LARIM 2023

#047 | Synthesis and inversion of Stokes parameters in the solar context applying Deep Learning Techniques.

Juan Esteban Agudelo Ortiz ¹ ; Germain Nicolás Morales Suarez ¹ ; Santiago Vargas Domínguez ¹ ; Sergiy Shelyag ²

1 - Universidad Nacional de Colombia. 2 - Flinders University.

[.pdf]

#239 | The effect of cross-section expansion on the evolution of coronal loops

Marcelo López Fuentes ¹ ; James A. Klimchuk ²

1 - Instituto de Astronomía y Física del Espacio (IAFE, CONICET-UBA). 2 - NASA Goddard Space Flight Center.

[.pdf]

#309 | Intermittent features in the solar wind: a case study

María Soledad Nakwacki ¹ ; Jerónimo Peralta Ramos ²

1 - Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina. 2 - Independent.

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#376 | Assessing the predictability of solar active regions using helioseismic holography: An exploratory data analysis

Daniel Alberto Rodríguez Torres ¹

1 - Universidad Nacional de Colombia.

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#433 | Terrestrial Influence of Solar Activity: The September 1941 Solar Storm and its Relationship with Unexplained Terrestrial Events

Freddy Moreno Cárdenas ¹ ;

Santiago Vargas Domínguez ² ; Juan Camilo Buitrago Casas ³

1 - Gimnasio Campestre. 2 - Universidad Nacional de Colombia. 3 - University of California, Berkeley.

[.pdf]

#548 | Study of magnetic field variations in high-cadence vector magnetograms during solar flares

Willinton Caicedo Tez ¹ ; Satiago Vargas ¹ ; Juan Camilo Buitrago ²

1 - Universidad Nacional de Colombia. 2 - Universidad de California, Berkeley.

[.pdf]

#172 | A density valley across stellar types

Julia Venturini ¹ ; María Paula Ronco ² ;

Octavio Guilera ² ; Jonas Haldemann ³ ; Christoph Mordasini ³ ; Marcelo Miller Bertolami ²

1 - University of Geneva. 2 - Instituto de Astrofísica de La Plata. 3 - University of Bern.

[.pdf]

#184 | The Influence of Stellar Activity on the Atmospheric Properties of Hot Jupiters

Micah G. C. Navia ¹ ; Luan Ghezzi ¹ ; Patricia Cruz ²

1 - Observatório do Valongo - UFRJ. 2 - Centro de Astrobiología (INTA-CSIC).

[.pdf]

Resumen:

During the last three decades, great advances have been made in the field of exoplanets. Among them, the discovery of an extreme class: the hot Jupiters. These exoplanets are objects with size and mass similar to Jupiter, but unlike the gas giant of the Solar System, their orbital period is less than ten days. This makes them extremely irradiated planets and, consequently, with higher temperatures. Since they are so close to their host stars, it is reasonable to assume that there is a direct stellar influence on the atmosphere of these objects. To study some of these effects, we can analyze the parameters obtained from secondary eclipses at infrared bands. These observations may provide important information, such as the brightness temperature and the presence or absence of thermal inversion layer in their atmospheres, when compared to models. Using a sample of 63 hot Jupiters with information on temperature inversion and stellar activity, we analyze the hypothesis that exoplanets without temperature inversion layer orbit active stars, while exoplanets with inversion orbit inactive stars. Furthermore, we reproduce two approaches from previous works that try to classify hot Jupiters according to their brightness temperatures and their relative fluxes. We did not find a clear correlation between the considered brightness temperatures and the stellar chromospheric activity index, except for the H and 5.8 µm bands that showed a weak correlation. In addition, we did not find a clear separation between exoplanets with or without thermal inversion as a function of stellar activity. We verified that the most irradiated exoplanets have atmospheric thermal inversion, while the least irradiated ones do not. Therefore, we conclude that stellar influence must be considered when studying the atmospheres of hot Jupiters. In the future, this research may serve as a basis for studying the atmosphere of rocky exoplanets.

#187 | Study of the dissipation times of gaseous disks in stellar populations

Jose L. Gomez ¹ ; Octavio M. Guilera ¹ ; Marcelo M. Miller Bertolami ¹ ; Paula M. Ronco ¹

1 - Instituto de Astrofísica de La Plata (UNLP-CONICET).

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#253 | Hot Jupiter - cold Jupiter. A complex sibling relation

Adriana Errico ¹

1 - UniSQ.

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#545 | Detailed abundance of the TESS$^\prime$ s First Circumprimary Planet in a very wide binary system

Jhon Joel Yana Galarza ¹ ; Thiago Ferreira ² ; Diego Lorenzo Oliveira ³ ; Henrique Reggiani ⁴ ; Adriana Valio ⁵

1 - The Carnegie Observatories. 2 - Universidade de Sao Paulo. 3 - Laboratorio Nacional de Astrofisica. 4 - NOIRLAB. 5 - Universidade Presbiteriana Mackenzie.

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#569 | Experimental simulation of a solar UV environment on Mars and its effects on germination and photosynthetic pigment content of Chenopodium quinoa

ERIKA PAOLA PUENTES LEÓN ¹ ; SANTIAGO VARGAS DOMÍNGUEZ ¹ ; ZAIDA ZARELY OJEDA PÉREZ ²

1 - UNIVERSIDAD NACIONAL DE COLOMBIA. 2 - UNIVERSIDAD PEDAGÓGICA Y TECNOLÓGICA DE COLOMBIA.

[.pdf]

#603 | A glass and a bottle of WINE: a prototypical transiting warm-Jupiter and a unique brown-dwarf detected by TESS

Matias Jones ¹

1 - ESO.

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#180 | Probing a laboratory asteroid model: mechanical characterization under loading-unloading cycles

Camila Sedofeito-Rajo ¹ ; Thomas Gallot ¹ ; Gonzalo Tancredi ¹

1 - Instituto de Física, Facultad de Ciencias, Universidad de la República.

[.pdf]

Resumen:

This study explores mechanical properties of asteroids as granular systems at the laboratory scale, exploring their significance in space mission design, Earth collision hazard assessment, and the comprehension of collisional processes. We present a comprehensive laboratory-scale characterization of granular media, focusing on both quasi-static and dynamic regimes. The use of laboratory-scale experiments provides a cost-effective alternative to in-situ measurements. The self-gravity of asteroids induces a stress distribution that remains poorly understood, but evidence suggests a gradient with increasing values towards the asteroid’s interior. The micro-gravity conditions on asteroids introduce unique mechanical properties, which are challenging to replicate on Earth. Despite being non-realistic, our experiments can be regarded as an accelerated aging representation of asteroids subjected to external stresses from impacts and emperature changes. They are particularly relevant for comprehending the propagation of seismic waves within asteroids ranging from a few km to tens of km in radius. The experimental results demonstrate that granular media exhibit quasi-elastic behavior during each compression cycle, with increasing elasticity. The stress-strain curve exhibits irreversible compaction with significant hysteresis during relaxation. Another focus of this study is understanding the nature of active asteroids, which could be due to a shaken mechanism induced by the propagation of seismic waves into the interior. Seismic waves generated by impacts and vibrations in our experimental device show high attenuation. The wave speed follows a power-law relationship $v \propto p^{1/2}$, and the elasticity of granular media depends on the time and strain scales. Remarkably, our experiments indicate that the speed of impact-generated and shaker-born seismic body waves does not exhibit a strong dependence on the origin mechanism. This suggests that safer wave-generating methods, may be used in low-gravity laboratory experiments instead of risky impact devices. Our research serves as foundational work for enhancing our understanding of asteroid interiors and boulder distribution.

#256 | Surface composition of the Trojan Asteroids, What to look for from the LUCY mission?

Mario Melita ¹

1 - IAFE (UBA-CONICET).

[.pdf]

#262 | Near Earth Observations from CASLEO’s Jorge Sahade (2.15m) telescope

Mario Melita ¹ ; Luis Mammana ² ; Daniela Lazzaro ³ ; Plicida Arcoverde ³ ; J.Weslley Pereira Da Silva ³

1 - IAFE (CONICET-UBA). 2 - CASLEO (CONICET-UNLP-UNSJ-UNC). 3 - Observatorio Nacional (RJ-Brasil).

[.pdf]

#292 | Physical properties of Near-Earth Objects derived from photometric observations at Observatório Astronômico do Sertão de Itaparica (OASI)

Weslley Pereira ¹ ; Plícida Arcoverde ¹ ; Mario Melita ² ; Luis Mammana ³ ; Eduardo Rondón ¹ ; Marçal Evangelista-Santana ¹ ; Jonatan Michimani ¹ ; Filipe Monteiro ¹ ; Teresinha Rodrigues ¹ ; Daniela Lazzaro ¹

1 - Observatório Nacional/MCTI. 2 - IAFE (CONICET-UBA). 3 - CASLEO (CONICET-UNSJ-UNLP-UNC).

[.pdf]

#308 | Ejection experiment in soft granular media

Valeria Abraham ¹ ; Thomas Gallot ¹ ; Gonzalo Tancredi ¹ ; Camila Sedofeito ¹

1 - Instituto de Física, Facultad de Ciencias, Universidad de la República.

