The Promise of the SPICA Observatory Marc Audard on behalf of the SPICA Collaboration

Ecogia Science meeting, 02.09.2019 FACULTÉ DES SCIENCES Département d'astronomie

SPICA science instrument payload

The SPICA payload has three main components; the SPICA Telescope Assembly (STA), a 2.5- meter diameter telescope cooled to below 8 K, and the plane instrument assembly with the instruments: SAFARI, a far-IR grating spectrometer and imaging polarimeter, and SMI, a mid-IR spectrometer/imager. The instruments also are maintained at cryogenic temperatures to achieve the required background-limited sensitivity.

Spacecraft and payload configuration The overall configuration of the SPICA spacecraft is shown in Figure 3-1, with the service module (SVM) below and on the top the payload module (PLM) with the Science Instrument Assembly (SIA), and the Cryogenic Assembly (CRYO) housing the passive and active cooling system for the SIA. The right hand panels in Figure 3-1 show the layout of the instruments and the two Focal Plane Attitude Sensors (FAS #1 and #2, part of the overall spacecraft pointing system) on the telescope optical bench (TOB) and the focal plane layout. The two science instruments together provide continuous spectroscopic coverage over the full 17 to 230 μm domain, with a wavelength resolution R between a few hundred and a thousand, combined with various efficient large area imaging and polarimetry modes at 100, 200 and 350 μm. By inserting a Martin-Puplett interferometer in the SAFARI/SPEC signal path the resolution can be further increased to R~1500-11000, allowing more detailed line profile studies. SMI provides a still higher resolution (R~28000) capability in the 12 to 18 μm window. SMI will also allow efficient, high sensitivity mapping of large areas in the 17 to 36 μm domain (see Figure 1-22). Both instruments utilise state-of-the-art detector technologies, which in combination with the cold 2.5-meter aperture provide the high sensitivity required to fulfil the main science goals (see Figure 1-2).

The Far-Infrared instrument SAFARI

The SAFARI spectrometer - SPEC With the evolution science outlined in section 1.1 as its main science driver, the SAFARI/SPEC spectrometer is primarily optimised to achieve the best possible sensitivity, within the bounds of the available resources (thermal, number of detectors, power, mass), at a moderate resolution of R~300, SPICA – An ESA/JAXA missionwith instantaneous coverage over the full 34 to 230 µm range. A secondary driver is the requirement to also study line profiles at higher wavelength resolution, e.g. to discern the in-fall and outflow of matter from active galactic nuclei. This leads to the implementation of an additional high resolution mode using ESA-led mission a Martin-Puplett interferometer to analyse the signal. With this design, the sensitivity of the R~300 SAFARI/LR mode will be about 5 x 10-20 W/m2 (5σ, with large JAXA contribution 1hr) for a TES (Transition Edge Sensor) detector NEP of 2 x 10-19 W/√Hz, compatible with the •‘ configuration’ sensitivity requirement as dictated by the SPICA • Size - ø4.5 m x 5.3 m science drivers (see Table 2-2). The design allows for further improvements in TES performance, • Mass-3450 kg (wet, with margin) these will directly lead to better overall instrument • Mechanical coolers, V-grooves sensitivity. •2.5 meter telescope, < 8K Figure 3-1 The SPICA spacecraft configuration. The scientific instruments are mounted on the – Warm launch optical bench on the rear of the telescope as shown •12 -230 μm spectroscopy in the middle panel. The SPICA instrument focal plane layout is indicated in the right panel. – FIR spectroscopy – SAFARI – MIR imaging spectroscopy – SMI – FIR polarimetry – B-BoP •Japanese launcher, L2 •5 year goal lifetime

Selected as M5 candidate mission 22 Ongoing Phase A Mission Selection Review (Apr 2021) à downselection from 3 to 1 mission Cryogenics to cool telescope and instruments

• Active cooling to 4K and 1.7K – Detector modules at 50mK with dedicated mK coolers (SAFARI, B-BOP) • V-grooves – passive cooling to 40K • Detachable support struts

4K JT

20K ST TheThe SPICA ‘sweet spot’ SPICA ‘sweet spot’– –the dusty universethe dusty universe

A unique observatory looking through the veils, enabling transformational science 106 reduction in background!

<8K

SPICA What is so unique? • A COLD, big mirror → true background limited Mid/Far-IR observing >2 orders of magnitude better raw sensitivity than Herschel • A cold, big mirrorà true background limited observing • ~20 to ~350 μm inaccessible for any observatory >2 →orders of magnitude better raw sensitivity than the wavelength domain where obscuredHerschel matter shines • ≈20 to ≈350 fillμm theinaccessible for any blind spot between JWSTobservatory and ALMA @ R~ few 1000 à fill the blind spot between JWST and ALMA @ R≈ few 1000 SAFARI/SPICA consortium mtg. #17 - mission status overview - P. Roelfsema 3

Figure 3-5 Left: A Martin-Puplett interferometer: a linearly polarised input signal is divided over two arms of the interferometer using a 45° grid. In both arms the beam goes via a flat mirror to a moving and a fixed rooftop and back, thus the polarization rotates 3 times by 90°. This 270° rotated signal from the left arm is transmitted through the grid while from the right arm it is reflected, allowing the recombined beams to interfere. By moving the central rooftop mirrors over a distance Δx an optical path length difference of 8Δx is created between the two arms. The interference pattern, encoded in the polarization of the output signal, can be recorded by the grating module, due to its inherently linear polarization. Right: The SAFARI/HR optical layout. The high resolution mode optics – the Martin-Puplett Interferometer In the high-resolution SAFARI/HR mode the signal is passed through a Martin-Puplett interferometer (Figure 3-5) imposing a modulation on all wavelengths entering SAFARI/SPEC. The resulting interference that occurs between the two beams of the interferometer is then distributed to the grating modules (Figure 3-4) of the four bands and post dispersed by the corresponding grating onto the detectors.

When the interferometer is scanned over its full optical displacement each of the detectors will measure a high resolution interferogram convolved with the grating filter function for that particular detector. Upon Fourier transformation, an individual interferogram produces a small bandwidth, high resolution The SPICA instrumentsspectrum. By combining the spectra from individual detectors a full spectrum at high resolution is obtained. In the current design a mechanical displacement of about 3 cm is envisaged, leading, with a folding factor of 8, to a maximum optical displacement of 25 cm. A short section of the mechanism stroke must be devoted to a short double-sided optical path difference measurement to enable phase SMI correction of the interferogram through accurate identification of the zero path difference position. The available Optical Path Difference • LR-CAM –(OPDlarge area low resolution surveyor) yields spectra with a resolution ranging from R~1500 at 230 • 17 – 36 μm, R = 50 µm to as high as– 120R~11000 at the shortest wavelength of 34 µm. • 4 slits (10’ long) with prism The SAFARI/SPEC Focal Plane Unit • Camera mode 10’x12’ FoVThe SAFARI/SPEC Focal Plane Unit (FPU) as it is mounted against • MR – medium resolution mapperthe back of the telescope is shown in Figure 3-6. The beam from the telescope secondary comes from the top left and is sent into the • 18 – 36 μm, R = 1200 instrument via the– pick2300,-off mirror on the top of the instrument box. • 1 slit (1’ long) with gratingFrom there it goes into the Offner relay optics and on to the Beam and Mode Distribution Optics. On the right the Martin-Puplett signal • HR – molecular physics/kinematicspath and its moving mirror stage can be seen. Three of the four • 12 – 18 μm, R = 28,000 (grating modules (red:à VLW,33,000) yellow: MW and green: SW) are visible on the bottom, the LW band GM (orange) isSAFARI at the back. Between Figure 3-6 The SAFARI/SPEC • 1 slit (4” long) with immersion gratingthe MW and SW grating modules the cooler unit (grey) is visible. • R≈300 mode à 1hr/5σ focal plane-5-7x10 unit. -20 W/m2 The SAFARI coolers • Martin-Puplett Interferometer to provide To cool the TES detectors to their 50 mK operating temperature, a dedicated hybrid ADR/Helium sorption cooler is used. The cooler design buildshigh -onR mode (R≈2000 heritage from the Herschel-11000) and Planck missions. B-BoP A full design has already been carried out for• 4 bands instantaneously covering 35 SAFARI, leading to the construction of an Engineering-230 µm 25 Polarization sensitive • Limited imaging capability: 3 pixels on-sky bolometers • 3 bands: 70, 220, 350 μm; simultaneous observations 2.5’x2.5’ An observatory for the community

• Observing time: mission will be open for all astronomers

– Guaranteed v.s. open time details TBD – Detailed implementation of e.g. ‘Key projects’ TBD – Time Allocation Committee

• International community oversight/cooperation – SPICA collaboration ≡ 3 instruments + overall SPICA (science) consortium – SPICA Science Study Team (ESA installed) – represents science community 6 – Later; Science advisory committee, SPICA executive board, TAC etc. The SPICA project

• Joint ESA-JAXA project – ESA overall responsibility – JAXA major partner …instruments also significant partner – Challenging organization – Total mission cost ≈ 1 billion €

‘European’ instruments JAXA ESA

7

Scientific Advisory Board on the basis of scientific merit. The SAB will subsequently ratify the observation programme with the priorities proposed by the TAC. It will also be the role of the SAB to Swiss involvementdefine what should be the proportion of KP in the OT.

In the nominal 3-year mission the first six months will be used for cooling of the telescope, and verification and validation of the observatory and its instruments. OT proposals will be assigned the largest fraction of theSwitzerland remaining 2.5 years,in whilecharge a more ofmodestdesigning part (<40%) andwill be dedicated to GT and a small (<5%) part will be reserved as DDT. In a possible mission extension, the proportion of GT will be small (< 10%),producing the DDT will remainthe the samehousing (< 5%) andstructure most of the timeand will be OT open to the world wide community. Details of the categories and time allocation are subject of discussions in Phase A between SPICA missionthermal/mechanical partners, and will be formalisedsuspension in the SPICA tosciencethe management plan. Figure 5-4 shows thefocal present planeconcept forunit the timefor divisionthe overSW/MW programmebands categories. The SPICA project is responsible for level 2 processing of the data, i.e., correction of instrument specific features and calibrationof the to makeSAFARI the data gratingready for scientificmodules analysis. SPICA data will be initially delivered to the proposers of the observations for scientific analysis. All science data will be archived, and after a proprietary period of one year open for access to the world-wide astronomical community.

Instrument consortia Switzerland leads the SAFARI Instrument Control SAFARI Centre, which is responsibleThe far-infraredfor instrumenti) software SAFARI willfor be provided by a consortium of institutes from calibration, characterizationEurope, Canadaand, the analysisUS, Japan andof Taiwan.the SAFARI instrument,Theii) basisinput for the SAFARIfor consortiuminstrument has been established already quite a number of years operations procedures,ago; led by SRONiii) for the Netherlands,monitoring with as major partners Spain France and the US, and instrument health,further iv) significantdefining/validating contributions from Italy, Belgium, Canada, Germany, the UK, Austria, observing modes, v)Switzerland,calibrating Sweden,the and Tinstrumentaiwan. Funding for the instrument will be provided directly by the during operations, etcparticipating… institutes and by national agencies. Figure 5-5 SAFARI management structure

The SAFARI consortium management structure is indicated in Figure 5-5. The project is led by the SAFARI principal investigator, who is also acting as the prime contact to the SPICA project. The ‘Heads Prodex funding for Phase A studies until Mission Selection Review (Sep 2021)of Nations’ represent the countries that support the SAFARI project, and address programmatic constraints and possibilities of the different participating nations and, together with the Co-PI’s, advise the PI on strategic, programmatic and when relevant on technical and science issues. The SAFARI project manager is responsible for the implementation and verification of the SAFARI instrument and its Instrument Control Centre, within the programmatic constraints set by the PI and the heads of nation.

For some years the consortium has already actively carried out research and development to establish an instrument design. In parallel with this process a distribution of responsibilities over the participating nations and institutes, commensurate with their (technical) capabilities and (funding) possibilities, has been established. Table 5-1 lists the current foreseen division of tasks for the partners supporting the SAFARI project (this is also schematically indicated in Figure 3-2). Additionally, all listed partners in any case expect to contribute to the implementation of the SAFARI ICC. The final division of responsibilities will depend on available funding in the partner countries and to some extent on technical trades and progress during Phase-A. It will be further optimised during Phase A to maximally utilise the expertise and resources available within the consortium. Additionally, interactions are ongoing with several institutions that have indicated a serious interest to contribute to the SAFARI project; in particular discussions with the Copernicus Astronomy Centre in Torun/Poland and the in Budapest/Hungary show great promise to lead to a concrete collaboration in the SAFARI hardware development. 45

The Promise of SPICA

10 pc

1 pc SPICA mission design drivers

• What are the roles of , accretion onto and feedback from central black holes and supernovae in shaping galaxy evolution over cosmic time?

• How are metals and dust produced and destroyed in ? How does the matter cycle within galaxies and between galactic discs, halos and intergalactic medium?

• How did primordial gas clouds collapse into the first galaxies and black holes?

• What is the role of magnetic fields at the onset of star formation in the Milky Way?

• When and how does gas evolve from primordial discs into emerging planetary systems?

• How do ices and minerals evolve in the planet formation era, as seed for Solar Systems? Star formation and black hole accretion

Why is the rate of galaxy evolution changing so dramatically over time?

Star formation feedback? AGN/quasar feedback?

SFR densities in the UV, uncorrected for dust Black hole accretion history from X-ray (red extinction (blue) in the far-IR (red), and in total line and green shading) and IR data (blue (i.e., UV+far-IR, green). (Burgarella et al. 2013). shading). (Madau & Dickinson 2014). High-velocity AGN-driven outflows

Local z=0.04 ULIRG OH spectra (Herschel/PACS) Dark blue: quiescent gas, light blue: high velocity outflow (1700 km s-1, -1 -1 100 Msun yr sr ), dashed light blue: low velocity outflow, green: low excitation Gonzalez-Alfonso 2014, A&A 561

SPICA simulation:

Mrk 231 @z 1,1.5,2 OH 85µm R≈300

10-30 Jy… Mrk 231 is too bright for SPICA/SAFARI à SPICA will do this for many objects out to z≈1.5-2! Evolution of infrared-luminous galaxies

Far-infrared diagnostic tools • Line-ratios à physical state of dust and ionised gas • Line profiles à outflow/infall, cycling of matter • Line strengths à metal enrichment • Discriminate between Active Galactic Nucleus and star formation

So far only we ‘only’ sampled the ‘local Universe’… …SPICA measures physical conditions 10 Gyr ago Spinoglio et al. 2017 Charting the unknown – SMI LR/CAM surveys

R=100@z=3 Large area blind R = 50–120 Multi slit survey 20 25 30 35 slit 10’x3.7” λ (µm) – 10 deg2 ≈ 600 hr – 300 x 2 hr/field (10’x12’) AGNs at z > 1 • Galaxy population 240,000 at 34 µm • Dust in galaxies • Stars with debris disks • … à follow up with SAFARI PAH galaxies z > 0.5 and SMI/MRS 82,000 spectra 3.2Debrisx3.2 disk (14,000 for z ~2-4)

3.3’x3.3’ 20 25 30 35 Spitzer / IRS-LL λ (µm) R = 60 – 120 For comparison: MS stars (F, G, K) Area for ≈600 hr surveys at similar depth JWST / MIRI-MRS 2’x2’ 11,000 spectra with Spitzer or JWST R = 2000 ~2000 debris disks >50 zodi. The first galaxies – H2 and PAH at ≈1 Gyr

Simulated SPICA observations of lensed galaxies at high redshift (z≈8/10 hr) - PAH features readily detected

- Shocked H2 lines out to high z

(C24H12)8

SPICA accesses PAH and silicate features at z≈5-7 beyond JWST à grain chemistry of the first dust Magnetic fields as driver of star formation?

Example: Taurus B211 filaments

Herschel 250 µm and PLANCK magnetic field

2.7 deg ≈ 3 pc

Herschel @5"-10" – galactic dust in thin filaments • E.Ntormousi • PLANCK @5' – large scale magnetic field seems perpendicular to filaments…and parallel to striations B-BOP will probe the link between magnetic field, low-density filaments (striations) and dense star-forming filaments characteristic filament width of 0.1 pc observable out to d ~ 350 pc Star and Planet Formation and Evolution

Unique areas of planet formation for SPICA: • The water trail à tracing the snow line • From pristine dust to differentiated bodies à making the link to the Solar System • The gas revolution: à measuring the gas reservoir in planet forming regions • Gas dissipation and photo-evaporation à setting the clock for planet formation HD – probing the mass of planetary disks

• HD 56/112 µm lines in the SAFARI bands – Direct tracer of gas mass in PPD’s Bergin et al. 2013 – Herschel detected HD J=1-0 in 3 disks! – Opens entirely new domain of disk masses

1 hr

10 hrs

Trapman et al 2017 1. LocatingH2O line profiles: snowlines and gaps/holes the H2O snow line

symmetric rings/gaps

spiral arms

Snow Line

[ALMA and SPHERE substructure in disks: ALMA Partnership 2015, Benisty et al.

