Participación Española en SAFARI/SPICA · 2011-07-04 · Paco Najarro – SEA 2010 Participación...

Paco Najarro – SEA 2010

Participación Española en SAFARI/SPICA

F. Najarro (CAB)

CAB

J. R. Goicoechea

J. Martín-Pintado

J. Gómez-Elvira

J. Torres

J. Bueno

INTA

L.M. González

T. Belenguer

M. Reina

C. Pastor

IAC

I. Pérez-Fournón


Themes Addressed by SPICA

1. What are the conditions for life

and planetary formation?

2. How does the Solar System

work?

3. What are the fundamental laws

of the Universe?

4. How did the Universe originate

and what is it made of?


What is SPICA? PI:Takao Nakagawa (JAXA-lead)+ESA partnership+others

* Observatory-class mission European access through ESA partnership *Telescope: 3.2m, Actively cooled to <6 K: monolithic mirror clean PSF * Core wavelength: 5-210μm: Δθ = 0.4 – 18 arcsec * Orbit: Sun-Earth L2 Halo * Warm Launch – Cooling in orbit Long lifetime ~ 3 yrs (5 yrs goal) * Launch: ~2018


Why observe in the Mid and Far-IR ?

Star light “recycled” by dust and gas

Complete picture only seen by observing in the mid- and far-IR

Galliano et al.

MIR

FIR

FIR

MIR


IR Natural Sky Background VS Thermal Telescope Emission

Why SPICA?


冷却方法の革新

ISO (60cm) (2000L He 2.6t)

HERSCHEL (3.5 m) (No Cryogen 2.6t)

Why SPICA?

Small Telescope Big Telescope


Huge Gain of Sensitivity !!!

2.5 orders

SPICA SPICA

1.5 orders

SPICA/SAFARI: TES detectors

TESTES

Ta absorberTa absorber SiSixxNNyy legslegs

TESTES

Ta absorberTa absorber SiSixxNNyy legslegsStraight leg:

not possible to realize required isolation for small pixels

SRON: a novel “parallel, straight leg” design and result

SRON: Focal Plane Array assembly

• Detector size hard limit: 90mm (4") Resulting side size: 45mm (10 mm reserved

for fixtures, structure)

• LC resonator chip-size estimate: 35x50mm for 2 channels of 160 pixels each

• Using this LC chip without folding allows for

a maximum of 12 channels (43x43 pixels) and a 50mK height of appr. 50mm.

• Required area for coil coupling on the

detector allows for 64x64 pixels based on current estimate. Thus this adds no

additional limitation.


SPICA FIR 35-210 m

SPICA FIR

arcmin

SPICA M IR 20-35 m - 30x5 arcsec

JWST MIRI 5-28 m - 4x4 to 8x8 arcsec

• JWST:

• 3 settings/ full waveband

• 30 hrs to get 10 sources

• SPICA:

• 30 hrs integration ~ same

sensitivity

Multiple sources in field -

comparable sensitivity

SPICA/JWST spectral volumes

superposed on deep GOODS 24m image

SPICA MIR/FIR: warm/cool gas + dust

SPICA multiplexing capability

SPICA instrument suite (NIR/MIR)

• Mid-IR Camera+Spectrometer (Japan) • Operating wavelength 5-38m

• Photometric + spectroscopic capability

• Camera: FoV ~6’x6’

– Spectroscopic: R~200 (5’ slit), R~700 (12”x6”/12),

R~30,000 (0.72/1.2”x3.5/6”: 4-8/12-18m)

High resolution spectroscopy NOT possible with JWST

• Mid-IR coronograph, SCI (Japan) • Operating wavelength 5-27m (possibly down to 3.5m)

• ~1’ x 1’ FoV

• Pupil mask: >106 contrast; Inner Working Angle ~3.3/D

• R~20 and 200

Spectroscopy NOT possible with JWST coronagraph…

(+ SCI cleaner PSF/higher contrast due to monolithic mirror)

• FPC-S: Focal plane guidance camera (Korea) • H, K, 2-5um, Imaging (R~3) + low resolution spectroscopy

(R~50 using LVF)

• 5’ x 5’ FoV

• SAFARI

• (European-lead+Canada+Japan):

• Imaging FTS, various R resolutions • 34-210m • FoV 2’x2’ • R~3 (photometry); R~50-100 (SED-mode); • R~2000 @ 100 µm (spectroscopy)

• 3 bands (simultaneous):

• 34-60/60-110/110-210 µm • 64x64, 38x38, 20x20 pixels (~6000 pixels total) • Diffraction-limited

• High sensitivity detectors • NEP = 2x10-19 W/√Hz → TES detectors (<100mK)

PI: SRON, NL (P. Roelfsema)

SPICA instrument suite, cont. (FIR)


Since ISO only mission covering full IR range!!


