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LISA Spain Meeting 2024

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Alberto Lobo Conference Room (Institute of Space Sciences (ICE, CSIC and IEEC))

Alberto Lobo Conference Room

Institute of Space Sciences (ICE, CSIC and IEEC)

Institute of Space Sciences (ICE, CSIC) Campus UAB Carrer de Can Magrans s/n 08193 Cerdanyola del Vallès (Barcelona) Zoom Connection: It will be send by e-mail to participants.
Carlos Sopuerta (ICE-CSIC ), Laura Martí (IEEC), Miquel Nofrarias (ICE-CSIC), Sascha Husa (ICE-CSIC)
Description

Welcome to the first LISA Spain meeting! The primary purpose of this meeting is the organization of the Spanish community interested in the Laser Interferometer Space Antenna (LISA) mission of the European Space Agency (ESA).  LISA was adopted in January, 25th 2024 and has entered the implementation phase.  There are many challenges and work to be done until the launch around 2035. If you are interested to contribute to any aspect of the mission, please attend the meeting. 

Group_picture_1.JPG Group_picture_2.JPG Laser_Interferometer_Space_Antenna_L3_proposal_1702.00786.pdf LISA_Definition_Study_Report_2402.07571.pdf LISA_Science_Requirements_Document.pdf The_Gravitational_Universe_Science_Theme_1305.5720.pdf
Participants
  • Alberto Rebassa-Mansergas
  • Alejandro Torres Forné
  • Alex Brown
  • Alicia M Sintes
  • Ana Pérez Ortega
  • Andreu Sanuy
  • Andrés Mínguez-Sánchez
  • Angeles Vazquez-Castro
  • Anna Heffernan
  • Antoni Ramos Buades
  • Antonio Gómez Bañón
  • Arnau Montava Agudo
  • Arshad Karimbu Vallappil
  • Arthur Suvorov
  • Borja Anguiano
  • Bradley Kavanagh
  • Brendan Devlin-Hill
  • Carlos Sopuerta
  • Cecilio García Quirós
  • Cristian Maria-Moreno
  • Daniel Guberman
  • Daniel Herencia
  • Daniel Serrano Rubio
  • Daniel Álvarez Franco
  • David Izquierdo-Villalba
  • David Pereñiguez
  • David Roma-Dollase
  • Diego Blas
  • Eduard Aguilar
  • Ema Dimastrogiovanni
  • Eric Madge
  • Francisco Rivas
  • Georgy Skorobogatov
  • Gerardo García Moreno
  • Giada Caneva Santoro
  • Gianluca Calcagni
  • Giuliano Iorio
  • Gonzalo Merino
  • Guillermo A. Mena Marugán
  • Helena Ubach Raya
  • Ignacio Mateos
  • Isabel Cordero-Carrión
  • Ivan Martin Vilchez
  • Jacopo Fumagalli
  • jam Sadiq
  • Jan Marc Costa
  • Jaume Garriga
  • Javier Castañeda Pons
  • Jiang Ji Ho Zhang
  • Jordi Portell de Mora
  • Jorge Valencia
  • Jose Juan Blanco-Pillado
  • Jose M Diego
  • Josep Maria Cirera i Perich
  • José M Senovilla
  • José-Luis Gálvez
  • Juan Garcia-Bellido
  • Juan Urrutia
  • Julen Morillas Alcarazo
  • Justo Hernán Ospino
  • Laura Martí Ramos
  • Luis Gil
  • Manuel Dominguez-Pumar
  • Mar Mezcua
  • Maria Caballero-Garcia
  • Maria Camisassa
  • Maria de Lluc Planas Llompart
  • Maria Rosselló Sastre
  • Marina Orta Terré
  • Martin Eriksen
  • Matteo Fasiello
  • Michele Lenzi
  • Miquel Canal
  • Miquel Nofrarias
  • Monica Seglar-Arroyo
  • Míriam Herrero-Valea
  • Nadejda Blagorodnova
  • Nicola Franchini
  • Nikolaos Karnesis
  • Oriol Pujolas
  • Ornella Juliana Piccinni
  • Pablo Barneo
  • Pablo Cárdenas-Fernández
  • Pablo Fernández de Alarcón Muguruza
  • Roberto Raddi
  • Roberto Ruiz de Austri
  • Roger Català
  • Ruben Sanchez-Ramirez
  • Ruxandra Bondarescu
  • Sachiko Kuroyanagi
  • Santiago Torres Gil
  • Sascha Husa
  • Sergio Lozano Althammer
  • Silvia Bonoli
  • Silvia Gasparotto
  • Simone D'Onofrio
  • Sofia Sisteré
  • Víctor Martín
  • Xavier Manyosa i Vilardell
  • Xisco Jimenez Forteza
  • Yumeng Xu
Contact Organization
  • Tuesday, 15 October
    • 10:00 → 11:00
      Registration and Welcome
      Conveners: Dr Carlos Sopuerta (ICE-CSIC), Dr Serenelli Aldo (ICE-CSIC)
    • 11:00 → 11:15
      The LISA mission after adoption 15m

      LISA, the Laser Interferometer Space Antenna, will be the first space mission ever to survey the Universe by detecting low-frequency gravitational waves. LISA is a space mission led by the European Space Agency (ESA) in collaboration with the US National Aeronautics and Space Administration (NASA). It was selected by ESA in 2017 and adopted in January 2024, which means it enters implementation with an expected launch in 2035. The science of LISA is very broad and revolutionary, covering outstanding questions in Astrophysics, Cosmology and Fundamental Physics. I will briefly describe the main features of the LISA mission and the different opportunities for contributing to this exciting mission.

      Speaker: Carlos Sopuerta (ICE, CSIC and IEEC)
      Carlos_Sopuerta_LISA_Spain_2024.pptx
    • 11:15 → 11:30
      Status of the Spanish contribution to LISA 15m

      Spain's contribution to the LISA mission focuses on critical hardware development, particularly the SDS (Sensing and Diagnostics Subsystem), which includes a suite of magnetic, thermal, and radiation sensors across the three spacecraft. These sensors are designed to characterize the noise environment surrounding the test mass. This talk will provide an overview of how the Spanish efforts are structured, as well as highlight key upcoming milestones and reviews the team is expected to accomplish in the coming years.

      Speaker: Laura Martí (IEEC)
      Laura_Marti_LISA_Spain_2024.pdf Laura_Marti_LISA_Spain_2024.pptx
    • 11:30 → 11:45
      Overview of the LISA Science Team 15m

      After an open call in February by ESA, and shortly thereafter by NASA, the LISA Science Team was announced in July this summer. The European selection consisted of 11 representatives from ESA member states, as well as a representative from the LISA consortium, 6 NASA-selected members, and project scientists from both NASA and LISA. The team acts as a focus for the interests of the scientific community in LISA, geared towards maximising the scientific returns of the mission. I will give a short overview and status update of the team and its objectives.

      Speaker: Anna Heffernan (University of the Balearic Islands)
      Anna_Heffernan_LISA_Spain_2024.pdf
    • 11:45 → 13:00
      Contributed Talks
      Conveners: David Roma-Dollase (ICE-CSIC), Guberman Daniel (ICCUB), Dr Miquel Nofrarias (ICE, CSIC)
      • 11:45
        ILIADA: In-Orbit LISA Diagnostics Demonstrator 25m

        ILIADA is an in-orbit demonstrator (IOD) planned to fly in 2026 as a part of an Earth Observation Cubesat in the framework of the NewSpace Strategy from the Generalitat of Catalonia. The primary goal of ILIADA is to raise the TRL of new technologies and sensor elements of the future LISA Diagnostics Subsystem. It will include temperature sensors, magnetometers (AMR and MEMs based) and a radiation monitor. The secondary objective of ILIADA is to detect the crossing of the spacecraft through the Birkeland currents —a set of electrical currents that flow along geomagnetic field lines connecting the Earth's magnetosphere to the Earth's high latitude ionosphere— by exploiting the use of high precision sensors on-board. In this contribution we will present the design and current status of the IOD.

        Speaker: Dr Miquel Nofrarias (ICE, CSIC)
        Miquel_Nofratias_LISA_Spain_2024.pdf
      • 12:10
        Temperature and Magnetic Diagnostic subsystem in LISA 20m

        The SDS task is to measure various physical parameters of the spacecraft such as temperature, radiation, and magnetism, since all these magnitudes can induce forces on the test masses that could not be discerned from a gravitational force. In this talk, we will be focusing on the instrumentation of the SDS used for the magnetic and temperature subsystem. First of all, a review of the requirements for this instrumentation will be shown. Then, both subsystems will be introduced. This is, on one hand, the magnetic subsystem, which is based on two sensing instruments acting at different frequency ranges: an audio-band coil, sensing in the 50 Hz to 500 Hz range; and a low-frequency magnetometer, based on Anisotropic Magneto-Resistive (AMR) sensors, sensing in the LISA measurement band. And on the other hand, the temperature subsystem which includes two kind of resistive sensors, NTC thermistors and Platinum RTDs, and also heaters, used to inject test signals to characterize the test mass thermal behaviour. Finally, the current development stage for both subsystems will be shown.