[.pdf]

#332 | What is the frequency of meteorite falls? Is there a preferred day?

Ismael Acosta ¹ ; Gonzalo Tancredi ¹

1 - Departamento de Astronomía, Instituto de Física, Facultad de Ciencias, Universidad de la República.

[.pdf]

#345 | Transitional objects: monitoring through archival images and new observations

Silvia Martino ¹ ; Gonzalo Tancredi ¹ ; Martin Banda-Huarca ² ; Julio Bueno Camargo ² ; Eduardo Rondon ² ; Daniela Lazzaro ² ; Javier Licandro ³

1 - Facultad de Ciencias, Universidad de la República, Montevideo. 2 - Observatório Nacional, Rio de Janeiro. 3 - Instituto de Astrofísica de Canarias.

[.pdf]

#363 | Tidal evolution in dwarf planets systems as an application of the creep model

Karyna Gimenez ¹ ; Adrián Rodríguez ¹

1 - Observatório do Valongo- Universidade Federal do Rio de Janeiro.

[.pdf]

#386 | Reviewing cometary-like asteroids in view of the DART experiment

Gonzalo Tancredi ¹

1 - Departamento de Astronomía, Udelar, Uruguay.

[.pdf]

Resumen:

Several objects in asteroidal orbits have presented comaes and tails like the ones presented by comets for short period of times. There are at present ~46 objects that has presented, at least for a brief period, this cometary-like appearance. These objects are generally coined “Active Asteroids”, implicitly implying that some kind of on-going endogenous or exogenous active process is the mechanism that produce the long-lasting tails. Nevertheless, what we observe is that those asteroids are temporally dressed as comets. Several hypotheses have been proposed to explain the “activity” of these object. {\bf Lessons from DART}: The NASA-DART experiment give us an opportunity to review our knowledge of this population. Following the impact of the space probe against asteroid Dimorphos on September 26, 2022, several thousand tons of material were ejected at a wide range of velocities. Tancredi et al. (2023) dubbed the DART experiment as the creation of the first artificial “Active Asteroid”. They proposed that the production of a large amount of low-speed ejected material could be described by the “cocoa effect”: the lofting of small particles from the top of a dust layer when shaking the ground. The combination of the impact induced seismic shaking plus the “cocoa effect” can produce the ejection of particles from a large fraction of the impacted hemisphere. They predicted a brightness increase due to a slowly moving dust cloud, the obscuration of Dimorphos’ surface by this cloud, and the generation of a long-lasting tail, which were confirmed by the close-by observations of LICIACube, as well as long-range tracking from HST and the ground. By July 2023, over 250 days after impact, the tail is still visible. Based on these results, we review the relevance of the different mechanism proposed to explain the appearance of the population of asteroids temporally dressed as comets.

#410 | The catalogue of asteroid polarization curves

Ricardo Gil-Hutton ¹

1 - Universidad nacional de San Juan y CONICET.

[.pdf]

#411 | An update of the comet candidates among the quasi-Hilda objects

Jorge Correa-Otto ¹ ;

Ricardo Gil-Hutton ¹ ; Esteban García-Migani ¹

1 - Universidad Nacional de San Juan y CONICET.

[.pdf]

#434 | Near-Earth asteroids in cometary orbits: a new study

Valentina Pezano ¹ ; Andrea Sosa ¹

1 - CURE - Universidad de la República.

[.pdf]

Resumen:

Asteroids and comets are the remnants of the accretion process that formed the planets about 4.6 billion years ago. Their physical nature, chemical composition, and orbital characteristics depend on the region of the solar system where they originally formed. Traditionally, asteroids are considered rocky, inert objects, while comets are icy, active bodies. Also, in general, asteroids have more stable orbits and longer dynamic lifetimes than comets, due to much less close encounters with the planets (especially Jupiter). However, this boundary has become more blurred, especially among near-Earth objects (defined as those reaching perihelion distances $q$ < 1.3 au). For instance, near-Earth asteroid 3552 Don Quixote shows cometary activity (Mommert et al. 2014, The Astrophysical Journal 781), and in the other hand some near-Earth comets were found to have stable orbits like asteroids (Fernández and Sosa 2015, Planetary and Space Science 118).\\ Following Fernández et al. 2014 (Icarus 238), we analyze a sample of 327 near-Earth asteroids (NEAs) that approach or cross Jupiter’s orbit (aphelion distances $Q$ > 4.8 au), with Tisserand parameters 2 < $T$ < 3 and orbital periods $P$ < 20 yr, i.e. resembling the orbital characteristics of the Jupiter family comets. We also constrain the sample to those objects with better quality orbits (i.e. condition codes < 6). We use the NASA JPL Small-Body Database. We integrated the orbits of the selected objects plus 50 clones of each one, for 10.000 yr in the past and in the future, to study their dynamic evolution. We also analyze the conditions for photometric observations of selected objects which could improve our physical knowledge of this population. We present the preliminary results, based in an updated and larger (by a factor of 2) orbital database of NEAs, and numerical integrations with ten times more clones than the previous work.

#505 | PRE- DISINTEGRATION STUDY OF COMET C/2021 A1 (Leonard)

Romina García ¹ ; Eduardo Fernández Lajús ² ; Romina Di Sisto ² ;

Ricardo Gil-Hutton ¹

1 - Universidad Nacional de San Juan y CONICET. 2 - Universidad Nacional de La Plata e IALP-CONICET.

[.pdf]

#534 | Rotational period determination of fortuitous asteroids

Johana Murcia-Rocha ¹ ;

Camilo Delgado-Correal ² ; Sergio Silva-Cabrera ³

1 - Orbitamautas Astronomy Group. 2 - Francisco José de Caldas District University of Bogotá. 3 - CONAHCYT - Instituto de Astronomía - UNAM.

[.pdf]

#537 | Evaluation of the AUTOBOL algorithm withh a sample of events detected by the BOCOSUR Network in Uruguay

Alvaro Guaimare ¹ ; Manuel Caldas ¹ ; Gonzalo Tancredi ¹ ; Juan Ballestrino ² ; Cecilia Deandraya ² ; Cristian Uviedo ² ; Ignacio Ramírez ² ; Valeria Abraham ¹ ; Lucía Velasco ¹ ; Lucas Barrios ¹ ; Matías Hernández ¹

1 - Departamento de Astronomía, Instituto de Física, Facultad de Ciencias, Universidad de la República.. 2 - Departamento de Ing. Eléctrica, Facultad de ingeniería, Universidad de la República..

[.pdf]

Resumen:

Since 2019 we have deployed a network of stations with allsky cameras for the detection of bright meteors (fireballs). By October 2021, 6 stations were installed in the south of Uruguay, in what made up the first stage of the {\it Red de Detección de Bólidos del Cono Sur (BOCOSUR)}. These first stations were built using a Watec 902H2 CCTV camera with an Arecont vision fisheye lens (f/2.0, 1.55mm). The stations run an application developed by our group (see Caldas et al. in this conference), which detects any change in brightness in consecutive frames. While the variations persist, a short video of less than 10 seconds is recorded. In these videos you can detect animals, planes, rain, clouds, lightning or other phenomena, in addition to the fireballs that are of interest to us. Therefore, a classification should be made between videos with and without fireball. Initially a manual classification was made. In 2022, a group of Electrical Engineering students (Ballestrino et al. 2022) developed an algorithm based on machine learning for the automatic classification of the videos, using the classification we had done as a training base. The algorithm called {\it Autobol} was developed in python, and is available at https://github.com/jpballestrino/AutoBol github. To train the {\it Autobol} package, we used the manual classification of at $\sim 8000$ videos, where 363 of them have fireballs. The classification was made by team members, as well as high-school students and teachers that participate in the project (see Velasco et al. in this conference for a description of the training workshops). In this poster we will present the results of applying these predictive classification models to a database of over 250,000 videos. We will present statistics on the performance of the network and the classification algorithm. References: Ballestrino, J. et al., https://hdl.handle.net/20.500.12008/32619

#156 | Random particle distribution gives rise to protostar and rings in a protoplanetary system

NICANOR POVEDA TEJADA ¹ ; Nelson Vera-Villamizar ¹

1 - Universidad Pedagogica y Tecnologica de Colombia.

[.pdf]

#231 | Dynamical characterization of the 6/1 mean motion resonance between Quaoar\textquotesingle s ring and Weywot

Adrián Rodríguez ¹ ; Bruno Morgado ¹ ; Nelson Callegari Jr. ²

1 - Observatório do Valongo, Universidade Federal do Rio de Janeiro. 2 - Instituto de Geoci\^encias e Ci\^encias Exatas.

[.pdf]

#238 | Variability of water vapor in the internal atmosphere of Mars associated with the solar activity cycle.

Johan Nicolás Molina Córdoba ¹ ; Santiago Vargas Domínguez ¹ ; Jorge Ivan Zuluaga ²

1 - Observatorio Astronómico Nacional, Universidad Nacional de Colombia. 2 - Universidad de Antioquia.

