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A toda la comunidad, <br>
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<div class="moz-forward-container"> <br>
los invitamos a asistir a las cinco (5) charlas que se brindarán
en el transcurso de la semana que viene en el marco de los
Seminarios FCAG, en el Salón Meridiano. A continuación les
enviamos los detalles de cada charla y los datos de conexión
para aquellas personas que no puedan acercarse al Salón
Meridiano.</div>
<div class="moz-forward-container"><b><br>
</b></div>
<div class="moz-forward-container"><b>-LUNES 11 - 14h: Seminario
"A black hole's gotta eat too: accretion on low-luminosity
AGN"</b>. La misma estará a cargo del <b>Lic. Iván López</b>
(Universidad de Bologna).
<br>
<br>
<b>Resumen:</b>
Spectral Energy Distribution (SED) fitting is a popular
technique to derive properties of galaxies, such as stellar
masses and Star Formation Rate
(SFR), and from their active nuclei, such as bolometric
Luminosities produced by the central black hole’s accretion. We
used the code Cigale on an X-ray-selected sample of active
galaxies until z<2.5 with data from X-ray to mid-IR and
obtained reliable values of the accretion luminosity.
We compared these properties to understand how they affect the
host
galaxy’s global properties in the co-evolution scenario. Now, we
are
applying a similar methodology with a nearby sample of galaxies
(<50Mpc,
based on the Palomar sample), extending the multiwavelength data
to far-IR
and radio. In this sample, we can focus our SED fitting in the
inner part
of the galaxy, obtaining better constraints on their accretion
luminosities, torus properties, and star-forming regions in the
inner
parsec.
We will present a new module for Cigale designed especially for
low-luminosity AGN that helps us to recover the black hole
properties even
for radiatively inefficient accretion disks (like
Advection-dominated
accretion flow (ADAF) or regular truncated disk). We can
understand the
Eddington rate distribution and Black Hole mass function in the
local
Universe by combining this sample with high-luminosity ones,
like BASS.
We also studied some sources of this sample to understand all
the details
of AGN Feedback in action. For one in particular, we will show
Spitzer IRS
spectral maps that reveal spectacular, extended H2 emission from
warm
(200-300 K) molecular gas in the inner 2.5 kpc of the spiral
galaxy M58
(NGC4579). Gemini NIRI imaging of the H2 1-0 S(1) emission line
and
archival ALMA CO 2-1 and HST multiband imaging show that most of
the H2
emission corresponds to lanes of dusty molecular gas that spiral
towards
the galaxy nucleus, where the PAH emission is consistent with
excitation by
UV radiation from old stars in the galaxy bulge rather than star
formation.
The most plausible scenario is that the inner radio jet is
shock-heating
the kpc-scale molecular disk. Jet-shocked H2 may impact star
formation and
help regulate the masses of the stellar bulges and SMBH in
otherwise normal
spiral galaxies. In the future, JWST will observe this galaxy
(Cycle 2, PI:
Lopez, IE) to resolve spatially and kinematically the jet-ISM
interactions
at a scale of 10 pc and determine what fraction of the molecular
and
ionized gas is heated in place and what fraction is an outflow.
JWST will
also yield the molecular and ionized gas outflow rates, which we
will compare to the SMBH accretion and nuclear star formation
rates to determine
how important these processes are in regulating both.
<br>
<br>
<b>-MARTES 12 - 11h: Seminario "Mapping the Hubble flow from z~0
to z~7.5 with HII galaxies"</b>. La misma estará a cargo del
Profesor Honorario <b>Dr. Roberto Terlevich</b>.</div>
<div class="moz-forward-container"><b><br>
</b>
<div dir="auto"><b>Resumen:</b> I will discuss the tight
relation between ionized gas velocity dispersions and Balmer
emission line luminosities in HII galaxies and Giant HII
regions, its implications and its use as distance indicator to
trace the expansion of the Universe up to z ~ 9 with JWST.
This approach yields tight independent constraints on H0, Ωm
and the Dark Energy equation of state parameter w. The
concordance between our determinations of H0, Ωm and w with
those from SNIa, BAO and Planck provides empirical support for
a universal IMF.</div>
<div dir="auto"><br>
</div>
<div dir="auto"><b>-MIÉRCOLES 13 - 13h: Seminario "<span
lang="EN-US">Modeling and simulation of geological
processes: phase
transition, dynamic fracture propagation, and compaction
band formation</span>"</b>. La misma estará a cargo del <b>Dr.
