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Cosmic Explosions 2019
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Rapport sur les
contributions
https://indico.in2p3.fr/e/17572Cosmic Explosio … / Rapport sur les contributions Bus Transfer Ajaccio Airport to C …
Contribution ID: 1 Type: not specified
Bus Transfer Ajaccio Airport to Cargese
We will provide a bus transfer from Ajaccio Airport to the school location in Cargese.
February 22, 2020 Page 1Cosmic Explosio … / Rapport sur les contributions Bus Transfer Ajaccio Airport to C …
Contribution ID: 2 Type: not specified
Bus Transfer Ajaccio Airport to Cargese
lundi 27 mai 2019 15:00 (1h 30m)
We will provide a bus transfer from Ajaccio Airport to the school location in Cargese on Monday
afternoon. It’s a small airport, so don’t worry: either you find us or we will find you.
February 22, 2020 Page 2Cosmic Explosio … / Rapport sur les contributions Registration & room distribution
Contribution ID: 3 Type: not specified
Registration & room distribution
lundi 27 mai 2019 16:30 (1h 30m)
Orateurs: GÖTZ, Diego (CEA Saclay); ACERO, Fabio (CEA/Saclay); KOSACK, Karl (CEA Saclay); BECK-
MANN, Volker (CNRS / IN2P3)
February 22, 2020 Page 3Cosmic Explosio … / Rapport sur les contributions Theory: Radiation Processes
Contribution ID: 4 Type: not specified
Theory: Radiation Processes
mardi 28 mai 2019 09:00 (1h 30m)
Orateur: Dr BELMONT, Renaud (IRAP)
February 22, 2020 Page 4Cosmic Explosio … / Rapport sur les contributions Theory: CRs & acceleration proces …
Contribution ID: 5 Type: not specified
Theory: CRs & acceleration processes
mardi 28 mai 2019 11:00 (1h 30m)
Orateur: Dr GABICI, Stefano
February 22, 2020 Page 5Cosmic Explosio … / Rapport sur les contributions Observation: Radio
Contribution ID: 6 Type: not specified
Observation: Radio
mardi 28 mai 2019 16:00 (45 minutes)
Orateur: BURGAY, Marta
February 22, 2020 Page 6Cosmic Explosio … / Rapport sur les contributions Observation: IR/optical
Contribution ID: 7 Type: not specified
Observation: IR/optical
mardi 28 mai 2019 16:45 (45 minutes)
Orateur: RIGAULT, Mickael (LPC)
February 22, 2020 Page 7Cosmic Explosio … / Rapport sur les contributions Objects: Supernovae
Contribution ID: 8 Type: not specified
Objects: Supernovae
mercredi 29 mai 2019 11:00 (1h 30m)
Orateur: VINK, Jacco (Anton Pannekoek Institute of Astronomy)
February 22, 2020 Page 8Cosmic Explosio … / Rapport sur les contributions Theory: relativity
Contribution ID: 9 Type: not specified
Theory: relativity
Orateur: DAIGNE, Frédéric (Institut d’Astrophysique de Paris - Université Pierre et Marie Curie)
February 22, 2020 Page 9Cosmic Explosio … / Rapport sur les contributions Theory: binarity in stellar evolution
Contribution ID: 10 Type: not specified
Theory: binarity in stellar evolution
Orateur: Dr LANGER, Norbert (AIfA)
February 22, 2020 Page 10Cosmic Explosio … / Rapport sur les contributions Theory: late stage of stellar evolution
Contribution ID: 11 Type: not specified
Theory: late stage of stellar evolution
mercredi 29 mai 2019 09:00 (1h 30m)
Orateur: LANGER, Norbert
February 22, 2020 Page 11Cosmic Explosio … / Rapport sur les contributions Supernova Remnants (SNRs)
Contribution ID: 12 Type: not specified
Supernova Remnants (SNRs)
mercredi 29 mai 2019 16:00 (1h 30m)
Orateur: VINK, Jacco (Anton Pannekoek Institute of Astronomy)
February 22, 2020 Page 12Cosmic Explosio … / Rapport sur les contributions Observation: Gamma-rays
Contribution ID: 13 Type: not specified
Observation: Gamma-rays
jeudi 30 mai 2019 09:45 (45 minutes)
Orateur: KOSACK, Karl (CEA Saclay)
February 22, 2020 Page 13Cosmic Explosio … / Rapport sur les contributions Observations: X-rays
Contribution ID: 14 Type: not specified
Observations: X-rays
jeudi 30 mai 2019 09:00 (45 minutes)
Orateur: GÖTZ, Diego (CEA Saclay)
February 22, 2020 Page 14Cosmic Explosio … / Rapport sur les contributions Objects: Gamma-Ray Bursts
Contribution ID: 15 Type: not specified
Objects: Gamma-Ray Bursts
jeudi 30 mai 2019 11:00 (1h 30m)
Orateur: DAIGNE, Frédéric (Institut d’Astrophysique de Paris - Université Pierre et Marie Curie)
February 22, 2020 Page 15Cosmic Explosio … / Rapport sur les contributions Lunch
Contribution ID: 16 Type: not specified
Lunch
February 22, 2020 Page 16Cosmic Explosio … / Rapport sur les contributions Observation: Neutrinos
Contribution ID: 17 Type: not specified
Observation: Neutrinos
jeudi 30 mai 2019 16:00 (45 minutes)
Orateur: VAN ELEWYCK, Véronique (APC)
February 22, 2020 Page 17Cosmic Explosio … / Rapport sur les contributions Observation: Gravitational Waves
Contribution ID: 18 Type: not specified
Observation: Gravitational Waves
jeudi 30 mai 2019 16:45 (45 minutes)
Orateur: LEROY, Nicolas (LAL IN2P3/CNRS)
February 22, 2020 Page 18Cosmic Explosio … / Rapport sur les contributions Theory: Accretion
Contribution ID: 19 Type: not specified
Theory: Accretion
vendredi 31 mai 2019 09:00 (1h 30m)
Orateur: DAIGNE, Frédéric (Institut d’Astrophysique de Paris - Université Pierre et Marie Curie)
February 22, 2020 Page 19Cosmic Explosio … / Rapport sur les contributions Objects: Black Holes
Contribution ID: 20 Type: not specified
Objects: Black Holes
vendredi 31 mai 2019 11:00 (1h 30m)
Orateur: Prof. MARKOFF, Sera (University of Amsterdam)
February 22, 2020 Page 20Cosmic Explosio … / Rapport sur les contributions Objects: Binaries
Contribution ID: 21 Type: not specified
Objects: Binaries
vendredi 31 mai 2019 16:00 (1h 30m)
Orateur: Prof. MARKOFF, Sera (University of Amsterdam)
February 22, 2020 Page 21Cosmic Explosio … / Rapport sur les contributions Projects: Introduction
Contribution ID: 22 Type: not specified
Projects: Introduction
samedi 1 juin 2019 11:00 (1h 30m)
Orateurs: ACERO, Fabio (CEA/Saclay); KOSACK, Karl (CEA Saclay); SCHANNE, Stéphane (CEA
Saclay); BECKMANN, Volker (CNRS / IN2P3)
February 22, 2020 Page 22Cosmic Explosio … / Rapport sur les contributions Projecs: From science requirement …
