Extremely massive young clusters in NGC 1365

Galliano, E.; Alloin, D.; Pantin, E.; Granato, G. L.; Delva, Pacôme; Silva, L.; Lagage, Pierre-Olivier; Panuzzo, P.

doi:10.1051/0004-6361:20077621

Cited by 29 publications

(32 citation statements)

References 46 publications

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“…We measured the fluxes and the equivalent widths (EW) of the [Ne ii ]

12.81 μ

m emission line and the 6.2 and

11.3 μ

m PAH features fitting Gaussian profiles to the lines and lines to the local continuum. Our measurements of the [Ne ii ] flux for clusters M4, M5 and M6 are in good agreement with those reported by Galliano et al () from ground‐based high angular resolution observations. Since the PAH features are broad, it has been noted in the literature that Gaussian profiles might not be appropriate to measure their flux because a large fraction of the energy in these bands in radiated in the wings.…”

Section: Observationssupporting

confidence: 91%

“…Assuming a foreground screen of dust and adopting the Rieke & Lebofsky () extinction law ( A V / S Si = 16.6), the observed apparent depths of the star‐forming regions in the circumnuclear region of NGC 1365 imply values of the visual extinction of between A V ∼ 4 ± 1 mag and A V ∼ 14 ± 1 mag for the regions of clusters M2+M3, and M4+M5+M6, respectively. The high value of the extinction derived for the latter region is entirely consistent with the values derived by Galliano et al () for the individual clusters using hydrogen recombination lines. Our value of the extinction in the region containing M2 and M3 is higher than the optical estimate for the L2 and L3 H ii regions from Kristen et al ().…”

Section: Spatially Resolved Ir Emission In the Ilr Regionsupporting

confidence: 90%

“…The ages and masses of the mid‐IR clusters (∼6–8 Myr and ∼10 7 M ⊙ , Galliano et al ) and the large amount of molecular gas available in the central regions of this galaxy (Sakamoto et al ) indicate that there is intense ongoing star formation activity there. We can use the IR observations of NGC 1365 to estimate the obscured SFR in the ILR region, and compare it with the unobscured SFR.…”

Section: Spatially Resolved Ir Emission In the Ilr Regionmentioning

confidence: 97%

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Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

Alonso‐Herrero

Sánchez‐Portal

Almeida³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present new far‐infrared (70–500 μm) Herschel Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) imaging observations as well as new mid‐IR Gemini/Thermal‐Region Camera Spectrograph imaging (8.7 and 18.3 μm) and spectroscopy of the inner Lindblad resonance (ILR) region (R < 2.5 kpc) of the spiral galaxy NGC 1365. We complemented these observations with archival Spitzer imaging and spectral mapping observations. The ILR region of NGC 1365 contains a Seyfert 1.5 nucleus and a ring of star formation with an approximate diameter of 2 kpc. The strong star formation activity in the ring is resolved by the Herschel/PACS imaging data, as well as by the Spitzer 24 μm continuum emission, [Ne ii] 12.81 μm line emission, and 6.2 and 11.3 μm PAH emission. The active galactic nucleus (AGN) is the brightest source in the central regions up to λ ∼ 24 μm, but it becomes increasingly fainter in the far‐infrared when compared to the emission originating in the infrared clusters (or groups of them) located in the ring. We modelled the AGN unresolved infrared emission with the clumpy torus models and estimated that the AGN contributes only to a small fraction (∼5 per cent) of the infrared emission produced in the inner ∼5 kpc. We fitted the non‐AGN 24–500 μm spectral energy distribution of the ILR region and found that the dust temperatures and mass are similar to those of other nuclear and circumnuclear starburst regions. Finally we showed that within the ILR region of NGC 1365, most of the ongoing star formation activity is taking place in dusty regions as probed by the 24 μm emission.

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“…We measured the fluxes and the equivalent widths (EW) of the [Ne ii ]

12.81 μ

m emission line and the 6.2 and

11.3 μ

Section: Observationssupporting

confidence: 91%

Section: Spatially Resolved Ir Emission In the Ilr Regionsupporting

confidence: 90%

Section: Spatially Resolved Ir Emission In the Ilr Regionmentioning

confidence: 97%

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Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

Alonso‐Herrero

Sánchez‐Portal

Almeida³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…The nuclear star cluster might easily dominate the observed MIR emission similar to NGC 3125, which would then lead to the observed excess. Note that off-nuclear young clusters with comparable MIR luminosities are found for example in NGC 1365 (Galliano et al 2008) and would be similarly unresolved at the distance of NGC 4303.…”