Victor Calo</b> (Curtin University, Perth, Australia).<span
lang="EN-US"><br>
</span></div>
<div dir="auto"><span lang="EN-US"><br>
</span></div>
<div dir="auto"><span lang="EN-US"><b>Resumen:</b> Our modeling
and simulation tools seek to describe the deformation of
large
geological structures. In particular, we describe various
complex rock
behaviours and simulate their evolution to understanding
geological phenomena
such as plate tectonics, rock properties, and their stress
fields. Our models
include the effects on rock deformation of its
microstructure, structural
discontinuities, fluid interactions, and induced pressure,
pressure solution,
stress corrosion, and different mineral reactions. </span><span
lang="EN-US">In this talk, to demonstrate the effectiveness
and robustness of our tools, we
will focus on a few exemplar applications to showcase the
tools we develop. In
particular, we will describe metamorphic rocks evolution
modeling where
chemo-mechanical interactions lead to phase transformation
and cracking. We
will also describe a new space-and-time adaptive scheme to
model complex
fracture propagation that circumvents typical mesh
dependency issues. Lastly,
we will study the compaction band formation in geomaterials,
specifically in
porous rocks.</span></div>
<div dir="auto"><b><br>
</b></div>
<div dir="auto"><b>-JUEVES 14 - 10h: Seminario "Los orígenes de
las Galaxias Ultra Difusas: Caracterización de su población
de cúmulos globulares en distintos entornos"</b>. La misma
estará a cargo del <b>Lic. Pablo Astudillo Sotomayor</b>
(Universidad de Concepción, Chile), invitado del Grupo ALAS.<span
lang="EN-US"><br>
</span></div>
<p></p>
<p><b><span
style="color: rgb(0, 0, 0); background-color: transparent; font-style: normal; font-variant: normal; text-decoration-skip-ink: none; vertical-align: baseline; white-space: pre-wrap;">Resumen:</span></b><span
style="color: rgb(0, 0, 0); background-color: transparent; font-weight: 400; font-style: normal; font-variant: normal; vertical-align: baseline; white-space: pre-wrap;"> Las galaxias ultra difusas (UDGs) son un subconjunto de galaxias de bajo brillo superficial (LSB) caracterizadas por sus grandes radios efectivos r_e > 1,5 kpc y bajo brillo superficial. Estas galaxias se han encontrado en una gran variedad de entornos, incluyendo el campo, grupos y cúmulos de galaxias. Las diferentes propiedades de las UDG y sus cúmulos globulares en función del entorno han planteado la cuestión del papel del entorno en la evolución de las UDG y los efectos del entorno en su población de cúmulos globulares (CG). En esta presentación, hablaremos de nuestro trabajo en curso para estudiar las propiedades de los UDG y sus cúmulos globulares en diferentes entorno utilizando sus CG como partículas trazadoras para restringir sus orígenes.</span></p>
<b>-JUEVES 14 - 12h: Seminario "La actividad del campo
Geomagnetico"</b>. La misma estará a cargo del <b>Geof. Julio
César Gianibelli</b><span
id="docs-internal-guid-f72d4bb1-7fff-977b-78e4-eef86b24566f">.</span><b><span
id="docs-internal-guid-f72d4bb1-7fff-977b-78e4-eef86b24566f"><br>
<br>
</span></b><b style="font-weight:normal;"
id="docs-internal-guid-f72d4bb1-7fff-977b-78e4-eef86b24566f">
<p dir="ltr"
style="line-height:1.3800000000000001;text-align: justify;margin-top:0pt;margin-bottom:0pt;"><b><span
style="color: rgb(0, 0, 0); background-color: transparent; font-style: normal; font-variant: normal; text-decoration-skip-ink: none; vertical-align: baseline; white-space: pre-wrap;">Resumen:</span></b><span
style="color: rgb(0, 0, 0); background-color: transparent; font-weight: 400; font-style: normal; font-variant: normal; text-decoration: none; vertical-align: baseline; white-space: pre-wrap;"> Diversas formas y particularidades se tienen en la determinación de la actividad del campo geomagnético. En la actualidad índices que representan esta fenomenología se editan y comunican por las redes. En esta presentación propongo la evaluación y determinación de un índice basado en la intensidad total F del campo geomagnético. </span></p>
</b><b style="font-weight:normal;"
id="docs-internal-guid-f72d4bb1-7fff-977b-78e4-eef86b24566f"><br>
</b><b style="font-weight:normal;"
id="docs-internal-guid-9900c2c0-7fff-a3eb-cd2d-42c502fb9543"><b
style="font-weight:normal;"
id="docs-internal-guid-84bbdb09-7fff-3b80-37a8-3bd0810a2176"><b>Datos
de conexión:</b> </b></b> <b style="font-weight:normal;"
id="docs-internal-guid-9900c2c0-7fff-a3eb-cd2d-42c502fb9543">
</b> <b style="font-weight:normal;"
id="docs-internal-guid-84bbdb09-7fff-3b80-37a8-3bd0810a2176">
</b> <b style="font-weight:normal;"
id="docs-internal-guid-84bbdb09-7fff-3b80-37a8-3bd0810a2176">
</b>
<div><b style="font-weight:normal;"
id="docs-internal-guid-84bbdb09-7fff-3b80-37a8-3bd0810a2176">
</b></div>
<div>Unirse a la reunión zoom: <a
href="https://us02web.zoom.us/j/89642687970"
class="moz-txt-link-freetext" moz-do-not-send="true">https://us02web.zoom.us/j/89642687970</a>
</div>
<div>ID de reunión: 896 4268 7970</div>
<div>Código de acceso: 526656</div>
<div><br>
</div>
<div><b>A fin de reducir el uso de residuos plásticos, les
solicitamos que se acerquen con sus propias tazas para el
café.</b></div>
<div>Aunque estos seminarios serán en formato híbrido, esperamos
contar con su presencia.</div>
<p>Saludos,</p>
<p>Secyt-FCAG<br>
</p>
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-- </div>
<pre class="moz-signature" cols="72">Secretaría de Ciencia y Técnica
Facultad de Ciencias Astronómicas y Geofísicas
Horario de atención: lunes a viernes de 8hs a 15hs</pre>
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