Projects

Gamma-ray binaries are stellar systems composed of a massive star and a compact object (such as a neutron star or a black hole) that orbit each other and produce very high-energy emissions. These systems serve as unique astrophysical laboratories for
studying particle acceleration and non-thermal emission processes under extreme conditions. The proposed project consists of an in-depth follow-up study of the gamma-ray binary LS I +61 303 at GeV energies. This is one of the most studied binary systems at high energies and exhibits a very distinctive behavior: in addition to its orbital period of approximately one month, it displays a superorbital modulation of about 4 years, observable at various wavelengths. Since the discovery of this phenomenon at GeV energies, the dataset obtained by the Fermi satellite has doubled. This project proposes to analyze the most recent dataset from the Fermi-LAT instrument for this source, with the aim of confirming or refuting the results published about ten years ago and conducting a detailed study of the system’s orbital behavior. The results of this work will be of great interest to the astrophysics community, as they will help to better understand the physical mechanisms governing high-energy emission in this type of system.

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The National Science Foundation and NASA have invested considerable resources in building high-precision spectrographs for ground-based detection of terrestrial planets. Unfortunately, Doppler planet searches are plagued by stellar signals that can mimic or mask Keplerian orbits. We propose to adapt a frequency-domain method used in Earth seismology and speech recognition to the planet validation problem. The cepstrum, or "spectrum of a spectrum," is a technique in which the logarithm of a power spectrum estimate is treated as a waveform in its own right. Originally formulated for detecting and timing complex echoes, the cepstrum is a promising method of estimating starspot lifetime that can be used to inform or validate Gaussian process models of stellar activity. A starspot lifetime estimator that does not rely on detecting rotational Doppler shifts is particularly valuable for modeling activity in stars with rotation axes parallel to the line of sight. Students will calculate cepstrum estimates from solar radial velocities and activity-indicator time series. The goal is to match features in the cepstrum with known physical processes in the sun. If time permits, we will work on observations of Habitable Worlds Observatory target stars.

This project proposes the integration of Artificial Intelligence (AI) frameworks, specifically generative models and AI-assisted programming, to design, document, and
optimize scientific code for cosmology and observational astronomy. The primary objective is to build a robust workflow (supporting Python, MATLAB, and Fortran) capable of processing astronomical images in FITS format (leveraging WCS and equatorial coordinates). The pipeline aims to produce sky mosaics with high photometric and visual uniformity, even under conditions of significant noise, varying observational constraints, or overlapping regions.

AI will be utilized for:
- Modular Architecture: Generating reusable modules for FITS handling, WCS extraction, astronomical reprojection, and image co-addition.
- Preprocessing Optimization: Proposing and benchmarking strategies for background subtraction, robust normalization, and multiscale filtering.
- Machine Learning Enhancements: Solving overlapping issues by selecting consistent data at intersections and minimizing "seams" through ML-suggested algorithms.

The solar wind is plasma, a gas of ionized particles, that streams out from the solar corona into the interplanetary space and drags the Sun’s magnetic field with it. It is a supersonic flow that expands non-adiabatically and whose heating mechanisms are properly constrained. Although the solar wind is usually characterised by its speed between slow (Vsw <500 km/s) and fast (Vsw >500 km/s), a richer classification based on the source region where the plasma originates, e.g., Coronal Holes, streamer belts, etc, offers the opportunity to establish whether the turbulence properties of a plasma parcel measured at one astronomical unit (au) preserve the signature from its origin or whether the nonlinear evolution of the plasma with heliospheric distance has removed any trace of the turbulence at its origin. To tackle this question, using measurements from instruments on board the European Space Agency (ESA) mission Solar Orbiter, and from the NASA mission Advance Composition Explorer (ACE), the student will explore and establish possible correlations between variability in the composition data and turbulence properties of the plasma parcel measured at two heliospheric distances.

NGC 1398 is located on the outskirts of the Fornax Cluster and appears to be falling into the cluster. We will use DECam images in an LSST-like filter set to explore its surroundings, including other stellar systems such as dwarf galaxies and globular clusters. The scientific goal is to search for evidence of perturbations caused by the cluster’s gravitational potential, as well as to obtain information about the galaxy’s assembly history using photometry and stellar population models.

Most exoplanets discovered to date have been found with the transit and radial velocity method. However, these techniques are notoriously difficult to apply to young stars due to their high levels of stellar activity. Direct imaging offers the best opportunity to study young planets, as they are brightest when young.Most direct imaging surveys have observed nearby stars to probe exoplanet populations at closer separations to their host stars. These surveys have mostly avoided observing stars within star-forming regions since the closest regions are more than 125 pc away. With the James Webb SpaceTelescope, we have developed direct imaging techniques to optimize point-spread function (PSF) modeling. With these models, we can remove the stellar flux contribution and search for emission directly from gas giants at separations > 30-60 au. This project will apply our PSF-fitting technique tohundreds of directly imaged young stars with ages of 1-3 Myr in order to search for young gas giant planets. In this project, the student will develop coding skills, gain experience with high-performance computing, work with NIRCam and NIRISS data from JWST, and learn about planetformation processes.

Fast radio bursts (FRBs) are extraordinarily bright, millisecond-duration radio transients that have emerged as a key area of study in radio astronomy. While growing evidence links FRBs to magnetars (highly magnetized neutron stars), their scientific power also lies in their potential as cosmological probes, as their dispersion measures encode information about the intergalactic medium. Realizing this potential requires identifying their host galaxies. LSST/Rubin will provide optimal optical imaging to identify low-z FRB host galaxies and search for associated optical transient counterparts. In this project, the student will develop the foundations of a pipeline to cross-match FRB localizations with LSST-derived data products or simulations and perform initial host galaxy characterization in advance of Data Release 1 (DR1).

The goal of this project is to provide the intern with practical experience in the design and implementation of contemporary science communication strategies in astronomy. The project will take place within the framework of the activities of the International Astronomical Union’s National Outreach Office (IAU-OAO Colombia), where the intern will apply innovative communication tools—including digital formats, transmedia narratives, and strategies for the social appropriation of knowledge—to real-world initiatives with national and international reach.

IAU-OAO Colombia is a network of groups committed to promoting the social appropriation of astronomy in various regions of the country. Through collaborations with universities, observatories, planetariums, schools, and both amateur and professional astronomy communities, the goal is to expand access to astronomical knowledge and inspire new generations. The project will allow the intern to participate in activities such as public talks, virtual mentoring for science clubs, organizing digital astronomy festivals (AstroFests), participating in national events, and producing outreach content, with a special emphasis on young people and post-conflict regions.

Have you ever wondered how stars live and die, or how stellar black holes are formed?

Open clusters are groups of stars born from a single star-formation burst, much like a cosmic family. As a result, they share key properties, such as age and chemical composition. Each cluster acts as a snapshot of stellar evolution frozen in time. By studying clusters of different ages, we can piece together the complete story of how stars evolve over time.

In this project, we will use open clusters as true space laboratories to study the fundamental parameters that govern the lives of stars—from their birth to their dramatic deaths.

Why choose this project?

• No prior astronomy experience needed: If you are interested in having closer contact with astrophysics but feel your knowledge in this field is limited, this project is designed exactly for you.

• Learn as you go: Throughout the development of the project, you will learn everything you need from the ground up, including what a star actually is and the physical principles that govern them.

• No advanced coding skills required: You do not need advanced coding skills. We will provide all the guidance and tools you need to succeed.