[.pdf]

Resumen:

The atmosphere of Mars has been the subject of study in numerous scientific investigations to understand its complex atmospheric phenomena. In this research work, we have explored the existence of an interesting relationship between the periodic oscillations of H$_2$O concentration in the Martian atmosphere and the Pectinton solar flux index in the 10.7 cm band, around the characteristic solar activity period of 11 years. To investigate this relationship, the H$_2$O abundance data package provided by SPICAM from Mars Express was analyzed, spanning the time window from 2004 to 2018. These data were compared with solar flux records obtained from the NOAA database. The analysis was carried out by calculating the Lomb-Scargle periodogram for both signals. Although this method is commonly used in the study of star light curves, its application to planetary atmospheres has shown promise, providing results consistent with models that describe periodic variations in the atmosphere, such as seasonal changes. To validate the effectiveness of this method, it was tested against data sets of abundances of different chemical species at various heights in the Earth's atmosphere. These data were obtained from the empirical model NRLMSISE-00 and covered a wide range of years between 1961 and 2021. The results obtained from both the terrestrial model and the data derived from SPICAM detections supported the usefulness of the method for the study of oscillatory phenomena. of long periods, such as days, months and years, that can occur in the atmosphere of a planet, or in its possible relationship with other factors. This research work brings new insights into the atmospheric dynamics of Mars and its connection to the solar cycle, which could have significant implications for the study of other celestial bodies and for a deeper understanding of them. climatic processes in planetary environments.

#257 | Tidal effects in resonant chains of close-in planets

Carolina Charalambous ¹ ; Anne-Sophie Libert ²

1 - Pontificia Universidad Catolica de Chile. 2 - Universidad de Namur.

[.pdf]

#290 | Like a wrecking ball: understanding giant planets as the key to finding Earths

Rob Wittenmyer ¹ ; Alex Venner ¹ ; Jonathan Horner ¹

1 - University of Southern Queensland.

[.pdf]

#342 | Coorbital dynamics: a semi-analytical approach to study equilibrium points in resonant coorbital configurations under extreme inclination and/or eccentricity

Nicolas Pan Rivero ¹ ; Tabare Gallardo ¹

1 - Facultad de Ciencias, UdelaR.

[.pdf]

#392 | Secular evolution of resonant planets in the elliptical coplanar case

Juan Pons ¹ ; Tabaré Gallardo ¹

1 - Facultad de Ciencias, UdelaR.

[.pdf]

#484 | Qualitative analysis of the evolution of planetary systems

Eduardo Verrone Sanches ¹ ; Tatiana Alexandrovna Michtchenko ¹

1 - Universidade de São Paulo.

[.pdf]

Resumen:

Discoveries of extrasolar planetary systems have shown that the configuration of our Solar System is an exception to the rule given the number of systems with high relative inclinations, large eccentricities and high mass planets in orbits with periods of hours. Due to these peculiar characteristics, our goal is to understand the processes that led planetary systems to acquire such characteristics, through mutual gravitational interaction and with the proto-planetary disk. To verify the quality of the observational data and the stability of the planetary systems in periods of at least 1Myr, we use the concepts of Hill Stability (Marchal \\& Bozis (1982) and Gladman (1993)) that consider the configuration of the systems in terms of total energy and orbital angular momentum; to evaluate their secular movements we work with the construction of Representative Plans that bring with them information of the long-period behavior of the system, based only on the mass ratio of the planets and the ratio of their semi-major axes; To analyze the temporal evolution, we use the theory of semi-analytical perturbation (Michtchenko \\& Malhotra, 2004) that allows us to explore systems of high eccentricities by not working with series expansions of the Disturbing Function. We work with models that simulate the process of planetary migration (Michtchenko \\& Rodríguez, 2011), which change the orbital elements in a forced way, seeking to relate the migration trajectories with known processes, interaction of the planet with proto planetary disk, accretion of matter and tidal effects. Using the stability criteria, we selected some planetary systems to start the analysis and, after verifying their secular behavior, we started the simulations of migratory processes to understand through which configurations the system passed until arriving in the current state, considering only the variation of the total energy of the system and the orbital angular momentum.

#489 | A local approach of planetesimal fragmentation applied to planet formation

Irina Luciana San Sebastián ¹ ;

Octavio Miguel Guilera ¹ ; Marcelo Miguel Miller Bertolami ¹

1 - Instituto de Astrofísica de La Plata.

[.pdf]

Resumen:

One of the challenges in planetary formation models is, including the main physical phenomena in that process, to explain the diverse architectures of planetary systems observed to date. The modelling of collisions and planetesimal fragmentation is key to reproducing planetary formation and evolution correctly. Depending on the particle sizes and impact velocities, these collisions may result in different outcomes, such as growth, rebound, erosion, mass transfer, fragmentation, craterization, compaction, or grinding. Our previous works show that the inclusion of a detailed model of planetesimal fragmentation, considering different compositions and relative velocities of planetesimals, may inhibit or favour the formation of giant planet cores, drastically changing the final planetary system architectures. However, in the planetary formation global models, the detailed modelling of these processes is extremely expensive from a computational point of view. Generally, these models include the planetesimal fragmentation process locally. In this work, we study and compare a local approximation of this process that simplifies the phenomenon numerically, significantly reducing the computing time required for our simulations. We compare these results to our detailed model of planetesimal fragmentation applied to giant planet formation and contrast it with other local approximations in the literature to determine its validity. Currently, the large amount of observational data provides us with statistical properties of the exoplanet population and constraints for planetary formation models. Population synthesis models allow us to link these properties with the physical processes that take part in the planetary formation process. For the future, our aim is to conduct a population synthesis study that includes planetesimal fragmentation into PLANETALP, our global model of planet formation.

#494 | The AGE-PRO ALMA Survey: A glimpse into the gas evolution in protoplanetary disk

Carolina Agurto ¹ ; Laura Perez ¹ ; Ke Zhang ² ; Anibal Sierra ¹ ; James Miley ³

1 - Universidad de Chile. 2 - University of Wisconsin–Madison. 3 - ALMA/European Southern Observatory.

[.pdf]

#100 | Astrochemical study of the young stellar object G29.862$-$0.0044 at core spatial scales

Naila Constanza Martinez ¹ ; Sergio Paron ¹ ; Damián Mast ² ; Martín Ortega ¹ ; Alberto Petriella ¹ ; Cecilia Fariña ³

1 - Instituto de Astronomía y Física del Espacio. 2 - Observatorio Astronómico de Córdoba, UNC. 3 - Instituto de Astrofísica de Canarias y Universidad de La Laguna.

[.pdf]

#154 | Study of Two Massive Molecular Clumps

Natacha L. Isequilla ¹ ; Martin Ortega ¹ ; Alejandro Marinelli ¹ ; Naila C. Martinez ¹ ; Sergio Paron ¹

1 - Instituto de Astronomía y Física del Espacio.

[.pdf]

#176 | A spectroscopic stellar parameters study of T Tauri Stars in the Orion Star Forming Complex – A LAMOST view

Jesús Hernández ¹ ; Luisa Zamudio ² ; Cesar Briceño ³ ; Nuria Calvet ⁴ ; Carlos Román ¹ ; Javier Serna ¹ ; Sergio Sanchez ¹ ; Maria Gracia Batista ⁵ ; Anlly Vélez Orozco ⁶ ; Cesar Millan ⁵ ; Ezequiel Manzo ¹ ; Lucia Adame ¹

1 - Universidad Nacional Autónoma de México, Instituto de Astronomía. 2 - Boston University. 3 - Cerro Tololo Inter-American Observatory NSF s NOIRLab. 4 - University of Michigan. 5 - Universidad de los Andes. 6 - Universidad de Antioquia.

[.pdf]

#211 | Investigating the Starspot Paradigm in T Tauri Stars.

Facundo Pérez Paolino ¹ ; Lynne Hillenbrand ² ; Jeff Bary ¹ ; Madison Markham ¹

1 - Colgate University. 2 - California Institute of Technology.

[.pdf]

Resumen:

Accurate age and mass determinations for the youngest stars are crucial for understanding Pre-Main-Sequence star-disk evolution and planet formation. This most important task has proven difficult, as these systems are characterized by strong magnetic fields that lead to significant magnetically-driven phenomena like starspots, flares, and the channeling of both inflowing and outflowing material. Due to the fully convective interiors of the youngest stars and these strong magnetic fields, the large-scale suppression of convection is possible in low-mass stars, leading to starspots covering large fractions of their surfaces. A number of observed phenomena support this: spectral type mismatches between optically determined and infrared spectral types, color differences with main sequence stars, radius inflation, large age spreads for stars in the same cluster, and periodic photometric variability. In the context of these struggles, we present results from multi-epoch near-infrared spectroscopy to characterize the spot-behavior of 32 T-Tauri Stars in Taurus-Auriga. We constructed composite models of spotted stars by combining BTSettl-CIFIST atmospheres to represent the spots and the photosphere along with accretion and disk continua. Using a Markov-Chain Monte-Carlo algorithm, we find the best-fit spot and photospheric temperatures, spot filling factors, as well as disk and accretion filling factors. This methodology allowed us to reproduce the 0.75-2.40 micron stellar spectra for all of our targets, disentangling the complicated multi-component emission. For a subset of the targets, fitting multi-epoch data spanning an entire stellar rotation, we are able to correlate K2 photometry with spectral variability on rotational timescales. Combining spot-corrected effective temperatures and Gaia distances, we calculate luminosities and use the Stellar Parameters of Tracks with Starspots (SPOTS) models to derive corrected masses and ages for our sample of stars. A proper treatment of starspots in young stars will be crucial to further refine our understanding of the earliest stages of stellar evolution.

