The ILIADA project, led by scientists from the Institute of Space Sciences (ICE-CSIC) and the Institut d'Estudis Espacials de Catalunya (IEEC) and in collaboration with the Institute of Cosmos Sciences of the University of Barcelona (ICCUB) and the Universitat Politècnica de Catalunya - BarcelonaTech (UPC), has been selected to test technology on board the next microsatellite of the NewSpace Strategy.

Last February, the Government of Catalonia and the Institute of Space Studies of Catalonia (IEEC — Institut d’Estudis Espacials de Catalunya) opened the call for the selection of the payload as an in-orbit technology demonstrator (IOD) to be embarked on the new Earth Observation satellite mission. This mission will give continuity to the Menut mission in the framework of the NewSpace Strategy of Catalonia, promoted by the Government of Catalonia with the collaboration of the IEEC, the i2CAT Foundation and the Cartographic and Geological Institute of Catalonia (ICGC).

The call aimed to offer the opportunity to companies, organisations or research centres based in Catalonia to present one of its innovative technologies to integrate it into the platform of this new satellite, with the aim of validating it in orbit, accelerate its introduction into the market or demonstrate additional capabilities.

The call aimed to offer the opportunity to companies, organisations or research centres based in Catalonia to present one of its innovative technologies to integrate it into the platform of this new satellite, with the aim of validating it in orbit, accelerate its introduction into the market or demonstrate additional capabilities.

After analysing all the applications received, the evaluation committee appointed by the Government of Catalonia and the IEEC has decided that the proposal IN-ORBIT LISA DIAGNOSTICS DEMONSTRATOR (ILIADA) will have the opportunity to integrate and fly on board the next microsatellite that will provide the fourth mission of the NewSpace Strategy of Catalonia to try to achieve the technical and scientific objectives it has proposed.

The ILIADA project will implement a first version of the Scientific Diagnostics Subsystem (SDS) sensors, the Spanish contribution to the LISA (Laser Interferometer Space Antenna) mission of the European Space Agency (ESA), which will put a gravitational wave observatory in space for the first time, as well as innovative sensor concepts developed in the IEEC framework. Through the use of high-precision magnetometers and the on-board radiation monitor, ILIADA will attempt to detect the electric currents that align with the Earth’s magnetic field lines as they pass through the poles. These measurements are used to better understand how our magnetic field is generated and can provide new insights into space weather, i.e. the real-time measurement and analysis of the set of physical properties of the Sun, the interplanetary medium, the magnetosphere, the atmosphere and the Earth’s surface that are influenced, directly or indirectly, by solar activity. Understanding space weather is important because of the impact it can have on our infrastructures, technology, society and health.

The ILIADA project is led by researchers and members of the IEEC at the Institute of Space Sciences (ICE-CSIC), with the collaboration of the Institute of Cosmos Sciences of the University of Barcelona (ICCUB) and the Universitat Politècnica de Catalunya – BarcelonaTech (UPC). Specifically, the groups involved are the following: Gravitational Astronomy – LISA (CSIC), Micro and Nano Technologies (UPC), the Technological Unit – instrumentation division (UB), and the Centre for Space Studies and Research – CERES, together with the engineering group 3Cat-Gea (IEEC).

The ICCUB Technology Unit is developing the radiation monitor for the LISA mission. The team, led by Daniel Guberman (ICCUB-IEEC), is preparing a reduced version for the ILIADA mission, that will be sent to be tested on a SmallSat together with the other LISA diagnostic systems developed by the IEEC.

Thanks to the Gaia mission, the European Space Agency’s (ESA) most ambitious project to detail the stellar mapping of our galaxy, a massive stellar black hole, Gaia BH3, has been discovered in the Milky Way. This type of black hole has been found before in distant galaxies by gravitational-wave observations, and is now identified for the first time in our galaxy. It is a dormant black hole, is the second closest to Earth — at a distance of 590 pc (or 1926 light-years) — is about thirty-three solar masses and forms a large binary system with its companion star.
This exceptional discovery confirms some theories and needs revision as well. This is an exciting result for the astronomical community, which raises the question of how many such black holes there are in space, or what mass ranges of black holes the Gaia mission will be able to discover.

This finding, published in the prestigious journal Astronomy & Astrophysics, involved a team of astronomers and engineers from the Department of Quantum Physics and Astrophysics, the Institute of Cosmos Sciences (ICCUB) of the University of Barcelona and the Institute of Space Studies of Catalonia (IEEC), who have been part of the Gaia mission, the most ambitious project of the European Space Agency (ESA) to study the history and structure of the Milky Way.

How can a dormant black hole be detected?

If the black hole is dormant, doesn’t that make it hard to spot it? Most known black holes are detected through the X-rays they emit when material from their stellar companion is “eaten”. With dormant black holes, little or no radiation is emitted by the source, so the black hole can only really be seen because of the gravitational effect it exerts on its companion star. Dormant black holes had never been detected before the Gaia mission. In particular, after the release of the third Gaia data release — the Gaia Data Release (DR3) — the first dormant black holes in our galaxy could be identified: Gaia BH1 and Gaia BH2.
"It's a real unicorn! It's like nothing we have ever seen," says expert Pasquale Panuzzo, from the Paris Observatory of the Centre National de la Recherche Scientifique (CNRS) in France, and lead author of the paper. “This is the kind of discovery you make once in your research life. So far, black holes this big have only ever been detected in distant galaxies by the LIGO–Virgo–KAGRA collaboration, thanks to observations of gravitational waves.”

