SPICA Space Infrared Telescope for Cosmology and Astrophysics
Eiichi Egami Steward Observatory, University of Arizona
on behalf of the SPICA consortium US is now an official SPICA SAFARI consortium member!
• NASA is already providing funding support for the SPICA/ SAFARI (=far-IR spectrometer) detector development.
• Matt Bradford (JPL) is leading this effort, actively working with the SAFARI team at SRON (The Netherlands).
• As a result, US researchers can now join the SAFARI consortium and take part in SAFARI activities.
• We are starting to create a mailing list for interested US researchers, so please contact me today or by email later ([email protected]). Please spread the word! Outline
• Motivation
• What is SPICA? + current status/next steps
• Instruments - SAFARI, SMI, & B-BOP
• Extragalactic reference surveys
• Summary Power of Cold Telescope in the Far-Infrared What is SPICA?
Herschel-heritage telescope
Planck-heritage spacecraft What is SPICA?
• Mid-/Far-IR space observatory with a D=2.5m telescope cooled down to < 8K and with 3 Herschel-heritage scientific instruments (SAFARI, SMI, and B- telescope BOP).
Planck-heritage spacecraft What is SPICA?
• Mid-/Far-IR space observatory with a D=2.5m telescope cooled down to < 8K and with 3 Herschel-heritage scientific instruments (SAFARI, SMI, and B- telescope BOP).
• ESA (Europe) - JAXA (Japan) collaboration with some US involvement now (PI: Peter Roelfsema, SRON; concept originated in Japan in late 1990’s).
Planck-heritage spacecraft What is SPICA?
• Mid-/Far-IR space observatory with a D=2.5m telescope cooled down to < 8K and with 3 Herschel-heritage scientific instruments (SAFARI, SMI, and B- telescope BOP).
• ESA (Europe) - JAXA (Japan) collaboration with some US involvement now (PI: Peter Roelfsema, SRON; concept originated in Japan in late 1990’s).
• Will be launched by JAXA’s next-generation H3 launch vehicle (into L2 orbit).
Planck-heritage spacecraft What is SPICA?
• Mid-/Far-IR space observatory with a D=2.5m telescope cooled down to < 8K and with 3 Herschel-heritage scientific instruments (SAFARI, SMI, and B- telescope BOP).
• ESA (Europe) - JAXA (Japan) collaboration with some US involvement now (PI: Peter Roelfsema, SRON; concept originated in Japan in late 1990’s).
• Will be launched by JAXA’s next-generation H3 launch vehicle (into L2 orbit).
• Nominal mission life time = 3 yrs (goal = 5 yrs), likely determined by the lifetime of mechanical coolers & supply of spacecraft Planck-heritage propellant. spacecraft SPICA’s power = