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SKA France The French community towards the Square Kilometre Array Chiara Ferrari Astronomer at Observatoire de la Côte d’Azur Director of SKA France
Timeline of the SKA project
2009 2010 2011 2012 2015 2016 2017 2018 2019
Revision of French roadmap
AS SKA-LOFAR
EMBRACE
Prospective
Institut National des Sciences de l’Univers
ch
Prospective
B U T : Fr e n
ra w al P0 for France
w i th d
h e S K A joining SKAO
fro m t
Astronomie et Astrophysique
2015-2020
Synthèse et Résumés éxécutifs
NenuFAR
LOFAR
SKA Swiss Days 2018 2
The SKA France coordination
Traitements*des*données
Visualisation des données
Partage des données
SKA: le plus grand défi “Big Data” en astronomie
Chiara Ferrari et Gabriel Marquette - Coordination SKA-France
Un radiotélescope géant et un projet international majeur
• Square Kilometre Array (SKA): l’un des projets majeurs de l’astronomie au sol au niveau mondial →
Depuis 2016 dans la catégorie Landscape de la Roadmap ESFRI
• Réseau interférométrique qui couvrira les bandes radio astronomiques métriques à centimétriques avec
une surface collectrice de 1 km2
• Première phase de son déploiement: SKA1 (environ 10% du réseau final) prévue à l'horizon 2020+
• SKA1 sera construit sur deux sites: SKA1-LOW (50-350 MHz) en Australie et SKA1-MID (350 MHz-15
GHz) en Afrique du Sud → Deux télescopes pour un observatoire
• La bande de fréquences de SKA et sa surface collectrice en font un radiotélescope exceptionnel →
Moyen unique pour cartographier les différentes phases de l’histoire de l’Univers, des premières sources
lumineuses aux systèmes d’astres évolués que nous observons aujourd’hui
• Projet international : 10 pays membres aujourd’hui et 7 pays observateurs, dont la France → SKA sera
piloté par une Organisation Inter-Gouvernementale (IGO) en cours de montage
Vision d’artiste des antennes de SKA1-LOW (gauche) SKA1-MID (droite) – Crédit : SKA Organisation
Un défi technologique particulièrement stimulant pour un très large sous-ensemble
des technologies de l’information haute performance
• Signaux électriques captés par des milliers d’antennes localisées dans les déserts australien et sud-
africain et transportés jusqu’aux super-ordinateurs installés à des centaines de kilomètre de distance
(Perth et Cape Town) → débits de plusieurs Tbit/s
• Ces données brutes deviendront des images 4D (position, temps, fréquence) du ciel à travers une chaine
algorithmique complexe → puissance de calcul de plusieurs centaines de Pflops
• Les produits prêts pour l’analyse scientifque seront mises à disposition de la communauté astronomique
→ taux de croissance de l’archive SKA de 50 à 300 Pbytes/an
• Le travail de préparation à l'échelle mondiale s’articule autour de groupes de travail scientifiques et
technologiques
• Dans cette phase de préparation, un rôle fondamental est joué par les différents précurseurs
internationaux de SKA, comme les réseaux d’antennes LOFAR en Europe, ASKAP et MWA en Australie,
MeerKAT en Afrique du Sud
• Un immense et passionnant « chantier de recherche » → perspective d’innovation et de sauts
Seminars
technologiques considérable pour le monde industriel dont on attend en particulier des retombées
importantes dans de nombreux domaines faisant appel aux technologies massives de l'information
Informations techniques principales pour SKA1-LOW (gauche) et SKA1-MID (droite) – Crédit : SKAO
Une forte mobilisation de la communauté française
• La France est impliquée de manière significative dans le projet SKA depuis ses études préparatoires (FP6)
