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<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Monday 11<sup>th</sup> May 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",sans-serif">Thomas Martin<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-size:16.0pt;color:black">Brownian Motion and Critical Dynamics</span></i><b><span style="font-size:16.0pt;color:black"><o:p></o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">---<o:p></o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Tuesdays at 11am, CAPT Foyer – Astro Coffee<br>
<br>
</span></b><b><span style="font-size:16.0pt;color:#0070C0">Tuesdays at 10am, A113 CAPT – Astronomy Journal Club</span></b><b><span style="font-size:16.0pt;color:black"><o:p></o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black"><o:p> </o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Tuesday 12<sup>th</sup> May at 1pm, C12 Physics – Particle Cosmology and Gravity Seminar<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Katy Clough (Queen Mary, London)<o:p></o:p></span></p>
<p class="elementtoproof" style="margin-bottom:16.0pt;background:white"><i><span style="font-size:16.0pt;color:black">Probing beyond GR and the Standard Model using gravitational waves<o:p></o:p></span></i></p>
<p class="MsoNormal"><span style="color:black">I will discuss recent numerical simulations that model deviations from the vacuum BH + GR paradigm in the strong field regime of comparable mass black hole mergers. I will review recent advances, and highlight
the challenges ahead to properly model these effects and test them in real data.<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="color:black"><o:p> </o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="color:black">Link to join:</span></b><span style="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><br>
</span><span style="font-size:16.0pt;color:black">---<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Wednesday 13<sup>th</sup> May at 2pm, A113 Physics – Particle Cosmology and Gravity Seminar<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Maria Mylova (IPMU, Japan)<o:p></o:p></span></p>
<p class="elementtoproof" style="margin-bottom:16.0pt;background:white"><i><span style="font-size:16.0pt;color:black">Gauge fixing in open quantum systems<o:p></o:p></span></i></p>
<p class="MsoNormal"><span style="color:black">Understanding how to gauge-fix open quantum field theories is essential for building consistent open frameworks for cosmology and gravity, where gauge symmetry must coexist with dissipation and noise and decoherence.
I will present our recent work developing explicit top-down constructions of open effective field theories (EFTs) for gauge degrees of freedom, with particular emphasis on the role of gauge fixing. We implement BRST quantisation on the Schwinger-Keldysh contour
and show that the in-in boundary conditions reduce the doubled global BRST symmetry to a single diagonal copy. This diagonal BRST symmetry is nevertheless sufficient to guarantee that the influence functional remains gauge invariant under two independent gauge
transformations, retarded and advanced, independently of the choice of initial state, the presence of symmetry-breaking phases, and whether the gauge theory is Abelian or non-Abelian. I will also remark that once a consistent quantisation scheme is chosen,
the Schwinger-Keldysh path integral is uniquely determined, and with it the rules that constrain the construction of open EFTs. I will conclude by outlining bottom-up implications, and how these principles provide a systematic route to causal, gauge-invariant
open EFTs suitable for cosmological and gravitational applications.<o:p></o:p></span></p>
<p class="MsoNormal"><span style="color:black"><o:p> </o:p></span></p>
<p class="MsoNormal"><span style="color:black">Based on:<o:p></o:p></span></p>
<p class="MsoNormal"><span style="color:black">Gauging Open EFTs from the top down
<a href="https://arxiv.org/abs/2512.17089">https://arxiv.org/abs/2512.17089</a> <o:p></o:p></span></p>
<p class="MsoNormal"><span style="color:black">Schwinger-Keldysh path integral for gauge theories
<a href="https://arxiv.org/abs/2604.26941">https://arxiv.org/abs/2604.26941</a><o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="color:black"><o:p> </o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="color:black">Link to join:</span></b><span style="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></span><span style="font-size:16.0pt;color:black"><o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:16.0pt;color:black"><o:p> </o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Wednesday 13<sup>th</sup> May at 3.45pm, C4 Physics – Astronomy Weekly Seminar<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Dr Giulia Lusetti (Open University)<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-size:14.0pt;color:black;mso-fareast-language:EN-US">From diffuse cluster emission to compact jets: a LOFAR perspective on the life cycle of radio plasma<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;color:black;mso-fareast-language:EN-US">Relativistic particles and magnetic fields trace some of the most energetic processes in the Universe. In galaxy clusters—the largest gravitationally
