Circumnuclear Star Formation in the Early-Type Resonance Ring Barred Spiral Galaxy NGC 1326

Buta, Ronald J.; Treuthardt, P.; Byrd, G. G.; Crocker, D. A.

doi:10.1086/301531

Cited by 38 publications

(65 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We do not detect emission within the ring and near the nucleus (central r ≈ 3 region). With our data, we confirm the asymmetry of the ring reported by Buta et al (2000) from the HST image of the Hα flux; our data is less affected by extinction than their optical data.…”

Section: Ionised Gassupporting

confidence: 88%

“…Crocker et al (1996) found that the inner ring is emitting 83% of the Hα luminosity. Buta et al (2000) detected an asymmetric Hα emission in the ring with less emission on the west side, which Combes et al (2019) do not see from CO(3-2) emission and thereby conclude that it is an extinction effect. Also the Buta et al (2000) analysis of two-colour plots revealed that about 80% of the stellar clusters in the ring are <50 Myr in age.…”

Section: Introductionmentioning

confidence: 82%

“…Buta et al (2000) detected an asymmetric Hα emission in the ring with less emission on the west side, which Combes et al (2019) do not see from CO(3-2) emission and thereby conclude that it is an extinction effect. Also the Buta et al (2000) analysis of two-colour plots revealed that about 80% of the stellar clusters in the ring are <50 Myr in age. Velocity fields suggest that the nuclear ring lies near the turn-over radius of the rotation curves (Storchi-Bergmann et al 1996;Buta et al 1998).…”

Section: Introductionmentioning

confidence: 82%

“…The total Brγ emission flux, in the part of the ring that we observe in our FOV, is F Brγ = 1.2 × 10 −14 erg s −1 cm −2 , which leads to an SFR ≈ 0.2 M yr −1 . Buta et al (2000) estimated the SFR in the nuclear ring of NGC 1326 using the extinction corrected Hα line (F Hα = 1.04 × 10 −12 erg s −1 ) and UV emission. For an area of 0.91 kpc 2 these authors find SFR ≈ 1.1 M yr −1 kpc −2 .…”

Section: Star Formation Ratesmentioning

confidence: 99%

See 3 more Smart Citations

Central kiloparsec of NGC 1326 observed with SINFONI

Fazeli

Busch

Eckart

et al. 2020

A&A

View full text Add to dashboard Cite

Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.

show abstract

Section: Ionised Gassupporting

confidence: 88%

Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 82%

Section: Star Formation Ratesmentioning

confidence: 99%

See 2 more Smart Citations

Central kiloparsec of NGC 1326 observed with SINFONI

Fazeli

Busch

Eckart

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…These results are comparable to the slopes of $ À2 found in other galaxies, such as the Antennae starburst galaxies (Whitmore et al 1999), the circumnuclear rings of NGC 2997 (Maoz et al 1996;), NGC 6951 , and NGC 1326 (Buta et al 2000), in NGC 7252 (Miller et al 1997), and in the interacting galaxies IC 2163 and NGC 2207 . A value of about À2 is also typical for the SSCs observed in some starburst galaxies, as shown by the results of Meurer et al (1995), Barth et al (1995), Maoz et al (1996), Carlson et al (1998), andMaoz et al (2001).…”

Section: Luminosity Functionsupporting

confidence: 87%

Circumnuclear Star Formation in the Spiral Galaxy NGC 3310

Elmegreen

Chromey

McGrath

et al. 2002

The Astronomical Journal

View full text Add to dashboard Cite

The star-forming properties of the circumnuclear ring in the starburst spiral galaxy NGC 3310 have been studied in B, I, J, H, and K bands using images from KPNO and from the HST archives. The colors and magnitudes of the star-forming regions indicate ages less than 10 Myr and masses of 10 4 to 10 5 M for the largest clumps. The luminosity distribution function of the diffuse circumnuclear clusters has a slope of about À2, which is typical of results both in circumnuclear rings and in the main disks of other galaxies. There are 17 candidate super star clusters (SSCs), primarily in the innermost southern spiral arm. The broad wavelength coverage allows a determination of reddening in the vicinity of the SSCs, which appears to be small. The locations of the SSCs in the circumnuclear ring and in an inner spiral are coincident with radio continuum and emission peaks, and may be the result of a suspected cannibalization of a dwarf galaxy in the last 10 Myr.

show abstract

Secular Evolution and the Growth of Pseudobulges in Disk Galaxies

Kormendy

Cornell

2004

Astrophysics and Space Science Library

View full text Add to dashboard Cite

Galactic evolution is in transition from an early universe dominated by hierarchical clustering to a future dominated by secular processes. These result from interactions involving collective phenomena such as bars, oval disks, spiral structure, and triaxial dark halos. A detailed review is in Kormendy & Kennicutt (2004). This paper provides a summary illustrated in part with different galaxies. Figure 2 summarizes how bars rearrange disk gas into outer rings, inner rings, and galactic centers, where high gas densities feed starbursts. Consistent with this picture, many barred and oval galaxies are observed to have dense central concentrations of gas and star formation. Measurements of star formation rates show that bulge-like stellar densities are constructed on timescales of a few billion years. We conclude that secular evolution builds dense central components in disk galaxies that look like classical -that is, merger-builtbulges but that were made slowly out of disk gas. We call these pseudobulges.Many pseudobulges can be recognized because they have characteristics of disks -(1) flatter shapes than those of classical bulges, (2) correspondingly large ratios of ordered to random velocities, (3) small velocity dispersions σ with respect to the Faber-Jackson correlation between σ and bulge luminosity, (4) spiral structure or nuclear bars, (5) nearly exponential brightness profiles, and (6) starbursts. These structures occur preferentially in barred and oval galaxies in which secular evolution should be most rapid. Thus a variety of observational and theoretical results contribute to a new paradigm of secular evolution that complements hierarchical clustering.

show abstract

Circumnuclear Star Formation in the Early-Type Resonance Ring Barred Spiral Galaxy NGC 1326

Cited by 38 publications

References 35 publications

Central kiloparsec of NGC 1326 observed with SINFONI

Central kiloparsec of NGC 1326 observed with SINFONI

Circumnuclear Star Formation in the Spiral Galaxy NGC 3310

Secular Evolution and the Growth of Pseudobulges in Disk Galaxies

Contact Info

Product

Resources

About