Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Glatt, K.; Grebel, Eva K.; Koch, Andreas

doi:10.1051/0004-6361/201014187

Cited by 170 publications

(245 citation statements)

References 91 publications

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“…4 we also report the age range covered by each evolutionary stage in our CMDs, although these are just estimates which do not take into account the spread of stars due to photometric errors. The youngest populations (a few Myr up to ∼100 Myr) in dwarf irregular galaxies are generally found in concentrated, actively star forming regions, which are located in the center as well as in offset knots (see, e.g., van Dyk et al 1998;Glatt et al 2010). This is clearly observed in the MS and/or BL/RSG density maps of our targets, where the relative star formation is confined to the dwarf's center.…”

Section: Spatial Distribution Of Stellar Populations As a Function Ofmentioning

confidence: 53%

“…This is clearly observed in the MS and/or BL/RSG density maps of our targets, where the relative star formation is confined to the dwarf's center. Active star forming regions tend to turn on and off in adjacent cells with time in a stochastic propagation fashion, with star forming complexes having lifetimes on the order of 10 2 Myr and sizes of up to some hundreds of pc in diameter (Seiden et al 1979;Dohm-Palmer et al 1997;Grebel & Brandner 1998;Dohm-Palmer et al 2002;Weisz et al 2008;Glatt et al 2010;Crnojević et al 2011a). Interestingly, the triangular shape of KK182 comes from an offset knot of star formation which is clearly recognized as a local enhancement in its MS and BL density maps, while it fades away in the RSG map.…”

Section: Spatial Distribution Of Stellar Populations As a Function Ofmentioning

confidence: 99%

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A close look at the Centaurus A group of galaxies

Crnojević

Grebel

Cole

2012

A&A

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Aims. We study a sample of five dwarf irregular galaxies in the CenA/M 83 group, which are companions to the giant elliptical CenA. We aim at deriving their physical properties over their lifetime and compare them to those of dwarfs located in different environments. Methods. We use archival HST/ACS data and apply synthetic color-magnitude diagram fitting in order to reconstruct the past star formation activity of the target galaxies. Results. The average star formation rate for the studied galaxies ranges from 10 −3 M yr −1 up to ∼7 × 10 −2 M yr −1 , and their mean metallicities correlate with their luminosities (from [Fe/H] ∼ −1.4 up to ∼−1.0). The form of the star formation histories varies across the sample, with quiescent periods alternating with intermittent enhancements in the star formation (from a few up to several times the average lifetime value). The dwarfs in this sample formed ∼35% to 60% of their stellar content prior to ∼5 Gyr ago. Conclusions. The resulting star formation histories for the CenA companions are similar to those found for comparable Local Group and M 81 group dwarfs. We consider this sample of dwarfs together with five previously studied M 83 dwarf irregular companions. We find no trend of the average star formation rate with tidal index or distance from the main galaxy of the group. However, dwarfs with higher baryonic masses do show higher average star formation rates, underlining the importance of intrinsic properties in governing the evolution of these galaxies. On the other hand, there is also a clear trend when looking at the recent (∼0.5−1 Gyr) level of activity. Namely, dwarfs within a denser region of the group appear to have had their star formation quenched while dwarfs located in the group outskirts show a wide range of possible star formation rates, thus indicating that external processes play a fundamental role, complementary to mass, in shaping the star formation histories of dwarf galaxies.

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Section: Spatial Distribution Of Stellar Populations As a Function Ofmentioning

confidence: 53%

Section: Spatial Distribution Of Stellar Populations As a Function Ofmentioning

confidence: 99%

A close look at the Centaurus A group of galaxies

Crnojević

Grebel

Cole

2012

A&A

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“…They conclude that the last tidal interaction between the MCs has triggered the formation of both clusters and field stars. Moreover, Glatt et al (2010) find two periods of enhanced cluster formation at 125 Myr and 800 Myr in the LMC and at 160 Myr and 630 Myr in the SMC. The cluster ages were determined by fitting Padova and Geneva isochrones.…”