Contribution ID: 23 Type: not specified
Projecs: From science requirements to missions
samedi 1 juin 2019 09:00 (1h 30m)
Orateur: TRIOU, Henri (CEA/Saclay)
February 22, 2020 Page 23Cosmic Explosio … / Rapport sur les contributions Objects: Neutron Stars
Contribution ID: 24 Type: not specified
Objects: Neutron Stars
lundi 3 juin 2019 09:00 (1h 30m)
Orateur: BURGAY, Marta
February 22, 2020 Page 24Cosmic Explosio … / Rapport sur les contributions Objects: Coalescence
Contribution ID: 25 Type: not specified
Objects: Coalescence
mardi 4 juin 2019 09:00 (1h 30m)
Orateur: PORTER, Edward (APC / CNRS / IN2P3)
February 22, 2020 Page 25Cosmic Explosio … / Rapport sur les contributions Project: work
Contribution ID: 26 Type: not specified
Project: work
lundi 3 juin 2019 16:00 (1h 30m)
February 22, 2020 Page 26Cosmic Explosio … / Rapport sur les contributions Project: Work
Contribution ID: 27 Type: not specified
Project: Work
February 22, 2020 Page 27Cosmic Explosio … / Rapport sur les contributions Project: work
Contribution ID: 29 Type: not specified
Project: work
mardi 4 juin 2019 11:00 (1h 30m)
February 22, 2020 Page 28Cosmic Explosio … / Rapport sur les contributions Project: Work
Contribution ID: 30 Type: not specified
Project: Work
mardi 4 juin 2019 16:00 (1h 30m)
February 22, 2020 Page 29Cosmic Explosio … / Rapport sur les contributions Project: Work
Contribution ID: 31 Type: not specified
Project: Work
February 22, 2020 Page 30Cosmic Explosio … / Rapport sur les contributions Bus Transfer to Ajaccio Airport
Contribution ID: 32 Type: not specified
Bus Transfer to Ajaccio Airport
All aboard!
February 22, 2020 Page 31Cosmic Explosio … / Rapport sur les contributions Practical Session: ”How to apply f …
Contribution ID: 33 Type: not specified
Practical Session: ”How to apply for stuff?”
samedi 1 juin 2019 13:30 (1h 30m)
• Some initial thoughts on the whole process
• Strategy/resources
• Different kinds of positions and other general advice for job hunting strategy
• How to write a good application & deal with letters of recommendation
• Group discussion (the most important part!)
Orateur: Prof. MARKOFF, Sera (University of Amsterdam)
February 22, 2020 Page 32Cosmic Explosio … / Rapport sur les contributions Practical Sessions
Contribution ID: 34 Type: not specified
Practical Sessions
lundi 3 juin 2019 11:00 (1h 30m)
February 22, 2020 Page 33Cosmic Explosio … / Rapport sur les contributions H. Abdalla: LIV Signatures in EBL …
Contribution ID: 35 Type: not specified
H. Abdalla: LIV Signatures in EBL absorption and
Compton scattering
mercredi 29 mai 2019 18:00 (10 minutes)
At energies approaching the Planck energy scale 1E19 GeV, several quantum-gravity theories pre-
dict that familiar concepts such as Lorentz (LIV) symmetry can be broken. Such extreme energies
are currently unreachable by experiments on Earth, but for photons traveling over cosmologi-
cal distances the accumulated deviations from the Lorentz symmetry may be measurable using
the Cherenkov Telescope Array (CTA). To study the spectral hardening feature observed in some
VHE gamma-ray blazars, we calculate the reduction of the EBL gamma-gamma opacity due to the
existence of underdense regions along the line of sight to VHE -gamma ray sources and we com-
pared with the possibility of a LIV signature. Considering the LIV effect, we found that the cosmic
opacity for VHE-gamma rays with energy more than 10 TeV can be strongly reduced. I will further
discuss the impact of LIV on the Compton scattering process, and how future CTA observations
may open an exciting window on studies of the fundamental physics.
Session Classification: Students’ presentations
February 22, 2020 Page 34Cosmic Explosio … / Rapport sur les contributions D. R. Aguilera-Dena: Pre- …
Contribution ID: 36 Type: not specified
D. R. Aguilera-Dena: Pre-explosion Core Properties
of Superluminous Supernova and Long Gamma-Ray
Burst Progenitors
mercredi 29 mai 2019 18:15 (10 minutes)
Modeling the evolution and mass loss history of rapidly rotating massive stars at low metallicity,
we found that chemically homogeneously evolving stars with enhanced rotational mixing could be
suitable candidates for both SLSNe in the magnetar-driven scenario and for lGRBs in the collapsar
scenario. They retain a high angular momentum in their cores, enough to power these types of
explosions, and have masses, abundances and magnetic fields that could also be consistent with
observations of SLSNe and the hypernovae associated with lGRBs; particularly reproducing the
observed the lack of He in their envelopes. The outcome of core collapse is determined by whether
core collapse results in the formation of a fast spinning neutron star or a black hole. We analyze the
evolution of these progenitors, as well as the parameter space where NS formation might favored
over BH formation, and properties of their cores and of their CSM at core collapse.
Orateur: AGUILERA DENA, David Ramon (Argelander Institut für Astronomie)
Session Classification: Students’ presentations
February 22, 2020 Page 35Cosmic Explosio … / Rapport sur les contributions E. Balakina: Peculiar velocities of …
Contribution ID: 37 Type: not specified
E. Balakina: Peculiar velocities of Type Ia
Supernovae in clusters of galaxies
mercredi 29 mai 2019 18:30 (10 minutes)
Type Ia supernovae (SNe) are excellent distance indicators. Observations of distant SNe Ia led to
the discovery of the accelerating expansion of the Universe. The most recent analysis of SNe Ia
indicates that considering a flat ΛCDM cosmology, the contribution of dark energy in the total
density of the Universe is ∼ 70%. Cosmological parameters are estimated from the “luminosity
distance-redshift” relation of SNe using the Hubble diagrams. Currently a lot of attention is paid
to standardization of SNe, i.e. to increase of the accuracy of luminosity distance determination.
