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BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Astronomy Colloquium
LOCATION:PMA 15.216B
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Title: TBA
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220823T153000
DTEND;TZID=America/Chicago:20220823T163000
SEQUENCE:0
RRULE:FREQ=WEEKLY;UNTIL=20221207T000000Z;INTERVAL=1;BYDAY=TU
EXDATE;TZID=America/Chicago:20221206T153000
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Fall Break
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221122T153000
DTEND;TZID=America/Chicago:20221122T163000
RECURRENCE-ID;TZID=America/Chicago:20221122T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:No talk scheduled
LOCATION:PMA 15.216B
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220823T153000
DTEND;TZID=America/Chicago:20220823T163000
RECURRENCE-ID;TZID=America/Chicago:20220823T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:No talk scheduled
LOCATION:PMA 15.216B
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220830T153000
DTEND;TZID=America/Chicago:20220830T163000
RECURRENCE-ID;TZID=America/Chicago:20220830T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Anson D'Aloisio, UC Riverside
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Recent Progress Toward Understanding Cosmological Reionization<
/p>
Abstract
When the first galaxies formed, their starl
ight likely reionized and heated the intergalactic hydrogen that had existe
d since recombination. In the past few years, there has been signific
ant progress toward understanding the reionization process. I will hi
ghlight this progress, including the possibility that we have already obser
ved evidence of reionization's tail end in the spectra of high-redshift qua
sars. I will also discuss the role that small-scale structure in the
cosmic web played in shaping reionization, and what we might learn about co
smology from reionization observables.
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220913T153000
DTEND;TZID=America/Chicago:20220913T163000
RECURRENCE-ID;TZID=America/Chicago:20220913T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:1-Minute Colloquium
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Astronomy Department and McDonald Observatory Personnel present overview
s of their work
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220906T153000
DTEND;TZID=America/Chicago:20220906T163000
RECURRENCE-ID;TZID=America/Chicago:20220906T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Postdoc Colloquium - 4 short talks
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Lauren Biddle, The University of Texas at Austin
<
em>Observing the Planet–Disk–Star Connection
Abstract
A major question in exoplanet science is the pathway f
or planetary formation and evolution. One approach to this problem is to in
fer the histories of planets by comparing the demographics of late-age plan
etary systems to those of young systems. However, in contrast to the wealth
of exoplanet discoveries at late ages, there are significantly fewer confi
rmed planets at early ages (<10 Myr), and even fewer detected at close-i
n orbits around Classical T Tauri Stars (CTTS). A leading reason for this i
s largely a result of strong magnetic activity in CTTS observed in the form
of long-lived cold spots and accretion hot spots, which can mimic planetar
y signatures and/or drown them out entirely. Using CI Tau as an example, I
present an assessment of the photometric variability of stellar accretion o
ver a range of timescales and its role in teasing out observational signatu
res of a hot-Jupiter orbiting near the inner edge of the disk.
Nika Jurlin, The Unive
rsity of Texas at Austin
Timing the Cycle of Life and Dea
th of Radio Galaxies
Jed McKinney, The University of Tex
as at Austin
Heating and Cooling in Dusty Galaxies <
/em>
Abstract
Star-formation depends on the physical conditions of t
he interstellar medium (ISM), where gas cooling, heating, and feedback from
stars and supermassive black holes all compete to drive the evolution of g
alaxies. My research focuses on characterizing the cold gas from which star
s form to better understand the origin of high star-formation rat
es in luminous, infrared (IR) galaxies today and in the past. I use combine
d spectroscopy from ALMA, the VLA, and Spitzer to measure physical&nbs
p;quantities of interstellar gas and dust at z=0 and z~2. Compact, IR-lumin
ous galaxies at all redshifts exhibit low gas heating efficiencies and
high star-formation efficiencies, suggesting a link between the parse
c-scale ISM properties of star-forming regions a
nd the global evolution of the galaxy. There is tentative evidence for systematically low gas
heating rates at z~2 which may contribute to the high star-formation rates
and star-formation efficiencies at early times. I will briefly present ongoing projects and upcoming programs to
statistically test this link between the efficiency of star-formation and
gas conditions, and discuss how JWST can be used to push diagnostics of the
ISM out to higher redshifts
Joseph Zalesky, The University of Texas at Austin
Understanding the Atmospheres of Substellar Worlds
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220920T153000
DTEND;TZID=America/Chicago:20220920T163000
RECURRENCE-ID;TZID=America/Chicago:20220920T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Steve Finkelstein and Micaela Bagley, The University of Texas at Austin
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
The JWST Cosmic Evolution Early Release Science Survey: Program Over
view, and First Results
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20220927T153000
DTEND;TZID=America/Chicago:20220927T163000
RECURRENCE-ID;TZID=America/Chicago:20220927T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Alisha Clark, University of Colorado Boulder
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
The Origin of Earth’s Water
Abstr
act
When the surfaces of terrestrial planets and moons in our solar
system are compared from space, the pale blue dot stands out in stark contr
ast to the barren reds and greys of the dry rocky bodies filling Earth’s so
lar neighborhood. The oceans are a likely venue for the origins of life and
because of their importance in the development of civilizations, humanity
has spent centuries mapping the breadth and depth of our water world. Only
50 years ago, Marie Tharp’s map of the ocean floor led to the discovery of
plate tectonics, revolutionizing our understanding of the dynamics of plane
tary processes. But where did all this water come from? This week’s seminar
will focus on how experimental data can help in understanding how the Eart
h gained and retained primordial water/volatiles during planet-forming proc
esses including major impact events.
