%0 Generic %1 roediger2014stripped %A Roediger, E. %A Kraft, R. P. %A Nulsen, P. E. J. %A Forman, W. R. %A Machacek, M. %A Randall, S. %A Jones, C. %A Churazov, E. %A Kokotanekova, R. %D 2014 %K halo hot icm pressure ram %T Stripped elliptical galaxies as probes of ICM physics: I. Tails, wakes, and flow patterns in and around stripped ellipticals %U http://arxiv.org/abs/1409.6300 %X (abridged) Elliptical cluster galaxies are successively stripped of their gaseous atmospheres due to their motion through the ICM. The stripped galactic gas forms a 'tail' in the galaxy's wake. Deep X-ray observations reveal the fine-structure of the gas tail and of the interface between galactic gas and ICM. This fine-structure depends on dynamic conditions (galaxy potential, initial gas contents, orbit in the host cluster), stripping stage (early infall, pre-/post-pericenter passage), and on the still ill-constrained ICM plasma properties (thermal conductivity, viscosity, magnetic field structure). In a series of papers, we aim at disentangling dynamic and plasma effects in order to use observed stripped ellipticals as probes of the ICM plasma properties. This first paper determines flow phases and flow patterns of successive gas stripping by means of hydrodynamical simulations. During quasi-steady stripping, the flow of ICM around the remnant atmosphere is similar to the flow around solid bodies, including a 'deadwater region' downstream of the remnant atmosphere. The size and shape of the galaxy's remnant atmosphere is shaped by the ambient flow. Gas removal takes place predominantly at the sides of the remnant atmosphere. The downstream atmosphere is shaped into a tail because it is shielded from the ICM wind and thus is not stripped easily. This remnant tail contains only unstripped, unmixed galactic gas. Paper II of this series describes the effect of viscosity on flow patterns and resulting observable features. While the qualitative results are generic, we aim at the most direct comparison to observations and tailored our simulations to the Virgo elliptical galaxy M89 (NGC 4552). Paper III of this series compares in detail new deep Chandra and archival XMM-Newton observations to our simulations.

@misc{roediger2014stripped, abstract = {(abridged) Elliptical cluster galaxies are successively stripped of their gaseous atmospheres due to their motion through the ICM. The stripped galactic gas forms a 'tail' in the galaxy's wake. Deep X-ray observations reveal the fine-structure of the gas tail and of the interface between galactic gas and ICM. This fine-structure depends on dynamic conditions (galaxy potential, initial gas contents, orbit in the host cluster), stripping stage (early infall, pre-/post-pericenter passage), and on the still ill-constrained ICM plasma properties (thermal conductivity, viscosity, magnetic field structure). In a series of papers, we aim at disentangling dynamic and plasma effects in order to use observed stripped ellipticals as probes of the ICM plasma properties. This first paper determines flow phases and flow patterns of successive gas stripping by means of hydrodynamical simulations. During quasi-steady stripping, the flow of ICM around the remnant atmosphere is similar to the flow around solid bodies, including a 'deadwater region' downstream of the remnant atmosphere. The size and shape of the galaxy's remnant atmosphere is shaped by the ambient flow. Gas removal takes place predominantly at the sides of the remnant atmosphere. The downstream atmosphere is shaped into a tail because it is shielded from the ICM wind and thus is not stripped easily. This remnant tail contains only unstripped, unmixed galactic gas. Paper II of this series describes the effect of viscosity on flow patterns and resulting observable features. While the qualitative results are generic, we aim at the most direct comparison to observations and tailored our simulations to the Virgo elliptical galaxy M89 (NGC 4552). Paper III of this series compares in detail new deep Chandra and archival XMM-Newton observations to our simulations.}, added-at = {2014-09-24T10:06:19.000+0200}, author = {Roediger, E. and Kraft, R. P. and Nulsen, P. E. J. and Forman, W. R. and Machacek, M. and Randall, S. and Jones, C. and Churazov, E. and Kokotanekova, R.}, biburl = {https://www.bibsonomy.org/bibtex/22a0b1b8018c12bc47224fe88549f1411/miki}, description = {[1409.6300] Stripped elliptical galaxies as probes of ICM physics: I. Tails, wakes, and flow patterns in and around stripped ellipticals}, interhash = {9bce8289c33fc87a7bc791ae73184e58}, intrahash = {2a0b1b8018c12bc47224fe88549f1411}, keywords = {halo hot icm pressure ram}, note = {cite arxiv:1409.6300Comment: submitted to ApJ. 15 pages, 10 figures}, timestamp = {2014-09-24T10:06:19.000+0200}, title = {Stripped elliptical galaxies as probes of ICM physics: I. Tails, wakes, and flow patterns in and around stripped ellipticals}, url = {http://arxiv.org/abs/1409.6300}, year = 2014 }