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<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Monday 2<sup>nd</sup> June at 1pm, A113 CAPT – Astronomy Lunch Talk</span></b><i><span style="font-family:"Aptos Display",sans-serif;color:black"><o:p></o:p></span></i></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">George Becker (UC Riverside)<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black">Exploring the End of Reionization<o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></i></p>
<p class="elementtoproof" style="background:white"><span style="color:black">Studying the epoch of reionization carries a high potential for discovering new things about the IGM and galaxies in the early Universe. How those discoveries are made, however, depends
partly on when reionization occurred. Over the past few years, multiple lines of evidence have strongly indicated that reionization ended later than previously thought, between redshifts five and six. This opens a number of observational opportunities, as
well as challenges. I will describe the evidence for late-ending reionization, discuss some of the new ways in this era is being explored observationally, and touch on some of the potential implications for the IGM, high-redshift galaxies, and cosmology.<br>
<br>
</span><o:p></o:p></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Monday 2<sup>nd</sup> June at 3pm, A113 CAPT – Theoretical Physics Student Seminar</span></b><b><span style="font-size:16.0pt"><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-family:"Aptos Display",sans-serif;color:black">'The' QCD Phase Diagram</span></i><b><span style="font-size:16.0pt;color:black"><br>
</span></b><span style="font-size:16.0pt;color:black">---</span><i><span style="font-family:"Aptos Display",sans-serif;color:black"><o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt;color:black">Tuesdays at 11am, CAPT Foyer – Astro Coffee</span></b><b><span style="font-size:16.0pt"><o:p></o:p></span></b></p>
<p class="elementtoproof" style="background:white"><b><span style="font-size:16.0pt"><o:p> </o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesday 3<sup>rd</sup> June at 11.30am, A113 CAPT – Astronomy Journal Club<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 3<sup>rd</sup> June at 1pm, A113 CAPT – Particle Cosmology and Gravity Seminar</span></b><span style="color:black"><br>
</span><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Elisa Todarello<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black">An overview of axion dark matter<br>
<br>
<o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><span style="color:black">In this overview talk, I will describe the mechanism through which QCD axions are produced in the early Universe. I will discuss the state-of-the-art simulations of topological defect
decay. Finally, I will introduce possible present-day axion small scale structures: miniclusters and axion stars.</span><o:p></o:p></p>
<p class="xmsonormal"><span style="font-family:"Aptos",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></span><span style="color:black"><br>
</span><span style="font-size:16.0pt;color:black;mso-ligatures:none;mso-fareast-language:EN-GB">---</span><span style="font-size:11.5pt;color:black"><o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Wednesday 4<sup>th</sup> June at 3.45pm, A113 CAPT – Astronomy Weekly Seminar<o:p></o:p></span></b></p>
<p class="elementtoproof" style="background:white"><span style="font-size:16.0pt;color:black">Dr. Francesca Frankoudi (Durham)</span><span style="font-size:16.0pt"><o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black">The formation, evolution, and dark matter content of barred galaxies in LCDM<o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></i></p>
<p class="MsoNormal" style="background:white"><span style="color:black">The advent of high resolution hydrodynamical cosmological simulations allows us to now study the internal dynamics of barred spiral galaxies -- such as our own Milky Way -- within the full
ΛCDM cosmological context. I will present what we have learnt about the formation and evolution of barred galaxies by comparing cosmological simulations to observations of both the Milky Way and nearby spiral galaxies. In particular, I will address the "When?"
and the "How?" of bar formation in ΛCDM, and discuss what this implies about our own Galaxy's formation history, as well as why some galaxies form bars and others don't. I will discuss how barred galaxies evolve throughout cosmic history, as well as the connection
between bars and their host dark matter halos, which can help shed light on both the amount and the nature of dark matter.<o:p></o:p></span></p>
<p class="MsoNormal" style="background:white"><span style="font-size:16.0pt;color:black;mso-ligatures:none;mso-fareast-language:EN-GB">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Thursday 5<sup>th</sup> June at 1pm, A113 CAPT – Astronomy Lunch Talk<o:p></o:p></span></b></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Guillaume Hewitt<o:p></o:p></span></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black">No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST<o:p></o:p></span></i></p>
<p class="elementtoproof" style="background:white"><i><span style="font-family:"Aptos Display",sans-serif;color:black"><o:p> </o:p></span></i></p>
<p class="MsoNormal" style="background:white"><span style="color:black">This talk presents a mid-infrared study of recently-quenched galaxies with JWST, with the aim of searching for obscured AGN activity. We focus on the transition class of post-starburst
galaxies (PSBs) which provide insight into the intermediate stage of galaxy evolution between star-forming and quiescent, a necessity for understanding what drives quenching and galaxy bimodality. For massive galaxies (M* > 10^10), quenching models frequently
invoke AGN feedback, and PSBs often exhibit strong outflows, consistent with this scenario. However, recent studies of massive PSBs have found no evidence of excess AGN activity from their X-ray and optical properties. This lack of activity indicates either
AGN are not the main quenching mechanism, are short-lived and do not linger into the PSB phase, or are heavily obscured. If dust obscured, the presence of AGN activity could still be detected through the infrared (IR) emission of this hot dust. To test this,
we use a sample of </span><span style="font-family:"Cambria Math",serif;color:black">∼</span><span style="color:black">150 photometrically-selected PSBs within the PRIMER-UDS field at 0.5 < z < 3.0, and utilise the 7.7 μm and 18 μm JWST/MIRI photometry (as
well as an additional eight NIRCam and three HST wavebands) to probe the IR dust emission of these galaxies. We find interesting differences between low and high-mass PSBs, and interestingly no excess dust emission within the high-mass galaxies. This indicates
there are no hidden AGN, or indeed residual star-formation within these galaxies. I will discuss the implications of these results on the current understanding of what quenches massive galaxies at these redshifts.<o:p></o:p></span></p>
<p class="MsoNormal" style="background:white"><span style="color:black"><o:p> </o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Thursday 5<sup>th</sup> June at 3pm, A113 CAPT – Particle Cosmology Journal Club<o:p></o:p></span></b></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt"><o:p> </o:p></span></b></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"><span style="font-size:16.0pt;color:black;mso-ligatures:none;mso-fareast-language:EN-GB">---</span><o:p></o:p></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt;color:black;mso-ligatures:none;mso-fareast-language:EN-GB">VISITORS<o:p></o:p></span></b></p>
<p class="MsoNormal"><span style="font-size:16.0pt;mso-ligatures:none;mso-fareast-language:EN-GB">Prof. George Becker (University of California, Riverside) is visiting the Astronomy group from Monday 2<sup>nd</sup> – Wednesday 4<sup>th</sup> June.<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">---<o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-family:"Calibri",sans-serif"><o:p> </o:p></span></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">
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