The uncertainty on the redshift is quite often considered negligible. The redshift used in “luminos-
ity distance-redshift” relation is a cosmological redshift, i.e. the redshift due to the expansion of
the Universe. In fact the redshift observed on the Earth also includes the contribution from the
unknown peculiar velocities. To minimize the influence of poorly constrained peculiar velocities,
in cosmological analyses a standard value of 300-400 km/s peculiar velocity dispersion is added in
quadrature to the redshift uncertainty. It has nonetheless been observed that velocity dispersion
can exceed 1000 km/s in galaxy clusters and therefore, the dispersion inside the cluster can be
greater than the one usually assumed in cosmological analyses and can affect the distance mea-
surements. To take this effect into account we study SNe Ia that are exploded in the galaxy clusters.
As a supernova sample we use ”Pantheon” — the largest combined sample of SN Ia (HST, SNLS,
SDSS, low-z samples and Pan-STARRS1) consisting of a total of 1048 objects ranging from 0.01 <
z < 2.3. For those SNe Ia that belong to the galaxy clusters we are going to use the galaxy cluster
redshift instead of the host galaxy redshift and examine the effect of this correction on the Hubble
diagram.
In the epoch of large transient surveys (such as LSST), a study of the second order effects and all
possible sources of systematical uncertainties in the cosmological analysis is of high priority.
Session Classification: Students’ presentations
February 22, 2020 Page 36Cosmic Explosio … / Rapport sur les contributions M. Breuhaus: Further support for …
Contribution ID: 38 Type: not specified
M. Breuhaus: Further support for a hadronic origin
for the γ-ray emission from η Carinae
η Carinae is a unique laboratory in which to study particle acceleration to high energies under
a wide range of conditions, including extremely high densities around periastron. So far no con-
sensus has emerged in the origin of the GeV γ-ray emission in this important system. With a
re-analysis of the full Fermi-LAT data set for η Carinae, we show that the spectrum is consistent
with a pion decay spectrum and not with a broken power law connecting to the X-ray emission
as has been claimed. We show with a simple physical model that pion-decay emission is the most
likely origin of all of the γ-ray emission, with inverse Compton emission from primary electrons
dominating the hard X-ray emission detected with NuSTAR at most phases. Very close to perias-
tron it seems possible that secondary electrons interacting away from the shock cap dominate the
emission. Future observations with H.E.S.S., CTA and NuSTAR should enable this scenario to be
further constrained.
Session Classification: Students’ presentations
February 22, 2020 Page 37Cosmic Explosio … / Rapport sur les contributions M. Bugli: The role of magnetic field …
Contribution ID: 39 Type: not specified
M. Bugli: The role of magnetic field topology in
core-collapse supernovae
mercredi 29 mai 2019 18:45 (10 minutes)
The characteristics of the initial magnetic field present in a supernova progenitor prior to collapse
and the dynamics of the field amplification due to different dynamo mechanisms (such as MRI,
convective motions, etc.) are to this date quite uncertain.
We investigate the effects of multipolar magnetic field topologies of different radial extents on
the dynamics of core-collapse supernovae and the properties of the forming proto-neutron star
(PNS). Using axisymmetric relativistic MHD simulations, we find that higher multipolar magnetic
configurations lead to generally less energetic explosions, with the central PNS increasing its spin
and becoming more massive. Models with a low order multipolar configuration tend to produce
more oblate PNS which in some cases are surrounded by a rotationally supported toroidal structure.
This change is the PNS shape can be directly associated with higher neutrino luminosities along
the equatorial plane but smaller along the poles.
Orateur: BUGLI, Matteo (CEA - Saclay)
Session Classification: Students’ presentations
February 22, 2020 Page 38Cosmic Explosio … / Rapport sur les contributions T. Bylund: Blazar observations wit …
Contribution ID: 40 Type: not specified
T. Bylund: Blazar observations with the HESS
telescope
jeudi 30 mai 2019 18:00 (10 minutes)
Imaging Atmospheric Cherenkov Telescopes (IACT) are among the most sensitive instruments
available to study the very high energy non-thermal sky, and the High Energy Stereoscopic System
(HESS) is the largest such system operating in the world. This makes HESS an excellent tool for
probing the extreme environment of Blazar jets. In this talk I will give a brief introduction to the
principles behind IACT’s, recent Blazar studies done by HESS, and report some preliminary results
on very distant BL Lac.
Session Classification: Students’ presentations
February 22, 2020 Page 39Cosmic Explosio … / Rapport sur les contributions M. Cardillo: CR and SNR love story …
Contribution ID: 41 Type: not specified
M. Cardillo: CR and SNR love story and
re-acceleration between them
jeudi 30 mai 2019 18:10 (10 minutes)
In the last years, the improvement of performances of high-energy instruments, both from Earth
and Space, has provided a great amount of data relating to Cosmic-Rays (CRs). In particular, in the
gamma-ray band, we had the first evidence of CR energization at the Supernova Remnant (SNR)
shocks. Several models were developed, assuming that the emission was due to freshly accelerated
CRs, in order to isolate the hadronic component from the leptonic one and to find the first direct
proof of CR acceleration at a SNR shock. Because of some spectral features in disagreement with
the Diffusive Shock Acceleration (DSA) theory, however, the role of pre-existing CR re-acceleration
was taken into account, finding that not only its contribution is not negligible but also that it could
explain some important characteristic of CR particle and gamma-ray spectra. Here we briefly
summarize the main results obtained in the study of CR re-acceleration, showing its fundamental
contribution in the middle-aged SNR shocks and, likely, in the forward shock (FS) of stellar winds.
Our aim is to fix the importance of re-energization of pre-existing CRs in the Galaxy and the need
to consider it in the explanation of detected CR particle and gamma-ray spectra.
Orateur: CARDILLO, Martina (INAF-Osservatorio astronomico di Arcetri)
Session Classification: Students’ presentations
February 22, 2020 Page 40Cosmic Explosio … / Rapport sur les contributions F. Carotenuto: The new black hole …
Contribution ID: 42 Type: not specified
F. Carotenuto: The new black hole transient MAXI
J1348-630 observed through MeerKAT’s eyes
vendredi 31 mai 2019 18:00 (10 minutes)
The very bright transient MAXI J1348-630 was discovered in X-rays by MAXI in January 2019 and
was then detected also in radio and optical. Immediately after its discovery, it was classified as a
black hole candidate based on its X-ray behaviour.
