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<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif">Monday 4<sup>th</sup> November A113 CAPT, 3pm – Theoretical Physics Student Seminar<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">Altay Etkin (Southampton)</span><o:p></o:p></p>
<p class="xmsonormal"><i><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">Late-Time Quantum Chaos and (Non)-Orientable Jackiw-Teitelboim Gravity<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",serif">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif">Tuesdays at 11am, CAPT Foyer – Astro Coffee</span></b><o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif"> </span></b><o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif">Tuesday 5<sup>th</sup> November, A113 CAPT at 11am – Astronomy Journal Club</span></b><o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif"> </span></b><o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",serif">Tuesday 5<sup>th</sup> November, A113 CAPT at 12.30pm – Particle Cosmology and Gravity Seminar</span></b><o:p></o:p></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">Yuyo Mo (Higgs Centre, Edinburgh)</span><o:p></o:p></p>
<p class="xmsonormal"><i><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">From On-shell amplitude in AdS to Cosmological correlators</span></i><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black"> <o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="font-family:"Aptos",serif;color:black">We will begin by discussing the motivation and setup of Mellin-momentum amplitudes, along with several examples, including the Feynman rules and their associated pole structures. Following
this, we will present the recursive on-shell bootstrap process, which is designed to compute higher-point Mellin-momentum amplitudes for YM and GR in AdS space. Additionally, the bootstrap can be used to derive the Class I soft theorem for Mellin-momentum
amplitudes in a diagrammatic fashion. If time permits, we will also introduce a recursive method for finishing the bulk scalar integrals, which connects Mellin-momentum amplitudes to boundary CFT correlators. This process leads to the wavefunction coefficients
through wick rotation, thereby providing the cosmological correlators. This talk is based on the works [2305.13894], [2402.09111], [2407.16052], and [2410.04875]. <o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-family:"Aptos",serif;color:black"><o:p> </o:p></span></p>
<p class="MsoNormal"><span style="color:black">Link to join: <a href="https://teams.microsoft.com/l/meetup-join/19%3ameeting_OGM3OTk5NzQtZWEwZS00ZmUyLTk3MGUtZjFhY2M5OTU2MjI1%40thread.v2/0?context=%7b%22Tid%22%3a%2267bda7ee-fd80-41ef-ac91-358418290a1e%22%2c%22Oid%22%3a%22f3250584-4b5f-48fa-a897-08e77f2246b7%22%7d" target="_blank" title="https://teams.microsoft.com/l/meetup-join/19%3ameeting_OGM3OTk5NzQtZWEwZS00ZmUyLTk3MGUtZjFhY2M5OTU2MjI1%40thread.v2/0?context=%7b%22Tid%22%3a%2267bda7ee-fd80-41ef-ac91-358418290a1e%22%2c%22Oid%22%3a%22f3250584-4b5f-48fa-a897-08e77f2246b7%22%7d" id="OWA3c051b92-9856-54cd-c7c0-3957c93660e0">
https://teams.microsoft.com/l/meetup-join/19%3ameeting_OGM3OTk5NzQtZWEwZS00ZmUyLTk3MGUtZjFhY2M5OTU2MjI1%40thread.v2/0?context=%7b%22Tid%22%3a%2267bda7ee-fd80-41ef-ac91-358418290a1e%22%2c%22Oid%22%3a%22f3250584-4b5f-48fa-a897-08e77f2246b7%22%7d</a><o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos Display",serif">---</span><o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",serif">Thursday 7<sup>th</sup> November at 1pm, A113 CAPT – Astronomy Lunch Talk</span></b><o:p></o:p></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">Hua Gao<o:p></o:p></span></p>
<p class="xmsonormal"><i><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">IllustrisTNG in the HSC-SSP: No Shortage of Thin Disk Galaxies in TNG50<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">We perform a thorough analysis of the projected shapes of nearby galaxies in both observations and cosmological simulations. We implement a forward-modeling approach
to overcome the limitations in previous studies, which hinder accurate comparisons between observations and simulations. We measure axis ratios of z = 0 (snapshot 99) TNG50 galaxies from their synthetic Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP)
images and compare them with those obtained from real HSC-SSP images of a matched galaxy sample. Remarkably, the comparison shows excellent agreement between the observations and the TNG50 simulation, challenging previous claims that ΛCDM models underproduced
the abundance of thin galaxies. Specifically, for galaxies with stellar masses 10</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⩽</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">log(M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⋆</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">/M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⊙</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">)</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⩽</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">11.5,
we find </span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">≲</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">0.1</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">σ</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">
tensions between the observations and the simulation, a stark contrast to the previously reported
</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">≳</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">10</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">σ</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">
tensions. We reveal that low-mass galaxies (M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⋆≲</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">10^9.5M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⊙</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">)
in TNG50 are thicker than their observed counterparts in HSC-SSP and attribute this to the spurious dynamical heating effects that artificially puff up galaxies. We also find that, despite the overall broad agreement, TNG50 galaxies are more concentrated than
the HSC-SSP ones at the low- and high-mass end of the stellar mass range of 9.0</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⩽</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">log(M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⋆</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">/M</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⊙</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">)</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black">⩽</span><span style="font-size:12.0pt;font-family:"Aptos",serif;color:black">11.2
and are less concentrated at intermediate stellar masses. But we argue that the higher concentrations of the low-mass TNG50 galaxies are not likely the cause of their thicker/rounder appearances. Our study underscores the critical importance of conducting
mock observations of simulations and applying consistent measurement methodologies to facilitate proper comparison with observations.<o:p></o:p></span></p>
<p class="xmsonormal"> <o:p></o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",serif">Thursday 7<sup>th</sup> November, A113 CAPT at 3pm – Particle Cosmology Journal Club</span></b><o:p></o:p></p>
<p class="MsoNormal">---<o:p></o:p></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt">Fridays at 2pm, A113 CAPT – CAPT Coding Club</span></b><o:p></o:p></p>
<p class="MsoNormal"> <o:p></o:p></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt">Fridays at 4pm, CAPT Foyer – CAPT Cakes</span></b><o:p></o:p></p>
<p class="MsoNormal">---<o:p></o:p></p>
<p class="MsoNormal"><span style="font-size:12.0pt">If you have any events/visitors you would like included in next week’s bulletin, please let me know</span><o:p></o:p></p>
<p class="MsoNormal"><o:p> </o:p></p>
<p class="MsoNormal"><o:p> </o:p></p>
<p class="MsoNormal"><span style="mso-fareast-language:EN-GB">Best wishes</span><span style="mso-ligatures:none;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:6.0pt;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial",sans-serif;mso-fareast-language:EN-GB">Ella<o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:6.0pt;font-family:"Calibri",sans-serif;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal"><b><span style="font-family:"Arial",sans-serif;color:#009BBD;mso-fareast-language:EN-GB">Ella Batchelor
</span></b><span style="font-family:"Arial",sans-serif;color:#009BBD;mso-fareast-language:EN-GB">(she/her)</span><o:p></o:p></p>
<p class="MsoNormal"><b><span lang="EN-US" style="font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">Administrator</span></b><span style="mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">School of Physics & Astronomy</span><span lang="ZH-CN" style="font-size:9.0pt;font-family:"MS Gothic";color:#0F1245;mso-fareast-language:ZH-CN">
</span><span lang="EN-US" style="font-size:9.0pt;font-family:"MS Mincho",serif;color:#0F1245;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
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<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">A112a Centre for Astronomy & Particle Theory</span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">University Park</span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
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<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"> <o:p></o:p></span></p>
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