The Fermi Summer School emphasizes the analysis of data from the Fermi instruments through lectures and hands-on workshops. Students spend time working directly with experts in instrumentation, analysis, theory and modeling to develop and extend their own research projects. Topics cover much of the gamma-ray band ranging from keV-MeV transients seen with Fermi's GBM to the highest energies observed by the LAT and the very high energies observed by ground-based gamma-ray telescopes. This year's school will be held at the University of Delaware Conference Center in Lewes, Delaware, from May 28 to June 7, 2024.
Material will be aimed at graduate students and post-doctoral researchers. Topics will include particle acceleration and gamma-ray production mechanisms; space-based and ground-based gamma-ray instrumentation; spectral, spatial, and time-based analysis of gamma-ray data; modeling and interpretation of gamma-ray data; and astrophysical source classes such as AGN, GRBs, Galactic pulsars and binary systems, supernova remnants, and pulsar wind nebulae as well as searches for dark matter and new physics.
The software necessary for the tutorials (such as the Fermitools) are distributed in the FermiBottle Docker Container, a fully-functional, self-contained analysis environment. Please go through the Summer School Checklist to make sure the container is functioning correctly.
On this page
Schedule
Go directly to Week 1 or Week 2. All times are in Eastern Daylight Time (UTC−04:00).
See our Code of Conduct and COVID-19 guidelines.
Week 1
| Tues, May 28 | Wed, May 29 | Thurs, May 30 | Fri, May 31 | Sat, June 1 |
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| 8:00 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
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| 9:00 | Welcome and Introductions - Liz
| Astroparticle Radiation and Acceleration I - Damiano Caprioli | Astroparticle Radiation and Acceleration II - Damiano
Lecture Notes on DSA DSA Detailed Notes | Astroparticle Radiation and Acceleration III - Damiano | Stats Lecture 5 - Cole QPO Information |
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| 10:00 | Intro to Fermi - Liz Fermi Survey Strategy - Joe Eggen | Intro to Fermi LAT - Liz | Impostor Syndrome workshop - All | Neutron Stars Part 2 - Cecilia | Student Talks / 1 Slide Summaries |
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| 11:00 | Break | Break | Break | Break (Photo!) | Break |
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| 11:30 | Stats Lecture 1 - Cole Miller | Neutron Stars - Cecilia Chirenti | Intro to Fermi GBM - Colleen Wilson-Hodge (remote) | Student Talks / 1 Slide Summaries | X-ray and Gamma-ray observations of pulsar wind nebulae - Jordan Eagle |
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| 12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
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| 1:30 | Getting started with Fermi: Tools and Resources - Joe Eggen, Joe Asercion, Alex Reustle, Sheimy, Paz, Nestor Mirabal (remote), Don Horner (remote) Data Exploration notebook Data Quicklook notebook | Stats Lecture 2 - Cole Getting Started with Likelihood Analysis - Liz, Joe
fermi-summer-school Github repository - See README file for instructions to download data and precomputed files for the 3C279 example analysis. 3C279 Example Analysis Likelihood Notebook Look here for a few project Ideas
| Stats Lecture 3 - Cole Intro to the LAT Photon Data Catalog - Sheimy Paz LAT Instrument Response and Next Steps with Likelihood - Liz
| Stats Lecture 4 - Cole Extended sources (3C 279 intro, W51C) - Liz, Jordan
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Making LAT Spectra and lightcurves |
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| 4:45 | End of the Day Tag-up | End of the Day Tag-up | End of the Day Tag-up | End of the Day Tag-up | End of the Day Tag-up |
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| Bike rental pick-up - leave by 4:30 |
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Week 2
| Mon, June 3 | Tues, June 4 | Wed, June 5 | Thurs, June 6 | Fri, June 7 |
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| 8:00 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
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| 9:00 | Lecture 1 - Qi Feng | Polarization - Haocheng Zhang | Lecture 2 - Qi | Magnetars - Oliver | 9:00 -9:30 Pack up.
9:30 - 10:30 Closing Session Feedback Form
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| 10:00 | The High-energy Universe with Fermi-GBM - Oliver Roberts | Student Talks / 1 Slide Summaries | Student Talks / 1 Slide Summaries | Gamma-ray Binaries - Jamie |
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| 11:00 | Break | Break | Break | Break | Break |
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| 11:30 | The Transient Gamma-ray Sky seen by Fermi-LAT - Niccolò Di Lalla | Student Talks / 1 Slide Summaries | Rubin LSST - Federica Bianco | Student Talks / 1 Slide Summaries | Complete packing up and return bikes. |
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| 12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
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| 1:30 | Burst analysis workshop - Niccolò Di Lalla: Analysis notebooks: - GRB 080916C with GBM
- GRB 190114C with LAT
- GRB 130427A with GBM, LLE and LAT
| Free Afternoon | Time-based analysis topics |
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| 4:45 | End of the Day Tag-up |
| End of the Day Tag-up | End of the Day Tag-up |
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Student Talks and 1 Slide Summary Schedule
Friday, May 31
Owen Henry - "Gamma-rays in Globular Clusters"
Abstract
Abstract: We use 13 years of data collected by the Large Area Telescope (LAT) aboard Fermi to search for a cumulative signal from undetected Globular Clusters. We aim to associate the gamma-rays detected with LAT with our globular clusters using a stacked population of 36 high latitude targets not detected in the Fermi Point Source Catalog (4FGL). So far, Fermi has detected 32 Globular Clusters (GCs) which make them a feasible target for studies of gamma-rays. Control fields used in this analysis were selected from a library of fields randomly distributed across the sky by matching the Galactic distribution of the target clusters. We find that the stacked population of undetected globular clusters has a significant separation in cumulative likelihood from the stack of control fields. We also investigate correlations between the stack luminosity and detected cluster observables, such as distance, absolute magnitude (i.e., mass), and stellar encounter rate.
Ava Webber - "A Systematic Study of Galactic Star-Forming Regions"
Abstract
Abstract: Star-forming regions (SFRs) are known sites of particle acceleration and may potentially be important sources of gamma-rays in the Galaxy. While a few Galactic SFRs have been associated with gamma-ray sources, the majority lack detections. Using all available Fermi data in combination with improved optical measurements, we are performing a systematic study of Galactic SFRs. The goal of our systematic study is to characterize the morphology and spectral emission of Galactic SFRs, and understand their energetics and particle acceleration processes. In this talk I will discuss the preliminary results of this project focusing on the connection of SFRs’ emission and their physical properties.
Pranab Deka - "Exponential Methods for Anisotropic Diffusion"
Abstract
Abstract: Anisotropic diffusion is imperative in understanding cosmic ray diffusion across the Galaxy, the heliosphere, and the interplay of cosmic rays with the Galactic magnetic field. The diffusion term contributes to the highly-stiff nature of the cosmic ray transport equation. In order to conduct numerical simulations of time-dependent cosmic ray transport, the implicit Crank-Nicolson integrator has been traditionally favoured over the CFL-bound explicit integrators to be able to take large time-step sizes. We propose exponential methods that directly compute the exponential of the underlying matrix (or the exponential-like functions) to treat the linear anisotropic diffusion equation. We consider time-dependent sources to emulate cosmic rays being ejected into the Galaxy at different points in time. We compare and contrast the performance of two second-order and one fourth-order exponential quadrature methods with that of Crank-Nicolson. The exponential methods allow us to take substantially large time-step sizes, thereby reducing the computational cost by almost an order of magnitude. The accuracy of the second-order exponential methods is similar to that of Crank-Nicolson (as one would expect) whilst the fourth-order solver yields highly accurate solutions. The boost in the performance offered by the exponential methods without compromising the accuracy of the solutions makes them an excellent alternative to the traditional methods for treating the time-dependent cosmic ray transport equation.
Zachary Metzler - "Opportunities for Multimessenger Observations of Millisecond Pulsars"
Abstract
Abstract: The first gravitational wave was detected by LIGO in 2015, and since that time over 100 events have been detected. However, these detections have been transient signals from binary mergers of black holes and neutron stars. In addition to transient, LIGO is sensitive to continuous gravitational waves. Millisecond pulsars are strong candidates for continuous gravitational waves, since the accretion from a nearby star can sustain spins >500 Hz and the accreting matter provides an inherent ellipticity. I will discuss the relationship between ellipticity, accretion rate, and gamma ray emission as well as discuss prospects for directly measuring these in the near future.
Saturday, June 1
Giovanni Cozzolongo - "Clustering analysis of Fermi-LAT unidentified point sources"
Abstract
Abstract: In this work we study clustering of unassociated Fermi-LAT sources and search for counterpart extended sources in TeV energies. The goal is to determine whether an extended source model is preferred compared to a cluster of point-like sources. The work is motivated by prior observations of extended TeV gamma-ray sources, such as HESS J1813-178, and their GeV counterparts. In the case of HESS J1813-178, two unidentified Fermi-LAT point sources were detected in the region. Subsequent multiwavelength analysis combining TeV and GeV data showed that a single extended source is a better description of the emission in this region than two point-like sources.
Jakub Juryšek - "Observation of the galactic PeVatron candidate LHAASO J2108+5157 with the Large-Sized telescope for the Cherenkov Telescope Array"
Abstract
Abstract: The Cherenkov Telescope Array (CTA) Observatory will be the next generation ground-based very-high-energy gamma-ray observatory, sensitive from 20 GeV up to 300 TeV. The Large-Sized Telescope prototype (LST-1), currently in the commissioning phase, was inaugurated in October 2018 on La Palma (Spain). It is the first of four LST telescopes for CTA, to be built on La Palma. In 2021, LST-1 performed observations of one of the Galactic PeVatron candidates, LHAASO J2108+5157, recently discovered by the LHAASO collaboration. In my contribution, I present results of our analysis of the LST-1 data, putting strong constraints on the emission of the source in the multi-TeV band. I also present results of multi-wavelength modeling, testing different scenarios for the parent particles producing the high energy emission and put constraints on their spectra.
Zachary Curtis-Ginsberg - "Calibrating a Camera: Electronics work for the prototype Schwarzschild-Couder Telescope"
Abstract
Abstract: The dual-mirrored Schwarzschild-Couder Telescope is a proposed medium-sized telescope candidate for the Cherenkov Telescope Array’s southern site (in Paranal, Chile). The Schwarzschild-Couder design has an energy range of 100 GeV to 10 TeV and a field of view of 8°. A prototype Schwarzschild-Couder Telescope (pSCT) has been built next to VERITAS at the Fred Lawrence Whipple Observatory and was inaugurated in January 2019. The initial camera had 1,600 pixels instrumented (out of the full 11,328) spanning a 2.7° field of view. Based on observations in 2020, the partially instrumented camera detected gamma-ray emission from the Crab Nebula at a significance of 8.6σ. The pSCT camera is undergoing an upgrade, both to improve its performance and to instrument the full 11,328 pixel camera. I will present the process and status of the camera upgrade.
Agostina Filócomo - "In search of evidence of flares in T Tauri stars as gamma-ray emitters"
Abstract
Abstract: NGC 2071 is a star-forming region positionally correlated with three unidentified gamma-ray sources detected by the Fermi satellite telescope. According to a preliminary model, T Tauri stars could produce gamma-ray emission under specific conditions. We performed a spectral and temporal analysis of the Fermi data to determine whether the detected emission was caused by flares occurring in T Tauri stars. We found that the gamma-ray source can only be detected in the first two years of observations at energies above 100 GeV. In addition, a variability analysis reveals that the expected frequency of events is compatible with flare activity with a minimum X-ray energy of 5 × 1037 erg. These observational results impose, for the first time, a substantial constraint on the energetic of flares in T Tauri stars that could explain the origin of unknown gamma-ray sources in star-forming regions.
Tuesday, June 4 Part 1
Ariel Perera - "Searching for Undetected Gamma Ray Bursts in Fermi GBM Data"
Abstract
Abstract: The recent discovery of simultaneous gravitational wave (GW) emission and short gamma-ray burst from a binary neutron star (BNS) merger has opened a new window to study such compact binary systems. The joint detection rate from this event is estimated at approximately 0.1 to 1.4 per year, with no other confirmed sources identified yet. In my research, I develop a GRB detection pipeline with rigorous statistical analysis to scan the Fermi GBM data, with the aim of increasing the search sensitivity. This will result in a larger number of known GRBs, and hence increased probability of another joint GRB-GW detection. This expectation is supported by a comparison of the detection probability of the pipeline and the significance of GBM triggering algorithm; our pipeline shows between 2 to 15 times higher signal-to-noise ratio, depending on source direction and intrinsic spectrum. Another feature of this pipeline is a statistical estimation of the location of the burst and discrimination between cosmological, terrestrial, and stellar origins. This allows for a robust classification of the signal, lowering the contamination of the sample. Our analysis includes operating the pipeline on ”time-slided” copies of the data, which allows exact significance assessment and pastro computation, akin to the state-of-the-art GW data analysis pipelines. This, along with a sky-map for the direction to the GRB, will facilitate a rigorous joint GW-GRB search on O3 and O4 LVK data.
Pádraig Mc Dermott - "Gamma ray detection with EIRSAT-1: Ireland’s first satellite!"
Abstract
Abstract: EIRSAT-1 is Ireland’s first satellite, it was developed by students in University College Dublin as a part of ESAs Fly your Satellite program. On December 1st 2023 EIRSAT-1 was launched into a Sun Synchronous Orbit from Vandenberg Space Base on a Space-X Falcon 9. It is a 2U CubeSat equipped with three payloads, one of which is GMOD; a gamma ray detecting module. GMOD uses a CeBr3 scintillator which produces flashes of light in the visible range when struck by gamma ray photons. The scintillations are measured with silicone photomultipliers (SiPMs) and read using an application specific integrated circuit (ASIC) known as SIPHRA. EIRSAT-1 is performing well in orbit and will soon be producing scientific data. This presentation will give an overview of the satellite subsystems with particular focus on the gamma ray detection module. The challenges faced in the lead up to launch and in the early operations phase will be presented. The results of the first few months of gamma ray detection with EIRSAT-1 will be discussed. Finally, the advantages and disadvantages of gamma ray detection with CubeSats will be presented using EIRSAT-1 as an example.
Marianna Dafčíková - "The First GRBAlpha and VZLUSAT-2 catalogue: gamma-ray transients and detector sensitivity"
Abstract
Abstract: In recent years there have been numerous efforts to build a constellation of small satellites which would provide an all-sky coverage and quick localization of gamma-ray bursts (GRBs). One of the mission proposals is the CAMELOT constellation with a newly developed gamma-ray detector composed of a CsI(Tl) scintillator coupled with silicon photomultipliers (SiPMs). The prototype of this detector is already employed in two space missions, GRBAlpha 1U CubeSat launched in March 2021 and VZLUSAT-2 3U CubeSat launched in January 2022. To date, the satellites have detected over 150 gamma-ray transients. In this presentation, I will show the first catalogue of the transients detected by these two missions and present the empirical sensitivity of the detector. The weakest GRB detection belongs to the faintest 10% of those observed by Fermi/GBM which demonstrates the detector potential for routine observation of GRBs.
