Gemini Spectroscopic Survey of Young Star Clusters in Merging/Interacting Galaxies. Iii. The Antennae

Bastian, N.; Trancho, Gelys; Konstantopoulos, I. S.; Miller, Bryan W.

doi:10.1088/0004-637x/701/1/607

Cited by 98 publications

(159 citation statements)

References 78 publications

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“…Taking the metallicity gradient into account, these metallicities (based also on diagnostics little affected by dust extinction) are consistent with the metallicity inferred through the far-IR fine-structure diagnostics. The situations is similar also for the Antennae galaxy, because its gaseous and stellar metallicities are close to or slightly less than the solar metallicity (Bastian et al 2006(Bastian et al , 2009. Although the comparisons discussed above do not provide a tight test for our new metallicity diagnostics based on far-IR fine structure lines, they do at least suggest a broad consistency with other metallicity diagnostics.…”

Section: Comparison With Observational Datamentioning

confidence: 72%

Metallicity diagnostics with infrared fine-structure lines

Nagao

Maiolino

Marconi

et al. 2011

A&A

109

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Although measuring the gas metallicity in galaxies at various redshifts is crucial to constrain galaxy evolutionary scenarios, only rest-frame optical emission lines have been generally used to measure the metallicity. This has prevented us to accurately measure the metallicity of dust-obscured galaxies, and accordingly to understand the chemical evolution of dusty populations, such as ultraluminous infrared galaxies. Here we propose diagnostics of the gas metallicity based on infrared fine-structure emission lines, which are nearly unaffected by dust extinction even the most obscured systems. Specifically, we focus on fine-structure lines arising mostly from Hii regions, not in photo-dissociation regions, to minimize the dependence and uncertainties of the metallicity diagnostics from various physical parameters. Based on photoionization models, we show that the emission-line flux ratio of ([Oiii] .21 can be used to measure and, therefore, account for the dependences on the gas density and ionization parameter, respectively. We show that these diagnostic fine-structure lines are detectable with Herschel in luminous infrared galaxies out z ∼ 0.4. Metallicity measurements with these fine-structure lines will be feasible at relatively high redshift (z ∼ 1 or more) with SPICA, the future infrared space observatory.

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Section: Comparison With Observational Datamentioning

confidence: 72%

Metallicity diagnostics with infrared fine-structure lines

Nagao

Maiolino

Marconi

et al. 2011

A&A

109

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“…Bastian et al 2009). The distribution can be considered to be independent of cluster formation history if the galaxy is known to have a quiescent history with a constant low star formation rate.…”

Section: ) While the Bottom Plot Includes All Clusters Below 100mentioning

confidence: 99%

Properties of the cluster population of NGC 1566 and their implications

Hollyhead

Adamo

Bastian

et al. 2016

Mon. Not. R. Astron. Soc.

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We present results of a photometric study into the cluster population of NGC 1566, a nearby grand design spiral galaxy, sampled out to a Galactocentric radius of ≈ 5.5 kpc. The shape of the mass-limited age distribution shows negligible variation with radial distance from the centre of the galaxy, and demonstrates three separate sections, with a steep beginning, flat middle and steep end. The luminosity function can be approximated by a power law at lower luminosities with evidence of a truncation at higher luminosity. The power law section of the luminosity function of the galaxy is best fitted by an index ≈ −2, in agreement with other studies, and is found to agree with a model luminosity function, which uses an underlying Schechter mass function. The recovered power law slope of the mass distribution shows a slight steepening as a function of galactocentric distance, but this is within error estimates. It also displays a possible truncation at the high mass end. Additionally, the cluster formation efficiency (Γ) and the specific U-band luminosity of clusters (T L (U )) are calculated for NGC 1566 and are consistent with values for similar galaxies. A difference in NGC 1566, however, is that the fairly high star formation rate is in contrast with a low Σ SF R and Γ, indicating that Γ can only be said to depend strongly on Σ SF R , not the star formation rate.

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“…We adopt the definition of Whitmore (2003) who defined "young" as having an age less than 500 Myr and "massive" as having masses ranging from 10 3 M to 10 8 M . Individual YMCs were analyzed in detail by Bastian et al (2006b), Mengel et al (2008), and Bastian et al (2009). The combined dataset of the three publications demonstrates that the median size of YMCs in the mass range between 10 5 M and 10 6 M is about 4 pc.…”

Section: An Eo Formation Scenariomentioning

confidence: 99%

A catalog of extended clusters and ultra-compact dwarf galaxies

Kroupa

2012

A&A

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Context. In the past decade, very extended old stellar clusters with masses in the range from a few 10 4 to 10 8 M and effective radii larger than 10 pc have been found in various types of galaxies in different environments. Objects with masses comparable to normal globular clusters (GCs) are called extended clusters (ECs), while objects with masses in the dwarf galaxy regime are called ultra-compact dwarf galaxies (UCDs). Aims. The paper analyses the observational parameters total luminosity, M V , effective radius, r eff , and projected distance to the host galaxy, R proj , of all known ECs and UCDs and the dependence of these parameters on the type and the total luminosity of their host galaxy. Methods. We searched the available literature to compile a catalog of star clusters with effective radii larger than 10 pc. As there is no clear distinction between ECs and UCDs, both types of objects will be called extended stellar objects -abbreviated "EOs" -in this paper.Results. In total, we found 813 EOs of which 171 are associated with late-type galaxies and 642 EOs associated with early-type galaxies. EOs cover a luminosity range from about M V = −4 to −14 mag. However, the vast majority of EOs brighter than M V = −10 mag are associated with giant elliptical galaxies. At each magnitude extended objects are found with effective radii between 10 pc and an upper size limit, which shows a clear trend: the more luminous the object the larger is the upper size limit. For EOs associated with early-and late-type galaxies, the EO luminosity functions peak at −6.40 mag and −6.47 mag, respectively, which is about one magnitude fainter than the peak of the GC luminosity function. EOs and GCs form a coherent structure in the r eff vs. M V parameter space, while there is a clear gap between EOs and early-type dwarf galaxies. However, there is a small potential overlap at the high-mass end, where the most extended EOs are close to the parameters of some compact elliptical galaxies. We compare the EO sample with the numerical models of a previous paper and conclude that the parameters of the EO sample as a whole can be very well explained by a star cluster origin, where EOs are the results of merged star clusters of cluster complexes.

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Gemini Spectroscopic Survey of Young Star Clusters in Merging/Interacting Galaxies. Iii. The Antennae

Cited by 98 publications

References 78 publications

Metallicity diagnostics with infrared fine-structure lines

Metallicity diagnostics with infrared fine-structure lines

Properties of the cluster population of NGC 1566 and their implications

A catalog of extended clusters and ultra-compact dwarf galaxies

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