        Speaker: David Roma-Dollase (ICE-CSIC)
        David_Roma_LISA_Spain_2024.pdf David_Roma_LISA_Spain_2024.pptx
      • 12:30
        Status of the LISA Radiation Monitor 20m

        Cosmic rays and solar energetic particles will be the main components of the background radiation affecting LISA. Monitoring their fluxes will be essential for understanding the charging background of the mission and to provide vetoes for fake gravitational-wave triggers. We designed a new radiation monitor, tailored to monitor the charging of the LISA Test Masses (TMs). It consists of a telescopic arrangement of absorbers and plastic scintillators coupled to silicon photomultipliers (SiPMs). The SiPM signals are processed and digitized with the BETA ASIC, which was specifically designed for SiPM readout in space applications. The monitor will output proton detection rates in a set of integral energy channels with thresholds ranging from ~70 MeV to ~1 GeV. It will be able to observe SEP events and short-term variations of the cosmic-ray proton and helium flux at ~1 AU from the Sun, in an energy band that is inaccessible for most radiation monitors. We describe the main characteristics of the radiation monitor and discuss the preliminary evaluation of its performance, resulting from dedicated test beams and Monte Carlo simulations.

        Speaker: Guberman Daniel (ICCUB)
        Daniel_Guberman_LISA_Spain_2024.pdf
    • 13:00 → 14:30
      Lunch Break 1h 30m
    • 14:30 → 16:10
      Contributed Talks
      Conveners: Borja Anguiano (Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA)), Diego Blas (IFAE/ICREA), Jam Sadiq (SISSA, Trieste, Italy), Juan Urrutia (KBFI), María Caballero-García (IAA-CSIC)
      • 14:30
        Spanish contribution to the ESA's THESEUS mission 20m

        The Transient High Energy Sky and Early Universe Surveyor (THESEUS) is a medium sized space mission (previous candidate for M5) of the European Space Agency (ESA), currently proposed for M7 for evaluation (phase A) and with possible launch (if approved) in 2037. Its main objectives are the Early universe research through the observation of gamma rays (GRBs) and the study of electromagnetic counterparts of gravitational waves (GWs) and neutrinos emission sources. On the other hand, its on board instruments, with a wide field X-ray telescope in the 0.3-5 KeV with optical technology based on the “Lobster-Eye” system, a gamma ray telescope with capacity to create images and spectra in the 2-20 MeV (XGIS) range plus an infrared telescope of 0.7 m including a medium resolution spectrograph in the near infrared in the 0.7-1.8 μm range (IRT) constitute the ideal elements for unprecedented discoveries and in the line of ground and spatial instrumentation available in the decades of 2030-2040. THESEUS has just been re-selected (Nov.+ 2023) for the Phase A study (which will extend until 2026). Spain is involved in the THESEUS mission since its very early stages (M4 call) and is part of an international Consortium (currently) constituted by 15 countries, in which Spain is occupying the fifth position in terms of contribution. Spain is involved in two instruments of the mission, i.e. SXI by INTA and XGIS by U. of Valencia. The first is led by U. of Leicester (UK) and the second by U. of Bologna (Italy). In this talk I will present an overview of the mission and the role of its Spanish contribution.

        Speaker: María Caballero-García (IAA-CSIC)
        Maria_Caballero_LISA_Spain_2024.pdf
      • 14:50
        LISA binaries to detect ultra-light dark matter 20m

        I will present our recent work to show how ULDM generates modulation of GWs to be detected by LISA, and how this can be used to detect ULDM in so far unconstrained parameter space.

        Speaker: Diego Blas (IFAE/ICREA)
        Diego_Blas_LISA_Spain_2024.pdf
      • 15:10
        White Dwarf Binaries across the H-R Diagram 20m