In the validation of the preliminary data processed by Gaia Data Release (DR4), and given the preliminary results for the non-single star pipeline, this galactic source required further checks to see if the detected data were correct or corrupt. At first, the Data Processing and Analysis Consortium (DPAC) team considered that these results could not be real. After many internal verifications, all the data suggested that it was a genuine detection, a scientific finding that is worth publishing before the release of the Gaia Data Release (DR4) to allow further follow-up of the discovery by the scientific community.

“While in the previous data release (Gaia DR3) we identified quite a few spurious black hole candidates that were traced back to data calibration issues, the quality of the latest data reduction has improved so much that we expect to publish quite a number of genuine black holes in Gaia DR4!” says Berry Holl of the Geneva Observatory, a member of the Gaia Collaboration.
“It’s impressive to see the transformational impact Gaia is having on astronomy and astrophysics,” notes Carole Mundell, ESA Director of Science. “Its discoveries are reaching far beyond the original purpose of the mission, which is to create an extraordinarily precise multidimensional map of more than a billion stars throughout our Milky Way."

The most massive black hole of stellar origin in our Galaxy

But what makes this finding so amazing? Most of all because of its high mass. With thirty-three solar masses, Gaia BH3 is not only the most massive black hole of stellar origin known in our galaxy, but it is also in line with results obtained by gravitational-wave observatories such as LIGO/VIRGO/KAGRA. These facilities found a population of black holes with masses that contradict models of stellar evolution through the observation of gravitational waves from black hole mergers. The Gaia finding confirms that massive black holes of stellar origin also exist in our own Milky Way.

Most black holes of stellar origin in our galaxy have a mass of about ten solar masses, and its record value until now was held by the Cyg X-1 black hole, with an estimated mass of about twenty times that of the Sun. Gaia BH3 goes much further and is the record for our galaxy. Its mass is pinned down with unparalleled accuracy as well (32.7 +/- 0.82 M_solar), putting it firmly in the 30 solar mass range.
“The mass distribution for the black hole population derived from gravitational wave observations shows a clear peak around thirty solar masses”, says Tsevi Mazeh of Tel Aviv University, a member of the Gaia Collaboration. “It is very interesting to see now that Gaia BH3 is right at this peak with its 33 solar masses. This provides strong scientific support for the existence of this peak”, he adds.

The second closest black hole to Earth

This black hole, which lies at a distance of 1926 light-years, is currently the second closest to Earth. Why is this black hole only visible now? The longer time span of observations that will form the basis of Gaia Data Release 4 (DR4) is crucial for answering this question. The orbit of the stellar companion around their common centre of mass is estimated to be 11.6 years. This means that, with 5.5 years of data being processed for the next DR4, Gaia can map half of its orbit. This is enough to distinguish the additional oscillation in the position and motion of the companion star. It is expected that, with a longer time period of Gaia observations, more and more wide binaries can be identified. Lots of results are therefore to be expected from Gaia’s data releases.

“In the visible wavelength range and the infrared, the light from the visible companion star outshines anything that might come from Gaia BH3 itself — or else the black hole would have been discovered much earlier, and without Gaia” says Uli Bastian, member of the Gaia Collaboration.

Comparison of the orbits of Gaia's black holes and their companion stars. To give insight in the orbit, the orbits of the Gaia BH3 system are projected onto the Solar System, with the Sun in the zero point. Gaia's black holes are dormant black holes detected due to the wobble seen in the position and motion of its companion star. It can be clearly seen that the star orbiting Gaia BH3 is in a wide orbit around their mutual centre of mass. These wider orbits are more easily distinguishable with longer time spans of observations. The orbital period of 11.6 years is about twice the time span of observations that will form the basis for Gaia Data Release 4.Also available as dark version here. Credits: ESA/Gaia/DPAC - CC BY-SA 3.0 IGO. Acknowledgement: P. Panuzzo CNRS/Observatoire de Paris/PSL. 

Because of its exceptional nature, and to rule out the possibility that the solution is spurious, a confirmation of the result with several ground-based observatories was performed. The UVES spectrum for this system was obtained from the ESO archive, and follow-up observations were performed with the HERMES spectrograph in Spain and the SOPHIE spectrograph in France. The radial velocities obtained with these ground observatories complement Gaia’s radial velocities, which confirms the orbital solution derived from Gaia's data.
“Gaia is a true black hole detection machine because each of the three instruments can detect them”, says Laurent Eyer of Geneva Observatory, member of the Gaia Collaboration.

How did this black hole in the Milky Way originate?

Gaia’s photometry and spectra, as well as spectra obtained from ground-based observations with HERMES, SOPHIE and UVES, allow us to further unravel the secrets of this binary system. Since we cannot see the black hole, most of the information must be deduced from the companion star, which is a single old giant star. However, it is hard to determine the age of this ancient giant star. By comparing the colours and magnitude with theoretical models, it is estimated to be older than 11 billion years old.