We present an intense radio monitoring of the transient at 1.284 GHz with the new MeerKAT radio
interferometer (64 antennas) located in the Karoo desert in South Africa, as part of the ThunderKAT
Large Survey Programme. All typical X-ray spectral states have been observed. A strong radio flare
(likely associated with an ejection event) was detected coincidently with a transition from the hard
to the soft accretion state, as inferred from Swift and INTEGRAL observations. We discuss the
overall behaviour of this binary during its outburst, along with results from the multi-wavelength
campaign.
Orateur: CAROTENUTO, Francesco (Université de Paris, CEA/Saclay-Irfu/Dap/AIM)
Session Classification: Students’ presentations
February 22, 2020 Page 41Cosmic Explosio … / Rapport sur les contributions S. Chakraborty: Jet inclination rel …
Contribution ID: 43 Type: not specified
S. Chakraborty: Jet inclination relative to the black
hole spin for the TDE Swift J1644+57
jeudi 30 mai 2019 18:25 (10 minutes)
An estimate of the jet inclination relative to the accreting black hole’s spin can be useful to probe
the jet triggering mechanism and the disc-jet coupling. Tidal Disruption Event (TDE) of a star
by a supermassive spinning black hole provides a unique astrophysical laboratory to study the
jet direction through the possibility of jet precession, induced by the Lense-Thirring precession
of the disc or by other mechanisms. In this work, we investigate the Swift XRT light curve of a
well-sampled jetted TDE, Swift J1644+57. We use a new method to compare some useful aspects
of the dips of this X-ray light curve with our jet precession model to find an upper limit of the jet
inclination angle. This method does not require a known jet precession period and works even if
many dips are not due to jet precession. Employing this method for the thick disc regime of the
X-ray light curve, we conclude that the jet inclination with respect to the black hole spin axis, or
the black hole spin-precession axis if the spin axis precesses, is likely less than 10 degrees for Swift
J1644+57. We will then discuss its effect on the stellar dynamics near the supermassive black hole.
Orateur: CHAKRABORTY, Sudip (Tata Institute of Fundamental Research, Mumbai, India)
Session Classification: Students’ presentations
February 22, 2020 Page 42Cosmic Explosio … / Rapport sur les contributions S. Ciprini: The binary supermassiv …
Contribution ID: 44 Type: not specified
S. Ciprini: The binary supermassive black hole
conjecture for two jetted gamma-ray blazars
The study of astrophysical accretion phenomenon and binary systems is undoubtedly useful to bet-
ter understand the role of gravitation in producing high-energy, X-ray and gamma-ray, emission.
In particular close gravitationally bound binaries of supermassive black holes (SMBHs) in some ac-
tive galactic nuclei and blazars are expected to induce cyclical modulations in the observed flux. In
the past years, two jetted gamma-ray blazars have been suggested to harbour binary SMBHs: i.e.,
OJ 287 and PG 1553+113. I will introduce these two peculiar blazars, and present recent achieve-
ments made possible thanks to 10-year continuous monitoring observations of their GeV gamma-
ray emission by the Fermi Large Area Telescope. In addition data collected thanks to dedicated
observations by the Swift, Kepler and Spitzer space telescopes will be also presented.
Session Classification: Students’ presentations
February 22, 2020 Page 43Cosmic Explosio … / Rapport sur les contributions F. Conte: Development of a Comp …
Contribution ID: 45 Type: not specified
F. Conte: Development of a Compact High-Energy
Camera for the Cherenkov Telescope Array
jeudi 30 mai 2019 18:40 (10 minutes)
The Cherenkov Telescope Array (CTA) project is a next generation observatory for Very-High
Energy gamma-ray astronomy. Two sites, in the northern and in the southern emisphere, have
already been officially announced by the CTA consortium and will constitute the world largest
detector for gamma rays. To push the energy sensitivity in the range of hundreds of TeV, about
70 small-sized telescopes (SSTs) will be deployed in the southern hemisphere, covering an area of
about four square kilometers. Here I present the development status of the Compact High-Energy
Camera (CHEC), the camera designed for SST-2M GCT (one of the proposed SST prototypes). It
focuses on the higher-end of CTA energy range and thanks to the use of dual-mirror optics CHEC
can be very compact and low-cost, despite a precision of 10 arcmin and a field of view of 8 degrees,
providing an unprecedented sensitivity and angular resolution with respect to any existing Imag-
ing Atmospheric Cherenkov Telescopes (IACTs). The camera contains 2048 pixels with a physical
size of 6×6 mm 2 . It relies on electronics based on TARGET (TeV Array Readout with GSa/s sam-
pling and Event Trigger) Application-Specific Integrated Circuits (ASICs) and Field Programmable
Gate Arrays (FPGAs) allowing a continuous sampling of the full waveform with the precision
of 1 ns. CHEC-S, the current prototype, features silicon photomultipliers (SiPM) which provide
many advantages over classical photomultiplier tubes (PMTs), and even over multi-anode PMTs
as proven with the first prototype, CHEC-M. This contribution is meant to give an overview on
CHEC-S design and status, showing in particular how it answers the peculiar needs of Cherenkov
ground-based gamma-ray detection, which requires a completely different approach with respect
to IR/optical detection. Finally, latest results from laboratory measurements and calibrations are
presented.
Orateur: CONTE, Francesco (Max-Planck-Institut für Kernphysik)
Session Classification: Students’ presentations
February 22, 2020 Page 44Cosmic Explosio … / Rapport sur les contributions J. Jacquemin Ide: Magnetically- …
Contribution ID: 46 Type: not specified
J. Jacquemin Ide: Magnetically-driven jets and winds
from MRI-active accretion disks
vendredi 31 mai 2019 18:30 (10 minutes)
Semi-analytical models of disk outflows have successfully described magnetically-driven, self-
confined super-Alfvenic jets from near Keplerian accretion disks (Ferreira 1997). These Jet Emitting
disks (JED) are possible for high levels of magnetization, close to the equipartition, leading to su-
personic accretion and deeply affecting the emitted spectrum (see eg. Marcel et al 2018). However,
these solutions prove difficult to compare with cutting edge numerical simulations, for the reason
that numerical simulations show wind-like outflows but in the domain of small magnetization. In
this work, we present for the first time self-similar solutions for accretion-ejection structures at
small magnetization. We will elucidate the role of the magneto-rotational instability in the accel-
eration processes that drive this new type of solutions. The generalized parameter space and the
astrophysical consequences will then be discussed. We believe that these new solutions could be
a stepping stone in understanding the way astrophysical disks drive either winds or jets.
Session Classification: Students’ presentations
February 22, 2020 Page 45Cosmic Explosio … / Rapport sur les contributions R. Diesing: On the spectrum of ele …
Contribution ID: 47 Type: not specified
R. Diesing: On the spectrum of electrons accelerated
in supernova remnants
vendredi 31 mai 2019 18:10 (10 minutes)
Using a semi-analytic model of non-linear diffusive shock acceleration, we model the spectrum
of cosmic ray (CR) electrons accelerated by supernova remnants (SNRs). Because electrons ex-
perience synchrotron losses in the amplified magnetic fields characteristic of SNRs, they exhibit
substantially steeper spectra than protons. In particular, we find that the difference between the
electron and proton spectral index (power law slope) ranges from 0.1 to 0.4. Our findings must be
reckoned with in theories of Galactic CR transport and may especially have implications for the
observed “positron excess.”
Session Classification: Students’ presentations
February 22, 2020 Page 46Cosmic Explosio … / Rapport sur les contributions R. Duque: Prospects for Electroma …
Contribution ID: 48 Type: not specified
R. Duque: Prospects for Electromagnetic
Counterparts to Neutron Star Mergers in the
Gravitational Wave Era
vendredi 31 mai 2019 18:20 (10 minutes)
The binary neutron star inspiral signal GW170817 was a historical event and inaugurated the era
of multi-messenger astronomy with gravitational waves. It was accompanied by electromagnetic
counterparts, namely a kilonova, a weak and short gamma-ray burst and a long-lasting multi-
wavelength afterglow. Altogether, these brought a wealth of information on the unraveling of the
merger and strengthened the link between neutron star mergers and the short gamma-ray bursts.
During the next science runs of the gravitational interferometer network, more such electromag-
netic counterparts are expected. This talk will concern the population of mergers we expect to
detect jointly in the gravitational wave and electromagnetic domains. We couple population meth-
ods to jet induced afterglow and kilonova models to describe the population of these counterparts
to come. This allows us to explore the new insights they will provide on the formation of neu-
tron star binaries, the environments of their mergers, the geometry of the ejectas therein and the
physics of short gamma-ray bursts.
Session Classification: Students’ presentations
February 22, 2020 Page 47Cosmic Explosio … / Rapport sur les contributions I. El Mellah: Enhanced accretion a …
Contribution ID: 49 Type: not specified
I. El Mellah: Enhanced accretion and wind-captured
discs in high mass X-ray binaries
vendredi 31 mai 2019 18:45 (10 minutes)
The historical gravitational wave detections of last years ushered in a new era for the study of mas-
sive binaries evolution. In high mass X-ray binaries, a transient albeit decisive phase preceding
compact binaries, a compact accretor orbits a massive star and captures part of its intense stellar
wind. From the stellar photosphere down to the vicinity of the compact object, the flow under-
goes successive phases. Our numerical simulations offer a comprehensive picture of the accretion
process along this journey. They unveil complex and highly variable geometries produced by the
wind beamed towards the accretor. Overdense small scale regions in the wind produce stochas-
tic variability but also trigger instabilities at the outer rim of the neutron star magnetosphere or
around the black hole, depending on the nature of the accretor. For wind speeds of the order of the
orbital speed, accretion is significantly enhanced and provided cooling is accounted for, transient
disc-like structures form, with dramatic consequences on the torques applied to the compact object.
The recent observational reports on the limited extent of the accretion disc in Cygnus X-1 suggest
that the disc is produced by this mechanism rather than a Roche lobe overflow of the companion
star. We will also discuss the consequences for Vela X-1 and the coupling between the flow and
the neutron star magnetosphere.
Session Classification: Students’ presentations
February 22, 2020 Page 48Cosmic Explosio … / Rapport sur les contributions J. Jacquemin Ide: Magnetically- …
Contribution ID: 50 Type: not specified
J. Jacquemin Ide: Magnetically-driven jets and winds
from MRI-active accretion disks
Semi-analytical models of disk outflows have successfully described magnetically-driven, self-
confined super-Alfvenic jets from near Keplerian accretion disks (Ferreira 1997). These Jet Emitting
disks (JED) are possible for high levels of magnetization, close to the equipartition, leading to su-
personic accretion and deeply affecting the emitted spectrum (see eg. Marcel et al 2018). However,
these solutions prove difficult to compare with cutting edge numerical simulations, for the reason
that numerical simulations show wind-like outflows but in the domain of small magnetization. In
this work, we present for the first time self-similar solutions for accretion-ejection structures at
small magnetization. We will elucidate the role of the magneto-rotational instability in the accel-
eration processes that drive this new type of solutions. The generalized parameter space and the
astrophysical consequences will then be discussed. We believe that these new solutions could be
a stepping stone in understanding the way astrophysical disks drive either winds or jets.
Session Classification: Students’ presentations
February 22, 2020 Page 49Cosmic Explosio … / Rapport sur les contributions S. Lescaudron: Black holes spin ev …
Contribution ID: 51 Type: not specified
S. Lescaudron: Black holes spin evolution in merging
galaxies
lundi 3 juin 2019 18:00 (10 minutes)
Most of the galaxies host a supermassive BH in their centre and we observe a co-evolution of the
galaxy and its central BH. The BH is expected to have a key role in the regulation of the quantity
of gas and stars : it accretes matter from its surrounding and releases a fraction of this rest-mass
energy into the host galaxy, providing “feedback”. The BH angular momentum or spin directly
influences the fraction of energy released and radiated during accretion events. On the other hand
galaxy mergers have a crucial role in triggering peaks of central BH activity, allowing strong gas
accretion. The spin of the BH changes with the combination of gas accretion and the possible
coalescence of BHs. Models of spin evolution during BHs merger will allow gravitational waves
predictions. In this context, I performed idealised simulations of galaxy mergers including mass
and spin evolution of supermassive black holes, using Ramses, an hydrodynamical and N-body
code with adaptive mesh refinement developed by Romain Teyssier (2002). These simulations are
run for different configurations of the angular momentum orientation of the galaxies, varying the
angle between the galactic angular momenta and the orbital angular momentum. The orbital con-
figuration influences the BHs encounter history, mass growth and spin evolution, which happen
either on the primary or on the secondary BH.
