is also thankful to Kathy Vivas and the staff of CTIO for their help and support while preparing and executing the DECam observations, and for the LSST helpdesk staff for assistance while adapting the LSST pipeline for use with DECam data. We also thank Eric Peng and Thomas Puzia for their generous permission to use their N662 narrowband filter for our DECam observations. would like to thank Enrichetta Iodice, Paolo Serra, and William Keel for useful discussion, and Amidou Sorgho for the GBT beam comparison. Note = "Funding Information: We thank the anonymous referee whose comments helped improve the quality of this paper. The high surviving H I content of the galaxies may suggest that the substructure or intragroup medium can protect them from the harshest effects of ram pressure, or that the galaxies are in fact on more tangential orbits.", The drag seen in the H I tails supports our preferred scenario that NGC 3312 and NGC 3314a are moving toward us as part of a foreground substructure which has already passed its pericenter and is on out fall from the cluster. In addition, we used the H I and stellar morphologies, combined with a Beta model of the hot intracluster medium, to constrain the real distances of the galaxies to the cluster center, and we used the chance alignment of NGC 3314b behind NGC 3314a to break the degeneracy between whether the galaxies are in front or in back of the cluster. A fourth ring galaxy at the same velocity does not show signs of ram pressure in H I. The estimated stellar mass in the tails is an order of magnitude less than the H I mass. yr- 1, and extends ∼ 30- 60 kpc from the main disk.In particular, we quantify the stripped material in NGC 3312, and NGC 3314a, which makes up between 8% and 35% of the gas still in the disk, is forming stars at ∼ 0.5 M We present a multiwavelength study of the center of the Hydra I galaxy cluster, including exquisite new MeerKAT H I and DECam Hα imaging which reveal conclusive evidence for ram pressure stripping in NGC 3312, NGC 3314a, and NGC 3314b through compressed H I contours, well-defined H I tails, and ongoing star formation in the stripped gas. The high surviving H I content of the galaxies may suggest that the substructure or intragroup medium can protect them from the harshest effects of ram pressure, or that the galaxies are in fact on more tangential orbits.Ībstract = "Cluster substructure and ram pressure stripping in individual galaxies are among the primary pieces of evidence for the ongoing growth of galaxy clusters as they accrete galaxies and groups from their surroundings. Cluster substructure and ram pressure stripping in individual galaxies are among the primary pieces of evidence for the ongoing growth of galaxy clusters as they accrete galaxies and groups from their surroundings.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |