The star formation history and evolution of the circumnuclear region of M100

Allard, Emma L.; Knapen, Johan H.; Peletier, Reynier F.; Sarzi, Marc

doi:10.1111/j.1365-2966.2006.10751.x

Cited by 87 publications

(126 citation statements)

References 71 publications

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“…The most convincing case is the nuclear ring in M 100, for which Ryder et al (2001) and Allard et al (2006) used NIR and optical absorption indices and emission lines to determine the stellar ages of the hot spots in the star-formation ring. Smith et al (1999) have claimed evidence for sequential star formation in the nuclear ring of NGC 7771 from the ratio of NIR to radio continuum.…”

Section: "Popcorn" or "Pearls On A String"?mentioning

confidence: 99%

A Sinfoni View of Galaxy Centers: Morphology and Kinematics of Five Nuclear Star-Formation Rings

Böker

Falcón-Barroso

Schinnerer

et al. 2008

The Astronomical Journal

111

164

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We present near-infrared (H -and K-band) integral-field observations of the circumnuclear star formation rings in five nearby spiral galaxies. The data, obtained at the Very Large Telescope with the SINFONI spectrograph, are used to construct maps of various emission lines that reveal the individual star forming regions ("hot spots") delineating the rings. We derive the morphological parameters of the rings, and construct velocity fields of the stars and the emission line gas. We propose a qualitative, but robust, diagnostic for relative hot spot ages based on the intensity ratios of the emission lines Brγ , He i, and [Fe ii]. Application of this diagnostic to the data presented here provides tentative support for a scenario in which star formation in the rings is triggered predominantly at two well-defined regions close to, and downstream from, the intersection of dust lanes along the bar with the inner Lindblad resonance.

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Section: "Popcorn" or "Pearls On A String"?mentioning

confidence: 99%

A Sinfoni View of Galaxy Centers: Morphology and Kinematics of Five Nuclear Star-Formation Rings

Böker

Falcón-Barroso

Schinnerer

et al. 2008

The Astronomical Journal

111

164

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“…The stars inherit the velocity pattern of the gas from which they form, so their velocity dispersion is lower than that of the older, 'underlying' stars. A young stellar population dominates an older population in luminosity, so the resulting spectrum is dominated by the lower velocity dispersion of the younger stars (see, e.g., Wozniak et al 2003, also Allard et al 2005Allard et al , 2006. This effect can be enhanced by a falling velocity dispersion of the gas towards the centre of a galaxy, due to a strong accumulation of gas in a dissipative disc that would cool the gas in a cold component (i.e., a cold disc as shown in Falcón-Barroso et al 2006).…”

Section: Introductionmentioning

confidence: 99%

On the morphology of sigma-drop galaxies

Comerón

Knapen

Beckman

2008

A&A

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Context. Local reductions of the stellar velocity dispersion in the central regions of galaxies are known as sigma-drops (σ-drops). Knowing the origin of these features can lead to better understanding of inner galactic dynamics. Aims. We present a sample of 20 σ-drop galaxies matched with a control sample of galaxies without σ-drop in order to search for correlations between σ-drops and the properties, primarily morphological, of the nuclear zones and discs of their host galaxies. Methods. We study the dust and Hα distribution at 0.1 arcsec scale, using Hubble Space Telescope imaging, in the circumnuclear zones of the two samples of galaxies, searching for differences and trying to establish a link between the nuclear kinematics and the host morphology. We have also considered the CO and H i emission of the galaxies and their luminosity profiles.Results. We classify the two samples following both morphological parameters and the luminosity profiles. We find a larger fraction of nuclear dust spirals and Hα rings in the σ-drop sample. We also find that the fraction of Seyfert galaxies in the σ-drop sample is bigger than that of LINERs and that the reverse is true for the control sample. Conclusions. Our findings are evidence that a σ-drop is very probably due to inflow-induced star formation in a dynamically cool disc, or in a gas ring, shock focused by an inner Lindblad resonance above a certain critical density level. The same mechanism that feeds the nuclear ring or the nuclear disc is probably reponsible for the higher rate of Seyfert galaxies among the σ-drop hosts.

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“…Our proposed model (Allard et al 2006) not only fits the data, but is also phenomenologically attractive: it stipulates the formation of the underlying bulge/disk component and the current SF activity in the ring, but also the long-lived nature of the ring, albeit not constantly forming stars at the same high rate as observed now. Our modelling thus confirms a picture in which the bar in M100, a stable configuration, constantly channels gas into the nuclear region, where it concentrates in the nuclear ring until it reaches a density high enough to collapse gravitationally, and enter the next starburst phase.…”

Section: Cold Gas Flowing In and Feeding The Starburstmentioning

confidence: 64%

“…Comparing SSP model predictions with the data points measured for the nuclear ring and centre of M100 shows that whereas the nucleus can be fitted well and yields an age of some 3 Gyr, the nuclear ring points cannot be fitted at all because the Hβ index values are much lower then expected for any reasonable SSP (Allard et al 2006). We thus introduce a family of composite models, which are characterised by a combination of an old underlying bulge and/or disk contribution and a series of much more recent SF events.…”

Section: Cold Gas Flowing In and Feeding The Starburstmentioning

confidence: 99%

“…M100 hosts a wellknown nuclear ring with prominent massive SF, which is located near a pair of ILRs induced by the bar (K95). We have obtained integral-field spectroscopic data with SAURON (Bacon et al 2001) on the William Herschel Telescope (WHT) of the central region of the barred spiral galaxy M100 (Allard et al 2005(Allard et al , 2006. These data allow us to derive maps of emission line intensities, line strength indices, and the gas velocity dispersion across the circumnuclear region.…”

Section: Cold Gas Flowing In and Feeding The Starburstmentioning

confidence: 99%

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Star Formation in the Central Regions of Galaxies

Knapen

Allard

Mazzuca

et al. 2008

Mapping the Galaxy and Nearby Galaxies

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Summary. Massive star formation in the central regions of spiral galaxies plays an important role in the dynamical and secular evolution of their hosts. Here, we summarise a number of recent investigations of the star formation history and the physical conditions of the gas in circumnuclear regions, to illustrate not only the detailed results one can achieve, but also the potential of using state-of-the-art spectroscopic and analysis techniques in researching the central regions of galaxies in general. We review how the star formation history of nuclear rings confirms that they are long-lived and stable configurations. Gas flows in from the disk, through the bar, and into the ring, where successive episodes of massive star formation occur. Analysing the ring in NGC 7742 in particular, we determine the physical conditions of the line emitting gas using a combination of ionisation and stellar population modelling, concluding that the origin of the nuclear ring in this non-barred galaxy lies in a recent minor merger with a small gas-rich galaxy.

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The star formation history and evolution of the circumnuclear region of M100

Abstract: The definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1111/j.1365-2966.2006.10751.

Cited by 87 publications

References 71 publications

A Sinfoni View of Galaxy Centers: Morphology and Kinematics of Five Nuclear Star-Formation Rings

A Sinfoni View of Galaxy Centers: Morphology and Kinematics of Five Nuclear Star-Formation Rings

On the morphology of sigma-drop galaxies

Star Formation in the Central Regions of Galaxies

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