Session Classification: Students’ presentations
February 22, 2020 Page 50Cosmic Explosio … / Rapport sur les contributions S. Mate: Simulation and Optimisat …
Contribution ID: 52 Type: not specified
S. Mate: Simulation and Optimisation of Space
Gamma-ray Camera SVOM/ECLAIRs : Detecting
Gamma Ray Bursts and High Energy Transients
lundi 3 juin 2019 18:20 (10 minutes)
The Space Variable Object Monitor (SVOM) is a Chinese-French astrophysics mission for the study
of high-energy transients, in particular Gamma-Ray Bursts. One of the key instrument on SVOM is
the ECLAIRs gamma-ray camera which is a large field of view (FoV) coded mask imager working in
the energy range of 4 -150 keV. The primary focus of the instrument is to detect and localize new
GRBs with help of onboard trigger software (in near real-time). Due to limitations on onboard
computing power, the onboard trigger uses conservative methods. Hence, an important part of
the program is to develop a software tools to detect GRBs on ground with more elaborate methods.
This is possible because all the detected photon events will be sent to the ground. The ground
search will be used in parallel to the onboard software (to detect longer timescale / faint GRBs)
as well as a substitute when the onboard trigger is switched off due to technical constraints. I’ll
will give a brief overview of SVOM mission in general and my PhD work which concerns the
development of these ground tools. I’ll cover different aspects of the work such as simulation of
raw data to create near real observing scenarios (with background, non-transient X-ray sources
and GRB events) and the methods we are working on to detect the GRBs in this data.
Orateur: MATE, Sujay (IRAP)
Session Classification: Students’ presentations
February 22, 2020 Page 51Cosmic Explosio … / Rapport sur les contributions A. Mohapatra: Physical conditions …
Contribution ID: 53 Type: not specified
A. Mohapatra: Physical conditions in high-z CIII
absorbers: origin and stability
lundi 3 juin 2019 18:30 (10 minutes)
In this talk, I will present detailed photoionization models of well-aligned optically thin doubly
ionized carbon (C III) absorption components at 2.1 ≤ z ≤ 3.4. Our inferred density and overdensity
(∆) favor the absorption originating from gas associated with circumgalactic medium and probably
not in hydrostatic equilibrium. We discuss statistically significant redshift evolution of our derived
parameters. We show L vs. [C/H] can be well reproduced if L is governed by the product of gas
cooling time and sound crossing speed as expected in the case of cloud formation under thermal
instabilities. As noted in the literature survivability of such cloud over longer time-scale is an issue.
Therefore, studying the optically thin C III absorbers over a large z range and probably correlating
their z evolution with global star formation rate density evolution can shed light to the physics of
circumgalactic medium formation and evolution.
Orateur: MOHAPATRA, Abhishek (NIT Rourkela, India)
Session Classification: Students’ presentations
February 22, 2020 Page 52Cosmic Explosio … / Rapport sur les contributions J. Muller: Airborne inter- …
Contribution ID: 54 Type: not specified
J. Muller: Airborne inter-calibration of H.E.S.S.
telescopes
lundi 3 juin 2019 18:40 (10 minutes)
Cherenkov telescope arrays such as H.E.S.S. or the planned future CTA are systems of imaging
atmospheric Cherenkov telescopes. They detect high energy photons above 10GeV (gamma-rays)
from cosmic sources based on the Cherenkov emission of charged particles produced when these
photons enter the atmosphere. They need to be calibrated to be able to compare and combine
the measurements of the different telescopes. So far this has been done with atmospheric muons
as the expected energy distribution of atmospheric muons can be well deduced from simulations.
This method has numerous drawbacks, such as the impossibility of a wavelength dependent inter-
calibration, which is needed for future high precision arrays such as CTA. I will talk about the first
single light source inter-calibration of a Cherenkov telescope array which was performed with an
LED mounted on a drone. To do this, first simulations of the situation have been run and then the
actual drone flights were operated above H.E.S.S. The inter-calibration with the data taken during
these flights was consistent within about 5% with the muon inter-calibration. This result could
even be improved by ameliorating, among other, the treatment of the drone-telescope distance,
the atmospheric absorption and the pixel boundaries.
Orateur: MULLER, Jacques
Session Classification: Students’ presentations
February 22, 2020 Page 53Cosmic Explosio … / Rapport sur les contributions T. Müller: PISCoLA: Python for In …
Contribution ID: 56 Type: not specified
T. Müller: PISCoLA: Python for Interactive
Supernova Cosmology Light-curve Analysis
mardi 4 juin 2019 18:00 (10 minutes)
Type Ia Supernovae (SNe Ia) have been studied for many years as standardisable candles for cos-
mological distance measurement. In addition, these objects have shown to be standard candles
in the Infrared (IR), where they are less affected by extinction, probing to be exceptional for cos-
mology. With the large number of on-going (e.g., ZTF, ATLAS, VEILS) and future surveys (e.g.,
LSST), both in the Optical and IR, the samples of SNe Ia is rapidly increasing. However, we need
not to focus only on the size of the samples, but also on how we analyse these data. Cosmology
with SNe Ia usually relies on templates for the light curve fits, which introduces biases due to the
underlying assumptions. For this reason we created “Python for Interactive Supernova Cosmol-
ogy Light-curve Analysis” (PISCoLA), a new light curve fitting tool. PISCoLA relies on Gaussian
Process, a non-parametric data-drive method, letting the data “speak” for itself. We analyse the
multi-color light curves with machine learning techniques to search for new parameters for the
standardisation of SNe Ia and further understanding of the physics behind these explosions.
Orateur: MÜLLER BRAVO, Tomas (University of Southampton)
Session Classification: Students’ presentations
February 22, 2020 Page 54Cosmic Explosio … / Rapport sur les contributions M. Palla: GRB hosts identification …
Contribution ID: 57 Type: not specified
M. Palla: GRB hosts identification through chemical
abundances
mardi 4 juin 2019 18:10 (10 minutes)
We try to identify the nature of high redshift long Gamma-Ray Bursts (LGRBs) host galaxies by
comparing the observed abundance ratios in the interstellar medium with detailed chemical evo-
lution models accounting for the presence of dust. What we have done is to compare abundance
data from LGRB afterglow spectra to abundance patterns as predicted by our models for different
galaxy types (irregulars, spirals, ellipticals) . We analysed in particular [X/Fe] abundance ratios
as functions of [Fe/H]. Different galaxies are, in fact, characterised by different star formation his-
tories, which produce different [X/Fe] ratios (“time-delay model”). This allows us to identify the
morphology of the hosts and to infer their age (i.e. the time elapsed from the beginning of star for-
mation) at the time of the GRB events. Relative to previous works, we use newer models in which
we adopt updated stellar yields and prescriptions for dust production, accretion and destruction.
In the sample considered we found host galaxies of all the morphological types. The calculated
ages of the host galaxies span from the order of 10 Myr to little more than 1 Gyr.
