%0 Generic %1 kadowaki2017spectroscopy %A Kadowaki, Jennifer %A Zaritsky, Dennis %A Donnerstein, R. L. %D 2017 %K cluster coma diffuse galaxies ultra %T Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster %U http://arxiv.org/abs/1703.02042 %X We present spectra of 5 ultra-diffuse galaxies (UDGs) in the vicinity of the Coma Cluster obtained with the Multi-Object Double Spectrograph on the Large Binocular Telescope. We confirm 4 of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half light radius $>$ 4.6 kpc) UDG, DF44, the systems we targeted all have projected half light radii $> 2.9$ kpc. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about $45$ Mpc behind the cluster. We observe Balmer and Ca II H & K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars (Fe/H $-1.5$). We also discover the first UDG with OII and OIII emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.

@misc{kadowaki2017spectroscopy, abstract = {We present spectra of 5 ultra-diffuse galaxies (UDGs) in the vicinity of the Coma Cluster obtained with the Multi-Object Double Spectrograph on the Large Binocular Telescope. We confirm 4 of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half light radius $>$ 4.6 kpc) UDG, DF44, the systems we targeted all have projected half light radii $> 2.9$ kpc. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about $45$ Mpc behind the cluster. We observe Balmer and Ca II H \& K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H] $\lesssim -1.5$). We also discover the first UDG with [OII] and [OIII] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.}, added-at = {2017-03-08T10:02:34.000+0100}, author = {Kadowaki, Jennifer and Zaritsky, Dennis and Donnerstein, R. L.}, biburl = {https://www.bibsonomy.org/bibtex/279a4072c8fdad50920a92d68cb96d777/miki}, description = {[1703.02042] Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster}, interhash = {92e76905b899245473e7ac00f34de3ee}, intrahash = {79a4072c8fdad50920a92d68cb96d777}, keywords = {cluster coma diffuse galaxies ultra}, note = {cite arxiv:1703.02042Comment: 5 pages, 4 figures}, timestamp = {2017-03-08T10:02:34.000+0100}, title = {Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster}, url = {http://arxiv.org/abs/1703.02042}, year = 2017 }