bound systems in the universe—these components are revealed through diffuse radio emission associated with mergers and shocks, as well as through radio galaxies powered by active galactic nuclei (AGN). Traditionally, these phenomena have been studied separately;
however, growing observational evidence suggests that they are physically connected through the life cycle of relativistic plasma.</span><span style="font-size:11.0pt;mso-fareast-language:EN-US"><o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:11.0pt;color:black;mso-fareast-language:EN-US">In this seminar, I will present results on diffuse radio emission and radio galaxies in cluster environment and discuss how AGN activity
may provide a seed population of relativistic electrons that is later re-accelerated by cluster-scale processes. All of this is viewed through the unique lens of LOFAR, whose combination of very low-frequency coverage and high sensitivity is revealing previously
“hidden” radio sky phenomena. Being a European-based array, LOFAR has recently demonstrated its strength not only in probing faint, diffuse emission, but also in reaching sub-arcsecond resolution through very long baseline interferometry (VLBI). In the second
part of the talk, I will showcase how these capabilities can be used to study galaxy-scale jet sources out to redshift 3 and beyond. Thanks to VLBI, it is now possible to resolve (<100 kpc) structures that were previously unresolved in standard LOFAR observations,
enabling detailed studies of their interplay with their host galaxies.</span><span style="font-size:11.0pt;mso-fareast-language:EN-US"><o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><span style="font-size:16.0pt;color:black">---<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Thursday 14<sup>th</sup> May at 1pm, A113 CAPT – Astronomy Lunch Talks<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Mathias Urbano<o:p></o:p></span></p>
<p class="MsoNormal"><i><span style="font-size:14.0pt;color:black;mso-ligatures:none">An overview of the Low Surface Brightness Science with the Euclid Space Telescope<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="color:black">During this talk, I will revisit the efforts carried out during my PhD to conduct some of the first studies with Euclid in the Low Surface Brightness (LSB) Universe regime. This will be illustrated through the
study of structures spanning three different angular scales: mock dwarf galaxies that I used to assess Euclid’s detection performance in the LSB regime for objects up to arcminute scales; tidal features investigated within the framework of Euclid’s first test
observations within a single observation (0.56 square degrees); and the intracluster light of the Fornax cluster, which extends over several degrees.<o:p></o:p></span></p>
<p class="xmsonormal"><span style="color:black"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Paloma Morilla<o:p></o:p></span></p>
<p class="xmsonormal"><i><span style="font-size:14.0pt;font-family:"Aptos",sans-serif;color:black;mso-fareast-language:EN-US">Signatures of fuzzy dark matter inside radial critical curves<o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></p>
<p class="xmsonormal"><span style="color:black">We explore how fuzzy dark matter (FDM) would modify strong gravitational lensing magnification, focusing on the region near radial critical curves. Using simulated galaxy-scale lenses, we compute magnification
maps for a range of halo configurations and axion masses. We find that, compared to standard cold dark matter (CDM), FDM produces a significantly higher probability of strong central magnification, an effect that is difficult to reproduce in CDM (even when
subhaloes are included). The strength and characteristic scale of this enhancement are set primarily by the de Broglie wavelength, and therefore by the axion mass and halo mass. For galaxy-mass haloes, axion masses in the range $m_\phi~10^{-22}-10^{-21}$ eV
lead to distinctive magnification distributions. These results suggest that observations of highly magnified, compact sources near radial arcs could provide a sensitive and complementary test of fuzzy dark matter.</span><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Thursdays at 3pm, A113 CAPT – Particle Cosmology Journal Club<o:p></o:p></span></b></p>
<p class="xmsonormal">---<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";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">
</span></b><a href="http://nottingham.ac.uk/"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:blue;mso-fareast-language:EN-GB">nottingham.ac.uk</span></a><span style="mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span style="mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span style="mso-ligatures:none;mso-fareast-language:EN-GB"><img border="0" width="484" height="109" style="width:5.0416in;height:1.1354in" id="Picture_x0020_2042549853" src="cid:image001.png@01DCE121.37CB8F50"></span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:9.0pt;font-family:"Arial",sans-serif;color:black;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><b><span lang="EN-US" style="font-size:9.0pt;font-family:"Georgia",serif;color:#15769E;mso-fareast-language:EN-GB">Follow us</span></b><span lang="EN-US" style="font-size:9.0pt;color:#191919;mso-fareast-language:EN-GB"><br>
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