STAR CLUSTER COMPLEXES IN NGC 1427AM. D. Mora1, J. Chanam´e1, and T. H. Puzia1 We report the...
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XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes RevMexAA (Serie de Conferencias), 44, 51–51 (2014) STAR CLUSTER COMPLEXES IN NGC 1427A M. D. Mora 1 , J. Chanam´ e 1 , and T. H. Puzia 1 We report the characterisation of star clus- ter complexes in the dIrr galaxy NGC 1427A, presently infalling towards the core of the For- nax galaxy cluster, likely for the first time. Using the spatial resolution of HST/ACS and auxiliary VLT/FORS ground-based observa- tions, we study the properties of the most re- cent episodes of star formation in this gas-rich galaxy, the only one of its type near the core of the Fornax cluster. Gas-rich galaxies in dense environments such as galaxy clusters and massive groups are deeply af- fected by a number of possible types of interactions with the cluster environment, which make their evo- lution radically different than that of field galax- ies. This is the case of NGC 1427A where we study the structural and photometric properties 12 bright young star cluster complexes with exceptionally blue colors (see Fig.1). The comparison of our broadband near-UV/optical photometry with GALEV (Kotulla et al. 2009) simple stellar population models yields ages below ∼ 4 × 10 6 years and stellar masses from a few thousand up to ∼ 3× 10 4 M ⊙ , slightly depen- dent on the assumption of cluster metallicity. Their grouping is consistent with hierarchical and fractal star cluster formation. Object sizes (FWHMs), mea- sured using the ISHAPE (Larsen 1999) task, cor- respond to relatively extended structures similar to star-cluster complexes already seen in other galaxies, with sizes from few parsecs up to tens of parsecs for the larger ones. Fig 1 shows the colors and sizes of our 12 star cluster complexes. Colors are consistent with the youngest population in agreement with the youngest ages provided by the SSP models. All these evidence hints at the very recent star formation episode in this galaxy. REFERENCES Kotulla, R., Fritze, U., Weilbacher, P., & Anders, P. 2009, MNRAS, 396, 462 Larsen, S. S. 1999, A&AS, 139, 393 1 Instituto de Astrof´ ısica, Pontificia Universidad Cat´ olica de Chile, Vicu˜ na Mackenna 4860, 7820436, Macul, Santiago, Chile ([email protected]). Fig. 1. Filled red and blue circles correspond to star cluster complexes. Top panel: Color-magnitude diagram of extended sources in NGC1427A. At the distance of NGC1427A 1 pix corresponds to ∼4 pc. Bottom: Color- color diagram. Tracks correspond to GALEV SSP mod- els for sub solar, solar and super solar metallicity. The filled square corresponds to the averaged color-color com- plex, which is consistent with the solar metallicity track. 51
Transcript of STAR CLUSTER COMPLEXES IN NGC 1427AM. D. Mora1, J. Chanam´e1, and T. H. Puzia1 We report the...
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RevMexAA (Serie de Conferencias), 44, 51–51 (2014)
STAR CLUSTER COMPLEXES IN NGC 1427A
M. D. Mora1, J. Chaname1, and T. H. Puzia1
We report the characterisation of star clus-ter complexes in the dIrr galaxy NGC 1427A,presently infalling towards the core of the For-nax galaxy cluster, likely for the first time.Using the spatial resolution of HST/ACS andauxiliary VLT/FORS ground-based observa-tions, we study the properties of the most re-cent episodes of star formation in this gas-richgalaxy, the only one of its type near the coreof the Fornax cluster.
Gas-rich galaxies in dense environments such asgalaxy clusters and massive groups are deeply af-fected by a number of possible types of interactionswith the cluster environment, which make their evo-lution radically different than that of field galax-ies. This is the case of NGC 1427A where we studythe structural and photometric properties 12 brightyoung star cluster complexes with exceptionally bluecolors (see Fig.1). The comparison of our broadbandnear-UV/optical photometry with GALEV (Kotullaet al. 2009) simple stellar population models yieldsages below ∼ 4 × 106 years and stellar masses froma few thousand up to ∼ 3× 104 M⊙, slightly depen-dent on the assumption of cluster metallicity. Theirgrouping is consistent with hierarchical and fractalstar cluster formation. Object sizes (FWHMs), mea-sured using the ISHAPE (Larsen 1999) task, cor-respond to relatively extended structures similar tostar-cluster complexes already seen in other galaxies,with sizes from few parsecs up to tens of parsecs forthe larger ones. Fig 1 shows the colors and sizes ofour 12 star cluster complexes. Colors are consistentwith the youngest population in agreement with theyoungest ages provided by the SSP models.
All these evidence hints at the very recent starformation episode in this galaxy.
REFERENCES
Kotulla, R., Fritze, U., Weilbacher, P., & Anders, P. 2009,
MNRAS, 396, 462
Larsen, S. S. 1999, A&AS, 139, 393
1Instituto de Astrofısica, Pontificia Universidad Catolicade Chile, Vicuna Mackenna 4860, 7820436, Macul, Santiago,Chile ([email protected]).
Fig. 1. Filled red and blue circles correspond to star
cluster complexes. Top panel: Color-magnitude diagram
of extended sources in NGC1427A. At the distance of
NGC1427A 1 pix corresponds to ∼4 pc. Bottom: Color-
color diagram. Tracks correspond to GALEV SSP mod-
els for sub solar, solar and super solar metallicity. The
filled square corresponds to the averaged color-color com-
plex, which is consistent with the solar metallicity track.
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