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<p>Dear all,</p>
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</p>
<p>Below is the Zoom link for today's OKC Cosmology & Gravity meeting, where our own Raffaella Capasso will present:</p>
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<p><b data-stringify-type="bold" style="box-sizing: inherit; color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">Galaxy
dynamics in clusters</b><span class="c-mrkdwn__br" data-stringify-type="paragraph-break" style="box-sizing: inherit; display: block; height: 8px; color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);"></span><span style="color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">The
phase-space distribution of tracers in galaxy clusters is a powerful tool that can be used to test the mass distribution of dark matter haloes as predicted in large-scale structure cosmological simulations, as well as to provide information about the formation
and evolution of cluster member galaxies. </span><br style="box-sizing: inherit; color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">
<span style="color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">Exploiting analytical and numerical
tools, I analysed the phase-space distribution of gravitationally interacting N-body systems. I performed a dynamical analysis applying the spherically-symmetric Jeans equation, using the cluster’s member galaxies as tracer of its gravitational potential. I
will present the results of this study, performed on a sample of 110 Sunyaev-Zel’dovich effect (SZE) selected galaxy clusters from the South Pole Telescope (SPT). I will compare the resulting dynamical masses to theoretical expectations, and examine the bias
between between these masses and the masses inferred from the SZE observable in a flat ËCDM cosmology consistent with Planck CMB data.</span><br style="box-sizing: inherit; color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">
<span style="color: rgb(29, 28, 29); font-family: Slack-Lato, appleLogo, sans-serif; font-size: 15px; font-variant-ligatures: common-ligatures; orphans: 2; white-space: pre-wrap; widows: 2; background-color: rgb(248, 248, 248);">Finally, I will show how to
extend this analysis to calibrate mass-observable relations, linking the mass of galaxy clusters to readily obtainable observables.</span><br>
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<p><br>
</p>
<p><br>
</p>
<p>Keir Rogers is inviting you to a scheduled Zoom meeting.</p>
<p><br>
</p>
<p>Topic: OKC C&G</p>
<p>Time: Mar 25, 2020 01:15 PM Stockholm</p>
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</p>
<p>Join Zoom Meeting</p>
<p>https://stockholmuniversity.zoom.us/j/113172569</p>
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<p>Meeting ID: 113 172 569</p>
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<p>Meeting ID: 113 172 569</p>
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<p>Meeting ID: 113 172 569</p>
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<p>Hope you will be able to join!</p>
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<p>Best,</p>
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<p>C&G organisers</p>
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