Orateur: PALLA, Marco (Università degli Studi di Trieste)
Session Classification: Students’ presentations
February 22, 2020 Page 55Cosmic Explosio … / Rapport sur les contributions A. Reboul-Salze: A global model of …
Contribution ID: 58 Type: not specified
A. Reboul-Salze: A global model of the
magnetorotational instability in proto-neutron stars
mardi 4 juin 2019 18:20 (10 minutes)
The magnetorotational instability (MRI) is considered to be a promising mechanism to amplify
the magnetic field in fast-rotating protoneutron stars. Many local studies have proven that the
magnetic field could be amplified on small scales. But to explain the dipolar magnetic field strength
of the magnetars (10¹⁴-10¹⁵ G), a large scale magnetic field needs to be generated by the MRI. To
study this question, a three dimensional pseudo-spectral code has been used to develop a global
model of the MRI in a proto-neutron star. The hypothesis of an incompressible fluid allow us to
simplify at maximum the model. We compare the turbulence in the global model and in local
simulations. We also show that a strength of the dipolar magnetic field consistent with the values
of magnetar’s strong fields can be generated by the MRI, even though it is lower than the small
scale magnetic field. Overall, the results presented in this talk support the ability of the MRI to
form magnetar-like large scale magnetic fields.
Orateur: REBOUL-SALZE, Alexis (CEA Saclay)
Session Classification: Students’ presentations
February 22, 2020 Page 56Cosmic Explosio … / Rapport sur les contributions P. Saikia: Lorentz factors of compa …
Contribution ID: 59 Type: not specified
P. Saikia: Lorentz factors of compact jets in black
hole X-ray binaries
mardi 4 juin 2019 18:30 (10 minutes)
Compact, continuously launched jets in black hole X-ray binaries (BHXBs) produce radio to optical–
infrared (OIR) synchrotron emission. These jets are launched in the hard X-ray state, and are
quenched in the soft state. They are not spatially resolved except in a few cases using VLBI radio
observations. One of the basic properties of these jets is the bulk Lorentz factor, which defines how
fast and how relativistic these jets are. The bulk Lorentz factor is notoriously difficult to measure,
with to date only weak constraints for a few BHXBs. Here, we adopt simple models to constrain
the Lorentz factor of the compact jets in several BHXBs using the amplitude of the jet fade and re-
covery at infrared (IR) wavelengths over state transitions. We investigate why some BHXBs have
prominent IR excesses and some do not, quantified by the amplitude of the IR quenching or recov-
ery over the transition from/to the hard state. Using the amplitude of the IR fade/recovery, known
orbital parameters and simple analytical models, we constrain for the first time the Lorentz factor
of compact jets in several BHXBs. We also find that the very high amplitude IR fade/recovery
seen repeatedly in GX 339–4 requires a much lower inclination angle than previously expected.
Our results are strongly supportive of the IR excess being produced by synchrotron emission in
a relativistic outflow, and demonstrates how useful OIR monitoring of BHXB is for studying jet
properties.
Orateur: SAIKIA, Payaswini (Nyuad)
Session Classification: Students’ presentations
February 22, 2020 Page 57Cosmic Explosio … / Rapport sur les contributions F. Samuelsson: The problematic co …
Contribution ID: 60 Type: not specified
F. Samuelsson: The problematic connection between
gamma-ray bursts (GRBs) and ultra-high energy
cosmic rays (UHECR)
mardi 4 juin 2019 18:40 (10 minutes)
The acceleration site for UHECR is still an open question despite extended research and GRBs
are considered one of the most promising source candidates. Under the likely assumption that
electrons are also accelerated at the UHECR acceleration site, synchrotron emission from these
co-accelerated electrons is inevitable. We characterize this synchrotron emission and compare it
to observed GRB spectra and find that for standard parameters, the synchrotron flux from these
electrons would be much too luminous. This result challenges both high- and low-luminosity GRBs
as accelerators of UHECR.
Orateur: SAMUELSSON, Filip (KTH Royal Institute of Technology)
Session Classification: Students’ presentations
February 22, 2020 Page 58Cosmic Explosio … / Rapport sur les contributions M. Senniappan: Signal over Backg …
Contribution ID: 61 Type: not specified
M. Senniappan: Signal over Background
discrimination for the ALTO observatory
mardi 28 mai 2019 18:20 (10 minutes)
ALTO is a future ground-based very high energy gamma-ray observatory based on water Cherenkov
technique, which samples the secondary particles produced in the extensive air showers. This
technique also provides long-term, continuous and wide field of view gamma-ray observations.
Despite many advantages, the detection technique alone cannot determine the type of primary
particle which gives rise to the shower. Hence every recorded event either belongs to the category
of gamma-ray induced (signal) or cosmic-ray induced (background) shower. In the data analysis,
the signal over background (S/B) discrimination procedure is performed to identify the event either
as a signal or background. In the presentation, I will discuss the procedure used for S/B discrim-
ination in the ALTO observatory and the practical difficulties in reaching complete background
rejection.
Orateur: SENNIAPPAN, Mohanraj (Linnaeus University)
Session Classification: Students’ presentations
February 22, 2020 Page 59Cosmic Explosio … / Rapport sur les contributions N. Smirnova: 3D Simulations of Pa …
Contribution ID: 62 Type: not specified
N. Smirnova: 3D Simulations of Pair Instability
Supernovae Explosions
mardi 28 mai 2019 18:10 (10 minutes)
PISN is the explosions of supermassive, up to 1000 solar masses, stars of the III generation with
low metallicity, which are on the cosmological distances from the Earth in the young universe. In
present time there are not many publications exist on this topic what is explained by observational
difficulties. These kinds of stars are unavailable for direct observations now, but the advanced
instruments are developed fastly and there is no doubt that in a few years the topic became very
popular branch of astrophysics.
For better understanding of the hydrodynamical process of pair instability supernovae explosion
numerical simulation is crucial. The results of the 3D hydrodynamic simulation of pair-instability
supernovae with core of 70, 90 and 100 solar masses will be presented. For each case the amount
of nuclear energy release and lost through neutrino losses during the explosion will be shown.
The results of 3D simulations will be compared with results of 1D and 2D simulations from other
works.
Orateur: SMIRNOVA, Nina (LAPTh)
Session Classification: Students’ presentations
February 22, 2020 Page 60Cosmic Explosio … / Rapport sur les contributions S. Scott: The Follow-up of Cosmic …
Contribution ID: 63 Type: not specified
S. Scott: The Follow-up of Cosmic Explosions with
VERITAS
mardi 28 mai 2019 18:30 (10 minutes)
Much can be learned about the particle acceleration and emission processes involved in cosmic
explosions through the study of gamma rays in the very-high-energy (VHE; E > 100GeV) regime.
