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RDATE:20241103T010000
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UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Galaxies and Cosmology Seminar
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Galaxies and Cosmology Seminar
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210118T120000
DTEND;TZID=America/Chicago:20210118T130000
SEQUENCE:0
RRULE:FREQ=WEEKLY;UNTIL=20210504T000000Z;INTERVAL=1;BYDAY=MO
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:MLK Holiday - No talk scheduled
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:MLK Holiday - No talk scheduled
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210118T120000
DTEND;TZID=America/Chicago:20210118T130000
RECURRENCE-ID;TZID=America/Chicago:20210118T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Jasleen Matharu, Texas A&M University
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:The Role of Galaxy Clusters in Shaping the Size Growth and Q
uenching of Galaxies
Abstract
h2>
The galaxy cluster environment is known to be capable of altering the
evolutionary paths of galaxies through a variety of mechanisms. High
relative velocities of satellite galaxies make minor mergers between t
hem rare. The presence of an intra-cluster medium makes it possible to rapi
dly quench star formation in satellite galaxies via gas stripping processes
. Galaxy clusters are therefore excellent laboratories for testing which ga
laxy size growth mechanisms dominate and how the quiescent population of ga
laxies builds up with redshift. I will present results from the HST WFC3 an
d grism follow up to GCLASS –the largest spectroscopic survey conducted on
10 clusters at z~1. Along with a field sample of galaxies from the 3D
-HST survey, I will demonstrate how minor merger suppression, Brighte
st Cluster Galaxy (BCG) growth, Intra-cluster light (ICL) growth and
the production of recently quenched galaxies can work simultaneously to mai
ntain a stellar mass—size relation that is independent of environment at lo
w redshifts. Last but not least, I will present the first spatially resolve
d H-alpha maps of cluster galaxies at z~1, and what these have uncovered ab
out environmental quenching at this crucial epoch in the history of cosmic
star formation.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210125T120000
DTEND;TZID=America/Chicago:20210125T130000
RECURRENCE-ID;TZID=America/Chicago:20210125T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Guang Yang, Texas A&M University
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:What Brives the Growth of Black Holes?
Abstract
There are supermassive black holes
(SMBHs) in the centers of most massive galaxies. Observations of nearby sy
stems have found that SMBH masses (M_BH) are tightly correlated with host-g
alaxy properties such as bulge masses (M_bulge). These local SMBH-galaxy re
lations suggest that SMBH growth is fundamentally linked to host galaxies o
ver cosmic history. Previous studies suggest that long-term average SMBH ac
cretion rate (BHAR) is intrinsically related to star formation rate (SFR) f
or the overall galaxy population. However, we show that BHAR is more strong
ly correlated with host-galaxy stellar mass (M_*) rather than SFR, and this
BHAR-M_* relation does not depend on cosmic environment. We further quanti
fy this BHAR-M_* relation and its cosmic evolution at z= 0.4–4.
However, we find this BHAR-M_* relation does not hold
for bulge-dominated galaxies, and their BHAR primarily depends on SFR. Thi
s BHAR-bulge SFR relation indicates that SMBHs only coevolve with galactic
bulges rather than the entire galaxies, consistent with the observations of
the local universe. Our best-fit BHAR/SFR ratio is similar to the typical
M_BH/M_bulge ratio observed in the local systems, indicating that the BHAR-
bulge SFR relation is indeed responsible for the local M_BH-M_bulge relatio
n. Our high-resolution hydrodynamical simulations suggest that a compa
ct circum-nuclear disk is the physical mechanism that drives the BHAR-bulge
SFR relation. Our recent ALMA observations support this idea.
