C OSMIC S TAR F ORMATION AND O BSCURATION : A M ULTI -W AVELENGTH P ERSPECTIVE T SUKUBA G LOBAL S CIENCE W EEK 2016 U NIVERSE E VOLUTION & M ATTER O RIGIN Denis Burgarella Aix-Marseille U niversity Marseille, France
Short CV PhD from Nice University, France • Post-doc from the French Space Agency in Laboratoire d’Astrophysique • de Marseille (LAM), France Post-doc from the European Space Agency at the Space Telescope • Science InsLtute (STScI), BalLmore, USA Astronomer in Laboratoire d’Astrophysique de Marseille (LAM), France • 2008 – 2010: President of the French Astronomical & Astrophysical • Society (during the InternaLonal Year of Astronomy 2009) 2013 – Now: President of the Astrophysical Division of the French • Physical Society (during the InternaLonal Year of Light 2015) 2015 – Now: President of the Galaxy Spectral Energy DistribuLons of the • InternaLonal Astronomical Union (IAU) FormaLon and EvoluLon of Galaxies •
Outline of the PresentaLon I. Some key InformaLon about Astronomy & Astrophysics in France II. Key QuesLons in ExtragalacLc Astrophysics III. A MulL-Wavelength Approach to the Understanding the FormaLon & EvoluLon of Galaxies IV. New ObservaLonal Projects to Search for the First Galaxies V. Conclusions & PerspecLves
I. Some key InformaLon about Astronomy & Astrophysics in France
• 15 French insLtutes are dedicated to Astrophysics. • They are mixed university & CNRS* units • About 1000 people listed in the directory managed by the French Society for Astronomy & Astrophysics with ~700 are acLve professional researchers • These researchers can have three statuses (about 1/3 each): o CNRS* researchers o Astronomers o University Researchers * Centre NaLonal de la Recherche ScienLfique
What are the main faciliLes accessible to the French community (biased by my knowledge): • Member of the European Southern Observatory (ESO) and can access to its telescopes in Chili, including the 4 VLTs, ALMA and the future 39m E-ELT. • Member of the European Space Agency (ESA), e.g. Juice (Jupiter), ATHENA (X-rays), Solar Orbiter, Euclid (Cosmology), PLATO (exo- planets) but also collaboraLon to NASA (HST, JWST) or JAXA missions (AKARI, BepiColombo). • Other faciliLes like IRAM (mm), Nancay (radio) and CFHT (opLcal). • A French-Italian staLon in AntarcLca (Dome C) with the ASTEP (AntarcLc Search for TransiLng Exoplanets) telescope. • High energy / astroparLcles projects like (Auger, HESS, Antares) • High Performance CompuLng faciliLes are organized in a pyramid from the regional (e.g., universiLes), to the naLonal and finally the European ones.
II. Key QuesLons in ExtragalacLc Astrophysics
« Nearby » Galaxies « proches » Andromeda galaxy contains about 200 billions stars, like the Sun. It is the closest neighbour galaxy to the Milky Way, sLll, at about 3 millions light-years from Earth.
The history of the universe in 1 slide Big Bang Now 13.7×10 9 ~0 Fme EvoluFon of galaxies RecombinaFon to what we see Today (380 000 yr aLer Big Bang) Universe Dark Ages fully ionized ? ? (no stars) < ------------ First Stars ------------ > < ---------- ReionizaFon ---------- > ∞ 6 1 0 redshiL
What are the Key Ques6ons in Extragalac6c Astrophysics ? If we look (for instance) at ESA’s Cosmic Vision 2015–2025: 4. How did the universe originate and what is it made of? And, more specifically: 4.2 The Universe taking shape: • Find the very first gravitaLonally-bound structures that were assembled in the Universe – precursors to today’s galaxies, groups and clusters of galaxies • and trace their evoluLon to the current epoch This is well inside the theme of this conference: Universe EvoluLon & Maoer Origin We can translate this into topics like: The cosmic star formaLon history as a funcLon of the redship • The co-evoluLon of black holes and star formaLon in galaxies • The chemical history of galaxies and the building of heavy • elements, like C, N, O, Fe in stars
III. A MulL-Wavelength Approach to the Understanding the FormaLon & EvoluLon of Galaxies
Let me know present a few relaLvely recent results on which I have been working • AKARI is a JAXA telescope. It observed in the wavelength range from 1.7μm (near-infrared) to 180μm (far-infrared). • AKARI was launched at an alLtude of approximately 750 km. • Aper carrying out a large numbers of observaLons, AKARI operaLons were completed on November 24, 2011. • We will focus on AKARI’s observaLons of the North EclipLc Pole (PI. H. Matsuhara, ISAS/JAXA).