Section: Introductionmentioning

confidence: 80%

Age – metallicity relation in the Magellanic Clouds clusters

Livanou

Dapergolas

Kontizas

et al. 2013

A&A

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Aims.We study small open star clusters, using Strömgren photometry to investigate a possible dependence between age and metallicity in the Magellanic Clouds (MCs). Our goals are to trace evidence of an age metallicity relation (AMR) and correlate it with the mutual interactions of the two MCs and to correlate the AMR with the spatial distribution of the clusters. In the Large Magellanic Cloud (LMC), the majority of the selected clusters are young (up to 1 Gyr), and we search for an AMR at this epoch, which has not been much studied. Methods. We report results for 15 LMC and 8 Small Magellanic Cloud (SMC) clusters, scattered all over the area of these galaxies, to cover a wide spatial distribution and metallicity range. The selected LMC clusters were observed with the 1.54 m Danish Telescope in Chile, using the Danish Faint Object Spectrograph and Camera (DFOSC) with a single 2k × 2k CCD. The SMC clusters were observed with the ESO 3.6 m Telescope, also in Chile, using the ESO Faint Object Spectrograph and Camera (EFOSC). The obtained frames were analysed with the conventional DAOPHOT and IRAF software. We used Strömgren filters in order to achieve reliable metallicities from photometry. Isochrone fitting was used to determine the ages and metallicities. Results. The AMR for the LMC displays a metallicity gradient, with higher metallicities for the younger ages. The AMR for LMC-SMC star clusters shows a possible jump in metallicity and a considerable increase at about 6 × 10 8 yr. It is possible that this is connected to the latest LMC-SMC interaction. The AMR for the LMC also displays a metallicity gradient with distance from the centre. The metallicities in SMC are lower, as expected for a metal-poor host galaxy.

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“…The ages of young star clusters given in Glatt et al (2010) is overplotted on the LSFE maps in Fig. 23.…”

Section: Comparison With the Hi Gas Distribution And Star Clustersmentioning

confidence: 99%

“…In contrast to , Noel et al (2009) did not find any quiescent epoch at the intermediate ages. Glatt et al (2010) studied the SFH of both the clouds based on star clusters with age <1 Gyr. They found that the cluster formation peaks at 160 Myr and 630 Myr for the SMC and 125 Myr and 800 Myr for the LMC.…”

Section: Introductionmentioning

confidence: 99%

The recent star-formation history of the Large and Small Magellanic Clouds

Indu

Subramaniam

2011

A&A

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Aims. Recent interactions between the Large and the Small Magellanic Clouds (LMC and SMC) and the Milky Way can be understood by studying their recent star formation history. This study aims to detect any directional or propagating star formation in the last 500 Myr. Methods. We traced the age of the last star-formation event (LSFE) in the inner Large and Small Magellanic Cloud (L&SMC) using the photometric data in V and I passbands from the Optical Gravitational Lensing Experiment (OGLE-III) and the Magellanic Cloud Photometric Survey (MCPS). The LSFE is estimated from the main sequence turn-off point in the color-magnitude diagram (CMD) of a subregion. After correcting for extinction, the turn-off magnitude is converted to age, which represents the LSFE in a region.Results. The spatial distribution of the age of the LSFE shows that the star-formation has shrunk to within the central regions in the last 100 Myr in both the galaxies. The location as well as age of LSFE is found to correlate well with those of the star cluster in both the Clouds. The SMC map shows two separate concentrations of young star-formation, one near the center and the other near the wing. We detect peaks of star-formation at 0-10 Myr and 90-100 Myr in the LMC, and 0-10 Myr and 50-60 Myr in the SMC. The quenching of star-formation in the LMC is found to be asymmetric with respect to the optical center such that most of the young star forming regions are located to the north and east. On deprojecting the data onto the LMC plane, the recent star-formation appears to be stretched in the northeast direction and the HI gas is found to be distributed preferentially in the north. We found that the centroid is shifted to the north during the time interval 200-40 Myr, whereas it is found to have shifted to the northeast in the last 40 Myr. In the SMC, we detect a shift in the centroid of the population younger than 500 Myr and as young as 40 Myr in the direction of the LMC. Conclusions. We propose that the HI gas in the LMC has been pulled to the north of the LMC in the last 200 Myr because of the gravitational attraction of our Galaxy at the time of perigalactic passage. The shifted HI gas was preferentially compressed in the north during the time interval 200-40 Myr and in the northeast in the last 40 Myr, owing to the motion of the LMC in the Galactic halo. The recent star-formation in the SMC is due to the combined gravitational effect of the LMC and the perigalactic passage.

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Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Cited by 170 publications

References 91 publications

A close look at the Centaurus A group of galaxies

A close look at the Centaurus A group of galaxies

Age – metallicity relation in the Magellanic Clouds clusters

The recent star-formation history of the Large and Small Magellanic Clouds

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