From the companion star’s spectrum, it can be deduced that it has a low metallicity. This suggests that Gaia BH3 was also formed from a massive metal-poor star. Following the findings of the extra-galactic black hole population in this mass range from gravitational wave observations, it has been suggested that these high mass black holes are remnants of massive metal-poor stars. Gaia BH3 now provides support for this theory.

An intriguing companion

The star orbiting Gaia BH3 at about 16 times the Sun–Earth distance is rather uncommon: an ancient giant star, which formed in the first two billion years after the Big Bang, at the time our galaxy started to assemble. It belongs to the family of the Galactic stellar halo and is moving in the opposite direction to the stars of the Galactic disc. Its trajectory indicates that this star was probably part of a small galaxy, or a globular cluster, engulfed by our own galaxy more than eight billion years ago.

It supports, for the first time, the theory that the high-mass black holes observed by gravitational wave experiments were produced by the collapse of primeval massive stars poor in heavy elements. These early stars might have evolved differently from the massive stars we currently see in our galaxy.
The composition of the companion star can also shed light on the formation mechanism of this astonishing binary system. ”What strikes me is that the chemical composition of the companion is similar to what we find in old metal-poor stars in the galaxy,” explains Elisabetta Caffau, member of the Paris Observatory (CNRS), and  also a member of the Gaia collaboration.

For now, the formation process of this binary system with a black hole poses many questions. This new black hole challenges our understanding of how massive stars develop and evolve. Most theories predict that, as they age, massive stars shed a sizable part of their material through powerful winds; ultimately, they are partly blown into space when they explode as supernovas. What remains of their core further contracts to become either a neutron star or a black hole, depending on its mass. Cores large enough to end up as black holes of thirty times the mass of our Sun are very difficult to explain.

The companion star has very few elements heavier than hydrogen and helium, indicating that the massive star that became Gaia BH3 could also have been very poor in heavy elements. This is remarkable sinceit supports, for the first time, the theory that the high-mass black holes observed by gravitational wave experiments were produced by the collapse of primeval massive stars poor in heavy elements. These early stars might have evolved differently from the massive stars we currently see in our galaxy.

There are also many questions about where this black hole came from. Although it is currently in the plane of the Milky Way, its motion puts it in a retrograde orbit with a large inclination to the plane of the Milky Way. The black hole may come from a merger event of a small galaxy or a globular cluster merged with our Milky Way. It is expected that further studies will provide more insight on how Gaia BH3 ended up in the Milky Way.

This video shows the Galactic orbit of Gaia Black Hole 3 or Gaia BH3. It is an extract of the longer video. Credits: ESA/Gaia/DPAC- CC BY-SA 3.0 IGO. Acknowledgements: Video Animation: Stefan Jordan, Toni Sagristá with Gaia Sky - Text: Stefan Jordan, Pasquale Panuzzo, Ulrich Bastian, Tineke Roegiers, Berry Holl - Artificial voice - Based on "Discovery of a dormant 33 solar-masses black hole in pre-release Gaia astrometry" by Gaia Collaboration, et al., published in April 2024 in Astronomy & Astrophysics Letters.

“A growing number of black holes being found in the Milky Way with different methods, including the microlensing one reported in 2022 by OGLE and HST, brings us closer to obtaining a broader picture of the population of these objects in the Galaxy and may shed light on the nature of dark matter if an excess of these black holes is detected nearby.” says Łukasz Wyrzykowski, from Warsaw University in Poland and member of the Gaia Collaboration.

“From an observational point of view, discovering Gaia BH3 is not that hard, and specialized astronomical instruments will be able to detect its signatures as well. The difficulty is that you need to know which of the millions of stars to point your telescope at. This is where the power of a uniform all-sky survey like Gaia comes into play. Since Gaia observes all celestial sources that are bright enough to be seen by its detectors, we
were able to find the needle in the haystack,” says Johannes Sahlmann, member of the Gaia Science Operations Team at the European Space Astronomy Centre in Spain.
To date, Gaia data have only revealed the tip of the iceberg. Longer time spans of Gaia future data releases will undoubtedly reveal other binary systems containing black holes, but also exoplanets and other exotic binary systems. The Gaia Data Release (DR4) will be based on 5.5 years of observations, almost double the time period of the third data release, with about 3 years of observations. Currently, the full lifetime of Gaia is expected to be about 10.5 years.

Visualisation of the Gaia BH3 system showing its orbit and the motion of the system in our Galaxy. The video also describes the discovery in more detail. Credits: ESA/Gaia/DPAC- CC BY-SA 3.0 IGO. Acknowledgements: Video Animation: Stefan Jordan, Toni Sagristá with Gaia Sky - Text: Stefan Jordan, Pasquale Panuzzo, Ulrich Bastian, Tineke Roegiers, Berry Holl - Artificial voice - Based on "Discovery of a dormant 33 solar-masses black hole in pre-release Gaia astrometry" by Gaia Collaboration, et al., published in April 2024 in Astronomy & Astrophysics Letters. 