New IOB design


SAFARI European SPICA Instrument

4 detector techn. study:

•Photoconductors

• Si Bolometers

•KIDs

•TES

Detector Selection

June 2010

TES


Participación española en SPICA (2006-7)

• CDTI ESAC Run second SOC

–User Support

–Proposal handling

–Observation planning

–Data processing, archiving and distribution

•Possible Spanish contributions:

–DAMIR, ICC, Electrónica de control

–IAC Warm-electronics, EGSE

•Coste aproximado de la participación española 4-5 M€


Participación española en SPICA (2008)

• CDTI ESAC Run second SOC

–User Support

–Proposal handling

–Observation planning

–Data processing, archiving and distribution

–ICC: pipeline??

•Possible Spanish contributions:

–DAMIR, ICC, Electrónica de control (cryocooler), mecánica: •FTS mechanism

•Subsystem structure

–IAC Warm-electronics, EGSE

•Coste aproximado de la participación española 5-8 M€


•Francisco Najarro (HoN) & Javier R. Goicoechea (Gal. Project Scientist)

•ICC. Ground Segment contribution + Running 2nd SOC (CDTI)

•Lead Structural Engineer (CAB)

•FPU chassis (horizontal & vertical Optical Bench, cover(s) and other

structural elements (CAB + INDUSTRY)

•Camera Optics Bay on optical bench including warm alignment .

•All mirrors (INTA + INDUSTRY)

•Input Optics Module, Filter Wheels & Alignment Engineer (INTA)

•Test house for end-to-end optical performance testing (AITV) (INTA)

•Contributions to ICC (CAB)

•Contributions to EGSE (IAC)

•Cooperate in context of Calibration testing e.g. with CSL (CAB-INTA)

•FPA testing (incl. cryostat) of one of the TES bands (CAB)

•Coste aproximado de la participación española 25 M€

Co-PI

Participación española en SPICA (2008) Participación española en SPICA (2010)

SPANISH ORGANIZATION & TEAM

Jesus Martin Pintado (CAB)

Amaya Moro-Martin(CAB)

José Cernicharo(CAB)

Guillermo Muñoz-Caro(CAB)

Luisa Lara (IAA-CSIC)

Ismael Perez-Fournon (IAC)

Ignasi Ribas (ICE-CSIC)

Almudena Alonso Herrera (DAMIR)

Pablo Perez Gonzalez( UCM)

Armando Gil de Paz (UCM)

Paco Najarro (HoN)

Science Coordination

Paco Najarro CAB

Galactic Project Scientist Javier R. Goicoechea

Engineering Management

Javier Gomez-Elvira (PM)

FPU

Josefina Torres (CAB) Filter Wheels & Opt. Input Module

Luis Gonzalez Fernandez (INTA)

Tomás Belenguer (INTA)

Carmen Pastor (INTA)

Manuel Reina Aranda (INTA)

Lola Sabau (INTA)

Detectors & Calibration

Juan Bueno Lopez (CAB)

Nuria Llombart (UCM)

Electrical Eduardo Sebastian (CAB)

EGSE Ismael Perez-Fournon ( IAC )

ICC Eduardo Sanchez(CAB)

LNA Juan Daniel Gallego(Yebes) TBC

II. STATUS OF THE MECHANICAL WORK : FPU PHASE A

PHASE A: 38Kg 20%margin, 150Hz first mode

July 09

Sep 09


SAFARI: SpicA FAR infrared Instrument

imaging Fourier Transform Spectrometer (iFTS)


FPU - Structure

Payloads and Space Instruments Area

14/06/2011-Area Cargas Utiles FW TEAM 26 / 2

FILTER WHEEL STATUS 1-FW Rig:

-Material Compatibility

Disc: Ti and Al.

Pinion: Torlon and Vespel.

-Position Sensors

Survival and Operation at 20K.

-Stepper Motor.

Survival and Operation at 20K.

• Status

• Japan: Official JAXA pre-project, final approval to progress anticipated to be made in 2011 (Japanese FY). SPICA passed the System Requirement Review (SSR) on 8th September 2010 (by the Steering Committee for Space Science).

• FPIs under review given mass and budgetary constrains.

• Europe:

• 2007: SPICA selected as M-class candidate mission by ESA.

“Assessment phase” concluded.

• 2010: “Mission of Opportunity” in the framework of ESA Cosmic Vision,

• final decision to progress awaiting project approval by JAXA.

(likely in end 2011 beginning 2012 bound to JAXA).

• USA: Discussions on how NASA will participate are underway.

• “Decadal review“ conclusions: need FIR, need SPICA

SPICA today

Paco Najarro – CDTI CV 09

•SPICA and Cosmic Vision • Advantages of SPICA in the Cosmic Vision competition

- Strong science case which is very relevant to Cosmic

Vision themes

- Well-developed mission concept

- Satisfies a large European FIR community for another

decade

- Builds on and extends European industrial capabilities

- Low cost to ESA – good value for money (MoO) - Major international collaboration

Arigatô

Participación Española en SAFARI/SPICA · 2011-07-04 · Paco Najarro – SEA 2010 Participación...

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