Recent Talks

The number of photons received allows radio astronomers to resolve the
Universe on timescales of nanoseconds. This has been demonstrated over
decades by observations of giant pulses from the Crab Pulsar, why more
recently, it has led to the establishment of the  new research field of
Fast Radio Bursts. The latter were initially discovered in archival data but are now
established as a population of radio sources at cosmological distances.
While their origin still remains a mystery, they promise to become powerful
cosmological tools. This talk will briefly review time domain astronomy in
the radio regime, describe some of the latest FRB results, and will also address
the challenges. These range from dealing with large amounts of raw data
(PB to EB) that need to be processed in real-time with machine learning methods,
to delivering reliable triggers for multi-wavelength follow-up at optical and higher
frequencies.

Astrophysical masers are among of the best tools in studying star
formation processes, especially in massive star-forming regions where
star formation cores are deeply embedded in a complex gaseous
environment.  In this talk, I will give examples of such studies where
physical conditions (e.g. magnetic fields) as well as kinematics of the
regions can be derived from.  I will also highlight time-domain studies of
masers which help us to understand not only the physics and dynamics
of the regions but also maser physics itself.  At the end of my talk,
I will briefly present the latest development of radio astronomy research
in Thailand including the new 40-m Thai National Radio Telescope (TNRT)
and its future key science.

We are living in a golden era for testing gravitational physics with precision experiments. This talk will present new results using a variety of tests with radio astronomy, ranging from binary pulsars to imaging black holes in the centre of galaxies. These results will be placed in context of other ongoing experiments, such as detecting gravitational wave with ground-based detectors or pulsar timing arrays, before giving an outlook into the future.

The dust component of active galactic nuclei (AGN) produces a broad infrared spectral energy distribution (SED), whose power and shape depends on the fraction of the source absorbed, and the geometry of the absorber respectively. This emitting region is expected to be concentrated within the inner ∼5 pc of the AGN which makes almost impossible to image it with the current instruments. The study of the infrared SED by comparison between infrared AGN spectra and predicted models is one of the few ways to infer the properties of the AGN dust. We explore a set of six dusty models of AGN with available SEDs, namely Fritz et al. (2006), Nenkova et al. (2008B), Hoenig & Kishimoto (2010), Siebenmorgen et al. (2015), Stalevski et al. (2016), and Hoenig & Kishimoto (2017). They cover a wide range of morphologies, dust distributions, and compositions.

We explore the discrimination among models and parameter restriction using synthetic spectra (Gonzalez-Martin et al. 2019A), and perform spectral fitting of a sample of 110 AGN with Spitzer/IRS drawn from the Swift/BAT survey (Gonzalez-Martin et al. 2019B). Our conclusion is that most of these models can be discriminated using only mid-infrared spectroscopy as long as the host galaxy contribution is less than 50%. The best model describing the sample is the clumpy disk-wind model by Hoenig & Kishimoto (2017). However, large residuals are shown irrespective of the model used, indicating that AGN dust is more complex than models. We found that the parameter space covered by models is not completely adequate. This talk will give tips for observers and modelers to actually answer the question: how is the dust arrange in AGN? This question will be one of the main subjects of future research using JWST in the AGN field.

David Calle, youtuber, fundador del portal educativo unicoos nos contará como surgió la idea y los retos a los que tuvo que enfrentarse. Y cómo el uso del vídeo está modificando la forma en la que el profesorado y alumnado interactúa en el proceso de enseñanza-aprendizaje (flipped classroom).

Esta charla servirá, también, como punto de partida de una futura colaboración conjunta para la creación de contenidos divulgativos y educativos (enseñanza reglada) que comenzaría con la selección de un equipo de astrofísicas/os, que tengan alguna relación con el IAC-ULL con el objetivo de desarrollar vídeos soporte para:

• las optativas de Astrofísica del Grado de Físicas
• las asignaturas del Máster de Astrofísica.

Since first light in 2004 the 2.0m Liverpool Telescope has been the world’s largest
fully robotic telescope. It specialises in time domain astrophysics and has
a dedicated instrument suite giving imagining, spectroscopic and
polarimetric capabilities. In this seminar I will describe how the robotic
operation of the telescope works and give examples of the science
accomplished in areas such as gamma ray burst follow-up and supernova
classification. I will also present our plans to develop a new 4.0m robotic telescope
in collaboration with colleagues at IAC which will deliver faster reaction and
increased sensitivity.

In this talk, I present a new technique that explores the hypothesis that
the structure producing the continuum emission at mid-IR and the reflection
component at X-ray are the same. If this is the case, they can be used
together to better constrain the physical parameters of the torus. Our
technique consists on a simultaneous fitting of Spitzer and NuSTAR spectra
using mid-IR and X-ray models available. During this talk, I will also show
the first results obtained when applying our technique to the nearby type-2
active nucleus IC 5063. Finally, I will talk about the work that we are
currently developing using this technique.

Until the advent in the late 1990’s of sensitive submillimetre arrays such as SCUBA, it was generally thought that the main sources for the interstellar dust found in galaxies were the dusty outflows from evolved AGB stars and M supergiants, although a dust contribution from supernovae had long been predicted on theoretical grounds. The detection at submillimetre wavelengths of very large dust masses in some high redshift galaxies emitting less than a billion years after the Big Bang led to a more serious consideration of core-collapse supernovae (CCSNe) from massive stars as major dust contributors. KAO and Spitzer mid-infrared observations confirmed that CCSN ejecta could form dust but it was not until the Herschel mission and subsequent ALMA observations that direct evidence has been obtained for the presence of significantly large masses of cold dust in young CCSN remnants. As well as using infrared spectral energy distributions to measure the amounts of dust forming in CCSN ejecta, dust masses can also be quantified from the analysis of red-blue asymmetries in their late-time optical emission line profiles. I will describe current results from these methods for estimating ejecta dust masses, and their implications.