Young Star Clusters in the Circumnuclear Region of NGC 2110

Durré, Mark; Mould, Jeremy

doi:10.1088/0004-637x/784/1/79

Cited by 12 publications

(19 citation statements)

References 60 publications

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“…Comparing our [Fe ii] λ 1.2570 µm kinematic maps with those obtained by Durré & Mould (2014) for the same emission line, we find that they are consistent each to other, considering that the spatial orientation of the maps originally published is incorrect. Their maps are rotated by 90 • , to have the north-south direction along the y-axis (Durré, M., private communication).…”

Section: Gaseous Kinematicssupporting

confidence: 85%

“…We concluded that the main H 2 excitation mechanism is heating of the gas by X-rays emitted from the AGN. Durré & Mould (2014) have also recently presented NIR IFS of the central region of NGC 2110 using J-band data obtained with the Keck I OSIRIS instrument and reported the detection of star clusters along with a 90×35 pc bar of shocked gas around the nucleus of NGC 2110. They derived a star formation rate of 0.3 M ⊙ yr −1 and argue that the star formation is triggered by the AGN feedback.…”

Section: Introductionmentioning

confidence: 99%

“…The white contours overlaid to the [Fe ii] flux and σ maps are from the 6 cm radio image of Ulvestad & Wilson (1984). White rectangles shown in the [Fe ii] maps indicate the FOV of the observations used byDurré & Mould (2014). The "+" sign marks the location of the nucleus.…”

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confidence: 99%

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Outflows, inflows, and young stars in the inner 200 pc of the Seyfert galaxy NGC 2110

Diniz

Riffel

Storchi‐Bergmann

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a two-dimensional mapping of stellar population age components, emission-line fluxes, gas excitation and kinematics within the inner ∼ 200 pc of the Seyfert 2 galaxy NGC 2110. We used the Gemini North Integral Field Spectrograph (NIFS) in the J and K bands at a spatial resolution of ∼ 22 pc. The unresolved nuclear continuum is originated in combined contributions of young stellar population (SP; age 100 Myr), a featureless AGN continuum and hot dust emission. The young-intermediate SP (100 2 Gyr) is dominant. The [Fe ii] λ 1.2570 µm emission-line flux distribution is correlated with the radio emission and its kinematics comprise two components, one from gas rotating in the galaxy plane and another from gas in outflow within a bicone oriented along north-south. These outflows seem to originate in the interaction of the radio jet with the ambient gas producing shocks that are the main excitation mechanism of the [Fe ii] emission. We estimate:(1) an ionized gas mass outflow rate of ∼ 0.5 M ⊙ yr −1 at ∼70 pc from the nucleus; and (2) a kinetic power for the outflow of only 0.05% of the AGN bolometric luminosity implying weak feedback effect on the galaxy.

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Section: Gaseous Kinematicssupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

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Outflows, inflows, and young stars in the inner 200 pc of the Seyfert galaxy NGC 2110

Diniz

Riffel

Storchi‐Bergmann

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Here, young stellar populations revealed by PCA tomography may be associated with a more massive cluster or, perhaps, a combination of many clusters. For example, Durré & Mould (2014) detected four young stellar clusters encircling the AGN of the galaxy NGC 2110. Using IFU data with adaptive optics in the IR, they associated [Fe II] emissions with shocks caused by winds and/or SNR emerging from these clusters.…”

Section: Discussionmentioning

confidence: 99%

A hot bubble at the centre of M 81

Ricci

Steiner

Giansante

2015

A&A

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Context. Messier 81 has the nearest active nucleus with broad Hα emission. A detailed study of this galaxy's centre is important for understanding the innermost structure of the AGN phenomenon. Aims. Our goal is to seek previously undetected structures using additional techniques to reanalyse a data cube obtained with the GMOS-IFU installed on the Gemini North telescope (Schnorr Müller et al. 2011, MNRAS, 413, 149). Methods. We analysed the data cube using techniques of noise reduction, spatial deconvolution, starlight subtraction, PCA tomography, and comparison with HST images. Results. We identified a hot bubble with T > 43 500 K that is associated with strong emission of [N II]λ5755 Å and a high [O I]λ6300/Hα ratio; the bubble displays a bluish continuum, surrounded by a thin shell of Hα + [N II] emission. We also reinterpret the outflow found by Schnorr Müller et al. (2011), showing that the blueshifted cone nearly coincides with the radio jet, as expected. Conclusions. We interpret the hot bubble as having been caused by post starburst events that left one or more clusters of young stars, similar to the ones found at the centre of the Milky Way, such as the Arches and the IRS 16 clusters. Shocked structures from combined young stellar winds or supernova remnants are probably the cause of this hot gas and the low ionization emission.

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“…Currently, there are 3 instruments that meet the combined requirements of a telescope in the 8-10m class, adaptive optics and a near infra-red IFU; these are SINFONI on VLT (Eisenhauer et al 2003), NIFS on Gemini North (McGregor et al 2003) and OSIRIS on Keck I (Larkin et al 2006). This paper is the second on the Mould et al (2012) galaxies, the first was on NGC 2110 (Durré & Mould 2014), which showed young, massive star clusters embedded in a disk of shocked gas from stellar winds which feed the black hole; the star formation rate is 0.3 M yr −1 , easily sufficient to produce the clusters on a million year timescale. The gas kinematics produced an estimate for the enclosed central mass of 3.2 − 4.2 × 10 8 M .…”

Section: Our Programmentioning

confidence: 99%

IC 630: Piercing the Veil of the Nuclear Gas

Durré

Mould

Schartmann

et al. 2017

ApJ

Self Cite

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IC 630 is a nearby early-type galaxy with a mass of 6 × 10 10 M with an intense burst of recent (6 Myr) star formation. It shows strong nebular emission lines, with radio and X-ray emission, which classifies it as an AGN. With VLT-SINFONI and Gemini North-NIFS adaptive optics observations (plus supplementary ANU 2.3m WiFeS optical IFU observations), the excitation diagnostics of the nebular emission species show no sign of standard AGN engine excitation; the stellar velocity dispersion also indicate that a super-massive black hole (if one is present) is small (M • = 2.25 × 10 5 M ). The luminosity at all wavelengths is consistent with star formation at a rate of about 1-2 M /yr. We measure gas outflows driven by star formation at a rate of 0.18 M /yr in a face-on truncated cone geometry. We also observe a nuclear cluster or disk and other clusters. Photo-ionization from young, hot stars is the main excitation mechanism for [Fe II] and hydrogen, whereas shocks are responsible for the H 2 excitation. Our observations are broadly comparable with simulations where a Toomre-unstable, self-gravitating gas disk triggers a burst of star formation, peaking after about 30 Myr and possibly cycling with a period of about 200 Myr.

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Young Star Clusters in the Circumnuclear Region of NGC 2110

Cited by 12 publications

References 60 publications

Outflows, inflows, and young stars in the inner 200 pc of the Seyfert galaxy NGC 2110

Outflows, inflows, and young stars in the inner 200 pc of the Seyfert galaxy NGC 2110

A hot bubble at the centre of M 81

IC 630: Piercing the Veil of the Nuclear Gas

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