Manuele Maistrello - "The dispersion of the 𝐸𝑝,𝑖− 𝐿𝑖𝑠𝑜 correlation of long gamma-ray bursts is partially due to assembling different sources"
Abstract
Abstract: Despite the prompt emission of gamma-ray bursts (GRBs) was discovered more than 50 years ago, there are still several aspects that need to be understood. One of them concerns some correlations that emerge when considering time-integrated spectra of long GRBs with known redshift. Specifically, it was found that the intrinsic peak energy, 𝐸𝑝,𝑖, of the 𝜐𝐹 𝜐 spectrum correlates with the isotropic-equivalent gamma-ray peak luminosity, 𝐿𝑝,𝑖𝑠𝑜. This correlation is also characterized by an intrinsic dispersion, 𝜎𝑖𝑛𝑡, whose origin is still unknown. Discovering the origin of the dispersion would give us insights about the radiative process (or processes) and dissipation mechanism at play, and would unlock the possibility of using GRBs as cosmological probes. Even if the 𝐸𝑝,𝑖− 𝐿𝑝,𝑖𝑠𝑜 correlation was discovered starting from time-integrated spectra of different GRBs, it was found that it holds within individual GRBs too, if the corresponding time-resolved quantities are considered, namely 𝐸𝑝,𝑖 and 𝐿𝑖𝑠𝑜. In this work, we focus on the time-resolved 𝐸𝑝,𝑖− 𝐿𝑖𝑠𝑜 correlation. The fact that the dispersion does not vanish within individual bursts is evidence that its origin cannot be entirely ascribed to properties that differ for each GRB. Yet, the question remains as to which extent the dispersion must be ascribed to the dissipation mechanism operating within individual bursts and what is, instead, due to assembling different sources. The aim of this work is to compare the values of the dispersion of individual GRBs with thedispersion of a whole sample of GRBs. In order to do so, we perform a time-resolved spectral analysis of 20 long GRBs detected by Fermi-GBM with known redshift and estimates of the jet opening angle, 𝜃 𝑗, and/or the Lorentz factor, Γ 0. In addition, we want to search for possible correlations between 𝜎𝑖𝑛𝑡, considered as a characteristic of individual bursts, and key observables related to the GRB physics, such as 𝜃 𝑗 and Γ 0.
Tuesday, June 4 Part 2
Rafael Diaz - "Studying VHE variability and flare for blazar B2 1811+31"
M Thunyapong Mahapol - "A Theoretical Fourier-Transformation Model for the Formation of X-ray Time Lags from Black Hole Accretion Disks"
Abstract
Abstract: The complex and rapidly varying X-ray emission from active galactic nuclei (AGNs) may provide insights to the thermal and dynamical structure of the central black hole accretion disk. To analyze the observed variability, X-ray time lags which are the temporal delays between Fourier transforms of light curves in hard and soft X-ray energy channels can be used. These time lags may be either hard lags or soft lags, depending on whether the variability in the hard energy channel follows that in the soft channel or vice versa. The source for the observed X-ray time lags from AGNs has been a subject of debate. In this study, we investigate the scenario where the X-ray time lags are generated by thermal and bulk Comptonization, as well as spatial reverberation of iron L-line and K-line seed photons, which are produced via fluorescence due to local instability. We model the inner region of the accretion flow as a hot, geometrically thick ADAF disc, with the outer radius equal to the shock formation radius located just outside the centrifugal barrier. Using a Fourier-transformed, vertically-averaged transport equation in cylindrical coordinates, we analyze the time-dependent radiative transfer in the inner ADAF region and simulate the X-ray time lag data. We then compare the simulated time lags to the observed time lags for model fitting. Our new model successfully reproduces the complex X-ray variability data for the Seyfert 1 galaxies 1H 0707-495 and Ark 564.
Aminabi Thekkoth - "Unprecedented Outburst in 4C 31.03: Exploring variability and multi-wavelength spectral properties."
