C OSMIC S TAR F ORMATION AND O BSCURATION : A M ULTI -W AVELENGTH P - - PowerPoint PPT Presentation

COSMIC STAR FORMATION AND OBSCURATION:

A MULTI-WAVELENGTH PERSPECTIVE

TSUKUBA GLOBAL SCIENCE WEEK 2016 UNIVERSE EVOLUTION & MATTER ORIGIN

Denis Burgarella Aix-Marseille University 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

• f 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):

• CNRS* researchers
• Astronomers
• 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

RecombinaFon (380 000 yr aLer Big Bang) Dark Ages (no stars) < ------------ First Stars ------------ > Universe fully ionized EvoluFon of galaxies to what we see Today < ---------- ReionizaFon ---------- >

Fme redshiL

~0 13.7×109

∞

? ?

1 6

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

• f Galaxies

Let me know present a few relaLvely recent results

• n 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
• bservaLons, 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

z

This is how many stars form per year in a reference volume of the universe:

SFR = Star FormaFon Rate

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 will create an unbiased census of ‘first-light’ objects that dwell in the early universe, before the end of reionisaFon in the same 1–5μm range than JWST, but over much larger fields

• f view (x100 JWST)
• Photometric selecFon: a few

hundred “First-Light” z ~ 15

• bjects (mAB=28) over 180deg2.
• Emission line selecFon: blind

integral-field spectroscopic survey over 1.6deg2.

• Pointed observaFons of

quasars and their early black holes at z > 6

FLARE (First Light And ReionizaFon Explorer)

an ESA M5 Proposal,hop://mission.lam.fr/flare/

Imaging and spectroscopic fields of view not at the same scale.

2Kx2K 2Kx2K

6 x 2K = 0.8 deg 2 x 2K = 0.4 deg 6 slits x 25 arcsec = 150 arcsec

ì time to build survey Imaging Spectroscopy

21

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

Vol (WFIRST)

Volume in which Galaxies with SFRUV > 100 Msun per year can be Detected as a funcFon of the RedshiL <=> Relevance of the Projects to StaFsFcally Study the Early Universe

Ngalaxies(FLARE) ~ 500 @ z = 14 - 15 Ngalaxies(JWST Wide) ~ 2 - 3 @ z = 14 - 15 Ngalaxies(JWST Deep) ~ 0.05 @ z = 14 - 15

z = 14 ó 3 Myrs aper Big Bang

• 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:
• The assessment of Dome C for astronomy,
• The idenLficaLon of the key astrophysical

programmes that would take maximum benefit from the site,

• 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

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

• f 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 Gyr of the universe.

FormaFon of the first stars and galaxies

• V. Conclusions

& PerspecLves

• I would like to thank the University of Tsukuba for
• rganizing this event and for promoLng exchanges

world-wide and for inviLng me to parLcipate.

• I think this meeLng will foster collaboraLons between

us and, allow to develop new ambiLous collaboraLve scienLfic projects and observatories to beoer understand the early universe and its components.

FIN

Marseille, France