<
div>
We have recently applied the BHAR-bulge SFR relation t
o track cosmic BH accretion density (BHAD) based on the measurements of bul
ge star-formation history (SFH) from Hubble grism data. Our derived BHAD at
z>4 is much higher than those observed from X-ray surveys, indicating t
hat a large population of Compton-thick AGNs is missing from X-ray observat
ions. Future JWST deep surveys will be able to identify these Compton-thick
AGNs.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210201T120000
DTEND;TZID=America/Chicago:20210201T130000
RECURRENCE-ID;TZID=America/Chicago:20210201T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:No talk scheduled
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210208T120000
DTEND;TZID=America/Chicago:20210208T130000
RECURRENCE-ID;TZID=America/Chicago:20210208T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Peter Senchyna, Carnegie Institute for Science
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:High-redshift Galaxies and Massive Stars Through the Lens of
Our Smallest Star-forming Neighbors
Abstract
Star-forming dwarf galaxies in the local Universe rep
resent a unique laboratory for the study of metal-poor massive star populat
ions and a fundamental anchor for stellar models applied across cosmic time
. With JWST poised to open a new window onto the rest-ultraviolet light of
primordial galaxies in the reionization era and beyond, and with our premie
r source of local ultraviolet spectra sadly approaching its retirement, con
fronting models for massive stars with high-quality local observations is o
f paramount importance. In this talk, I will present results from several H
ST campaigns which have obtained ultraviolet spectra probing simultaneously
both stellar continuum light and the hot nebular gas ionized by these same
stars. I will argue that the long-mysterious He II line, which appears bot
h in gas and stellar wind emission, may actually be a powerful probe of som
e of the most uncertain products of massive star evolution. Finally, I will
preview several large UV programs and smaller-scale optical campaigns whic
h chart a path towards calibrating stellar population models in the uncerta
in metallicity regime that JWST data will routinely rely upon.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210301T120000
DTEND;TZID=America/Chicago:20210301T130000
RECURRENCE-ID;TZID=America/Chicago:20210301T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Amy Sardone, The Ohio State University
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Gas Beyond the Disk: The Diffuse Neutral CGM Around Nea
rby Galaxies
Abstract
Th
e circumgalactic medium (CGM) is host to large reservoirs of gas around gal
axies, potentially on its way to becoming the fuel for galactic star format
ion. As gas flows from the intergalactic medium (IGM) and on into the CGM,
we should be able to detect it as cold gas accretion. Much of this cold gas
is too diffuse for easy detection, however if a telescope stares far enoug
h and long enough, we should be able to see it. I will be focusing on recen
t results from our program to map the CGM of 18 galaxies in the MHONGOOSE s
urvey in neutral hydrogen (HI) with the Green Bank Telescope. For this prog
ram we obtained deep observations with high HI column density sensitivity,
and focused on the diffuse HI detected outside the disks of each galaxy. By
quantifying the fraction of diffuse HI in the CGM, we were able to look fo
r correlations with other properties of the galaxies, such as the baryonic
and halo masses. We also analyzed each map as a function of radius, creatin
g column density and cumulative flux profiles for each galaxy in our sample
. Most galaxies showed an increasing cumulative flux profile at large radii
, suggesting that either an HI truncation radius was not reached, or that w
e are seeing the large-scale diffuse structure from the IGM.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210308T120000
DTEND;TZID=America/Chicago:20210308T130000
RECURRENCE-ID;TZID=America/Chicago:20210308T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Spring Break - No talk scheduled
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Spring Break - No talk scheduled
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210315T120000
DTEND;TZID=America/Chicago:20210315T130000
RECURRENCE-ID;TZID=America/Chicago:20210315T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Annalisa Citro, University of Wisconsin Milwaukee
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
J1059+4251: a highly magnified gravitationally lensed z~2.8
galaxy. ESI observations of the rest frame UV spectrum
<
!-- START: Sliders -->
<
a href="https://astronomy.utexas.edu/calendar/icals.icalevent/-?evid=1591&i
cf=1&tmpl=component#abstract-6" class="accordion-toggle rl_sliders-toggle n
n_sliders-toggle rl_sliders-item-scroll nn_sliders-item-scroll collapsed" d
ata-toggle="collapse" id="slider-abstract-6" data-id="abstract-6" data-pare
nt="#set-rl_sliders-6" role="button" aria-controls="abstract-6" aria-expand
ed="false"> A
bstract
Abstract
Detailed analyses of high-redshift
galaxies are challenging due to their faintness, but this difficulty can be
overcome with gravitational lensing, in which the magnification of the flu
x enables high signal-to-noise ratio (S/N) spectroscopy.
We pre
sent the rest-frame ultraviolet (UV) Keck Echellette Spectrograph and Image
r (ESI) spectrum of the newly discovered z=2.79 lensed galaxy SDSS J1059+42
51. With an observed magnitude F814W = 18.8 and a magnification factor mu=
31± 3, J1059+4251 is both highly magnified and intrinsically luminous, maki
ng it one of the brightest lensed galaxies observed so far. With stellar ma
ss M*= 3.7 x 1010 M☉, star formation rate SFR=73 M☉ yr-1, and stellar metal
licity Z*=0.004, J1059+4251 is typical of bright star-forming galaxies at s
imilar redshifts.
Thanks to the high S/N and the spectral resolution
of the ESI spectrum, we are able to separate the interstellar and stellar f
eatures and derive properties that would be inaccessible without the aid of
the lensing. We find evidence of a gas outflow with speeds up to - 1000 km
s-1, and of an inflow that is probably due to accreting material seen alon
g a favorable line of sight.