2015, Kataoka et al. 82016] 3-10 hr holes T Tauri disk integration time

out in Science goals SMI: • gas disk dispersal processes – snow line Herbig disk and gaps/holes opening in inner disks

[17.8 µm water line profile by T. Onaka based on disk models: Notsu, Nomura et al. 2016a,b] Dust polarization in disks

3.1 mm (ALMA Band 3) HL Tau HL Tau [Kataoka et al. 2015] scattering alignment with radiation

[polarization changes with increasing wavelength from self-scattering to alignment due to anisotropic radiation field: Kataoka et al. 2017, Stephens et al. 2017]

Science goals B-BOP: • detect and resolve polarization at far-IR wavelength for bright nearby debris disks, e.g. b Pic, , Fomalhaut, e Eri, t Cet • characterize grain sizes, porosity and alignment mechanism Gas dissipation/photo-evaporation

[Pontoppidan et al. 2011 jet Baldovin-Saavedra et al. 2012 Aresu et al. 2012]

[NeII] shift observed vs modelled profile [Pascucci et 2012] al. [Pascucci

wind

[H2 S(1) and S(2) non-detections: Carmona et al. 2008; H2 predictions from disk models: Nomura et al. 2008] disk

Science goals SMI/HRS and MRS: • gas disk dispersal processes – trace directly launching of inner disk hot gas

Tracers: H2 S(2)+S(1) and S(0) (SMI/MRS more sensitive than JWST/MIRI), [Ne II], HD (compl. to SAFARI), other lines, e.g., [Ne III] à discriminate EUV/X-ray irradiation, [Fe II] Mineralogy – e.g. debris discs

The mineralogy of micron-sized dust particles in discs directly probes the composition of their parent bodies • SPICA provides access to the far-IR resonances of several minerals, allowing a precise determination of their composition and structures • Access to the composition of refractory dust de Vries et al. (2012) in exo-comets and make a direct comparison with our Solar System Ice histories: Pristine versus disk origin

Ices in emission @ 40 and/or 60 mm SPICA will probe the history of [TT: McClure et al. 2013, 2015; HAe: Malfait et al. 1999, à Meeus et al. 2001, Min et al. 2016] water ice in hundreds of T Tauri disks

1.00 crystalline ice (140 K, reference) cooldown (formed in warm environment, transported in disk) 0.95 direct deposit (formed in situ in disk)

/s] warmup (formed in cold environment, 2 transported in disk) 0.90 erg/cm -10 0.85 [10 ν F ν 0.80 includes noise of 10 min exposure (R=300)

0.75

0.70 40 50 60 70 80 λ [micron] Zodiacal analogous with SPICA

Calcite CaCO3 Spitzer (Prev. works) Olivine (Mg,Fe)2SiO4 (Kobayashi&Tanaka 10)

) Pyroxene (Mg,Fe)SiO3 Dolomite CaMg(CO3)2 / F

disk 20 40 60 µm 20 40 60 µm F ( Silicates Phyllosilicates, formed Carbonates Solar system at high-T formed at Disk flux low-T with

CO2 & H2O

Stellar age (Gyr) Survey of fainter disks including zodi analogous → high sensitivity & stability Slide from D. Ishihara SPICA 2019 conference Summary

• SPICA: a mid-far infrared space observatory • 2.5 m diameter mirror, actively cooled to 8 K à unprecedented sensitivity in mid/far IR Spectroscopy/photometry of the obscured universe, straddling the gap between JWST and ALMA

• SPICA - joint ESA-JAXA project • Mission final selection – 2021 • Phase 0/A - started re-iteration of capabilities and design • Science goals/capabilities to be revisited/upgraded

SPICA information: www.spica-mission.org