Abstract
Abstract: The blazar 4C 31.03 has bee reported by Fermi-LAT for exhibiting a major 𝛾- ray outburst at the beginning of 2023 after a prolonged quiescent phase. We performed a comprehensive study of this extraordinary outbreak in temporal and multi-wavelength aspects. From the statistical analysis of the 𝛾gamma-ray lightcurves using Bayesian blocks, we identified 3 epochs of prominent flares. The variability analysis performed using a 12 hour binned 𝛾gamma-ray lightcurve resulted the shortest timescale of 5.453 hours. The highest energy of gamma-ray photons found from the source during the active phase is ∼ 82 GeV. Subsequently, using the transparency of gamma-rays against pair production and light crossing time argument, we could obtain the minimum jet Doppler factor as ∼ 17 and the upper limit on emission region size to be∼1016cm. The broadband spectral energy distribution study performed using synchrotron, SSC and EC emission processes supports the external Compton scattering of IR photons as the likely mechanism for the 𝛾gamma-ray emission from the source. The results of our analysis support the scenario of the emission site in 4C 31.03, being located beyond the Broad line region from the central black-hole. The long-term 𝛾gamma-ray flux distribution depicts a double log-normal variability, indicating that two distinct flux states are active in this energy band. The index distribution also reveals a two distinct variability pattern and hints that the 𝛾gamma-ray spectrum can be more precisely described by two photon indices.
Krishna Teja Vedula - "Study of Blazar Polarization in Gamma Rays with COSI"
Abstract
Abstract: The Compton Spectrometer and Imager (COSI) Mission, slated for launch in 2027 is focused on bridging the MeV gap in gamma-ray observations. COSI employs innovative polarimetric data collection methods using Compton scattering which puts it in a very unique position in addressing the challenging MeV range. The cutting-edge technology and analytical tools employed by COSI, including MEGAlib and Python-based frameworks which are being built on the same principles and frameworks as the Fermi Tools, underscore its potential to revolutionize the understanding of blazars, contributing to the elucidation of particle acceleration mechanisms, magnetic field order, and turbulence in extragalactic gamma-ray objects. Preliminary blazar analyses for COSI depend upon spectra from the Fermi mission.
Wednesday, June 5
Adithiya Dinesh - "A systematic search for extreme gamma-ray blazars using Fermi-LAT"
Abstract
Abstract: Blazars are active galactic nuclei with relativistic jets pointing towards our line of sight. These sources are the most powerful persistent gamma-ray emitters in the Universe, and can be classified by the frequency of their synchrotron peak emission from low to extreme synchrotron peak blazars at frequencies larger than 10 is an ongoing observational challenge in gamma-ray astrophysics. In this pioneering search, we will systematically look for the most extreme of these blazars, by finding a transition between a synchrotron peak and the inverse Compton region that could lie at the GeV energy range, where the Large Area Telescope on board the Fermi Gamma-ray Space Telescope is most sensitive. Our results will allows us to understand the recurrence, time-scales, and energetics of these events, which are expected to happen in flares, and their role in the blazar sequence.
Laenita De Jonge - "Study of the hadronic synchrotron mirror model for orphan flares in blazars - Application to 3C279"
Abstract
Abstract: Blazars are a class of Active Galactic Nuclei (AGN), found in the centres of elliptical galaxies, that are radio loud and have a small angle between the jet and the observer’s line of sight. In some cases, flaring events in one frequency band are not accompanied by flaring in other bands. Such events are called orphan flares. The causes of this variability and conditions in and location of the high energy emission region are not completely understood. As a possible explanation for rapid orphan gamma-ray variability, the hadronic synchrotron mirror model has been suggested in previous work. A TeV orphan flare was observed on the 28th of January 2018 by the H.E.S.S. observatory from 3C 279. A primary flare was observed 11 days earlier by Fermi-LAT. The hadronic synchrotron mirror model, is applied to this flare. A study is done using the SED and multi-wavelength light curve results to see which parameters provide the best fit and to draw conclusions about the radiation mechanism that caused this orphan flare. A search for neutrino emission is also conducted to establish if orphan flares are a possible source.
Paolo Cristarella Orestano - "Study of Periodicity in Blazar Light Curves"
Abstract
Abstract: Long term periodicity in gamma-ray Blazar light curves could be linked to the innermost zone of the complex structure of AGN, like possible presence of binary system of supermassive black holes, or it could shed light on the origin of gamma-rays emission. The work analyses 1525 sources, whose 14 years light curves come from the Fermi LAT Light Curve Repository (LCR), making use of Lomb-Scargle Periodogram (LSP) and wavelet weighted Z transform (WWZ), to express the significance we performed simulations using the Emmanoulopoulos algorithm. All the available possibilities for the light curves in the LCR, such as different temporal samplings and the use of photon flux and energy flux, are taken into account in order to ensure more reliable results. We found out high significance periodicity in less than 1% of the sources considered, and in few other sources hints of possible periodicity. Our results are compliant with the findings of recent literature focused on searches of periodic modulation in AGNs.