• Montée en puissance de la participation française dans SKA: mise en place de l’Action Spécifique SKA-
LOFAR en 2010 et de la coordination SKA-France en 2016 (CNRS/INSU, Observatoires de Paris et de la
Côte d’Azur, l’Universités de Bordeaux et d'Orléans)
• SKA-France: Coordination nationale des activités scientifiques, techniques et industrielles → Objectif:
construire la solution SKA France pour permettre aux équipes scientifiques et aux porteurs de projet
industriels d’occuper les positions de leader auxquels ils peuvent dans SKA
• Ateliers technologiques « SKA-France : HPC & Traitement du Signal » : participation des entreprises
majeures du secteur, implantées en France et de plusieurs organismes de recherche → co-design pour
optimisation du traitement du signal: construire un groupe français qui guide les développements
algorithmiques pour les données d’interférométrie radio (CNRS/INSU & CEA) en collaboration étroite avec les
constructeurs (industriels) et la recherche informatique (INRIA)
Participants au dernier atelier « SKA-France : HPC / Big Data » (9 septembre 2016, Paris)
SKA constitue aujourd’hui le Graal scientifique pour la communauté astronomique mondiale et deviendra une réalité dès lors que les défis fantastiques Big Data et HPC - production de
données équivalente au trafic internet mondial d’aujourd’hui - ainsi qu’énergétique, auront été relevés avec succès.
C’est dans cette perspective que les communautés scientifique et industrielle françaises se sont mobilisées pour prendre la place à laquelle ils prétendent légitimement dans le projet. SKA.
SKA ne pourra atteindre le degré d’excellence et de performances visées sans les contributions françaises, jugées au niveau mondial comme indispensables pour relever les défis
scientifiques, numériques et énergétiques.
UMR$7293$Laboratoire$Lagrange$&$CNRS/INSU$–$Bd.$de$l’Observatoire$06304$Nice$&$3$rue$MichelHAnge$75016$Paris$
chiara.ferrari@oca.eu$&$gabriel.marqueQe@cnrsHdir.fr$pour$la$CoordinaSon$SKAHFrance$
Workshops Web page Big events
Monthly bulletins
SKA Swiss Days 2018 3
The French SKA White Book
176 authors from
French SKA White Book
The French community towards the Square Kilometre Array
40 French research institutes
Editor in Chief:
6 private companies
C. Ferrari
Editors:
G. Lagache, J.-M. Martin, B. Semelin — Cosmology and Extra-galactic astronomy
M. Alves, K. Ferrière, M.-A. Miville-Deschenes, L. Montier — Galactic Astronomy
E. Josselin, N. Vilmer, P. Zarka — Planets, Sun, Stars and Civilizations
S. Corbel, S. Vergani — Transient Universe
S. Lambert, G. Theureau — Fundamental Physics
S. Bosse, A. Ferrari, S. Gau↵re — Technological Developments
G. Marquette — Industrial Perspectives and Solutions
arXiv:1712.06950
SKA Swiss Days 2018 4
A wider and wider community and strong
interdisciplinary incentives
Planck
ASKAP (AUS) MeerKAT (SA)
All SKA Science Working Groups have French
participants
Sixteen French researchers (co-)authors of more
JVLA (US) GMRT (IN) than 30 out of the 135 chapters of the SKA
Science Book
LOFAR (EU)
NenuFAR (FR)
VLBI
SKA Swiss Days 2018 5
e↵orts to observe FRBs at Nançay
seen thus far have been detected byOcvirk+ 16 data from Adapted
analysing from
1.4-GHz Staveley-Smith conducted
observations & Osterloo 15 & Fernàndez+ 13
elescope, often as part of the High Time Resolution Universe (HTRU) pulsar survey (see
et al. 2016). FRB 121102 (discussed above), discovered at 1.4-GHz at Arecibo, was the
at Parkes (Spitler et al. 2014); and the discovery of FRB 110523 with the Green Bank
-GHz demonstrated that FRBs can be seen at these lower frequencies (Masui et al. 2015).
(2017) reported the discovery of three FRBs in a survey of the southern sky at 0.8-GHz
servatory Synthesis Telescope. It will be particularly interesting to see how many FRBs
onstruction in Canada, will detect between 0.4 and 0.8-GHz, and also if instruments such
will be able to detect FRBs despite the strongly dispersed and scattered signals at these
ies (note that a search for FRBs at 145-MHz using LOFAR stations in France and in the
ection, see Karastergiou et al. 2015 for details). The estimated FRB rate based on the
Temperature distribution in a 45 h70 1 Mpc x 45 h70 1 Mpc x 0.03 h70 1 Mpc slice of the CODA
is of several thousands FRBs per sky and per day (see e.g. Champion et al. 2016).
t half-reionisation (Ocvirk et al. 2016). Orange regions show photo-heated, ionised material, while
l neutral medium appears in blue.
Figure 21: A simulation showing the distribution with redshift of H i masses of galaxies likely to be detected with
Courtesy: Cognard+
ct 3D (2D+time) tomography of the 21 cm signal (Madau et al. 1997). SKA1 in the representative tiered set of 1,000 hr surveys discussed by Staveley-Smith & Oosterloo (2015). Blue
will be used to investigate the connection between the sources (first galaxies and AGNs) and the corresponds to the “medium wide” survey, green to the “medium deep” and red to the “deep”. The turn-over
tance the evolving geometries of a Reionisation powered by a few bright galaxies or abundant fainter of the H i mass Schechter distribution function M(HI)* at z=0 is displayed as the dashed horizontal line. The
ected to be di↵erent (see e.g. McQuinn et al. 2007; Chardin et al. 2012). Imaging will also provide diagram inserted at right, corresponding to the black rectangle inserted at left, shows what is possible to do now,
w of the actual Reionisation history experienced by biased regions (and therefore galaxies): structures
in 50 hours of observations with the JVLA, from the pilot survey of Fernàndez et al. (2013).
and turnover are difficult to constrain by non-simultaneous observations in various spectral ranges. But we found
eionised earlier than the Universe as a whole and often on large durations (up to ⇠ 200 Myrs, see e.g.
4). The details of these timings could be important to investigate the suppression of star formation
a signal down to 50 MHz with an overall shape compatible with observations
by radiation (Ocvirk & Aubert 2011; Ocvirk et al. 2014). atthehigher
this fraction closer to universal frequencies.
fraction of 17%, while supernovae and AGN feedback have been implicated
werful AGNs are expected to create large H ii regions with radii of 10s of Mpc (see e.g. Datta et
in reducing it to less than 4% today? Obtaining rotation curves extending to the outskirts is time consuming
16): detections with SKA1-LOW should be possible with 1000 hrs of observation and will provide
on AGNs or IGM high-z properties. Such prospects open the possibility of linking the population of at high z, but much will be learned from a well-selected sample of ⇠ 100 galaxies. A deep integration of 100h
with e.g. the luminosity functions (LF) of galaxies and AGNs : first constraints on LFs are already with SKA1-MID, with 15kpc spatial resolution (2.4 arcsec at z=0.5 and 1.8 arcsec at z=1 and beyond), will be
Girard+ 16
g. Bouwens et al. 2015; Giallongo et al. 2015) and will be further refined with future experiments
ST or ATHENA. SKA will provide an alternate view of the first sources by putting constraints on
required to reach H i column densities of 4.1 and 7.5 1020 cm 2 respectively, at 5 , in 20km/s channels. The
study of a more significant sample could be done only at lower resolution and higher sensitivity with SKA1 and
ce on their environment : as such, SKA will be essential component to deepen our understanding of only then by exploiting the relation between luminosity and rotation speed (i.e., Tully-Fisher relation). Studying
mation in its earliest stages. It would also provide key insights on the relative contribution of star
galaxies at even higher redshifts, up to z=2, will have to wait for the sensitivity provided by SKA2.
The growth of angular momentum in galaxies
19
The angular momentum of nearby disk galaxies is about that predicted for their dark matter halos (Steinmetz
& Navarro 1999). How can a dissipative and non-dissipative matter have the same specific angular momentum,
when one is found on much smaller scales than the other? Models of the cosmological accretion of gas driven
Courtesy: Charlot+ by the growth of large scale structure have made significant progress in solving this issue (Danovich et al. 2015)
but even then, these models do not follow the gas down to galaxy (kpc) scales. The angular momentum as a
function of redshift, should vary as j(z) / (1 + z)3/2 (Mo et al. 1998). This is something we can test rather
uniquely with SKA observations of many galaxies in H i.
Figure 37: Left: resolved brightness distribution of Jupiter’s synchrotron emission with LOFAR at 127-172 MHz,
with dipolar field lines superimposed. Center: LOFAR image contours (red) compared to VLA ones43at ⇠5 GHz,
by 10% steps. Right: measurements of Jupiter’s synchrotron spectrum, obtained with the VLA between 1991
and 2004, and with LOFAR in 2011 and 2013 (Girard et al. 2016a,b). Blue and red curves were fitted by de
Pater et al. (2003). Decametre emission (DAM – not shown) dominates the spectral range below 40 MHz.
SKA covering
SKA, Swiss Days entire range of Jupiter’s synchrotron emission with resolved images, will bring unique con- Rosado + 15
the 2018 6
straints to the distribution of energetic electrons in Jupiter’s inner magnetosphere in all energy ranges (100s of
A wider and wider community and strong
interdisciplinary incentives
Planck
Euclid ELT LSST JWST
The richest synergy chapter ever
4MOST DESI Athena CTA published about SKA vs. other projects,
including:
instruments covering the whole
electromagnetic spectrum
LIGO & Virgo Post-Planck ALMA gravitational wave detectors
SVOM
SKA Swiss Days 2018 7
Planck coll. 16
Figure 64: Left: spectral distribution of polarised foreground emission at 1 deg
between 80Vazza
and+90%
17 sky coverage. Units are r.m.s brightness temperature. Ta
X (2016). Right: angular power spectra showing primordial B modes, lensing B
-25 modes, as well as the total contribution of polarised B-mode foregrounds (dust p
the cleanest 1% to 90% of the sky, at 100 and 200 GHz. From Errard et al. (201
1050
Peak X-ray luminosity (erg s-1)
-20
Absolute peak magnitude MV
The presence of polarised extragalactic sources constitutes an additional source
the compact
1045
source contribution does not impact the large angular scales (near t
-15 play an important role on intermediate and small angular scales. It is likely tha
to be removed with a combination of masking or subtracting individual sources,
power-spectrum
1040 level. We can seek to improve the source detection process using
compact sources detected by SKA. It should also be noted that a large fraction o
-10 detected in CMB experiments are variable. One way of addressing this problem is
1035
of sources in such a way that these observations are performed near simultaneous
-5
1 102 104 Adapted from Jonker+ 13
Time scale (s)
SKA
Figure 67: Swiss Days 2018
The characteristic absolute optical magnitude (red) and X-ray luminosity (grey) versus characteristic
8
timescale for various classes of object which could be studied by SVOM. The optical/X-ray scales are on the
eft/right axes. Sources/phenomena that have been relatively poorly studied are plotted without border and
Building this fantastic machine:
technological developments in France
50 PFLOPS
8.8 Tb/s
Design Consortia
SKA1-MID 5 Tb/s
7.2 Tb/s
Design Consortia 100 PFLOPS
Design Consortia
~2 Pb/s
SKA1-LOW
SKA Swiss Days 2018 9
SKA Swiss Days 2018 10
France within the organisation of the SKA
European Regional Data Centre
Regional Centres Concept:
Users
Regional
Centre 1
Science Users
Processing
Centre
Regional Users
AUS Centre 2
Users
Science Users
Processing
Centre
Users
RSA Regional
Centre N Users
Observatory User Community