The infrared side of the Cosmic Star FormaLon History This is how many stars form per year in a reference volume of the universe: SFR = Star FormaFon Rate z
The infrared side of the Cosmic Star FormaLon History • Herschel was a space observatory built and operated by the European Space Agency (ESA). • It was acLve from 2009 to 2013, and was the largest infrared telescope ever launched, carrying a 3.5m mirror. • Its instruments were sensiLve to the far infrared and submillimetre (55 to 672 µm). • My insLtute (LAM) was responsible for the opLcal design the the longest wavelength instrument (250 - 500 µm) SPIRE, used in the following result.
The Total Cosmic Star FormaLon History To carry out this project, it was crucial to combine the mulF- wavelength informaFon: • the ultraviolet from NASA’s satellite GALEX, • the opFcal from ESO’s VLT, • the far-infrared from ESA’s Herschel. SFR from UV SFR from IR Total SFR
The Total Cosmic Star FormaLon History How many stars are hidden by dust grains (opaque in opFcal light but transparent in innfrared)? • Takeuchi, Buat, Burgarella (2005) to z ~ 1 • Burgarella et al. (2013) to z ~ 4
The complementarity of UV and IR to understand star formaLon
The Total Cosmic Star FormaLon History What could we predict at even higher redshiLs, closer to the big bang? Very likely a conFnuous decrease , linked to the low metallicity (heavy elements).
IV. New ObservaLonal Projects to Search for the First Galaxies Among the various projects ( JWST, E-ELT, W-FIRST, ALMA, IRAM/NOEMA, etc. ), I will focus on: • FLARE, that I will submit to ESA in response to the call for Medium-sized projects • A 10-m Terahertz Telescope at Dome C, the French-Italian staLon in AntarcLca.
FLARE ( First Light And ReionizaFon Explorer ) an ESA M5 Proposal,hop://mission.lam.fr/flare/ 21 FLARE will create an unbiased census of ‘first-light’ objects that dwell in the early universe, 6 x 2K = 0.8 deg 2 x 2K = 0.4 deg 6 slits x 25 arcsec = 150 arcsec before the end of reionisaFon in 2Kx2K the same 1–5μm range than JWST, 2Kx2K but over mu ch la rg er fields of view (x100 JWST) Photometric selecFon: a few • hundred “First-Light” z ~ 15 objects (m AB =28) over 180deg 2 . Emission line selecFon: blind • integral-field spectroscopic survey over 1.6deg 2 . Pointed observaFons of • Spectroscopy Imaging quasars and their early black ì time to build survey holes at z > 6 Imaging and spectroscopic fields of view not at the same scale.
Volume in which Galaxies with SFR UV > 100 M sun per year can be Detected as a funcFon of the RedshiL <=> Relevance of the Projects to StaFsFcally Study the Early Universe Vol (WFIRST) Vol (FLARE) Vol (JWST- Wide) = 1% Vol (FLARE) Vol (JWST- Medium) = 0.1% Vol (FLARE) Vol (JWST – Deep) = 0.01% Vol (FLARE) RedshiL: 0 1 5 10 15 Time: 13.7 5.7 1.1 0.5 0 Gyr
z = 14 ó 3 Myrs aper Big Bang N galaxies ( FLARE ) ~ 500 @ z = 14 - 15 N galaxies ( JWST Wide ) ~ 2 - 3 @ z = 14 - 15 N galaxies ( JWST Deep ) ~ 0.05 @ z = 14 - 15
A Japan/France/Italy 10-m Terahertz Telescope In AntacLca • Dome C is located inside the AntarcLc conLnent on the high plateau 3200m above sea level. • The French Polar agencies (IPEV) and Italian (PNRA) have decided in 1993 to install a new permanent scienLfic base, the Concordia staLon.
A Japan/France/Italy 10-m Terahertz Telescope In AntacLca • ARENA xas a consorLum of 22 European funded by the European Commission from 2006 to 2010. • The main objecLves were: o The assessment of Dome C for astronomy, o The idenLficaLon of the key astrophysical programmes that would take maximum benefit from the site, o The characterizaLon and preliminary studies of large faciliLes. • One of the conclusions: at Dome C, temperatures can reach -80°C… Thus, the atmosphere contains very few water vapor and aerosols which retain heat. Consequently, the site of Dome C is ideal to carry out astronomical observaFons in the infra-red and in the submillimeter wave range.
A Japan/France/Italy 10-m Terahertz Telescope In AntacLca Japan (P.I: Pr. Nakai) proposes a 10-m TeraHertz telescope at Dome C with a large field of view, at frequencies of 200 to 1,500 GHz, i.e., 1.5mm to 0.2mm, about the same range than Herschel to discover rare galaxies in the early universe, during the first FormaFon of the Gyr of the universe. first stars and galaxies
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