Stephanie Tonnesen

Star Formation in Ram Pressure Stripped Tails

We investigate the impact of star formation and feedback on ram pressure stripping using high-resolution adaptive mesh simulations, building on a previous series of papers that systematically investigated stripping using a realistic model for the interstellar medium, but without star formation. We find that star formation does not significantly affect the rate at which stripping occurs, and only has a slight impact on the density and temperature distribution of the stripped gas, indicating that our previous (gas-only) results are unaffected. For our chosen (moderate) ram pressure strength, stripping acts to truncate star formation in the disc over a few hundred million years, and does not lead to a burst of star formation. Star formation in the bulge is slightly enhanced, but the resulting change in the bulge-to-disc ratio is insignificant. We find that stars do form in the tail, primarily from gas that is ablated from the disc and the cools and condenses in the turbulent wake. The star formation rate in the tail is low, and any contribution to the intracluster light is likely to be very small. We argue that star formation in the tail depends primarily on the pressure in the intracluster medium, rather than the ram pressure strength. Finally, we compare to observations of star formation in stripped tails, finding that many of the discrepancies between our simulation and observed wakes can be accounted for by different intracluster medium pressures.

X-Ray Emission Line Profile Modeling Of Hot Stars

The launch of high-spectral-resolution x-ray telescopes (Chandra, XMM) has provided a host of new spectral line diagnostics for the astrophysics community. In this paper we discuss Doppler-broadened emission line profiles from highly supersonic outflows of massive stars. These outflows, or winds, are driven by radiation pressure and carry a tremendous amount of kinetic energy, which can be converted to x rays by shock-heating even a small fraction of the wind plasma. The unshocked, cold wind is a source of continuum opacity to the x rays generated in the shock-heated portion of the wind. Thus the emergent line profiles are affected by transport through a two-component, moving, optically thick medium. While complicated, the interactions among these physical effects can provide quantitative information about the spatial distribution and velocity of the x-ray-emitting and absorbing plasma in stellar winds. We present quantitative models of both a spherically symmetric wind and a wind with hot plasma confined...

Probing the Dependence of the Intergalactic Medium on Large-scale Environment Using the Low-redshift Lyα Forest

We examine the statistics of the low-redshift Ly-alpha forest in an adaptive mesh refinement hydrodynamic cosmological simulation of sufficient volume to include distinct large-scale environments. We compare our HI column density distribution of absorbers both with recent work and between two highly-refined regions of our simulation: a large-scale overdensity and a large-scale underdensity (on scales of approximately 20 Mpc). We recover the average results presented in Kollmeier et al. (2014) using different simulation methods. We further break down these results as a function of environment to examine the detailed dependence of absorber statistics on large-scale density. We find that the slope of the HI column density distribution in the 10

Erratum: “Chandra HETGS Multiphase Spectroscopy of the Young Magnetic O Star θ1 Orionis C” (ApJ, 628, 986 [2005])

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ERRATUM: “THE TAIL OF THE STRIPPED GAS THAT COOLED: H I, Hα, AND X-RAY OBSERVATIONAL SIGNATURES OF RAM PRESSURE STRIPPING” (2010, ApJ, 709, 1203)

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Testing the Breathing Mode in Intermediate-mass Galaxies and Its Predicted Star Formation Rate-size Anti-correlation

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Enhanced Star Formation in Both Disks and Ram-pressure-stripped Tails of GASP Jellyfish Galaxies

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GASP – XII. The variety of physical processes occurring in a single galaxy group in formation

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THE TAIL OF THE STRIPPED GAS THAT COOLED: H I, Hα, AND X-RAY OBSERVATIONAL SIGNATURES OF RAM PRESSURE STRIPPING (2010, ApJ, 709, 1203)

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