#311 | The IMF in Orion OB1b from $0.05M_\odot$ to $8M_\odot$ \\ using public surveys

Rodrigo Cabral-Fontes ¹ ; Juan José Downes ¹

1 - Facultad de Ciencias, Universidad de la República, Montevideo.

[.pdf]

#317 | Signaling star formation in metal-poor dwarf galaxies: massive stars in Leo A.

Maria Jose Chavolla ¹

1 - Universidad de las Americas Puebla.

[.pdf]

#500 | Small-scale dust structures in Taurus Transition Disks around low mass stars

Marie M. Rodriguez S. ¹

1 - Universidad de Chile.

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#166 | A New Family of SNe that Do Not Follow the Relation to Measure Distances with Type Ia SNe as Standard Candles

Jonathan Pineda-García ¹

1 - Universidad Andres Bello.

[.pdf]

#208 | New evidence for a black hole in the X-ray binary system Swift J1910.2-0546

Jesus Corral-Santana ¹

1 - European Southern Observatory (ESO).

[.pdf]

#245 | Cepheid pulsation mode identification via unsupervised machine learning

Santiago Henao Castellanos ¹ ; Alejandro García ¹

1 - Universidad de los Andes.

[.pdf]

#296 | Exploring Star Cluster through Eclipsing Binary members

Luciana V. Gramajo ¹ ; Tali Palma ¹ ; Dante Minniti ² ; Juan J. Claria ¹

1 - OAC-UNC. 2 - UNAB.

[.pdf]

#395 | Inferring the production rate of intermediate-age RR Lyrae stars using Magellanic Clusters

Bolivia Cuevas Otahola ¹ ; Cecilia Mateu ² ; Gustavo Bruzual ³ ; Fabiola Hernandez Perez ⁴ ; Gladis Magris ⁵ ; Ivan Cabrera Ziri ⁶

1 - Benemerita Universidad Autonoma de Puebla. 2 - Universidad de la Republica. 3 - Instituto de Radioastronomia y Astrofisica. 4 - Centro de Estudios de Física del Cosmos de Aragón. 5 - Centro de Investigaciones de Astronomia. 6 - Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg.

[.pdf]

#479 | Early-time observations of type II supernovae

Keila Ertini ¹ ; Gastón Folatelli ¹ ; Joseph Anderson ²

1 - Instituto de Astrofísica de La Plata. 2 - European Southern Observatory.

[.pdf]

#553 | Detecting Variable stars in Ultra Faint Dwarves without filters: The case of Reticulum II

Heinz Frelijj ¹ ; Christian Moni Bidin ¹

1 - Universidad Católica del Norte.

[.pdf]

#163 | Open clusters under the nIR lense

Karla Peña Ramírez ¹ ; Sebastián Ramírez Alegría ¹ ; André-Nicolás Chené ² ; Leigh Smith ³ ; Philip Lucas ⁴ ; Dante Minniti ⁵

1 - Universidad de Antofagasta. 2 - Gemini Observatory. 3 - University of Cambridge. 4 - University of Hertfordshire. 5 - Universidad Andrés Bello.

[.pdf]

#288 | Internal structure of open clusters with close companions

Tali Palma ¹ ; Valeria Coenda ² ; Gustavo Baume ³ ; Carlos Feinstein ³ ; Celeste Parisi ²

1 - OAC - UNC. 2 - IATE, OAC - UNC. 3 - IALP, UNLP.

[.pdf]

#471 | Ca triplet metallicities and velocities for 12 globular clusters toward the galactic bulge

Doug Geisler ¹ ; Celeste Parisi ² ;

Bruno Dias ³ ; Sandro Viallanova ⁴ ; Franceso Mauro ⁵ ; Ivo Saviane ⁶ ; Roger Cohen ⁷ ; Christian Moni Bidin ⁵ ; Dante Minniti ⁸

1 - ULS. 2 - IATE-OAC. 3 - UTA. 4 - UdeC. 5 - UCN. 6 - ESO. 7 - Rutgers. 8 - UNAB.

[.pdf]

#475 | Recharacterization of open clusters in optical and near-infrared wavelengths using machine learning methods

Daniela Barrios López ¹ ; Karla Peña Ramírez ¹

1 - Universidad de Antofagasta.

[.pdf]

#030 | BETIS: Bidimensional Exploration of the warm-Temperature Ionized gaS

Raúl González Díaz ¹ ; Fabián Rosales Ortega ¹ ; Lluís Galbany ²

1 - Instituto Nacional de Astrofísica, Óptica y Electrónica. 2 - Instituto de Ciencias del Espacio.

[.pdf]

#109 | The nature of the enigmatic highly-variable high-mass Class I young stellar object Mol 12. What we know so far

Mauricio Tapia ¹

1 - Instituto de Astronomia, UNAM, Ensenada, Mexico.

[.pdf]

#127 | G353.41 protocluster: $N_2$H$^+$ dense gas kinematics of a collapsing star forming region.

Rodrigo Álvarez-Gutiérrez ¹ ; Amelia Stutz ¹

1 - Universidad de Concepción.

[.pdf]

Resumen:

The ALMA-IMF Large Program mapped 15 dense, massive ($2-32\times 10^{3}$~M$_{\odot}$), and ``typical" Milky Way protoclusters down at matched physical resolution of 2~kAU. Here we present N$_2$H$^+$ dense gas kinematic analysis of the G353.41 protocluster, with a mass of 2500~M$_{\odot}$ over 1.7~pc$^2$. To simplify the N$_2$H$^+$ line profile we extract the isolated hyperfine line component for kinematic analysis. We model this single line with up to 3 Gaussian components to constrain the kinematics of the dense gas immediately associated with star formation. The velocity components are well separated, most of the 1.3 mm-detected cores are located in subregions with 2 to 3 components, indicating kinematic complexity even at $\sim$ 2~kAU scales. Other core velocity tracers match the N$_2$H$^+$ velocities, indicating that the cores are still kinematically coupled to the maternal dense gas. The intensity-weighted position-velocity (PV) diagram shows 9 obvious ``V-shaped" converging velocity gradients (Figure A: top right panel) on $\sim$~small scales. These gradients have timescales of $\sim$67~kyr. This is short compared to the free fall time t$_{ff}\,=\,\,0.21$~Myr of the cloud, but large compared to the mean t$_{ff}\,=\,\sim$13~kyr of cores. We derive core mass accretion rates for the V-shapes. The values, in the range of 0.3~-~12.4~$\times~10^{-4}$~M$_{\odot}$~yr$^{-1}$, are consistent with literature values. The traditional PV diagram highlights the large-scale velocity structures in this region (Figure B: background emission map). We create a simple model of an infalling sphere, with a power law density profile. Its PV diagram matches the large scale structure present in the data (Figure B: gray shaded area), indicating that this protocluster is collapsing under gravity. From the large and small scale features, we conclude that cores form concurrently with the large-scale collapse in gas-dominated protoclusters, and required a time in the order of $\sim$~70~kyr to build up their mass (short compared to the $\sim$~500~kyr protostar lifetime).

#145 | Dense gas kinematics in the massive G351.77 protocluster: ALMA-IMF Large Program observations of N$_2$H$^+$

Nicolás Antonio Sandoval Garrido ¹ ; Amelia Stutz ¹

1 - Universidad de Concepción.

[.pdf]

Resumen:

The ALMA-IMF Large Program observed 15 massive protoclusters in two bands (1.3 and 3 mm), capturing multiple line, and continuum emission (e.g., Ginsburg et al. 2021; Motte et al. 2021). Here we study the massive filamentary protocluster G351.77, located at a distance of $\sim$ 2 kpc (Reyes et al. submitted). We trace the dense gas emission and kinematics via the N$_2$H$^{+}$ (1-0) line. To recover the emission, the 12M and 7M arrays were both combined and reduced to then be feathered with Total Power data, obtaining an image that captures the N$_2$H$^{+}$ emission over the protocluster and down to 2 kAU scales. The N$_2$H$^{+}$ hyperfine line profile is modeled with PySpecKit, fitting two velocity components, obtaining the Excitation temperature, Optical depth, Centroid velocity and Line width for each velocity component. In combination with the optical depth and an H$_2$ column density map derived from the 1.3 mm band, we estimated the N$_2$H$^{+}$ relative abundance $\sim$ (3.192 $\pm$ 0.813) $\times$ $10^{-10}$. We estimated a total mass of $\sim$ 864 $\pm$ 220 M$_{\odot}$. By examining the position-velocity diagrams at small scales, we observe infall signatures associated with 1.3 mm cores. In some cases, similar signatures were observed without related cores, suggesting the existence of cores below the 1.3 mm detection limits. The most prominent v-shape has an average of mass accretion rate $\sim$ 2.035 $\times$ $10^{-4}$ M$_{\odot}$/yr and an average timescale $\sim$ 18.67 kyr. The position-velocity diagram on large scales shows that the mother filament is separated into two velocity components in the protocluster. Most cores are found to be associated with the more blue-shifted sub-filament. Our analysis reveals that multiple velocity components pervade the protocluster, indicating kinematic complexity in the dense gas. Cores seem to prefer one velocity component of the gas, and their mass buildup timescales are $\sim$ 33 kyr.