Ground-based imaging atmospheric Cherenkov telescopes (IACTs), which are sensitive to VHE
gamma-ray photons, therefore have much to contribute in the effort to characterize these tran-
sients. VERITAS, an IACT array located at Whipple Observatory in southern Arizona, has actively
followed up gamma-ray bursts (GRBs) since 2006. In the last few years, VERITAS has also initiated
programs to investigate LIGO/Virgo gravitational wave events and IceCube neutrino alerts. This
presentation will cover the current status and future of the VERITAS transient follow-up programs.
Orateur: SCOTT, Skyler (UCSC)
Session Classification: Students’ presentations
February 22, 2020 Page 61Cosmic Explosio … / Rapport sur les contributions G. Verna: Searching for galactic P …
Contribution ID: 64 Type: not specified
G. Verna: Searching for galactic PeVatrons with CTA
mardi 28 mai 2019 18:40 (10 minutes)
One of the major scientific objectives of the future Cherenkov Telescope Array (CTA) Observa-
tory is the search of PeVatrons. PeVatrons are the cosmic-ray factories able to accelerate nuclei
at least up to the knee feature seen in the spectrum of Cosmic-Rays measured from Earth. CTA
will perform a survey of the full Galactic plane at TeV energies and beyond with unprecedented
sensitivity. The determination of efficient criteria to identify PeVatron candidates during the sur-
vey observations is essential in order to trigger further dedicated observations. At CPPM we are
working to determine these criteria through a study based on a full simulation. The outcome of
this study is a PeVatron figure of merit, which is a metric that provides relations between spectral
parameters, observation times and spectral cut-off energy lower limit.
I will give a general overview of this study with particular attention on the results obtained us-
ing the two prototype scientific tools for CTA: Ctools and GammaPy. The possibility of different
observation strategies particularly suitable for PeVatron search will be also mentioned.
Orateur: VERNA, Gaia
Session Classification: Students’ presentations
February 22, 2020 Page 62Cosmic Explosio … / Rapport sur les contributions G. Weerasekara: The effect of pec …
Contribution ID: 65 Type: not specified
G. Weerasekara: The effect of peculiar motion of
galaxies when calculating the gravitational lensing
time delay
mardi 28 mai 2019 18:50 (10 minutes)
An intervening galaxy acts like a gravitational lens and produces multiple images of a single source
such as a more remote galaxy. In such a scenario the source, the lens and the observer all have
peculiar motions in any random direction in addition to the overall expansion of the universe due to
the dark energy. There is a difference in light arriving times from images of a single source, known
as the time delay. In calculating such time delays, the peculiar motions of the source, the lens and
the observer are generally neglected. In this study, realistic time delays are calculated considering
such peculiar motions. The results show that peculiar motions contribute to measurable differences
to the observed time delays.
Orateur: M. WEERASEKARA, Gihan (University of Colombo)
Session Classification: Students’ presentations
February 22, 2020 Page 63Cosmic Explosio … / Rapport sur les contributions N. Dagoneau: Image the hard X- …
Contribution ID: 66 Type: not specified
N. Dagoneau: Image the hard X-ray sky with the
ECLAIRs telescope onboard the SVOM mission,
application to the detection of ultra-long gamma ray
bursts.
lundi 3 juin 2019 18:10 (10 minutes)
It has recently been pointed out that ultra-long gamma-ray bursts (ULGRBs), with very atypical
durations of more than 1000 seconds, could form a new class of GRBs (Levan+13). ULGRBs could
have a different progenitor than standard GRBs and be produced by the core collapse of a low
metallicity supergiant blue star (Gendre+13) or the birth of a magnetar following the collapse of
a massive star (Greiner+14). However ULGRBs could also just represent the tail of the standard
long GRB distribution (Virgili+13). In any case, it is clear that the duration of these bursts make
them peculiar. To progress, the few ULGRBs detected so far by the Swift Burst Alert Telescope
and some other instruments has to be increased. SVOM (Space-based multi-band astronomical
Variable Objects Monitor, Wei, Cordier+16) is a French-Chinese mission dedicated to GRBs and
transient events, currently under development and scheduled for launch after 2020. SVOM will
help understanding ULGRBs, since its orbit and pointing strategy will permit to image the same
portion of the sky continuously during nearly one day with the onboard coded-mask telescope
ECLAIRs. Thanks to the image trigger foreseen onboard (Schanne+15), we expect to increase the
sample of ULGRBs with SVOM. In this talk, I will present various methods developed to clean detec-
tor images from X-ray background and known X-ray source contributions in the onboard imaging
process. Methods are based on detector model fitting (X-ray background model plus known X-ray
source illuminations on the detector) and wavelet cleaning to remove large scales mainly contain-
ing the X-ray background. The cleaning performances of the methods will be presented. I will also
focus on the capability of the image trigger to detect the currently available ULGRBs as well as a
synthetic population of fainter and more distant ones, which help us to determine the ECLAIRs’
redshift horizon.
Orateur: DAGONEAU, Nicolas (CEA/Saclay - IRFU/DAp/LISIS)
Session Classification: Students’ presentations
February 22, 2020 Page 64Cosmic Explosio … / Rapport sur les contributions Theory: late stage of stellar evolution
Contribution ID: 67 Type: not specified
Theory: late stage of stellar evolution
mercredi 29 mai 2019 15:00 (1 heure)
Orateur: LANGER, Norbert
February 22, 2020 Page 65Cosmic Explosio … / Rapport sur les contributions CTA: Cargèse Telescope Array
Contribution ID: 68 Type: not specified
CTA: Cargèse Telescope Array
jeudi 30 mai 2019 19:00 (10 minutes)
Orateur: SCHANNE, Stéphane (CEA Saclay)
February 22, 2020 Page 66Cosmic Explosio … / Rapport sur les contributions Telescope observations
Contribution ID: 69 Type: not specified
Telescope observations
mercredi 29 mai 2019 22:00 (3 heures)
Orateurs: DAGONEAU, Nicolas (CEA/Saclay - IRFU/DAp/LISIS); SCHANNE, Stéphane (CEA Saclay)
February 22, 2020 Page 67Cosmic Explosio … / Rapport sur les contributions CTA: Cargèse Telescope Array ob …
Contribution ID: 70 Type: not specified
CTA: Cargèse Telescope Array observations
jeudi 30 mai 2019 22:30 (2 heures)
We set up the telescope on the road towards the villa
Orateur: SCHANNE, Stéphane (CEA Saclay)
February 22, 2020 Page 68Vous pouvez aussi lire