Reference article:
Gaia Collaboration; Panuzzo. P et al.«Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry». Astronomy & Astrophysics, April 2024. Doi: 10.1051/0004-6361/202449763
 

With 5,000 tiny robots in a mountaintop telescope, researchers can look 11 billion years into the past. The light from far-flung objects in space is just now reaching the Dark Energy Spectroscopic Instrument (DESI), a project managed by the Lawrence Berkeley National Laboratory (LBNL), enabling us to map our cosmos as it was in its youth and trace its growth to what we see today. Understanding how our universe has evolved is tied to how it ends, and to one of the biggest mysteries in physics: dark energy, the unknown ingredient causing our universe to expand faster and faster.

To study dark energy’s effects over the past 11 billion years, DESI has created the largest 3D map of our cosmos ever constructed, with the most precise measurements to date. This is the first time scientists have measured the expansion history of the young universe with a precision better than 1%, giving us our best view yet of how the universe evolved. Researchers shared the analysis of their first year of collected data in multiple papers that will be posted today on the arXiv and in talks at the American Physical Society meeting in the United States and the Rencontres de Moriond in Italy. These are the first 4th generation results on dark energy.  

 In this 360-degree video, take an interactive flight through millions of galaxies mapped using coordinate data from DESI. Credit: Fiske Planetarium, CU Boulder and DESI collaboration

“At the moment it looks like the first results from DESI are in agreement with the predictions of the current model”, said Hui Kong, postdoctoral researcher at IFAE, Barcelona, and  main author of one of the studies made public today. “There are some hints pointing at small temporal variations in the density of dark energy, but we will need more data to confirm them.”

Our leading model of the universe is known as Lambda CDM. It includes both a weakly interacting type of matter (cold dark matter, or CDM) and dark energy (Lambda). Both matter and dark energy shape how the universe expands – but in opposing ways. Matter and dark matter slow the expansion down, while dark energy speeds it up. The amount of each influences how our universe evolves. This model does a good job of describing results from previous experiments and how the universe looks throughout time.
 
However, when DESI’s first-year results are combined with data from other studies, there are some subtle differences with what Lambda CDM would predict. As DESI gathers more information during its five-year survey, these early results will become more precise, shedding light on whether the data are pointing to different explanations for the results we observe or the need to update our model. More data will also improve DESI’s other early results, which weigh in on the Hubble constant (a measure of how fast the universe is expanding today) and the mass of particles called neutrinos.  

“DESI, even with just the data from its first year, is already the spectroscopic survey with most collected data in the history and it goes on increasing this quantity with one million galaxies per month”, said Eusebio Sánchez, a researcher at CIEMAT, Madrid. “This amazing data sample makes possible to measure the expansion history of the Universe with an unprecedented precision. We are sure that DESI will increase our knowledge about the Universe and perhaps will allow us to make revolutionary discoveries”.
DESI’s overall precision on the expansion history across all 11 billion years is 0.5%, and the most distant epoch, covering 8-11 billion years in the past, has a record-setting precision of 0.82%. That measurement of our young universe is incredibly difficult to make. Yet within one year, DESI has become twice as powerful at measuring the expansion history at these early times as its predecessor (the Sloan Digital Sky Survey’s BOSS/eBOSS), which took more than a decade.

Traveling back in time

DESI is an international collaboration of more than 900 researchers from over 70 institutions around the world. The instrument was constructed and is operated with funding from the DOE Office of Science, and sits atop the U.S. National Science Foundation’s Nicholas U. Mayall 4-meter Telescope at Kitt Peak National Observatory, a program of NSF’s NOIRLab. 

Looking at DESI’s map, it’s easy to see the underlying structure of the universe: strands of galaxies clustered together, separated by voids with fewer objects. Our very early universe, well beyond DESI’s view, was quite different: a hot, dense soup of subatomic particles moving too 

fast to form stable matter like the atoms we know today. Among those particles were hydrogen and helium nuclei, collectively called baryons.

Tiny fluctuations in this early ionized plasma caused pressure waves, moving the baryons into a pattern of ripples that is similar to what you’d see if you tossed a handful of gravel into a pond. As the universe expanded and cooled, neutral atoms formed and the pressure waves stopped, freezing the ripples in three dimensions and increasing clustering of future galaxies in the dense areas. Billions of years later, we can still see this faint pattern of 3D ripples, or bubbles, in the characteristic separation of galaxies – a feature called Baryon Acoustic Oscillations (BAOs). 

Researchers use the BAO measurements as a cosmic ruler. By measuring the apparent size of these bubbles, they can determine distances to the matter responsible for this extremely faint pattern on the sky. Mapping the BAO bubbles both near and far lets researchers slice the data into chunks, measuring how fast the universe was expanding at each time in its past and modeling how dark energy affects that expansion.

This animation shows how baryon acoustic oscillations act as a cosmic ruler for measuring the expansion of the universe. Credit: Claire Lamman/DESI collaboration and Jenny Nuss/Berkeley Lab

“DESI is already more precise than all previous BAO surveys over the whole cosmic history”, said Violeta González Pérez, a researcher at the Theoretical Physics Department of the Universidad Autónoma from Madrid. “Its data allow us to study cosmic mysteries that lie beyond our current understanding of the Universe”.
Using galaxies to measure the expansion history and better understand dark energy is one technique, but it can only reach so far. At a certain point, light from typical galaxies is too faint, so researchers turn to quasars, extremely distant, bright galactic cores with black holes at their centers. Light from quasars is absorbed as it passes through intergalactic clouds of gas, enabling researchers to map the pockets of dense matter and use them the same way they use galaxies – a technique known as using the “Lyman-alpha forest.” 

