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<p>Reminder, happening today at 12:00 pm. </p>
<div class="moz-cite-prefix">On 10/9/25 6:35 PM, Pooyan Goodarzi
wrote:<br>
</div>
<blockquote type="cite"
cite="mid:1bf932f5-6d1a-4ec2-954c-12c85f216520@email.ucr.edu">
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<p>Hi all,</p>
<p><br>
</p>
<p>We will have a PASS talk by Michael next <b>Wednesday, </b>October
15, at noon.<b> </b>Please note that this is different from our
usual weekly time. Michael's talk about feedback and dust in
galaxies will be a dry run of his advance to candidacy exam
later next week. Please join us at noon (<b>from 12:00 to 1:00
pm</b>) in the <b>Nebula Room</b> (PHYS 3027) to hear about
his research, give him feedback on slides, and wish him the best
for his exam. </p>
<p><br>
</p>
<p align="center"><b>Michael Wozniak, PhD Student</b><br>
Wednesday, 12:00 pm, Nebula Room (PHYS 3027)</p>
<p align="center"><b>Impact of Galactic Feedback and Dust Geometry
on Metallicity and Star-Formation Rates in z~2 Star-Forming
Galaxies</b></p>
<p align="center"><b><br>
</b></p>
<div align="center">Dust production and baryon cycling are
critical components of galaxy evolution. Galaxies accrete cold
gas, convert the gas into stars, and eject both dust and
metal-rich gas into the interstellar medium. Within this cycle,
galactic outflows regulate star formation and redistribute
metals, while dust obscuration shapes how we measure
star-formation rates (SFRs).</div>
<div align="center"><br>
</div>
<div align="center">In the first part of the talk, I will discuss
the role of galactic outflows in regulating metallicity. Using
rest-frame optical and UV spectroscopy, we investigate how
outflow velocities correlate with deviations from the
fundamental metallicity relation (FMR), and find tentative
evidence that faster outflows are associated with larger
deviations below FMR-based metallicities.</div>
<div align="center"><br>
</div>
<div align="center">In the second part, I will compare nebular
reddening and SFRs derived from Balmer and Paschen lines. On
average, Paschen-based measurements agree with Balmer values,
but in galaxies with patchy dust geometries, the Paschen lines
reveal star formation in the most heavily dust-obscured regions
that Balmer lines alone fail to measure.</div>
<p align="center"><br>
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<div
id="m_-7314571423100097885m_-3414541767872711075m_9215603032040371864m_-1672972118947443868gmail-:1f4">
<div>
<div dir="ltr"><br>
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<div dir="ltr">If you’re interested in sharing your work as a
speaker, please feel free to add your name to this
spreadsheet [<a
href="https://docs.google.com/spreadsheets/d/1N3ncf43jdB6aHYHhyWmyHMycxDg4_phHZXLkQvviO0o/edit?usp=sharing"
target="_blank" moz-do-not-send="true">Google Sheet</a>].
Recordings of all the previous talks are available on our
website: <a href="https://ucrpass.arxiv.social/"
target="_blank" class="moz-txt-link-freetext"
moz-do-not-send="true">https://ucrpass.arxiv.social</a>
<div><br>
</div>
<div><br>
</div>
Best,<br>
Pooyan<br>
Physics and Astronomy Student Seminar (<span><span>PASS</span></span>)
<br>
<a href="https://ucrpass.arxiv.social/" target="_blank"
class="moz-txt-link-freetext" moz-do-not-send="true">https://ucrpass.arxiv.social</a></div>
</div>
</div>
<div><br>
<br>
</div>
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