        We created the APOGEE-GALEX-Gaia catalog to study white dwarf (WD) binaries. This database aims to create a minimally biased sample of WD binary systems identified from a combination of GALEX, Gaia, and APOGEE data to increase the number of WD binaries with orbital parameters and chemical compositions. We identify 3414 sources as WD binary candidates, with non-degenerate companions of spectral types between F and M, including main-sequence stars, main-sequence binaries, subgiants, sub-subgiants, red giants, and red clump stars. Among our findings are (a) a total of 1806 systems having inferred WD radii R < 25 R ⊕, which constitute a more reliable group of WD binary candidates within the main sample; (b) a difference in the metallicity distribution function between WD binary candidates and the control sample of most luminous giants (M H < -3.0); (c) the existence of a population of sub-subgiants with WD companions; (d) evidence for shorter periods in binaries that contain WDs compared to those that do not, as shown by the cumulative distributions of APOGEE radial velocity shifts; (e) evidence for systemic orbital evolution in a sample of 252 WD binaries with orbital periods, based on differences in the period distribution between systems with red clump, main-sequence binary, and sub-subgiant companions and systems with main-sequence or red giant companions; and (f) evidence for chemical enrichment during common envelope (CE) evolution, shown by lower metallicities in wide WD binary candidates (P > 100 days) compared to post-CE (P < 100 days) WD binary candidates.

        Speaker: Borja Anguiano (Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA))
        Anguiano_LISA.pdf
      • 15:30
        The dark timbre of gravitational waves 20m

        Gravitational wave timbre, the relative amplitude and phase of the different harmonics, can change due to interactions with low-mass halos. We focus on binaries in the LISA range and find that the integrated lens effect of cold dark matter structures can be used to probe the existence of Mv ≲ 10 M⊙ halos if a single binary with eccentricity e = 0.3−0.6 is detected with a signal-to-noise ratio 100 − 10^4.

        Speaker: Juan Urrutia (KBFI)
        Juan_Urrutia_LISA_BCN_2024.pdf
      • 15:50
        Population Analysis of PopIII Massive Black hole Binaries with LISA using Iterative weighted KDE 20m

        Reconstructing the properties of the astrophysical population of binary compact objects in the universe is a key science goal of gravitational wave detectors. This goal is hindered by the finite strain, frequency sensitivity and observing time of current and future detectors: implying that we can in general observe only a selected subset of the underlying population, with limited event statistics, and also nontrivial observational uncertainties in the parameters of each event. In this work, we will focus on observations of massive black hole binaries in the Laser Interferometer Space Antenna (LISA). If suchblack holes grow from population III star remnants (``light seeds''), then a significant fraction of the binary population at low masses and high redshift will be beyond LISA's observational reach; thus, selection effects have to be accounted for. Here we propose an iterative, kernel density estimation (KDE)-based nonparametric method, in order to tackle these statistical challenges in reconstructing the astrophysical population distribution from a finite number of observed signals. We test the method against a set of simulated LISA observations in a light seed scenario: we find that it is successful at reconstructing the underlying intrinsic astrophysical distribution in mass and redshift, except in parameter regions where zero or order(1) signals are observed. Thus, we expect to be able to access the full astrophysical information from LISA data, restricted only by the fundamental detection horizon.

        Speaker: Jam Sadiq (SISSA, Trieste, Italy)
        Jam_Sadiq_LISA_Spain_2024.pdf
    • 16:10 → 16:40
      Coffee Break 30m
    • 16:40 → 19:10
      Contributed Talks
      Conveners: Carlos Sopuerta (ICE, CSIC and IEEC), Cecilio García Quirós (University of Zurich), Ivan Martín Vílchez (ICE-CSIC), Jordi Portell de Mora (ICCUB), Jorge Valencia (University of the Balearic Islands), Dr Sascha Husa (Institute of Space Sciences (ICE, CSIC))
      • 16:40
        LISA DDPC and waveform modelling 30m

        The Distributed Data Processing Center (DDPC) is the entity within the European Science Ground Segment, organised by ESA member states, that extracts the scientific products (L3 Data) from the noise corrected data (L1 data). The talk will first summarise the objectives and organisation of the DDPC, and then focus on the challenge of developing waveform models for LISA science, and of implementing them for the LISA data analysis workflow with the DDPC.

        Speaker: Dr Sascha Husa (Institute of Space Sciences (ICE, CSIC))
        Sascha_Husa_LISA_Spain_2024.pdf
      • 17:10
        LISA Parameter Estimation with Time Domain Response 20m

        Parameter estimation with full Bayesian inference remains one of the outstanding challenges for the LISA data analysis infrastructure. Very few studies have focused on this issue and have been reduced to the use of Fourier domain waveforms. The limiting factor of this approach is the need for the development of approximate transfer functions that replicate the TDI response in the Fourier domain and pose an extra theoretical challenge for precessing and eccentric waveforms. In this work, we explore the use of waveforms in the time domain, which would allow us to obtain the TDI response for any kind of signal, without any extra theoretical development or approximate assumptions. Apart from allowing us to do parameter estimation with templates with new physical features, it would also serve as a complementary and validation tool for the parameter estimation studies with Fourier domain waveforms. I will present the status of current parameter estimation runs with a novel GPU implementation of the IMRPhenomT waveform family and the LISA response.

