Wide-field Infrared Projects in Europe Denis Burgarella, LAM, - PowerPoint PPT Presentation

Wide-field Infrared Projects in Europe Denis Burgarella, LAM, France denis.burgarella@lam.fr 1

Outline of the Talk 1. Wide-field IR Telescope Projects (in which I am involved) 1.1. ESA White Paper « Voyage 2050 » 1.2. SPICA ( à 松原英雄 ) 1.3. Origins Space Telescope – MISC 1.4. VLT-MOONS 1.5 Mauna Kea Spectroscopic Explorer (MSE) 2. Galaxies before the end of reionization 2.1. NIR-MIR Science Cases 2.2. Recent Result of Interest 3. Perspectives of Collaborations (Japan – France) 3.1. International Research Network NECo 3.2. With my team and LAM: • Expertise in Optics, Data Analysis • Adaptation of CIGALE for Fast & Massive Fitting of Photometry + Spectroscopy (ongoing PhD in Maths/Astro) and Simulations for MOONS à SPICA, PFS, Others? 2

1.1 ESA White Paper « Voyage 2050 »

1.1 ESA White Paper « Voyage 2050 » Initial Assumptions: • Assume a 4m-class primary mirror • Built on the M5 FLARE and NASA OST science cases 1. Science Questions 1.1.The Origins of Elements 1.1.1. When Did the First Galaxies Appear? 1.1.2. What is the History of The Rise of Metals in the Universe? 2.1.The Origins of Stellar Systems in the Milky Way 2.1.1. How Stellar Systems Form? 2.1.2. What is the Dust/Metal Cycle? 2.1.3. When did the Milky Way / Universe Became Habitable?

1.1 ESA White Paper « Voyage 2050 » Initial requirements (TBC by Science Team) are 1 instrument (M mission) or 2 instruments (L mission) : o Spectro-imager NIR-MIR ( ∽ 3 - 30 microns): MUSE-like IFU or MOS ß Maximum priority o Spectro sub-mm (500+ microns) ß Lower priority but strong interest by Cosmology community for all-sky survey (i.e. M5 Core+ project) o Wide instantaneous field of view: about 1 sq. deg o Angular resolution: about 0.2’’in NIR-MIR and Herschel-like in sub-mm o Pixel scale: ∽ 0.2’’

1.1 ESA White Paper « Voyage 2050 » 2. Which Science Mission to Address the Science Questions? 2.1. Summary of the Requirements from these Science Questions 2.2. What can we do with an L Science Mission? 2.3. What if we assume an M Mission? 3. International Space Context 4. Technology Challenges 4.1. Lightweight Large Mirror (~4m) 4.2. Deformable Mirror for Active Optics 4.3. Wide-field Integral-Field Spectrograph 4.4. Micro-Mirror Arrays

1.1. Connections with Delabrouille’s cosmological WP (former M5 Core+) Survey MIR NEP All-Sky Survey mm Survey MIR MW Disk All-Sky Survey mm Survey MIR SEP T 0 T 1 7

1.2. SPICA

1.3 Origins Space Telescope - MISC

1.3 Origins Space Telescope - MISC

1.4 VLT-MOONS Milestones • Preliminary Design Review (PDR) – 03/2016 • Final Design Review (FDR) – 03/ 2017 • Start of scientific operations - 2021

1.4 VLT-MOONS • Two spectrographs are required due to the large number of fibres. • A single cryostat will contain both of them, in order to reduce the overall mass and volume of the instrument. • Each spectrograph will simultaneously obtain spectra in the three wavebands, namely RI, YJ and H. • A CCD detector will be used for the shortest waveband (RI), while Teledyne Hawaii 4RG detectors will be used for the two longer wavebands (YJ and H).

1.4 VLT-MOONS Scientific Objectives Galactic archeology The study of the resolved stellar populations of the Milky Way and other Local Group galaxies. Follow-up of Gaia and for Galactic surveys with VISTA. The near-IR coverage of MOONS will allow to investigate the nature of the heavily-obscured regions of the Galactic bulge. The growth of galaxies Tracing the assembly history of galaxies over cosmic time by exploiting the large multiplex and wavelength coverage of MOONS. High quality spectra for a statistically significant number of galaxies (~1 million) at z > 1. The first galaxies and Reionization The unique combination of the 8m VLT aperture, wide-area coverage, and near-IR spectroscopy offered by MOONS will provide accurate distances, relative velocities and emission-line diagnositcs for statistical samples of z > 7 galaxies. MOONS will provide the essential deep spectroscopic follow-up of current and future optical and near-IR imaging surveys (e.g. VISTA, VST, Pan-STARRS, LSST) and space mission (e.g. WISE, Athena) in the Southern hemisphere.

1.5 Mauna Kea Spectroscopic Explorer (MSE)

2. Galaxies before the end of reionization

2.1. NIR-MIR Science Cases

2.1. NIR-MIR Science Cases z \ mA 25 25 26 26 27 27 28 28 29 29 mAB SFR vs. Mstar 5 6741 257674 2.8E+06 20084 73187 54 6 12773 307300 3873 20241 0 7 325 23164 532 4282 0 8 4 1165 55 730 0 9 0 44 5 96 0 10 10 0 1 0 13 This table provides the number of galaxies detected by the two WFIRST Wide (yellow) and Deep (blue) surveys at 5 < z < 10 that OST-MISC could detect. The objective of this GO proposal is to estimate M « and SFR for a sample of at least 10 galaxies per bin for WFIRST-detected objects è Needs NIR-MIR for M « and FIR for SFR.

2.1. NIR-MIR Science Cases Rise of Metals • Measuring the metallicty of most galaxies at z > 5 cannot be done from mid-IR emission line. • We need to find another way, or simply drop the science case…

2.1. NIR-MIR Science Cases Two options: 1. Use the bright optical (but redshifted optical lines) Needs NIR-MIR over at 3 - 10 𝜈 m

2.1. NIR-MIR Science Cases Two options: 2. Use the (also) redshifted PAH3.3 𝜈 m Note that this option works pretty well for OST/MISC & SPICA/SMI (lower z)

2.2. Recent Result of Interest (to be submitted to Nature: Burgarella, Nanni, Hirashita, Theulé et al.)

2.2. Recent Result of Interest We use ALMA-observed Lyman break galaxies (detections but also upper limits) at 5 < z < 10 and we have about 25 objects.

2.2. Recent Result of Interest sM dust = M dust / M star IMF A strong modelling effort was needed. This case was not (or badly) assumed by previous models. sSFR = SFR / M star

2.2. Recent Result of Interest sM dust Constraints on IMF Our results present thr strong advantage of being globally consistent for several galaxy populations at all redshifts in a global context (not ad- hoc modelling for LBG populations). Age

2.2. Recent Result of Interest IRX ∽ A FUV ? z formation redshift

3. Perspectives of Collaborations 3.1. International Research Network NECo

3. Perspectives of Collaborations 3.1. International Research Network NECo

3. Perspectives of Collaborations 3.1. International Research Network NECo

3. Perspectives of Collaborations 3.2. With LAM and/or CIGALE Team: • Expertise in Optics, Data Analysis for ground-based and space projects • Adaptation of CIGALE for Improved Statistics + Fast & Massive Fitting of Photometry + Spectroscopy (ongoing PhD in Maths/Astro) o Simulations and Data Analysis for VLT-MOONS à also use for SPICA, PFS, Others? o Should use Neural Network for each CIGALE scientific module to speed-up already fast CIGALE

ありがとうございました Merci 31