#175 | Molecular gas in low metallicity galaxies

Monica Rubio ¹

1 - Universidad de Chile.

[.pdf]

#333 | Spectroscopic characterization of new planetary nebulae and symbiotic stars from VPHAS+ and AllWISE

Giovanna Liberato ¹ ; Denise R. Gonçalves ¹ ; Luis A. Gutierrez-Soto ² ; Stavros Akras ³ ; Belén Mari ¹ ; Mateus Dias Ribeiro ¹ ;

Marco Laversveiler ¹ ; Vasiliki Fragkou ¹ ; Jackeline S. Rechy-García ¹

1 - Valongo Observatory. 2 - Institute of Astrophysics La Plata. 3 - National Observatory of Athens.

[.pdf]

#369 | Astrochemical analysis of the nuclear and extranuclear environments of galaxies in the local universe

Yahira Mendoza Moncada ¹ ; Diana Paula Andrade ¹ ; Karín Menéndez-Delmestre ¹ ; Rayssa Guimarães Silva ¹

1 - Observatório do Valongo.

[.pdf]

Resumen:

Building upon previous research on the emission of polycyclic aromatic hydrocarbons (PAHs) in the mid-infrared (mid-IR), the present work studies a sample of 28 local galaxies (D $\lesssim$ 30Mpc) from the Spitzer Survey of Near-infrared Galaxies (SINGS). All objects show optical signatures of an active galaxy nucleus (AGN), and PAHs are also detected. The sample covers 28 nuclear regions, one for each galaxy, and 40 extranuclear regions corresponding to some galaxies. Molecules in each region were identified by fitting them with the NASA Ames PAH IR Spectroscopic Database (PAHdb). The molecules present were categorized into families based on their composition: PAH, amorphous (molecules that contain only carbon in their formula), Polycyclic Aromatic Nitrogenous Hydrocarbons (PANH), and Polycyclic Aromatic Hydrocarbons with heteroatom (any atom other than hydrogen, carbon, or nitrogen). With this categorization, it is easy to notice, in general, that PAHs and amorphous ones, such as C24, have the highest flux contribution in the studied regions. Also, the C24 molecule has a remarkable contribution to the flux of some galaxies. In this preliminary study, when categorizing the molecules considering only the nuclear region, it is possible to notice that the percentage of PAH is predominant in most of the galaxies, while the amorphous ones predominate in the others. The percentages of PANH and heteroatom change little or nothing between the nuclear and extranuclear regions. The next goal of the research is to determine what conditions are causing the different flux contribution of each family of molecules depending on the environment. In addition, laboratory studies using the C24 molecule and PAHs with 24 carbon atoms will be carried out using the techniques of time-of-flight mass spectrometry (TOF-MS) and infrared spectroscopy (FTIR), to verify the stability and the pathways of break-down of these species under radiation field.

#490 | The control of the radial cold HI mass fraction by velocity dispersion and magnetic field

Adriana Gazol ¹ ; Francisco I. García Torres ¹

1 - IRyA, UNAM.

[.pdf]

#495 | Magnetic flux transport in the turbulent interstellar medium

Camila Naomi Koshikumo' ¹ ; Reinaldo' Santos de Lima ¹

1 - Instituto de Astronomia, Geofísica e Ciências Atmosféricas da Universidade de São Paulo.

[.pdf]

Resumen:

Turbulence and magnetic fields are components of our Galaxy’s interstellar medium and are tightly interconnected through complex plasma processes. In particular, the magnetic flux transport in the presence of magneto-hydrodynamic (MHD) turbulence in molecular clouds is an essential factor for understanding different processes involved in star formation. The theory of turbulent Reconnection Diffusion (RD), predicts the dependence of the effective diffusion coefficient of the magnetic field with the Mach Alfvénic number $M_A$ (which is the ratio between the turbulent velocity and the local Alfvén velocity). However, the current RD theory does not take into account the effects of compressibility which should be important in the regime of supersonic MHD turbulence present in molecular clouds. Therefore, we aim to determine, with 3D MHD turbulence simulations, the dependence of the magnetic flux in different regimes of compressible turbulence, characterized by different sonic Mach numbers $M_S$. In order to measure the diffusion of the magnetic field in the simulations, we analyze the temporal statistics of the tracer particles' velocity to obtain their diffusion rate. Our results confirm the RD hypothesis of the correspondence of the magnetic field lines’ diffusion with the fluid Lagrangian particles' diffusion. Nonetheless, the incompressible turbulence is shown to behave as predicted by RD theory: the presence of a strong magnetic field suppresses the diffusion and, therefore, $D \propto M^3_A$. In our compressible simulations, the RD efficiency seems to increase when the turbulence is supersonic, with $D \propto M^1_A$ in our simulations with $M_S = 3$. This quantitative characterization of the effective diffusion coefficient is important for modeling protostellar disk formation in turbulent molecular clouds and for the evaluation of the efficiency of this transport process when compared to other mechanisms, for instance Ambipolar Diffusion.

#523 | Revealing dense gas kinematics in the G012.80 protocluster

Javiera Salinas ¹ ; Amelia Stutz ¹

1 - Universidad de Concepción.

[.pdf]

#608 | Similarity of supernova remnant radio continuum spectra and the properties of the interstellar medium

Mario Abadi ¹

1 - Observatorio Astronómico de Córdoba, Instituto de Astronomía Teórica y Experimental (IATE) CONICET-UNC.

[.pdf]

#010 | Abundance Patterns of Dwarf-galaxy Stellar Streams

Guilherme Limberg ¹ ; Silvia Rossi ¹ ; Alexander Ji ²

1 - Universidade de São Paulo. 2 - University of Chicago.

[.pdf]

#135 | Unraveling the Chemical Evolution of Astrophysical Ices under Ionizing Radiation: A Computational Approach Employing the PROCODA code

Sergio Pilling ¹

1 - UNIVAP.

[.pdf]

Resumen:

Astrophysical ices play a crucial role in the chemical evolution of space environments, as they undergo ionizing radiation-induced reactions and desorption processes. Here, we present our pioneering computational methodology, PROCODA, aimed at elucidating the intricate chemical evolution of experimentally investigated ices under photolysis/radiolysis processes until chemical equilibrium phase (CE) is attained. The code solves a system of coupled differential equations, effectively traces the evolution of molecular abundances over time during the radiation processing of ices. Our investigation primarily focuses on pure H2O, CO, and CO2 ices subjected to different types of ionizing radiation, such as cosmic rays, UV and energetic electrons [1,2,3]. For CO and CO2 ices, we consider 11 distinct chemical species within the ice, encompassing 4 observed species (CO2, CO, O3, and CO3) and 7 non-observed or unknown species (O, O2, C, C2, C2O, C2O2, and C2O3). Additionally, we account for 100 reaction routes, including direct dissociation reactions, bimolecular reactions, and radiation-induced desorption processes. For H2O ices, our analysis involves 9 different chemical species, including 5 observed species (H2, H2O, O2, H2O2, and virtually zero O3) and 61 coupled reactions. The best-fit models obtained through PROCODA provide not only the rate coefficients for the considered equations but also yield invaluable insights into desorption parameters and the characterization of the CE phase. The determined values from our comprehensive study hold significant potential for incorporation into future astrochemical models, enabling the mapping of chemical evolution within astrophysical environments under the influence of ionizing radiation. We gratefully acknowledge the generous financial support of the Brazilian agencies FAPESP, CAPES, and CNPq, which has made this research possible. References: [1] Pilling et. al. 2022, ApJ, 925, 147 (CO2) [2] Pilling et. al. 2023, ApJ, 952, 17 (CO) [3] Pilling et. al. 2023, MNRAS, 523, 2858 (H2O)

#177 | Stellar Winds in the Galactic Centre: Variable Accretion and Formation of a Disc

Diego Calderón ¹ ;

Jorge Cuadra ² ; Christopher Russell ³

1 - Universität Hamburg. 2 - Universidad Adolfo Ibáñez. 3 - University of Delaware.

[.pdf]

#189 | Kinematics of RR Lyrae stars in the Milky Way Bulge

Julio Olivares Carvajal ¹ ; Manuela Zoccali ¹ ; Rodrigo Contreras Ramos ¹ ; Carlos Quezada ¹ ; Alvaro Rojas-Arriagada ² ; Elena Valenti ³ ; Rogelio Albarracin ¹ ; Alvaro Valenzuela Navarro ¹

1 - PUC/MAS. 2 - USACH/MAS. 3 - ESO.