        Speaker: Cecilio García Quirós (University of Zurich)
        Cecilio_Garcia_Quiros_LISA_Spain_2024.pdf
      • 17:30
        Data analysis efforts at UIB from the ground up 20m

        The talk will summarise ongoing efforts at UIB in gravitational wave data analysis for LISA, and for ground based detectors from a LISA perspective, focussing on waveform modelling, including numerical relativity,
        and parameter estimation.

        Speaker: Jorge Valencia (University of the Balearic Islands)
        Jorge_Valencia_LISA_Spain_2024.pdf
      • 18:10
        Lessons learned from Gaia data processing and analysis 20m

        The Gaia space astrometry mission of ESA is collecting data from more than one billion stars of the Milky Way and beyond, meaning over 136 TB of raw data, nearly 260 billion combined measurements (star transits) and over 2.5 trillion astrometric measurements so far. Even though these numbers may seem "manageable" with nowadays technology, it was a huge challenge back in 2005 when the Gaia Data Processing and Analysis Consortium (DPAC) was being defined. In this talk, I will summarize some of the lessons learned (including data processing and analysis approaches and best practices in software development) that may be applicable to LISA, highlighting similarities and differences between these two groundbreaking missions.

        Speaker: Jordi Portell de Mora (ICCUB)
        Jordi_Portell_LISA_Spain_2024.pdf
      • 18:30
        From the LISA Data Challenges towards a LISA Global Fit algorithm 20m

        LISA will be the first space-based gravitational-wave and will operate in the milli-Hertz frequency band, with is rich in different astrophysical and cosmological sources. LISA is a signal-dominated detector which means that the data stream always contains overlapping sources, among them millions of galactic ultracompact binaries. In order to detect and estimate the physical parameters of these sources it is then necessary to use a "global fit" algorithm that can avoid biases due to single source detection and parameter estimation. In this talk I will describe the efforts at the ICE in the context of the LISA data challenges and the Data Distributed processing center.

        Speakers: Carlos Sopuerta (ICE, CSIC and IEEC), Ivan Martín Vílchez (ICE-CSIC)
        Carlos_Sopuerta_and_Ivan_Martin_Vilchez_LISA_Spain_2024.pdf
  • Wednesday, 16 October
    • 09:30 → 11:30
      Contributed Talks
      Conveners: Arthur Suvorov (University of Alicante), Eric Madge (Instituto de Física Teórica (IFT-UAM/CSIC)), Giuliano Iorio (ICCUB, Universitat de Barcelona), Guillermo A. Mena Marugán (Instituto de Estructura de la Materia, CSIC), Matteo Fasiello (IFT Madrid), Silvia Gasparotto (IFAE)
      • 09:30
        Dual-line detectability of ultra-compact X-ray binares: LISA and LVK 20m

        Ultra-compact X-ray binaries are promising sources for LISA because of their short orbital periods. For such binaries with neutron-star primaries, that have been spun-up by angular momentum donations to ~ms periods, internal quadrupole moments sourced by accretion-built mountains may be large (e.g. in 4U 1728−34 and 4U 1820−30). Such systems may thus be simultaneously visible to LVK/ET and LISA. I will discuss how a "dual-line" detection of this sort could provide constraints on the neutron-star equation of state, in addition to information on other areas of astrophysics.

        Speaker: Arthur Suvorov (University of Alicante)
        Arthur_Suvorov_LISA_Spain_2024.pdf
      • 09:50
        A new tool on the workbench: the rapid population synthesis code SEVN for gravitational wave astronomy 20m

        LISA will play a crucial role in unveiling the universe of gravitational wave sources, particularly by probing the inspirals and mergers of binary compact objects (BCOs) such as black holes, neutron stars, and white dwarfs over cosmological distances. To fully exploit the wealth of data that LISA will provide, we need accurate predictions for the properties and rates of these binary mergers across cosmic time. This requires state-of-the-art binary population synthesis tools that can evolve large stellar populations, track complex binary interactions, and account for diverse stellar environments. In this talk, I present SEVN (Stellar EVolution for N-body codes), a new state-of-the-art population synthesis code specifically designed to model the formation and evolution of BCOs. Unlike many traditional population synthesis codes, which rely on outdated stellar evolution models and offer limited flexibility, SEVN uses a fully modular approach. The code interpolates stellar evolution from pre-computed look-up tables, allowing users to dynamically switch between different sets of stellar models without modifying or recompiling the code. The code’s adaptive time-stepping method ensures both high-resolution modeling of critical phases (e.g., Roche Lobe overflow) and a significant reduction in computational time. In this presentation, I will showcase the first scientific applications of SEVN, particularly focusing on the formation and properties of BCOs from Population I, II, and III stars. I will discuss how the choice of stellar evolution models can dramatically affect predictions for BCO merger rates and properties, providing valuable insight for future gravitational wave observations with LISA. This modular and scalable approach makes SEVN a powerful tool for studying the binary systems that LISA is poised to detect, offering a versatile framework that scales seamlessly from personal computers to large clusters.

        Speaker: Giuliano Iorio (ICCUB, Universitat de Barcelona)
        Giuliano_Iorio_LISA_Spain_2024.pdf
      • 10:10
        Memory effect in LISA sources: prospects and relevance 20m

        Gravitational wave memory is a non-linear prediction of general relativity that informs us about the fluxes emitted by gravitational wave sources. Its detection is more challenging than the ordinary waveform, and requires dedicated studies. On the other hand, the information in the memory is complementary to the main signal and may even break some degeneracies of the latter, or probe new aspects of GR. In this talk, I will present the most up to date analysis of how LISA may detect GW memory, also considering the up to date population models. I will finally discuss some implications for parameter estimation.

        Speaker: Silvia Gasparotto (IFAE)
        Lisa_Spain_slides.pdf
      • 10:30
        Gravitational waves from first-order phase transitions in LISA: reconstruction pipeline and physics interpretation 20m

        We develop a tool for the analysis of stochastic gravitational wave backgrounds from cosmological first-order phase transitions with LISA: we initiate a template databank for these signals, prototype their searches, and forecast their reconstruction. The templates encompass the gravitational wave signals sourced by bubble collisions, sound waves and turbulence. Accounting for Galactic and extra-Galactic foregrounds, we forecast the region of the parameter space that LISA will reconstruct with better than ~10% accuracy, if certain experimental and theoretical uncertainties are solved by the time LISA flies. We illustrate the accuracy with which LISA can reconstruct the parameters on a few benchmark signals, both in terms of the template parameters and the phase transition ones. To show the impact of the forecasts on physics beyond the Standard Model, we map the reconstructed benchmark measurements into the parameter spaces of the singlet extension of the Standard Model and of the classically conformal invariant $U(1)_{B-L}$ model.

        Speaker: Eric Madge (Instituto de Física Teórica (IFT-UAM/CSIC))
        Eric_Madge_LISA_Spain_2024.pdf
      • 10:50
        Global quantum effects on gravitational radiation in the era of the LISA mission 20m

        The Loop Quantum Gravity group at IEM-CSIC studies global quantum effects that may influence the emission of gravitational radiation during the final stages of supermassive black hole coalescence. We use Hamiltonian formalisms that allow us to relate black holes with cosmological backgrounds and establish a correspondence between the quantum field theories for gauge invariants in both cases. We aim to extract predictions with consequences for the fundamental physics of the LISA interferometer.

        Speaker: Guillermo A. Mena Marugán (Instituto de Estructura de la Materia, CSIC)
        Guillermo_Mena_Marugan_LISA_Spain_2024.pdf
      • 11:10
        Testing axion inflation with LISA 20m

        I will review the mechanism for primordial gravitational wave generation in axion-inflation models comprising a gauge sector coupled via a Chern-Simons term. I will survey both the Abelian and non-Abelian cases and provide details on the concrete possibility of primordial black hole production. I will elaborate on specific examples whose gravitational signal is detecteable by LISA.

        Speaker: Matteo Fasiello (IFT Madrid)
        Matteo_Fasiello_LISA_Spain_2024.pdf
    • 11:30 → 12:00
      Coffee Break - GROUP PICTURE 30m
    • 12:00 → 13:40
      Contributed Talks
      Conveners: Daniel Rubio Serrano (ICE-CSIC and IEEC), Miriam Herrero-Valea (IFAE), Sofia Sisteré (ICE-CSIC), Xavier Manyosa (UPC), Yumeng Xu (Universitat de les Illes Balears)
      • 12:00
        Time-frequency domain coherent search from ground-based detector to LISA 20m

        Time-frequency domain coherent search has played a significant role in the analysis of data from ground-based detectors. It does not rely on an accurate waveform and noises model, making it well-suited for identifying unexpected sources. This presentation will introduce the ongoing development of the time-frequency domain coherent search pipeline and explore its potential application to LISA.

        Speaker: Yumeng Xu (Universitat de les Illes Balears)
        Yumeng_Xu_LISA_Spain_2024.pdf
      • 12:20
        Time series forecasting for fast waveform evaluation 20m

        One of the primary challenges in analyzing gravitational wave data from future ground and space-based experiments is the need for rapid waveform and likelihood evaluation to expedite Bayesian analysis. Although surrogate models are commonly used to address this, they are limited to finite regions of the parameter space, and their computational cost can escalate significantly as higher precision is demanded. In this work, we leverage the efficiency and fast evaluation times of state-of-the-art time forecasting techniques and large language models, such as transformers, to tackle this challenge. Specifically, we design models capable of generating the latter part of a binary black hole merger waveform (merger and ringdown) based on information from the inspiralling phase, which can be analytically obtained using post-Newtonian methods. Our models can be trained using waveforms produced by traditional surrogates and numerical relativity, employing Monte Carlo dropout and active learning to dynamically select the most efficient training data.

        Speaker: Miriam Herrero-Valea (IFAE)
        Miriam_Herrero_Valea_LISA_Spain_2024.pptx
      • 12:40
        Estimate of the magnetic contribution to acceleration noise in LISA Pathfinder 20m

        LISA Pathfinder was a mission designed to test key technologies required for gravitational wave detection in space. Magnetic forces have an important impact on the instrument sensitivity in the low frequency regime below the millihertz. A precise characterization of the magnetic properties of LISA Pathfinder free falling test-masses is of special interest for future gravitational wave observatory in space. We report on the magnetic injection experiments performed throughout LISA Pathfinder operations. We show how these experiments allowed a high precision estimate of the instrument magnetic parameters. The remanent magnetic moment was found to have a modulus of (0.245 ± 0.081) nAm2, the x-component of the background magnetic field within the test masses position was measured to be (414 ± 74) nT and its gradient had a value of (−7.4 ± 2.1) μT/m. The test mass magnetic susceptibility was measured to be (−3.3723 ± 0.0069)×10−5 in the low frequency regime. Finally, magnetic forces couple to the test mass motion, introducing a contribution to the relative acceleration noise between the free falling test masses. Our results set the magnetic-induced acceleration noise during the February 2017 noise run of 0.25-0.08+0.15 fm s-2Hz-1/2 at 1 mHz and 1.01-0.24+0.73 fm s-2Hz-1/2 at 0.1 mHz. We also discuss how the non-stationarities of the interplanetary magnetic field can affect these values during extreme space weather conditions. All results are in agreement with on-ground estimates.

        Speaker: Daniel Rubio Serrano (ICE-CSIC and IEEC)
        Daniel_Serrano_LISA_Spain_2024.pdf
      • 13:00
        Optical-based temperature sensors for future gravitational wave experiments 20m

        High precision temperature measurements are becoming a transversal need in a wide variety of fields that span from applied to fundamental physics. Resistive-based sensors are nowadays the preferred temperature sensors used in space missions, given their reliability and long heritage. In recent years, optical metrology experiments have shown promising results. The use of fiber optic sensors is of particular interest as these are both non-magnetic and also relatively poor conductors, both qualities of particular interest for the LISA mission. Furthermore, Whispering Gallery Mode resonators which are monolithic crystal resonators that can provide narrow resonances that are suitable for high stability and resolution measurements. Our group is currently studying several solutions aiming a noise floor of 1 uK/√Hz at 1 mHz, a noise performance that would match the one achieved by a previous activity which is based in resistive technology. In this presentation, I will provide a comprehensive overview of the ongoing work, highlighting key developments and progress made so far. Additionally, I will discuss the challenges and limitations that have emerged as well as strategies being explored to overcome them.

