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<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Monday 24<sup>th</sup> March at 3pm, A113 CAPT – Theoretical Physics Student Seminar<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black;mso-fareast-language:EN-US">Peter Du<o:p></o:p></span></p>
<p class="xmsonormal"><i><span style="font-size:12.0pt;font-family:"Aptos",sans-serif;color:black">Unitarisation from Geometry</span></i><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesdays at 11am, CAPT Foyer – Astro Coffee<o:p></o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesday 25<sup>th</sup> March at 1pm, A113 CAPT – Particle Cosmology and Gravity Seminar<o:p></o:p></span></b></p>
<p class="MsoNormal" style="background:white"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black;mso-ligatures:none">Peter Millington (University of Manchester)<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="color:black">Pseudo-Hermitian Quantum Field Theories from First Principles<o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><i><span style="color:black"><o:p> </o:p></span></i></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;font-family:"Aptos Display",sans-serif;color:black">It is now well established that quantum theories described by non-Hermitian Hamiltonians can exhibit real spectra and a unitary
evolution. The viability of these “pseudo-Hermitian” quantum theories often relies on the invariance of the Hamiltonian under antilinear spacetime symmetries; namely, the combined action of parity and time-reversal transformations. Spacetime symmetries play
a special role in quantum field theory, and this makes the second quantization of pseudo-Hermitian mechanics more intricate. In this talk, I will describe how self-consistent pseudo-Hermitian quantum field theories can be built from first principles and highlight
novel implications for high energy physics phenomenology.<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></p>
<p class="MsoNormal" style="background:white"><b><span style="font-size:11.5pt;color:black">Link to join:</span></b><span style="font-size:11.5pt;color:black"> <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">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="elementtoproof" style="background:white"><span style="font-size:11.0pt;font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></p>
<p class="MsoNormal" style="background:white"><span style="font-size:12.0pt;font-family:"Aptos Display",sans-serif;color:black;mso-ligatures:none;mso-fareast-language:EN-GB">The speaker will be also available for a discussion with students from 10:30 to 11:30
in A113</span><span style="color:black"><br>
</span><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black">---<o:p></o:p></span></p>
<p class="MsoNormal" style="background:white"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black">Wednesday 26<sup>th</sup> March at 3pm, B13 Physics – School Colloquium<o:p></o:p></span></b></p>
<p class="MsoNormal" style="background:white"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black">Professor Jo Dunkley (Princeton)<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="color:black">New maps and cosmological results from the Atacama Cosmology Telescope<o:p></o:p></span></i></p>
<p class="MsoNormal" style="background:white"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;font-family:"Aptos Display",sans-serif;color:black">I will show new results from the Atacama Cosmology Telescope (ACT), including cosmological constraints and data products from
the sixth data release, DR6. Using data gathered from 2017 - 2022, the new maps cover 40% of the microwave sky with five times the angular resolution and three times the depth in polarization as the Planck satellite. The improved cosmic microwave background
(CMB) measurements at small scales complement the larger-scale information from Planck. I will describe how we use these datasets, along with tracers of large-scale-structure, to probe the fundamental physics of the universe across epochs and scales.<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;font-family:"Aptos Display",sans-serif;color:black">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">Thursday 27<sup>th</sup> March at 1pm, A113 CAPT – Astronomy Lunch Talk</span></b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;mso-fareast-language:EN-US"><o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;mso-fareast-language:EN-US">Alfonso Aragon-Salamanca<o:p></o:p></span></p>
<p class="xmsonormal"><i><span style="font-size:12.0pt;font-family:"Aptos",sans-serif;color:black">The separate effect of halo mass and stellar mass on the evolution of massive disc galaxies<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-family:"Aptos Display",sans-serif;mso-fareast-language:EN-US"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="font-family:"Aptos Display",sans-serif;color:black">We analyse a sample of massive disc galaxies selected from the fourth-generation Sloan Digital Sky Survey/Mapping Nearby Galaxies at Apache Point Observatory survey to investigate
how the evolution of these galaxies depends on their stellar and halo masses. We applied a semi-analytic spectral fitting approach to the data from different regions in the galaxies to derive several of their key physical properties. From the best-fitting
model results, together with direct observables such as morphology, colour, and the Mgb/<Fe> index ratio measured within 1Re , we find that for central galaxies both their stellar and halo masses have a significant influence in their evolution. For a given
halo mass, galaxies with higher stellar mass accumulate their stellar mass and become chemically enriched earlier than those with smaller stellar mass. Furthermore, at a given stellar mass, galaxies living in more massive haloes have longer star formation
time-scales and are delayed in becoming chemically enriched. In contrast, the evolution of massive satellite galaxies is mostly determined by their stellar mass. The results indicate that both the assembled halo mass and the halo assembly history impact the
evolution of central galaxies. Our spatially resolved analysis indicates that only the galaxy properties in the central region (0.0–0.5 Re ) show the dependencies described above. This fact supports a halo-driven formation scenario since the galaxies’ central
regions are more likely to contain old stars formed along with the halo itself, keeping a memory of the halo formation process.<o:p></o:p></span></p>
<p class="xmsonormal"><span style="color:black"><o:p> </o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">Thursday 27<sup>th</sup> March at 3pm, A113 CAPT – Particle Cosmology Journal Club</span></b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;mso-fareast-language:EN-US"><o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif;mso-fareast-language:EN-US">Student Journal Club<o:p></o:p></span></p>
<p class="xmsonormal"><span style="color:black"><br>
</span>---<span style="color:black"><o:p></o:p></span></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt">Fridays at 4pm, CAPT Foyer – CAPT Cakes<o:p></o:p></span></b></p>
<p class="MsoNormal">---<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";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">University of Nottingham</span><span lang="EN-US" style="font-size:9.0pt;font-family:"Calibri",sans-serif;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">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>
<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">Nottingham, NG7 2RD</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;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">+44 (0) 115 74 86778<b> </b></span><b><span lang="EN-US" style="font-size:9.0pt;color:#0F1245;mso-fareast-language:EN-GB">| </span></b><b><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">
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<p class="MsoNormal" style="text-autospace:none"><span style="mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
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