[.pdf]

#195 | Exploring the hierarchical formation of the Milky Way with hypervelocity stars

Julio A. Carballo-Bello ¹ ; Camila Navarrete ² ; Jesus M. Corral-Santana ³ ; Marcelo D. Mora ⁴

1 - IAI - Universidad de Tarapaca. 2 - Observatoire de la Cote dAzur. 3 - European Southern Observatory. 4 - Las Campanas Observatory.

[.pdf]

#310 | Investigating the resilience of dwarf spheroidal galaxies within the gravitational potential of the Milky Way

Nicholas Souza ¹ ; Rubens Machado ²

1 - Universidade Federal do Paraná (UFPR). 2 - Universidade Tecnológica Federal do Paraná (UTFPR).

[.pdf]

Resumen:

Studying dwarf galaxies and their interactions with the Milky Way (MW) is crucial for reconstructing the MW formation history, it also helps us improve constraints on cosmological models. Furthermore, the field of galactic dynamics emphasizes the importance of understanding the stability of stellar systems. In such context, the identification of parameters that influence the resilience of stellar systems against disruption by MW tidal forces plays a crutial role in grasping the evolution of the Galaxy and its constituents. This work aims to investigate the key properties of dwarf spheroidal galaxies (dSph) and their orbits around the MW, determining how susceptible their core structures are to disruption. To achieve this, we use semi-analytical $N$-body simulations: embedding an $N$-body system, representing a dSph, in a MW analytical axisymmetric potential. By studying the fate of different systems, we aim to identify combinations of structural and orbital parameters that either preserve or dismantle their cores. Preliminary findings suggest that the initial concentration and the orbit's inclination with respect to the galactic plane are significant factors in this problem. More specifically, when considering Plummer spheres with a total mass $M_{\rm total} = 10^{10} \ \rm{M_{\odot}}$, initial scale lengths $a_1 = 0.5 \ \rm{kpc}$ (less concentrated) and $a_2 = 0.3 \ \rm{kpc}$ (more concentrated), both consisting of $N = 10^4$ particles, and placed on two distinct orbits ($xy$-plane and $yz$-plane), the polar orbit and the initially less concentrated cases show the most persistent cores. Further investigations into the structures of the parameter and phase spaces are expected to deepen our understanding of the related phenomena. Additionally, exploring more extreme orbits may lead to insights on the disruption of globular clusters, and incorporating the time dependent potential of the bar could enrich the analysis.

#406 | The kinematics, metallicity and age of stars in the inner 2x2 degrees of the Milky Way

Carlos Quezada ¹ ; Manuela Zoccali ¹ ; Elena Valenti ² ; Rodrigo Contreras-Ramos ¹ ; Alvaro Rojas ³ ; Julio Olivares ¹

1 - PUC-MAS. 2 - ESO. 3 - USACH-MAS.

[.pdf]

#425 | Unraveling the Sagittarius Dwarf Spheroidal Galaxy at Low Galactic latitudes

Jorge Anais Vilchez ¹ ; Javier Alonso García ¹

1 - Universidad de Antofagasta.

[.pdf]

#551 | Comparing dynamical properties of bars and spiral arms models in U-V plane

Willian Nacafucasaco ¹ ; Tatiana Michtchenko ¹

1 - Instituto de Astronomia, Geofísica e Ciências Atmosféricas da Universidade de São Paulo (IAG-USP).

[.pdf]

#594 | IGRINS Chemical Tagging of Stars in Streams to Progenitors

Sebastian Cabrera-Astudillo ¹ ; José Gregorio Fernández-Trincado ¹

1 - Instituto de Astronomía, Universidad Católica del Norte.

[.pdf]

#357 | Chemical properties of the SMC Main Body traced by star clusters

Celeste Parisi ¹ ; Bruno De Bórtoli ² ; Lilia Bassino ³ ; Doug Geisler ⁴ ;

Bruno Dias ⁵ ; German Gimeno ⁶ ; Mateus Angelo ⁷ ; Francesco Mauro ⁸

1 - IATE-OAC. 2 - FCAGLP. 3 - IALP. 4 - ULS. 5 - UTA. 6 - Gemini Observatory. 7 - CeFeT-MG. 8 - UCN.

[.pdf]

#463 | VISCACHA SURVEY: the SMC Southern Bridge in 8D

Celeste Parisi ¹ ; Raphael Oliveira ² ; Mateus Angelo ³ ;

Bruno Dias ⁴ ; Francisco Maia ⁵ ; Saroon Sasi ⁶ ; Carlos Feinstein ⁷ ; VISCACHA Survey Team ⁸

1 - IATE-OAC. 2 - USP. 3 - CCEFET MG. 4 - UTA. 5 - UFRJ. 6 - UNAB. 7 - FCAGLP. 8 - International collaboration.

[.pdf]

#029 | CAPOS: The bulge Cluster APOgee Survey IV. Elemental Abundances of the bulge globular cluster NGC 6558

Danilo González-Díaz ¹ ; José G. Fernández-Trincado ¹

1 - Universidad Católica del Norte.

[.pdf]

#064 | The formation of the smallest galaxies

Michael Fellhauer ¹

1 - Departamento de Astronomia, Universidad de Concepcion, Chile.

[.pdf]

#089 | Reveiling the effects of environment on galaxy bars: the case of the Virgo cluster

Virginia Cuomo ¹ ; Alfonso Aguerri ² ; Lorenzo Morelli ¹

1 - Universidad de Atacama. 2 - IAC.

[.pdf]

Resumen:

Barred structures are hosted by a considerable fraction of galactic discs, spanning diverse environments and galaxy luminosities. The environment likely exerts a significant influence on bar formation, with tidal interactions leading to the emergence of elongated features resembling bars within galaxy discs. It is plausible that the structural parameters of bars resulting from tidal interactions in high-density galactic environments differ from those formed through internal disc instabilities in isolated galaxies. To test this scenario, a viable approach is to compare the structural parameters of bars in galaxies situated within distinct environments. We present the comparison between the two key structural parameters of bars, strength and radius, derived using a Fourier analysis on SDSS r band images, in galaxies situated within the Virgo cluster spanning a wide range in luminosities and galaxies of comparable luminosities found in environments characterized by lower galaxy densities. The analysis reveals that the bar radius exhibits a correlation with galaxy luminosity, indicating that larger bars are typically found in more luminous galaxies. When comparing galaxies with fixed luminosities, the field galaxies display larger bar radii compared to those in the Virgo cluster. However, when the bar radius is scaled by the size of the galaxy, the disparity diminishes. This is because galaxies of similar luminosities tend to be larger in the field environment compared to the cluster. Consequently, the scaled bars in the Virgo cluster and the field exhibit similar sizes. The findings of this study indicate that the size of galaxies is the parameter that is influenced by the environment, while the bar radius remains independent of the environment when scaled by the galaxy size. These results support the notion that the internal dynamics and intrinsic characteristics of galaxies play a dominant role in the formation and evolution of bars, regardless of the surrounding environment.

#094 | In the Shadows of Bright Neighbors: The Case of CGCG014-074 and NGC4546

Natalia Guevara ¹ ; Carlos Gabriel Escudero ¹ ; Favio Raúl Faifer ¹

1 - IALP - CONICET - UNLP.

[.pdf]

#196 | Investigating the interface between Relic galaxies and compact massive Early Type Galaxies (ETGs) through simulations: Insights into local dynamics and the global environmental framework

Micheli Moura ¹ ; Ana L. Chies-Santos ¹ ; Cristina Furlanetto ¹ ; Ling Zhu ²

1 - Universidade Federal do Rio Grande do Sul (UFRGS). 2 - Shanghai Astronomical Observatory (SHAO).

[.pdf]

#219 | Are backsplash galaxies the response to the conformity signal produced by low-mass central galaxies at the periphery of massive systems?

Daniela Palma ¹ ; Iván Lacerna ¹ ; M. Celeste Artale ² ; Antonio Montero-Dorta ³

1 - Universidad de Atacama. 2 - Universidad Andrés Bello. 3 - Universidad Técnica Federico Santa María.

[.pdf]

#250 | Star formation efficiency per free-fall time in a galaxy merger

Sofia Guevara-Montoya ¹ ; Christine Wilson ²

1 - Universidad Nacional de Colombia. 2 - McMaster University.

[.pdf]

#306 | Metal enrichment of galaxies inhabiting halos of different masses in a $\Lambda$-CDM cosmology

Yamila Daniela Burrafato ¹ ; María Emilia De Rossi ² ; Salvador Esteban Grimozzi ² ;

María Soledad Nakwacki ³ ; María Cecilia Tomasini ¹ ; Lucas Jesús Zenocratti ⁴ ; María Candela Zerbo ²

1 - Departamento de Física, Facultad de Ciencias Exactas y Naturales, UBA, Argentina. 2 - Instituto de Astronomía y Física del Espacio, CONICET-UBA, Argentina; Facultad de Ciencias Exactas y Naturales, UBA, Argentina. 3 - Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina. 4 - Facultad de Ciencias Astronómicas y Geofísicas, UNLP, Argentina; Instituto de Astrofísica de La Plata, CONICET-UNLP, Argentina.