        Speaker: Sofia Sisteré (ICE-CSIC)
        Sofia_Sistere_Vinuales_LISA_Spain_2024.pptx
      • 13:20
        Magnetic field modulation for space: from MELISA to ILIADA 20m

        Measurement of magnetic field fluctuations is one of the key objectives in many space missions. In LISA mission, magnetometers are key to characterize the force and torque disturbances generated on the test masses by the magnetic field fluctuations. For LISA it is necessary to achieve a noise amplitude spectral density (ASD) below 10 nT/sqrt(Hz) from 0.1 to 0.1 Hz, below the interplanetary magnetic field. In those low frequencies, the intrinsic 1/f noise is the predominant issue when trying to have a low noise floor.
        In order to reach that noise goal, a magnetometer system has been developed using a microelectromechanical system (MEMS) cantilever, resonating over a Tunneling Magnetic Resistor (TMR). A high magnetic permeability material has been deposited on the tip of the cantilever. Then, by exciting the MEMS at its resonance, the low-frequency content of the magnetic field can be modulated to frequencies where the 1/f noise fades, to be afterwards demodulated computationally, therefore drastically mitigating any 1/f noise contribution.
        First results obtained within the internal IEEC project named MELISA (MEMS for LISA) indicated that is possible to obtain a noise floor below 10nT/sqrt(Hz) between 0.1mHz and 0.1Hz. A maximum modulation depth of 39% was also been obtained. Now, this design is being adapted to be incorporated in the ILIADA (In-Orbit Lisa Diagnostics Demonstrator), to raise its TRL level.

        Speaker: Xavier Manyosa (UPC)
        Xavier_Manyosa_LISA_Spain_2024.pdf Xavier_Manyosa_LISA_Spain_2024.pptx
    • 13:40 → 15:00
      Lunch Break 1h 20m
    • 15:00 → 17:30
      Contributed Talks + Roadmap for the Spanish contribution to LISA
      Conveners: Andrés Mínguez-Sánchez (IEM-CSIC), David Pereñiguez (Niels Bohr Institute), Luis Gil (FTAE, Universidad de Granada)
      • 15:00
        Dimensionally reduced EFTs for cosmological phase transitions 20m

        The upcoming launch of LISA has recently strengthened the interest in exploring Standard Model extensions where a gravitational wave-producing, strong first-order electroweak phase transition (SFOEWPT) occurs in the early universe. One of the preferred approaches to the study of thermally induced FOPTs is through the construction of a dimensionally reduced effective field theory (3dEFT). In this talk we will summarize the key aspects of this approach. We shall provide a rigorous perturbative method to compute the essential magnitudes for modeling the GW production during a SFOPT. We will discuss the importance of including higher-order effective operators in these computations, which drastically change the predictions of GW-related magnitudes and are, as far as the authors know, often overlooked in the current literature.

        Speaker: Luis Gil (FTAE, Universidad de Granada)
        Luis_Gil_LISA_Spain_2024.pdf
      • 15:20
        Perturbative gauge invariants in the Hamiltonian formalism for spherically symmetric backgrounds 20m

        The Hamiltonian formalism of perturbation theory in general relativity is a powerful tool for exploring physical aspects beyond the mathematical formulation of an astrophysical system. Its broad range of applications makes the analysis of spherically symmetric backgrounds particularly interesting. The Loop Quantum Gravity group at IEM-CSIC has focused on studying the final stages of supermassive black hole coalescence. This approach provides an opportunity to investigate quantum aspects, such as gravitational radiation. In this context, we aim to present a compelling method for identifying perturbative gauge invariants within the Hamiltonian formalism. These quantities may lead to predictions with implications for fundamental physics, including potential consequences for the LISA interferometer.

        Speaker: Andrés Mínguez-Sánchez (IEM-CSIC)
        Andres_Minguez_Sanchez_LISA_Spain_2024.pdf
      • 15:40
        Perturbation Theory from Curvature Wave Equations and Ringdown Nonlinearities 20m

        The prospect of observing loud ringdowns from massive black hole mergers with LISA opens an unprecedented window into the strong-field regime of gravity. Using this opportunity hinges on our ability to extend the current paradigms of black hole perturbation theory and ringdown modelling to account for dynamical non-linearities. In this talk, I will present a new approach to black hole perturbation theory in spherical symmetry, based on the so-called curvature wave equations, and provide a systematic derivation of a number of important results in the literature. As an application, I will discuss an effective model to describe the ringdown of a mass-varying spacetime and its potential to capture absorption-induced excitations. To conclude, I will discuss some recent progress in understanding late-time ringdown tails driven by either sources or non-linear effects.

        Speaker: David Pereñiguez (Niels Bohr Institute)
        David_Pereniguez_LISA_Spain_2024.pdf
      • 16:00
        DISCUSSION ON A ROADMAP FOR LISA SPAIN CONTRIBUTIONS 1h 30m

        Discussion on the contributions of the Spanish community to the LISA mission, in particular to its science and the key items (instrument, data analysis/ground segment, and other deliverables)

        Slides_for_discussion.pdf
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