“We use quasars as a backlight to basically see the shadow of the intervening gas between the quasars and us,” said Andreu Font-Ribera, a scientist at the Institute for High Energy Physics (IFAE) in Spain who co-leads DESI’s Lyman-alpha forest analysis. “It lets us look out further to when the universe was very young. It’s a really hard measurement to do, and very cool to see it succeed.”
 

Researchers used 450,000 quasars, the largest set ever collected for these Lyman-alpha forest measurements, to extend their BAO measurements all the way out to 11 billion years in the past. By the end of the survey, DESI plans to map 3 million quasars and 37 million galaxies.

State-of-the-art science

DESI is the first spectroscopic experiment to perform a fully “blinded analysis,” which conceals the true result from the scientists to avoid any subconscious confirmation bias. Researchers work in the dark with modified data, writing the code to analyze their findings. Once everything is finalized, they apply their analysis to the original data to reveal the actual answer.

"The fact that the analysis was carried out using data-blinding techniques provides us with an extra level of confidence in the results obtained," says Héctor Gil Marín, researcher at the Institute of Cosmos Sciences of the University of Barcelona (ICCUB) and the Institut d’Estudis Espacials de Catalunya (IEEC). Blind analyses are already standard practice in fields such as experimental particle physics or clinical studies. Gil-Marín and other researchers at ICCUB have developed and implemented what turned out to be a very robust and difficult-to-decipher way to conceal the results of galaxy clustering in DESI until the analysis is completed. "We are confident that the extra effort involved in this will enhance the confidence and integrity of the DESI results," says Gil-Marín.

DESI’s data will be used to complement future sky surveys such as the Vera C. Rubin Observatory and Nancy Grace Roman Space Telescope, and to prepare for a potential upgrade to DESI (DESI-II) that was recommended in a recent report by the U.S. Particle Physics Project Prioritization Panel.

“It is exciting to see how the DESI results provide a precise view of how the Universe is” mentioned Francisco Javier Castander, a researcher of the Instituto de Ciencias del Espacio (ICE-CSIC) and the Institut d’Estudis Espacials de Catalunya (IEEC). “Moreover, this is only the beginning, with the new data we are gathering our measurements will be even more precise”.

DESI is supported by the DOE Office of Science and by the National Energy Research Scientific Computing Center, a DOE Office of Science user facility. Additional support for DESI is provided by the U.S. National Science Foundation; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Humanities, Sciences, and Technologies of Mexico; the Ministry of Science and Innovation of Spain; and by the DESI member institutions.

The DESI collaboration is honored to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation.

Spanish participant institutions in DESI include the Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), the Instituto de Ciencias del Espacio (ICE-CSIC), the Institut de Ciències del Cosmos de la Universitat de Barcelona (ICCUB), the Institut de Física d'Altes Energies (IFAE), the Instituto de Física Teórica (IFT - UAM/CSIC), the Instituto de Astrofísica de Andalucía (IAA) and the Instituto de Astrofísica de Canarias (IAC).
A complete list of participant institutions and more information about DESI is available in: https://www.desi.lbl.gov.

The Institute of Cosmos Sciences of the University of Barcelona proudly announces that five of its researchers have been awarded highly competitive fellowships from the "La Caixa" Foundation. 

The five distinguished recipients are Fotios Fronimos, Pau Solé, and Jéssica Gonçalves, who have been awarded INPhINIT doctoral fellowships, and Pablo Cano and Adrià Gómez, who have been granted Junior Leader postdoctoral fellowships.

”La Caixa” Foundation has awarded 105 new doctoral and postdoctoral scholarships to excellent researchers to carry out their projects at universities and research centers in Spain and Portugal. With the INPhINIT doctoral scholarships and the Junior Leader postdoctoral scholarships, the ”la Caixa” Foundation pursues the double objective of retaining and attracting talent to promote excellent research in these countries.

These scholarships offer competitive salaries and cross-training. In the case of doctoral programs, issues such as scientific communication, the emotional well-being of the researcher, leadership and funding opportunities are reinforced. In postdoctoral scholarships, an independent scientific career is promoted as an option for a professional future and innovation and leadership are encouraged.

Xavier Luri, Director of the Institute of Cosmos Sciences who also attended the ceremony, expressed his satisfaction in incorporating these five researchers at the institute, "The recognition of their talent and dedication by the 'La Caixa' Foundation is a testament to the exceptional quality of research being conducted at the Institute of Cosmos Sciences as a María de Maeztu Unit of Excellence." 

The Institute of Cosmos Sciences extends its heartfelt congratulations to Fotios Fronimos, Pau Solé, Jéssica Gonçalves, Pablo Cano, and Adrià Gómez on their well-deserved achievements. Their success not only reflects their individual excellence but also underscores the ICCUB's commitment to fostering a culture of scientific accomplishment.

For more information about the Institute of Cosmos Sciences at the University of Barcelona, please visit https://icc.ub.edu/.