[.pdf]

#362 | Perturbation effects and the evolution of giant Low Surface Brightness Galaxies: the case of Malin 1

Roy Omar Edgar Bustos Espinoza ¹ ; Gaspar Galaz ¹ ; Matías Blaña ¹

1 - Instituto de Astrofísica - Pontificia Universidad Católica de Chile (IA - PUC).

[.pdf]

#377 | The origins of Ultra Diffuse Galaxies: Characterization of their globular cluster population across different environments

Pablo Astudillo-Sotomayor ¹ ; Nathan W. C. Leigh ¹ ; Ricardo Demarco ¹ ; Analía V. Smith Castelli ²

1 - Departamento de Astronomía, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción. 2 - Instituto de Astrofísica de La Plata, UNLP, CONICET.

[.pdf]

#393 | Exploring the Evolution of Galaxies: A Comparative Study Using Two Semi-Analytic Codes

Lucas Almonacid ¹ ; Dominik Schleicher ¹ ; Matías Liempi ¹

1 - Universidad de Concepción.

[.pdf]

#394 | The Formation of Faint and Ultra-Faint dwarf spheroidal galaxies: Modeling formation of Ursa Major II with AMUSE

Javier Cabello ¹ ; Michael Fellhauer ¹ ; Diego Matus ¹

1 - Departamento de Astronomía, Universidad de Concepción, Chile.

[.pdf]

#418 | Quenching of star formation in galaxies up to large clustercentric distances

Maite Muckler ¹ ; Marina Trevisan ¹ ; Gary Mamon ² ; Rodrigo Flores-Freitas ¹ ; Allan Schnorr-Muller ¹ ; Vitor Bootz ¹

1 - Universidade Federal do Rio Grande do Sul. 2 - Institut d Astrophysique de Paris.

[.pdf]

#422 | The mystery of extremely HI rich galaxies

Victor Capa ¹ ; Helga Denes ¹

1 - Yachay Tech University.

[.pdf]

#464 | Neighbourhood Watch: A Survey of Baryonic Substructures in the Nearby Universe

Rohan Rahatgaonkar ¹ ; Bryan Miller ² ; Thomas Puzia ¹ ; Yasna Ordenes-Briceño ¹ ; Paul Eigenthaler ¹ ; Tuila Ziliotto ³ ; Mathew Taylor ⁴

1 - Pontificia Universidad Católica de Chile. 2 - Observatorio Gemini Sur, NOIRLAB. 3 - Università degli studi di Padova. 4 - University of Calgary.

[.pdf]

Resumen:

The Neighbourhood Watch is a survey to complete a census of all baryonic structures out to at least the virial radius in a sample of galaxy groups within 18 Mpc in the optical filters u'g'r'i' and H-alpha with CTIO/DECam and in the NIR J,K filters with ESO/VIRCAM. The observations reach unprecedented point source depths of 2.5 magnitudes beyond the peak of the globular cluster luminosity function (GCLF) which will detect $>99\%$ of all compact objects, i.e. globular clusters (GCs) and ultra-compact dwarf galaxies (UCDs), and reveal all low-surface brightness baryonic structures down to $\sim 28 \text{mags/arcsec}^2$. This dataset will allow us for the first time: to derive a complete GCLF out to the virial radius for these galaxies, search for spatial over-densities and unique age/metallicity distribution functions (ADF/MDF) in the GC population, detect 10-100 new low-surface brightness dwarf galaxies for each target group to test current state-of-the-art cosmological simulations and measure their luminosity function in different environments, and probe the complex interaction/merger/accretion history of these groups. Survey targets the NGC2997, NGC3115, NGC6744, and NGC4594 groups, complementing the CenA group (Taylor et al. 2017), the Virgo Cluster (NGVS, Ferrarese et al. 2012), and the Fornax Cluster (NGFS, Munoz et al. 2015; Ordenes-Briceno et al. 2018). Given the DECam community pipeline’s inability to properly determine the sky levels around large galaxies, a custom data reduction pipeline is being designed for this particular dataset to fulfil the aforementioned objectives. The preliminary findings indicate that utilising a multi-step approach that employs a combination of techniques (convolution masking for image artifacts, distortion reduction in chip gap, and better sky modal) leads to the retrieval of low surface brightness dwarf galaxies that are observable in the final stacks. This poster will provide an overview of the survey and present the initial outputs from data reduction process.

#549 | Probing the formation histories of NSCs in the Fornax Galaxy Cluster using UVIT

Prasanta Kumar Nayak ¹ ; Thomas H. Puzia ¹ ; Yasna Ordenes-Briceño ¹ ; Paul Eigenthaler ¹ ; Bryan Miller ² ; Mareclo Mora ³ ; Evelyn Johnston ⁴ ; Tuila Ziliotto ⁵

1 - Pontificia Universidad Católica de Chile. 2 - Gemini Obseratory/NSF’s NOIRLab. 3 - Las Campanas Observatory. 4 - Universidad Diego Portales. 5 - Università degli studi di Padova.

[.pdf]

#090 | Slow bars in dwarf galaxies from the Virgo Cluster

Virginia Cuomo ¹ ; Lorenzo Morelli ¹

1 - Universidad de Atacama.

[.pdf]

Resumen:

Dwarf barred galaxies are the perfect candidates for hosting slowly-rotating bars. They are common in dense environments and they have a shallow potential well, making them prone to be heated by interactions. They are expected to reside in massive and centrally-concentrated dark matter halos, which should slow down the bar rotation through dynamical friction. When an interaction induces bar formation and when dynamical friction is efficient, the bar should rotate slowly. Despite being predicted within the cold dark matter cosmology, measurements of bar pattern speed, using the Tremaine-Weinberg method, find that slow bars seem to be rare in the local Universe. We present a photometric and kinematic characterisation of bars hosted by two dwarf galaxies NGC 4483 and NGC 4516 members of the Virgo Cluster. We derive the bar length and strength using the Next Generation Virgo Survey deep imaging and the circular velocity, bar pattern speed, and bar rotation rate using dedicated spectroscopy from the Multi Unit Spectroscopic Explorer at the Very Large Telescope. By considering the previously studied IC 3167, we compare the bar properties of the three dwarf galaxies with those of their massive counterparts from literature. Bars in dwarf galaxies are shorter and relatively weaker, and rotate slightly slower with respect to those in massive galaxies, in agreement with theoretical studies and simulations. This could be due to a different bar formation mechanism and/or to the presence of a large dark matter fraction in the centre of dwarf galaxies. We show that it is possible to push the application of the Tremaine-Weinberg method to the galaxy low mass regime, when the targets are carefully selected and dedicated high quality data are available. However, it is necessary to increase the sample of characterised bars in dwarf galaxies to give stronger constraints on their formation and evolution.

#119 | Properties of the Spiral Patterns of NGC 2619 through Morphological Analysis.

Katalina Forero ¹ ; Mauricio Diaz ¹ ; Nelson Vera ¹ ; Jorge Valderrama ¹

1 - Universidad Pedagógica y Tecnológica de Colombia.

[.pdf]

#120 | Study of bifurcations in NGC 2756 using 2DFFT

Erica Gonzalez ¹ ; Jose Mauricio Diaz ² ; Nelson Vera ² ; Jorge Valderrama ²

1 - Universidad Pedagógica y Tecnológica de Colombia. 2 - Universidad Pedagógica y Tecnológica de Colombia.

[.pdf]

#129 | Tidal stripping and truncation scenario: from dwarf elliptical to utra compact galaxy?.

Fernanda Urrutia Zapata ¹ ; Michael Fellhauer ¹ ; Pavel Kroupa ²

1 - Universidad de Concepcion. 2 - Universidad de Bonn.

[.pdf]

#139 | impact on black hole population due to seed formation in runaway star collisions in nuclear star clusters

M. Liempi ¹ ; D.R.G. Schleicher ¹ ; Andrew Benson ² ; Andrés Escala ³ ; Lucas Almonacid ¹

1 - Departamento de Astronomía, Universidad de Concepción, Chile. 2 - Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101. 3 - Departamento de Astronomía, Universidad de Chile, Chile.

[.pdf]

#227 | Characterization of arms of spiral galaxies from the study of the field of individual stars

Ximena Cano Gómez ¹ ; Esteban Silva Villa ¹

1 - Universidad de Antioquia.

[.pdf]

#236 | ON THE CORRELATION BETWEEN MORPHOLOGY OF GALACTIC SPIRAL STRUCTURE AND THE EXTRAGALACTIC ENVIRONMENT

Daniel Niño Villegas ¹ ; Juan Carlos Muñoz Cuartas ¹

1 - Universidad de Antioquia.

