%0 Generic %1 mulia2016cluster %A Mulia, Alexander J. %A Chandar, Rupali %A Whitmore, Bradley C. %D 2016 %K cluster destruction formation %T Star Cluster Formation and Destruction in the Merging Galaxy NGC 3256 %U http://arxiv.org/abs/1607.03577 %X We use the Advanced Camera for Surveys on the Hubble Space Telescope to study the rich population of young massive star clusters in the main body of NGC 3256, a merging pair of galaxies with a high star formation rate (SFR) and SFR per unit area ($\Sigma_SFR$). These clusters have luminosity and mass functions that follow power laws, $dN/dL L^\alpha$ with $= -2.23 0.07$, and $dN/dM M^\beta$ with $= -1.86 0.34$ for $< 10$ Myr clusters, similar to those found in more quiescent galaxies. The age distribution can be described by $dN/d^ \gamma$, with $-0.67 0.08$ for clusters younger than about a few hundred million years, with no obvious dependence on cluster mass. This is consistent with a picture where $80 \%$ of the clusters are disrupted each decade in time. We investigate the claim that galaxies with high $\Sigma_SFR$ form clusters more efficiently than quiescent systems by determining the fraction of stars in bound clusters ($\Gamma$) and the CMF/SFR statistic (CMF is the cluster mass function) for NGC 3256 and comparing the results with those for other galaxies. We find that the CMF/SFR statistic for NGC 3256 agrees well with that found for galaxies with $\Sigma_SFR$ and SFRs that are lower by $1-3$ orders of magnitude, but that estimates for $\Gamma$ are only robust when the same sets of assumptions are applied. Currently, $\Gamma$ values available in the literature have used different sets of assumptions, making it more difficult to compare the results between galaxies.

@misc{mulia2016cluster, abstract = {We use the Advanced Camera for Surveys on the Hubble Space Telescope to study the rich population of young massive star clusters in the main body of NGC 3256, a merging pair of galaxies with a high star formation rate (SFR) and SFR per unit area ($\Sigma_{\rm{SFR}}$). These clusters have luminosity and mass functions that follow power laws, $dN/dL \propto L^{\alpha}$ with $\alpha = -2.23 \pm 0.07$, and $dN/dM \propto M^{\beta}$ with $\beta = -1.86 \pm 0.34$ for $\tau < 10$ Myr clusters, similar to those found in more quiescent galaxies. The age distribution can be described by $dN/d\tau \propto \tau ^ \gamma$, with $\gamma \approx -0.67 \pm 0.08$ for clusters younger than about a few hundred million years, with no obvious dependence on cluster mass. This is consistent with a picture where $\sim 80 \%$ of the clusters are disrupted each decade in time. We investigate the claim that galaxies with high $\Sigma_{\rm{SFR}}$ form clusters more efficiently than quiescent systems by determining the fraction of stars in bound clusters ($\Gamma$) and the CMF/SFR statistic (CMF is the cluster mass function) for NGC 3256 and comparing the results with those for other galaxies. We find that the CMF/SFR statistic for NGC 3256 agrees well with that found for galaxies with $\Sigma_{\rm{SFR}}$ and SFRs that are lower by $1-3$ orders of magnitude, but that estimates for $\Gamma$ are only robust when the same sets of assumptions are applied. Currently, $\Gamma$ values available in the literature have used different sets of assumptions, making it more difficult to compare the results between galaxies.}, added-at = {2016-07-14T10:55:20.000+0200}, author = {Mulia, Alexander J. and Chandar, Rupali and Whitmore, Bradley C.}, biburl = {https://www.bibsonomy.org/bibtex/23df5e45e28945564c47a369383dc188f/miki}, description = {[1607.03577] Star Cluster Formation and Destruction in the Merging Galaxy NGC 3256}, interhash = {1933dc562f4e47ff7d7c3f6e2638e7ad}, intrahash = {3df5e45e28945564c47a369383dc188f}, keywords = {cluster destruction formation}, note = {cite arxiv:1607.03577Comment: 18 pages, 15 figures, accepted for publication in ApJ. Image quality on some figures has been degraded to comply with arxiv file limitations}, timestamp = {2016-07-14T10:55:20.000+0200}, title = {Star Cluster Formation and Destruction in the Merging Galaxy NGC 3256}, url = {http://arxiv.org/abs/1607.03577}, year = 2016 }