Pol Bordas, researcher from the High Energy Astrophysics group at the Institute of Cosmos Sciences of the University of Barcelona and the Institute of Space Studies of Catalonia (ICCUB-IEEC), has been recently designated as the deputy Physics Coordinator of the Large-Sized Telescope (LST) Collaboration, marking a significant milestone in his scientific career.

In the next years, Dr. Bordas will play a pivotal role in shaping the scientific direction of the collaboration, facilitating the interdisciplinary cooperation among the different working groups and laying out their strategic research topics, in alignment with the overall CTAO’s science case. His appointment as Deputy Physics Coordinator represents a significant endorsement of his scientific trajectory in the field and of his proven expertise and leadership skills.

The LST Collaboration is an international consortium of leading research institutions responsible for the design and construction of the Large-Sized Telescopes (LSTs), one of the three classes of telescopes required to cover the Cherenkov Telescope Array Observatory (CTAO) energy range, from 20 GeV to 300 TeV. Four LSTs will be arranged at the centre of the CTAO’s northern hemisphere array, located on La Palma (Spain), and an enhancement plan of the current layout includes also two LSTs in the southern array in the Atacama Desert (Chile). 

The LSTs are optimized to cover the low-energy sensitivity of the Observatory, between 20 and 150 GeV. Although these telescopes stand 45 metres tall and weigh around 100 tonnes, they are extremely nimble, with the ability to reposition within 20 seconds to capture brief, low-energy gamma-ray signals. Both the fast-repositioning speed and the low-energy threshold provided by the LSTs are critical for CTAO’s studies of transient gamma-ray sources in our own Galaxy and for the study of active galactic nuclei and gamma-ray bursts at high redshift. Thus, the LST research topics are very broad: from studying the sources of gamma rays in both galactic systems (X-ray binaries, pulsars and their nebulae, stellar-mass black holes, supernova remnants, or star forming regions) and extragalactic sources (active galactic nuclei, gamma ray bursts or galaxy clusters), to shedding new light into fundamental physics questions, such as the origin of cosmic rays or the nature of dark matter in a multi-messenger context.

"I am deeply honoured to assume the role of Deputy Physics Coordinator," said Pol Bordas. "The LSTs will play a key role within the CTAO, which will become the most sensitive Gamma-Ray Observatory worldwide and so I look forward to witnessing the discoveries that the first data now being collected will bring."

High Energy Physics at the ICCUB-IEEC

The High-energy Astrophysics group at the ICCUB-IEEC has been present in the collaboration since the inception of its predecessors, the MAGIC telescopes. Our researchers make significant contributions to LST in both the technical area (working on data analysis as well as hardware and electronics design) and the scientific area. ICCUB-IEEC members initially focused on the study of possible gamma ray sources like galactic binaries and microquasars. Some of the suggested sources were later observed by the Cherenkov Telescopes, like the detection of LS I +61 303 which resulted in the first publication of the MAGIC Collaboration in Science.

Thanks to this initial involvement, the High-Energy Astrophysics group started taking on bigger and bigger areas and growing in members. The Technological Unit of the ICCUB, led by Dr. David Gascón, opened a new research line focused on improving the LST hardware, and on the design and development of its electronics, which have undergone a huge advance in recent years and are now basic components of the telescope. The team counts also with a new PhD researcher to work on the Data Analysis and Software Development for the LST, making the ICCUB-IEEC present in both the Scientific, Instrumentation and Computation areas of the Collaboration.

“Our idea is to continue these lines of research in Cherenkov Astrophysics. The fact that I have been offered this new responsibility, makes it our goal to establish this branch of astrophysics as what I personally think it is: a new window for the study the very high-energy Universe,” says Pol Bordas.

About the Large-Sized Telescope Collaboration

The Large-Sized Telescope (LST) Collaboration consists of more than 400 scientists and engineers from twelve countries dedicated to the development and operation of these cutting-edge telescopes for the study of gamma-ray astrophysics. Comprising leading scientists and engineers from around the world, the collaboration is committed to advancing our understanding of high-energy astrophysical phenomena and pushing the boundaries of scientific exploration, as part of the Cherenkov Telescope Array Observatory (CTAO), which will be the first open ground-based gamma-ray observatory and the world’s largest and most sensitive instrument for the exploration of the high-energy Universe.

When gamma rays reach the Earth’s atmosphere they interact with it, producing cascades of subatomic particles. These cascades are also known as air or particle showers. Nothing can travel faster than the speed of light in a vacuum, but light travels 0.03 percent slower in air. Thus, these ultra-high energy particles can travel faster than light in air, creating a blue flash of “Cherenkov light” (discovered by Russian physicist Pavel Cherenkov in 1934) similar to the sonic boom created by an aircraft exceeding the speed of sound. Although the light is spread over a large area (250 m in diameter), the cascade only lasts a few billionths of a second. It is too faint to be detected by the human eye but not too faint for the CTAO. The CTAO’s large mirrors and high-speed cameras will detect the flash of light and image the cascade generated by the gamma rays for further study of their cosmic sources.