We measure relative elemental abun
dances from the interstellar absorption lines and find that alpha-capture e
lements are overabundant compared to iron-peak elements, suggestive of rapi
d star formation.
However, this trend may also be affected by dust de
pletion, which is particularly high in J1059+4251. Thanks to the high data
quality, our results represent a reliable step forward in the characterizat
ion of typical galaxies at early cosmic epochs.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210322T120000
DTEND;TZID=America/Chicago:20210322T130000
RECURRENCE-ID;TZID=America/Chicago:20210322T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Dustin Davis, The University of Texas at Austin
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Lyman Continuum from Galaxies 3.0 < z < 3.5
em>
Abstract
In this talk, we review t
he selection of a pure sample of high redshift (3.0 < z < 3.5) Lyman-
Alpha Emitting galaxies and stack their low-resolution spectra to measure t
he average escape of Lyman Continuum emission from the ensemble. We report
a 3-sigma detection of 0.10 uJy Lyman Continuum emission and an evolution w
ith UV Luminosity supporting a potentially dominant role of lower-mass, rap
idly star-forming galaxies in the ionizing photon budget during the Epoch o
f Reionization.
p>
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210329T120000
DTEND;TZID=America/Chicago:20210329T130000
RECURRENCE-ID;TZID=America/Chicago:20210329T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Oscar Chavez Ortiz, The University of Texas at Austin
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Constraining Reionization: Correlating Galaxy Properties wit
h Lyman-Alpha Emission Strength
Abstract
Abstract
Reionization is the period of the universe where it transi
tioned from a neutral state to an ionized state. Many questions around this
epoch still persist, such as when did reionization occur, what were the dr
iving mechanisms, and how long did reionization last? I set out to answer t
hese questions and better understand reionization by focusing on how galaxy
properties correlate with Lyman-Alpha emission. To this end, I will use th
e HETDEX spectroscopic survey, paired with Bayesian SED fitting to make a p
redictive distribution for Lyman Alpha strength that is tied to galaxy prop
erties. This can be used as an improved estimate of the emergent Lyman-Alph
a emission from distant galaxies, improving constraints on reionization. Th
us far, I have worked on a small sample of galaxies in the North-Ecliptic P
ole (NEP) working on getting SED fitting to determine global galaxy propert
ies. Using the best-fit galaxy property values, binning them according to s
tellar mass, dust attenuation, etc. will reveal if there are any correlatio
n between the given property and its Lyman-Alpha line strength. Once correl
ations between a given galaxy property and Lyman-alpha emission are found,
I will work on making a predictive model that will tell anyone for a given
set of galaxy properties the Lyman-Alpha line strength that it corresponds
to.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210405T120000
DTEND;TZID=America/Chicago:20210405T130000
RECURRENCE-ID;TZID=America/Chicago:20210405T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Jackie Champagne, The University of Texas at Austin
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
The Hunt for LBGs in the Environments of z=6 Quasars
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210412T120000
DTEND;TZID=America/Chicago:20210412T130000
RECURRENCE-ID;TZID=America/Chicago:20210412T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Two Talks
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Taha Dawoodbhoy, The University of Texas at Austin
Cosmological Structure Formation in Scalar Field Dark Matter with Repu
lsive Self-Interaction
Rebecca Larson, The University of
Texas at Austin
Islands of Reionization
Abstract
While the end of reionization is a
frequent target of observations, how this process begins, and what causes
it are presently unconstrained. One scenario allows reionization to start l
ate and complete rapidly, where moderately luminous galaxies dominate the i
onizing photon budget (Robertson et al. 2015). Another scenario allows a sm
ooth temporal evolution of reionization, where very faint galaxies, common
at early times, dominate the photon budget (Finkelstein et al. 2019). These
models differ drastically in their predictions for the ionized fraction at
z~9 (~20% vs. ~60%), and our recent MOSFIRE program has sought Lyα emissio
n at this epoch to distinguish between these two possibilities. We have imp
lemented improved data reduction and stacking of spectra, which accounts fo
r the drift of objects in the slits throughout the night, and unknown offse
ts of our objects from the expected location in the slit. In this talk, I w
ill show our Lyα detection at z=8.661 in the EGS field in 9.53 hours of int
egration. This galaxy lies physically close (3.5 pMpc) to another confirmed
galaxy in this field, with Lyα detected at z=8.684 (Zitrin et al. 2015).&n
bsp; Our sources might suggest the presence of the highest redshift overden
sity in the reionization era, indicate the existence of ≥1Mpc ionized bubbl
es as early as 500Myr after the Big Bang, and shed light on galaxy growth i
n the early universe.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210419T120000
DTEND;TZID=America/Chicago:20210419T130000
RECURRENCE-ID;TZID=America/Chicago:20210419T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Two Talks
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Olivia Cooper, The University of Texas at Austin
<
em>Dusty Needles in a Haystack: 2mm follow-up of Dusty Star-Forming Galaxie
s in SSA22
Abstract
Dus
ty Star-Forming Galaxies (DSFGs) dominate cosmic star formation at its peak
epoch and yet their volume density in the early Universe is highly unconst
rained, where their existence impacts our models of dust and metal producti
on and massive galaxy assembly in the first few Gyr. Empirical modeling sug
gests 2mm imaging of existing, bright samples of DSFGs selected at 850um-1m
m can quickly and easily separate DSFGs by redshift, isolating the "needle
in a haystack" DSFGs that sit at z>4 or beyond. With follow-up ALMA 2mm
imaging for a sample of 850um-bright DSFGs in protocluster field SSA22, we
characterize the galaxies' IR SEDs, identify the highest redshift candidate
DSFGs, and estimate their contribution to the cosmic star formation rate d
ensity.