• J.-P. Vilotte (CNRS):
member of the External Advisory Board
(with I. Bird @ CERN & M. Zwaan @ ESO)
• C. Ferrari (OCA):
chair of the General Assembly4.1.17 JIV-ERIC
The Joint Institute for VLBI ERIC (JIVE) is the central node of the European
VLBI Network (EVN, http://www.evlbi.org/), a distributed array of radio
SKA Swiss Days 2018 telescopes, in and outside of Europe, offering astronomers the highest resolution 11
view of radio sources. JIVE provides the scientific data product as well asAdvanced Instrumentation Programme
Design Consortia
12 3 4 5
See Miroslav’s talk
350 MHz 15.3 GHz
SKA Swiss Days 2018 12Industrial perspectives and solutions
Intérêt industriel Multiples défis pour la construction
Industry
Intérêt industriel Multiples défis pour la construction
- Apport et distribution d’énergie
- Ingéniérie système
- Big data -(FaitApport et distribution
partie des projets d’énergie
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emblématiques du clustersystème
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- Digitalisation haute fréquence
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des très grands volumes de
données - Digitalisation haute fréquence
- Archivage
- Algorithmes
-Traitement des très grands volumes de
données
• Nice, December 2015: First SKA French Industry Day
- Archivage
• Paris, July & September 2016: Workshops HPC/Big Data
• Paris, September, October & November 2016: Workshops Energy
SKA Swiss Days 2018 13- Big data (Fait partie des projets
données
• Nice, December 2015: First SKA French Industry Day
emblématiques du cluster - Archivage
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SKA Swiss Days 2018 14Industrial perspectives and solutions
Multiples défis pour la construction
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SKA Swiss Days 2018 15Industrial perspectives and solutions
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SKA Swiss Days 2018 16Industrial perspectives and solutions
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50 PFLOPS
8.8 Tb/s
SKA1-MID 5 Tb/s
7.2 Tb/s
100 PFLOPS
~2 Pb/s
SKA1-LOW
SKA Swiss Days 2018 17- Big data (Fait partie des projets données
• Nice, December 2015: First SKA French Industry Day
emblématiques du cluster - Archivage
Industrial perspectives and solutions
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SKA Swiss Days 2018 18French SKA White Book
The French community towards the Square Kilometre Array
SKA-France milestones Industry
Intérêt industriel Multiples défis p
Industry
Intérêt industriel
- Apport et dis
- Ingéniérie sy
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SKA-France Day on October 16, 2017 emblématiqu
Editor in Chief:
ASTERICS)
- Digitalisat
C. Ferrari
Editors:
G. Lagache, J.-M. Martin, B. Semelin — Cosmology and Extra-galactic astronomy
-
M. Alves, K. Ferrière, M.-A. Miville-Deschenes, L. Montier — Galactic Astronomy
E. Josselin, N. Vilmer, P. Zarka — Planets, Sun, Stars and Civilizations
S. Corbel, S. Vergani — Transient Universe
Algorithme
S. Lambert, G. Theureau — Fundamental Physics
A new structure : « Maison SKA France »
Traitemen
S. Bosse, A. Ferrari, S. Gau↵re — Technological Developments
G. Marquette — Industrial Perspectives and Solutions -
données
• Nice, December 2015: First SKA French Industry Day
- Archivage
PPP: instrument in response to the necessity of an • Paris, July & September 2016: Workshops
• Nice, DecemberHPC/Big Data
2015: First SKA F
• Paris, September, October & November
July & 2016: Workshops E
innovative financial approach
• Paris, September 2016: Wor
• Paris, September, October & Nove
Kick-off meeting on February 1st, 2018
Biennial revision of the National Roadmap for Large
Research Infrastructures
SKA in as a project: announcement on May 17, 2018
French application for joining the SKAO company with
financial contribution of MSF
Next French roadmap revision in 2020
SKA Swiss Days 2018 19THANKS! 20
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