The CTAO will use three types of telescopes: the Large-Sized Telescopes (LST), the Medium-Sized Telescopes (MST) and the Small-Sized Telescopes (SST). More than 60 telescopes will be distributed between two telescope array sites: CTAO-North in the northern hemisphere at the Instituto de Astrofísica de Canarias’s (IAC’s) Roque de los Muchachos Observatory on La Palma (Spain), and CTAO-South in the southern hemisphere near the European Southern Observatory’s (ESO’s) Paranal Observatory in the Atacama Desert (Chile).

The European Space Agency’s Science Programme Committee has approved today the Laser Interferometer Space  Antenna (LISA) mission, the first scientific endeavour to detect and study gravitational  waves from space. The scientific contribution in Spain is led by the Institute of Space Sciences (ICE-CSIC) and the Institute of Space Studies of Catalonia (IEEC) and it counts with the participation of the Institute of Cosmos Sciences of the University of Barcelona (ICCUB).

ESA recognises through this step, formally called ‘adoption’, that the mission concept and  technology are sufficiently advanced, and gives the go-ahead to build the instruments and  spacecraft. This work will start in January 2025 once a European industrial contractor has  been chosen.  

LISA is not just one spacecraft but a constellation of three. They will trail Earth in its orbit around the Sun, forming an exquisitely accurate equilateral triangle in space. Each side of  the triangle will be 2.5 million km long (more than six times the Earth-Moon distance), and the spacecraft will exchange laser beams over this distance. The launch of the three spacecraft is planned for 2035, on an Ariane 6 rocket. The ICCUB Technology Unit will participate actively in two aspects: the construction of a radiation sensor on board the satellites, and the definition of the distributed data processing center in Barcelona.

Bringing ‘sound’ to the cosmic movie 

Just over a century ago, Einstein made the revolutionary prediction that when massive  objects accelerate, they shake the fabric of spacetime, producing miniscule ripples known as  gravitational waves. Thanks to modern technological developments, it is now possible  to detect these most elusive of signals. 

LISA will detect, across the entire Universe, the ripples in spacetime caused when huge black  holes at the centres of galaxies collide. This will enable scientists to trace the origin of these  objects, to chart how they grow to be millions of times more massive than the Sun and to establish the role they play in the evolution of galaxies.  

“LISA is an endeavour that has never been tried before. Using laser beams over distances of  tens of kilometres, ground-based instrumentation can detect gravitational waves coming  from events involving star-sized objects – such as supernova explosions or merging of hyper dense stars and stellar-mass black holes. To expand the frontier of gravitational studies we  must go to space,” explains LISA lead project scientist Nora Lützgendorf. 

The mission is poised to capture the predicted gravitational ‘ringing’ from the initial  moments of our Universe and offer a direct glimpse into the very first seconds after the Big  Bang. Additionally, because gravitational waves carry information on the distance of the  objects that emitted them, LISA will help researchers measure the change in the expansion of the Universe with a different type of yardstick from the techniques used by the Euclid space mission and  other surveys, validating their results. 

In our own galaxy, LISA will detect many merging pairs of compact objects  like white dwarfs or neutron stars and give us a unique insight into the final stages of the evolution of these systems. By pinpointing their position and distances, LISA will further our grasp of the structure of the Milky Way. 

To detect gravitational waves, LISA will use pairs of solid gold-platinum cubes – so called test masses (slightly smaller than Rubik’s cubes), free-floating in special housing at the heart of  each spacecraft. Gravitational waves will cause tiny changes in the distances between the masses in the different spacecraft, and the mission will track these variations using laser interferometry. 

This technique requires shooting laser beams from one spacecraft to the other and then  superimposing their signal to determine changes in the masses’ distances down to a few  billionths of a millimetre. The spacecraft must be designed to ensure that nothing, besides the geometry of spacetime itself, affects the movement of the masses, which are in freefall. 

Spanish contribution to LISA

Led by ESA, LISA is made possible by a collaboration between ESA, NASA, and an international consortium of scientists (the LISA consortium). The Spanish contribution is led by the ICE-CSIC together with the Institute of Cosmos Sciences of the Barcelona University (ICCUB) and the Universitat Politécnica de Cataluña - BarcelonaTech (UPC), through researchers all of them affiliated members of IEEC.

The Spanish contribution focuses on the Science Diagnostics Subsystem (SDS), one of the three main flight subsystems. Its goal is to measure the environmental disturbances on board each satellite in the constellation in order to differentiate them from the effect that gravitational waves would produce. The SDS will have temperature, magnetic field and radiation sensors on each satellite.

“In order to detect gravitational waves, LISA will measure the displacement between free falling masses in each of the three satellites in space at an unprecedented level down to the picometre level, roughly speaking the size of atoms”, says Miquel Nofrarias, experimental researcher at ICE-CSIC and IEEC, and member of the LISA Consortium. “SDS sensors will have to reach levels of precision and stability also unprecedented in space to be able to differentiate the effect of tiny environmental fluctuations from the one produced by a gravitational wave”, he adds.

Besides the contribution to the LISA instrument, the ICE-CSIC will also lead the development of a Spanish Data Distribution Center together with the necessary algorithms for the science exploitation. "The main goal is to provide the Spanish scientific community with the tools required to make the science potential of LISA a reality, so that we can make revolutionary discoveries with impact in Astrophysics, Cosmology and Fundamental Physics", says Carlos F. Sopuerta, ICE-CSIC and IEEC researcher and member of ESA’s LISA Science Study Team.