Olive Zhang - "Search for anisotropic pair halos associated with blazar jets"
Abstract
Abstract: Magnetic fields found in the galaxies are believed to grow from weaker “seed” fields whose origin is still unknown. The weaker “seed” fields might be preserved in the interstellar medium. However, its strength is too weak to be measured by traditional methods such as the Faraday rotation and Zeeman effect. Pair halos around the blazar jets might provide a way to measure the strength of the intergalactic magnetic field (IGMF). Because the IGMFs deflect the charged particles produced by TeV photons emitted by the blazars, extended GeV gamma-rays will develop around the projected jet direction. We propose to use Fermi-LAT data to look at certain high-synchrotron-peaked BL lacs (HBLs) and intermediate-synchrotron-peaked BL Lacs (IBLs) objects and search for any anisotropic pair halos.
Thursday, June 6
Eliza Neights - "Studying GRBs Using COSI"
Abstract
Abstract: Gamma-ray bursts (GRBs) are energetic phenomena that serve as probes for extreme physics, but their emission mechanisms, jet geometry, and magnetic field structure are not well understood and require new detection capabilities. The Compton Spectrometer and Imager (COSI) is a gamma-ray space telescope set to launch in 2027 that aims to further our understanding of GRBs, in addition to studying positron annihilation and nucleosynthesis in the Galaxy. COSI’s wide field-of-view, excellent energy resolution, sub-degree localizations, and polarization capabilities may reveal insight into GRB prompt emission. In this presentation, I will give a brief overview of the COSI mission and discuss the GRB science it enables.
Cuán de Barra - "GIFTS (Gamma-Ray Investigation of the Full Transient Sky)"
Abstract
Abstract: Gravitational waves were detected in 2015 for the first time. In 2017, gravitational waves from a binary neutron star merger were detected in coincidence with a gamma-ray burst (GRB) confirming that some short events are produced by mergers. The multi-messenger astrophysics era began, and the discovery highlighted the importance of space missions to detect and localise bursts at a time when gravitational wave systems are becoming more sensitive to merger events. Currently there is a lack of large future gamma-ray missions to enable similar measurements and scientific discovery. Consequently we propose to build Gamma-ray Investigation of the Full Transient Sky (GIFTS), a novel 6U CubeSat, which has been designed, prototyped and demonstrated previous work by the PI. The proposed design is based on detailed in-house instrument development and on the gamma-ray detector in the 2U CubeSat EIRSAT-1 which launched in 2023. GIFTS will comprise six gamma-ray detectors and will detect and localise 70 GRBs per year including 11 short GRBs. Detailed design and simulations demonstrate it will detect up to 2 GRBs per year coincident with GW detections. We will build and prepare GIFTS for operation when GW detectors reach peak sensitivity.
Zoe Brisson-Tsavoussis - 1-slide
Ieva Jankute - 1-slide
Group Photos
Supporting Material
- Primary announcements will be sent out via an e-mail list.
- Secondary announcements, interaction between sessions. instructor-student, and student-student communication will be handled via Slack. Instructions on joining the Summer School Slack will be sent to attendees by e-mail.
- This confluence page will be the home for the schedule as well as the presentation and supporting materials.
- There are a number of video tutorials for Fermi data analysis already available. You can also find tutorials posted on the FSSC's Data Analysis section.
- Presentation and material for Josh Wood's presentation on GRB analysis
Interesting repositories for Fermi analysis
Stay up-to-date with the gamma-ray sky
Additional Resources for gamma-ray astronomy and astrostatistics
Things to Do in Lewes
