stanic & Rieke 2012;Sani et al 2012;Hönig et al 2013), often accompanied by star formation (e.g., Davies et al 2007;Storchi-Bergmann et al 2012). The dust distribution looks quite complex, with the hot dust located in compact structures, while the warm one is more diffuse (see Hönig et al 2013).…”

Section: The Reservoirmentioning

confidence: 99%

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Lapi

Raimundo

Aversa

et al. 2014

ApJ

117

114

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We exploit the recent, wide samples of far-infrared (FIR) selected galaxies followed-up in X rays and of X-ray/optically selected active galactic nuclei (AGNs) followed-up in the FIR band, along with the classic data on AGN and stellar luminosity functions at high redshift z 1.5, to probe different stages in the coevolution of supermassive black holes (BHs) and host galaxies. The results of our analysis indicate the following scenario: (i) the star formation in the host galaxy proceeds within a heavily dust-enshrouded medium at an almost constant rate over a timescale 0.5 − 1 Gyr, and then abruptly declines due to quasar feedback; over the same timescale, (ii) part of the interstellar medium loses angular momentum, reaches the circum-nuclear regions at a rate proportional to the star formation and is temporarily stored into a massive reservoir/proto-torus wherefrom it can be promptly accreted; (iii) the BH grows by accretion in a self-regulated regime with radiative power that can slightly exceed the Eddington limit L/L Edd 4, particularly at the highest redshifts; (iv) for massive BHs the ensuing energy feedback at its maximum exceeds the stellar one and removes the interstellar gas, thus stopping the star formation and the fueling of the reservoir; (v) afterwards, if the latter has retained enough gas, a phase of supply-limited accretion follows exponentially declining with a timescale of about 2 e-folding times. We also discuss how the detailed properties and the specific evolution of the reservoir can be investigated via coordinated, high-resolution observations of starforming, strongly-lensed galaxies in the (sub-)mm band with ALMA and in the X-ray band with Chandra and the next generation X-ray instruments.

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TWO-DIMENSIONAL MAPPING OF YOUNG STARS IN THE INNER 180 pc OF NGC 1068: CORRELATION WITH MOLECULAR GAS RING AND STELLAR KINEMATICS

Cited by 68 publications

References 46 publications

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

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

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

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