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221004T153000
DTEND;TZID=America/Chicago:20221004T163000
RECURRENCE-ID;TZID=America/Chicago:20221004T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Ruth Murray-Clay, UC Santa Cruz
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Evaporating Planets and Growing Planetesi
mals
Abstract
I will discus
s recent modeling results from two different areas of exoplanet theory. First, Lyman-alpha
transits have long been used to probe the outflows from planets experienci
ng atmospheric evaporation.
Often, observed transits are interpreted in terms of mass loss
rates, but these interpretations are generally model-dependent. I will demonstrate that L
yman-alpha transits can more cleanly be used to constrain the outflow veloc
ity of the escaping gas, a key property that can be used to distinguish whe
ther photo-evaporation and core-powered mass loss models better describe ob
served outflows. Second, I will discuss how accretion of ices by growing solids in the out
er regions of protoplanetary disks may affect not only the compositions of
planetesimals but also the global distribution of planet-forming material.&
nbsp;
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221011T153000
DTEND;TZID=America/Chicago:20221011T163000
RECURRENCE-ID;TZID=America/Chicago:20221011T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Andrea Banzatti, Texas State University
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Infrared Spectroscopy of Molecules in Planet-Forming Disks - Where W
e Are and Where We Are Going
AbstractIn this talk, I will review the
status of infrared spectroscopy of molecules in planet-forming (Class II) d
isks from 20 years of data from ground- and space-based observatories. 
;I will discuss multiple science angles from studying different kinematic c
omponents that trace gas in inner disk rings and winds at 0.01-10 au: their
physical and chemical structure, kinematics, excitation, and evolution. I will also present spexodis
ks.com, a new database of infrared (1.4-35 um) spectra from VLT-
CRIRES, IRTF-iSHELL, Keck-NIRSPEC, VLT-VISIR, Spitzer-IRS (and recently IGR
INS too!) that is now available to the community in support of new observin
g and modeling efforts worldwide. I will conclude by demonstrating how the
synergy of data from multiple instruments is supporting the analysis of JWS
T observations, in the context of the spectral range, molecular tracers, an
d resolving power that each instrument offers.
<
/div>
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221018T153000
DTEND;TZID=America/Chicago:20221018T163000
RECURRENCE-ID;TZID=America/Chicago:20221018T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:No colloquium
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
No talk scheduled - see Thursday's Cosmos Seminar
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221025T153000
DTEND;TZID=America/Chicago:20221025T163000
RECURRENCE-ID;TZID=America/Chicago:20221025T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Aarynn Carter, UC Santa Cruz
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Kickstarting a New Generation of Exoplanet Observations: Early
Release Science with JWST
Abstract
<
div class="">Over the last few months, JWST has been conducting its first s
cientific observations through the Director’s Discretionary Early Release S
cience (ERS) programs, which were designed under the primary goal of rapidl
y informing the community on JWST’s performance and capabilities. With resp
ect to the study of exoplanets, only two ERS programs exist: “The Transit C
ommunity Early Release Science Program”, and “High Contrast Imaging of Exop
lanets and Exoplanetary Systems”. In this talk I will cover the latest resu
lts from both of these programs, including: high contrast imaging of the ex
oplanet HIP 65426b from 2-16 micron, direct spectroscopy of the planetary m
ass object VHS1256b from 1-21 micron, and transmission spectroscopy from 1-
5 micron of the exoplanet WASP-39b. These data have provided a wealth of ne
w information about the bulk and atmospheric properties of these objects wh
ich I will discuss in the context of the unprecedented capabilities that JW
ST can provide. Finally, I will use these early results to provide glimpses
of what additional science may be possible in the coming decade.
