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<p>A toda la comunidad, <br>
</p>
<p>les recordamos que en el día de hoy, lunes 11 de diciembre a las
14h, en el Salón Meridiano, se brindará la siguiente charla en el
marco de los Seminarios de la FCAG<b> "A black hole's gotta eat
too: accretion on low-luminosity AGN"</b>.<b> </b>La misma
estará a cargo del<b> </b><b>Lic. Iván López</b> (Universidad de
Bologna). <b></b>A continuación les dejamos el resumen y los datos
de conexión para aquellos que no puedan acercarse al Salón
Meridiano.<b> <br>
</b></p>
<p><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. </p>
<p><b style="font-weight:normal;"
id="docs-internal-guid-9900c2c0-7fff-a3eb-cd2d-42c502fb9543"> </b></p>
<p dir="ltr"
style="line-height:1.3800000000000001;text-align: justify;margin-top:0pt;margin-bottom:0pt;"><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></p>
<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">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 este seminario será en formato híbrido, esperamos contar
con su presencia.</div>
<p> Saludos, <br>
</p>
<p>Secyt-FCAG</p>
<p></p>
<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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