[.pdf]

Resumen:

For decades, various models have been proposed to explain the mechanism of formation of spiral arms in disk galaxies (density waves, swing amplification, tidal perturbations, etc.), however, to this day it is not fully understood under which conditions each of these mechanisms operates. In this work we study the correlation between the morphological features of the spiral arms in disc galaxies and the extragalactic environment in which they reside with the aim to analyze how this relationship can be interpreted in terms of the formation models. To achieve this goal, a sample of 2323 images of spiral galaxy was selected from the NASA-Sloan-Atlas catalog. Using GALFIT (Peng et al. 2010), the surface brightness distribution of each object is studied in order to highlight the spiral structures in each image and P2FFT (Davis et al. 2012, Hewitt \\& Treuthardt 2020) is used to determine the geometric properties of the spiral arms. To quantify the characteristics of the extragalactic environment, we use the mass density field reconstruction methods presented in Muñoz-Cuartas et al. (2011). Then, the environment of each galaxy is identified and classified following different criteria: zones of high and low density, galaxies with close neighbors in a distance range, galaxies with neighboring pairs, galaxies in filaments, etc. When the properties of the spiral arms are correlated with the environment in which the galaxy is located, it is found that there is no strong correlation between the intensity of the spiral arms and the density of the environment. On the other hand, a weak bias is found indicating that galaxies with symmetrical spiral arms have neighboring pairs, suggesting an interaction as the origin for the formation of the arms. The results of this work suggest that different arm formation mechanisms may be activated under different environmental conditions of the host galaxy.

#237 | Morphological and dynamic Study of Spiral Galaxies with Multiple Arms

Jose Mauricio Diaz Fonseca ¹ ; Nelson Vera Villamizar ² ; Nicanor Poveda Tejada ³

1 - Universidad pedagógica y tecnologica de colombia. 2 - Universidad Pedagógica y Tecnológica de Colombia. 3 - Universidad pedagogica y tecnologica de colombia.

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#352 | Revealing the orbital histories of strongly perturbed galaxies in the Abell cluster A496

Martha Margarita Lopez Gutierrez ¹ ; Hector Bravo Alfaro ¹ ; Jacqueline van Gorkom ² ; Rahna P.T. ³

1 - Departamento de Astronomía, Universidad de Guanajuato, 36000, Mexico. 2 - Department of Astronomy, Columbia University, New York, NY 10027, USA. 3 - Centro de Estudios de Física del Cosmos de Aragón (CEFCA).

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#378 | MORPHOLOGICAL STUDY OF INTERACTING GALAXIES: NGC 2207-IC 2163

jorge valderrama ¹ ; nelson vera villamizar ¹ ; nicanor poveda tejada ¹

1 - Universidad Pedagógica y Tecnológica de Colombia.

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#387 | Rotation decrease in dwarf disk galaxies

Diego Matus Carrillo ¹ ; Michael Fellhauer ¹

1 - Universidad de Concepción.

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#430 | The dynamically active NGC5098 group: sloshing and diffuse intragroup light

Gastao B. Lima Neto ¹ ; Florence Durret ² ; Hugo Capelato ³

1 - IAG/USP. 2 - IAP. 3 - UniCid.

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#531 | Study of the widths of spiral galaxy arms in the CALIFA survey

Lina Marcela Giraldo-Murillo ¹ ; Esteban Silva-Villa ¹ ; Jorge K. Barrera-Ballesteros ²

1 - Universidad de Antioquia. 2 - Universidad Nacional Autónoma de México.

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Resumen:

Spiral galaxies form a significant portion of Local Universe galaxies, hosting predominant star formation within their spiral arms. To comprehend arm genesis, identifying key parameters like pitch angle (winding degree) and arm width is crucial. Yet, arm width remains less explored. Our research focuses on unraveling spiral arm width, enhancing insights into galaxy structure. Our research utilizes CALIFA survey data containing approximately 1000 elliptical and spiral galaxies. Employing the Integral Field Unit (IFU) technique, the survey offers comprehensive spatial insight through analysis of spectroscopic elements. Pertinent to CALIFA galaxies are data on both gas and stellar components. Our selection process focuses on galaxies meeting specific criteria: inclination angles $\leq 40^o$, absence of interactions, and distinct spiral formations. Our investigation will employ multiple indicators to identify arms, encompassing the widely referenced $H_\alpha$ emission, derived from ionized gas in star-forming zones. Other indicators consist of emissions from young stellar constituents (O and B stars) in the blue spectrum and from aged stellar elements in the red and infrared spectrum, revealing recognizable spiral structures. After tracing the arms using some of the aforementioned tracers, we measured their width by making cuts across them with an approximate width of $3.5$ kpc, which is the average width of arms in grand design galaxies according to Savchenko et al. (2020). Subsequently, arm width was determined using two methods: (1) conventionally via the $1\sigma$ distribution width; and (2) by pinpointing the flux equilibrium where arm and non-arm regions meet. We have selected five spiral galaxies for investigation: NGC234, NGC309, NGC776, NGC7653, and UGC12224. For each galaxy, we traced the arms using the stellar population (as shown in the pseudo-V-mag map, see Figure) and gas ($H_\alpha$ emission). Our observations have revealed distinctions that present challenges in terms of explanation within the context of current models.

#057 | A study of the Globular Cluster system of the Fornax Cluster as seen through the S-PLUS data: methodology and preliminary results

Luis Fernando Lomelí Núñez ¹ ; Arianna Cortesi ¹ ; Maria Luisa Buzzo ² ; Analía Smith Castelli ³ ; Jairo Andres Alzate Trujillo ⁴

1 - Observatório do Valongo, UFRJ. 2 - Centre for Astrophysics and Supercomputing, Swinburne University. 3 - Instituto de Astrofisica de La Plata. 4 - CEFCA.

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#225 | Unraveling the Link between Type II Supernova Luminosity and Host Galaxy Velocity Dispersion

Alejandra Hernández ¹ ; Felipe Olivares ¹ ; Lorenzo Morelli ¹

1 - Universidad de Atacama.

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#435 | Globular cluster population in the Fornax Cluster core region: A Multi-wavelength study with NGFS data and Machine Learning techniques for selection.

Yasna Ordenes-Briceño ¹ ; Thomas Puzia ¹ ; Bryan Miller ² ; Paul Eigenthaler ¹ ; Rohan Rahatgaonkar ¹ ; Evelyn Johnston ³ ; NGFS team ⁴

1 - Pontificia Universidad Católica de Chile. 2 - Observatorio Gemini Sur, NOIRLAB. 3 - Universidad Diego Portales. 4 - NGFS team institutions.

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Resumen:

Globular clusters (GCs) are stellar systems relics. In the core of a galaxy cluster such as Fornax, they might reside either in the gravitational potential of their parent galaxies or in the galaxy cluster, intra-cluster medium (ICM). The scaling relations of GC populations with respect to the environment they inhabit provide evidence in the assembly history of the galaxy cluster.\\ We use the Next Generation Fornax Survey (NGFS) that maps the Fornax cluster up to its virial radius (1.4Mpc), in the optical with u'g'i' (DECam) and Near-infrared with JKs (VIRCam). This pilot sample covers the Fornax core region (r $\sim 350$kpc $\sim 3deg^2$) with u'g'i'JKs psf photometry. To have the cleanest photometric selection, we implement a supervised machine-learning method (support vector machine, SVM) for source classification. More than 1500 objects were selected as Fornax GCs. We compute individual age, metallicity and mass of GCs using color, magnitudes and simple stellar population models.\\ In this talk, we will present the analysis and results of the GC population in the Fornax core region, in terms of color and mass distributions, fractions of metal poor and metal rich and old vs “young” GCs and the spatial distributions of the above properties, together with their scaling relations for their host galaxy and for the galaxy core cluster overall.\\ One of the many interesting results of this research, is about the GC spatial distribution in terms of metallicity sub-populations: a large number of GCs with intermediate-metallicity are preferentially located along the East-West direction of Fornax, centered on NGC 1399, and the most metal-rich GCs are concentrated in the vicinity of NGC 1399 and the brightest Fornax galaxies. These different distributions constrain the mass assembly history of the Fornax cluster. More evidence will come soon, when expanding this methodology to the survey area, Fornax virial radius.

#482 | Stellar mass distribution in barred galaxies through multi-band decomposition in the mid-IR

Yasmin Cavalcante-Coelho ¹ ; Karín Menéndez-Delmestre ¹ ; Arianna Cortesi ²

1 - Valongo Observatory/UFRJ. 2 - Institute of Physics/UFRJ.

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#491 | Photometric Synthesis with AI of S-PLUS galaxies

Vitor Cernic ¹ ; Laerte Sodré Jr. ¹

1 - Universidade de São Paulo.

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#506 | Mapping the Zoo of Rest-Frame Galaxy SEDs using Unsupervised Machine Learning

Paulina Contreras Miranda ¹ ; Luca Tortorelli ² ; Daniel Grün ² ; Milagros Zeballos Rebaza ¹

1 - Universidad de las Américas Puebla. 2 - Ludwig Maximilian University Munich.

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#592 | Invisible Features: Exposing low-surface brightness characteristics with numerical techniques

Doris Stoppacher ¹ ; P. Tissera ² ; G. Galaz ² ; Y. Rosas-Guevara ³ ; J. Oñorbe ⁴

1 - Pontificia Universidad Católica de Chile, Universidad Autónoma de Madrid and Universidad de Sevilla. 2 - Pontificia Universidad Católica de Chile. 3 - Donostia International Physics Center. 4 - Universidad de Sevilla.

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#543 | Revisiting the Merging Cluster A2744 - The Pandora Cluster

Eduardo Cypriano ¹

1 - Universidade de São Paulo.

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