Lindsay
House, The University of Texas at Austin
Power of the Peo
ple: Using Citizen Science to Fuel Our Search for Dark Energy
<
div class="accordion-heading panel-heading" role="heading" aria-level="2">
Abstract
Abstract
During five years of observ
ations, the Hobby-Eberly Dark Energy Experiment (HETDEX) will find over one
million galaxies that are 9 billion to 11 billion light-years away, and wi
ll yield the largest map of the universe ever produced. The map will allow
us to measure how fast the universe was expanding at different times in its
history. Changes in the expansion rate will reveal the role of dark energy
at different epochs, but the most difficult task is determining which gala
xies come from our epoch of interest (at z~2-3) and which ones are nearby.
These one million sources require visual classification for the most accura
te results, yet this requires many working hours. Over the past year, I hav
e used Zooniverse, the worlds largest citizen science platform, to train pa
rticipants all over the world to efficiently classify these objects. The pr
oject has been live for less than 2 months and we have already had 750,000
classificiations. I will discuss the methods we have used and how citizen s
cience can be applied to big data astronomy and preliminary applications to
machine learning.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210426T120000
DTEND;TZID=America/Chicago:20210426T130000
RECURRENCE-ID;TZID=America/Chicago:20210426T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Katie Chworowsky, The University of Texas at Austin
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Constructing a Catalog of High-z Massive Quiescent Galaxies<
/strong>
Abstract
Under
standing the formation and evolution of massive quiescent galaxies are nece
ssary to understanding how galaxies grow and cease star-formation. Recent o
bservations with sensitive near-infrared imaging cameras have detected a po
pulation of massive quiescent galaxies in the early Universe (z~3-5), at an
abundance that current cosmological simulations are unable to produce. One
key challenge with characterizing these galaxies arise from uncertainties
in their photometric redshifts. Degeneracies between SEDs of low redshift (
z~1) dusty star forming galaxies (DSFG) and high-z massive quiescent galaxi
es implies that based purely on photometric fitting, a catalog of high-z ma
ssive quiescent galaxies will have a high contamination rate of low-z sourc
es. While a redshift-luminosity prior combined with photometric fitting wil
l greatly reduce contamination by nearby DSFGs, previously used priors do n
ot allow the presence of any moderately bright galaxies at z > 3. In thi
s talk, I will present a new redshift luminosity prior generated from the r
ecent "Santa Cruz" semi-analytic model (Somerville et al. 2015), and how it
can be used to constrain redshift probabilities for massive high-z galaxie
s. We will use this prior to generate a high confidence sample of massive g
alaxies at z~3-5, from which we can constrain the quiescent sample and pave
the way for future spectroscopic observations of these enigmatic sources t
o understand their formation.
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210503T120000
DTEND;TZID=America/Chicago:20210503T130000
RECURRENCE-ID;TZID=America/Chicago:20210503T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Postponed
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Seminar postponed to next week
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210215T120000
DTEND;TZID=America/Chicago:20210215T130000
RECURRENCE-ID;TZID=America/Chicago:20210215T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:5de9c3904d692ef6f889d4132bf519e5
CATEGORIES:Galaxies and Cosmology Seminar
SUMMARY:Christopher Agostino, Indiana University
LOCATION:Online
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Robustness of AGN selection with optical emission lines and
the physical drivers of AGN emission line diversity
DTSTAMP:20240329T041439Z
DTSTART;TZID=America/Chicago:20210222T120000
DTEND;TZID=America/Chicago:20210222T130000
RECURRENCE-ID;TZID=America/Chicago:20210222T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
END:VCALENDAR