The spacecraft follows in the footsteps of its predecessor LISA Pathfinder, which demonstrated that it is possible to keep the test masses in freefall to an astonishing level of precision. The Spanish contribution to LISA Pathfinder, launched in 2015, was also led by ICE-CSIC and IEEC within the Gravitational Astronomy research group of the ICE-CSIC.

Science is often imagined as purely objective and rational, but being a human endeavor, it shares the same lights and shadows of all the other human enterprises. In particular according the Matthew effect there is an imbalance in the way credit for scientific work is assigned by peers: roughly speaking, this means that in the case of collaborative work or multiple simultaneous discoveries, the already famous scientists get all or most of the credit. 

In this paper led by researcher Livia Conti (former head of Virgo Outreach), and with the collaboration of Pablo Barneo from the Institute of Cosmos Sciences of the University of Barcelona (ICCUB-IEEC), researchers consider the specific case of LIGO, Virgo and KAGRA, where we detect a similar pattern of imbalance in the assignment of due credit by many members of the wider scientific community.
In 2015, scientists from LIGO and Virgo made a groundbreaking discovery: they found gravitational waves (GW), a phenomenon predicted by Einstein a century earlier. This important finding was announced to the public in early 2016. Since then, the collaboration between LIGO, Virgo, and KAGRA has detected nearly a hundred signals during three observing runs, using Advanced LIGO detectors in the US and the Advanced Virgo detector in Italy. These discoveries have sparked widespread interest, turning GW-based astrophysics and cosmology into a thriving area of scientific research.
 
Although the LIGO and Virgo Collaborations have been acting as a single collaboration since 2007, the team noted that this is not always recognized in the wider scientific community where it is frequent to find that shared results are attributed to LIGO only: in other words the narrative of the scientific developments is biased, with a potential impact on the history of science itself as well as on the careers of young scientists associated with Virgo or KAGRA. This problem propagates to funding agencies, which are influenced by the media mirroring the incomplete credits given by some of the problematic papers.

The observation of this biased narrative in a steadily growing number of papers prompted the team to implement an approach to systematically detect it, and if possible correct it. For 1 year starting from January 2022 they check all preprints appearing daily in the arXiv repository citing 'LIGO': we find on average 8 problematic, corresponding to about 9% of all papers containing the word “LIGO”.
 
The study not only focuses on identifying the problem at hand, but it also presented a solution. The team started asking the authors of problematic papers to fix their texts with the goal to convince the scientific community of the necessity of a correct scientific narrative. This initiative received replies from 48% of the recipients of requests, and the vast majority expressed understanding and their willingness to edit the preprints at the next occasion. The researchers found that their actions did partially correct the situation, as a follow-up analysis verified that some of the papers are indeed fixed.
 
The knowledge of the social dynamics of this particular cognitive bias is still quite poor and lots of work could be done to answer several remaining questions. In particular, it would be interesting to detect and quantify the time that the scientific community takes to correct this bias: this would shed light on socially accepted habits in this field of science. Similar studies in other fields of knowledge could yield different values that could help characterize the different scientific communities.
 
Finally we note that here we have focused on issues related to the visibility of the Virgo Collaboration. However, the LIGO Scientific Collaboration and Virgo Collaboration have been joined in the beginning of 2021 by the KAGRA Collaboration in co-authoring observational results from the full third observational period O3. Hence, it would be interesting to extend the study of cognitive bias by considering KAGRA as well.

Reference: https://doi.org/10.1140/epjh/s13129-023-00066-z

The conference will be opened by the vice-rector for research of the UB, Jordi Garcia Fernández. Leading researchers will analyze the contributions of the Catalan scientist in fields such as chemistry, physics and biology at the morning session organised by the UB. Joan Anton Català, curator of the Oró Year and science communicator, will give the lecture "Joan Oró, the dream of searching for the origin of life". Carme Jordi, professor at the UB Faculty of Physics and researcher at the Institute of Cosmos Sciences of the UB (ICC-UB), will give the lecture "Search for life beyond the solar system". Andrea Butturini, lecturer at the UB Faculty of Biology, will give a talk titled "Controversies surrounding methane on Mars". Josep Maria Ribó, lecturer in the Faculty of Chemistry at the UB, will speak on "The origin of biological homochirality".

Xavier Palau, representative of the Joan Oró Foundation, will then explain the connection that the Catalan biochemist had with the Montsec Mountain. Xavier Molí, from the Montsec Astronomical Park, will give the talk "Montsec Astronomical Park: discovering the best sky in Catalonia". Finally, Marc Ribó, lecturer at the Faculty of Physics, will give a talk on "The Montsec Observatory and research with the Joan Oró Telescope". The morning session will be moderated by Xavier Luri, professor at the Faculty of Physics and director of the ICCUB.

The year 2023, officially declared Joan Oró Year by the Catalan Government, has been the setting for various activities, talks and workshops in tribute to the figure of the biochemist from Lleida.

Joan Oró i Florensa studied biochemistry at the UB and devoted his career to studying the origin of life, a field in which he made major contributions that have inspired later generations of scientists.