Section: Ngc 4303 -M 61mentioning

confidence: 88%

Mid-infrared properties of nearby low-luminosity AGN at high angular resolution

Asmus

Gandhi

Smette

et al. 2011

A&A

117

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We present high spatial resolution mid-infrared (MIR) 12 μm continuum imaging of low-luminosity active galactic nuclei (LLAGN) obtained with VLT/VISIR. Our goal is to determine whether the nuclear MIR emission of LLAGN is consistent with the existence of a dusty obscuring torus, the key component of the unification model for AGN. Based on available hard X-ray luminosities and the previously known tight correlation between the hard X-ray and 12 μm luminosities, we selected a sample of 17 nearby LLAGN without available VISIR N-band photometry. Combined with archival VISIR data of 9 additional LLAGN with available X-ray measurements, the dataset represents the bulk of southern LLAGN currently detectable from the ground in the MIR. Of the 17 observed LLAGN, 7 are detected, while upper limits are derived for the 10 non-detections. This increases the total number of AGN detected with VLT/VISIR to more than 50. All detections except NGC 3125 appear point-like on a spatial scale of ∼0.35 . The detections do not significantly deviate from the known MIR-X-ray correlation but exceed it by a factor of ∼10 down to luminosities <10 41 erg/s with a narrow scatter (σ = 0.35 dex, Spearman rank ρ = 0.92). The latter is dominated by the uncertainties in the X-ray luminosity. Interestingly, a similar correlation with a comparable slope but with a normalization differing by ∼2.6 orders of magnitude has been found for local starburst galaxies. In addition, we compared the VISIR data with lower spatial resolution data from Spitzer/IRS and IRAS. By using a scaled starburst template spectral energy distribution and the polycyclic aromatic hydrocarbon (PAH) 11.3 μm emission line, we were able to restrict the maximum nuclear star-formation contamination of the VISIR photometry to 30% for 75% of the LLAGN. Exceptions are NGC 1097 and NGC 1566, which may possess unresolved strong PAH emission. Furthermore, the MIR-X-ray luminosity ratio is unchanged over more than 4 orders of magnitude in accretion rate within the uncertainties. These results are consistent with the existence of the dusty torus in all observed LLAGN, although a jet or accretion disk as origin of the MIR emission cannot be excluded. Finally, because the MIR-X-ray correlation holds for all LLAGN and Seyferts, this is a very useful empirical tool for converting between the MIR and X-ray powers of these nuclei.

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“…Similarly, the whole of the central region of NGC 1365 (Fig. 1.26) is undergoing a starburst (Kristen et al 1997;Galliano et al 2008;Elmegreen et al 2009) A less intense but still prototypical example is NGC 1300 ( Fig. 1.6; Knapen et al 2006;Comerón et al 2010).…”

mentioning

confidence: 99%

Secular evolution in disk galaxies

Kormendy¹

2013

Secular Evolution of Galaxies

124

138

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Self-gravitating systems evolve toward the most tightly bound configuration that is reachable via the evolution processes that are available to them. They do this by spreading -the inner parts shrink while the outer parts expand -provided that some physical process efficiently transports energy or angular momentum outward. The reason is that self-gravitating systems have negative specific heats. As a result, the evolution of stars, star clusters, protostellar and protoplanetary disks, black hole accretion disks and galaxy disks are fundamentally similar. How evolution proceeds then depends on the evolution processes that are available to each kind of self-gravitating system. These processes and their consequences for galaxy disks are the subjects of my lectures and of this Canary Islands Winter School.I begin with a review of the formation, growth and death of bars. Then I review the slow ("secular") rearrangement of energy, angular momentum, and mass that results from interactions between stars or gas clouds and collective phenomena such as bars, oval disks, spiral structure and triaxial dark halos. The "existence-proof" phase of this work is largely over: we have a good heuristic understanding of how nonaxisymmetric structures rearrange disk gas into outer rings, inner rings and stuff dumped onto the center. The results of simulations correspond closely to the morphology of barred and oval galaxies. Gas that is transported to small radii reaches high densities. Observations confirm that many barred and oval galaxies have dense central concentrations of gas and star formation. The result is to grow, on timescales of a few Gyr, dense central components that are frequently mistaken for classical (elliptical-galaxy-like) bulges but that were grown slowly out of the disk (not made rapidly by major mergers). The resulting picture of secular galaxy evolution accounts for the richness observed in galaxy structure.

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Extremely massive young clusters in NGC 1365

Cited by 29 publications

References 46 publications

Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

Mid-infrared properties of nearby low-luminosity AGN at high angular resolution

Secular evolution in disk galaxies

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