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221101T153000
DTEND;TZID=America/Chicago:20221101T163000
RECURRENCE-ID;TZID=America/Chicago:20221101T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:No Colloquium
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
No talk scheduled - see Thursday's Cosmos Seminar
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221108T153000
DTEND;TZID=America/Chicago:20221108T163000
RECURRENCE-ID;TZID=America/Chicago:20221108T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Kathryne Daniel, University of Arizona
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Resonant Evolution: The internal dynamical history of the Milky Way<
/em>
Abstract
Dynamical res
onances are essential to the evolution of disk galaxies. These resonan
ces arise in the presence of massive structures, like Giant Molecular Cloud
s, spiral patterns and satellites, acting to reshape a galaxy as they diffu
se, shepherd and rearrange stellar populations. Until recently, many
of the signatures that would reveal the past dynamical evolution of the Mil
ky Way have been obscured, limited by observational uncertainties and simul
ation resolution. We are now entering a new era, rich with high preci
sion chrono-chemodynamic (kinematic, chemical, and age) data. Current and u
pcoming observatories and surveys are revealing complex post-resonant struc
tures in this multidimensional space and opening exciting opportunities to
reconstruct the dynamical history of the Milky Way. Many of these phe
nomena are reproduced in specialized and high-resolution simulations, where
additional trends arise when exploring galaxies that occupy a range of par
ameter space. There is an ongoing need to further develop the theoret
ical framework necessary to interpret this flood of high precision data.&nb
sp; In this talk, I will demystify the physics that governs various resonan
t phenomena in disk galaxies. I will then discuss a few case studies
that demonstrate how analytic theory can inform the interpretation of obser
ved and simulated data. Finally, I will describe current and future transfo
rmative science that is emerging from this interdisciplinary approach.
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221115T153000
DTEND;TZID=America/Chicago:20221115T163000
RECURRENCE-ID;TZID=America/Chicago:20221115T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:f78474348549df437b9b622e36fb5b36
CATEGORIES:Astronomy Colloquium
SUMMARY:Jennifer Burt, Jet Propulsion Laboratory
LOCATION:PMA 15.216B and online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Chasing TESS Planet Candidates With Bright Futures
Abstract
NASA's TESS mission has produced more tha
n 5000 planet candidates to date, and the TESS community has thoroughly sur
passed the mission's level one science requirement of delivering masses for
50 new, small, TOI planets. With such a large starting pool, however, deci
ding which candidates to follow up next requires the collaboration of numer
ous ground based facilities. I will discuss the flow down from TESS Object
of Interest (TOI) to confirmed planet through the lens of two recent confir
mations. TOI-824 b, is a hot, sub-Neptune planet orbiting a K4V star that s
its in a crowded section of the night sky. Follow up efforts revealed an in
correct initial TESS radius estimate due to biased background estimates, de
monstrating the importance of higher resolution ground based photometric fo
llow up. TOI-1231 b, is a temperate, Neptune-sized planet orbiting a nearby
M3V star. Exhibiting only one transit per sector of TESS monitoring, the p
lanet is one of the coolest small planets detected in the primary mission.
Models of atmospheric observations suggest that it will be possible to dete
ct spectral features in an atmosphere similar to that of K2-18 b enabling t
he first comparative planetology in the 250-350 Kelvin temperature range. T
hese new planets offer promising atmospheric follow up possibilities from t
he ground and from space, and make up a small but exciting portion of TESS’
s contribution to exoplanet science. I'll also show some early confirmation
results for two TESS super-Earth planets from the MAROON-X spectrograph wh
ich is proving to be a competitive force in the follow up of small TESS pla
nets orbiting cool stars
DTSTAMP:20240329T110018Z
DTSTART;TZID=America/Chicago:20221129T153000
DTEND;TZID=America/Chicago:20221129T163000
RECURRENCE-ID;TZID=America/Chicago:20221129T153000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
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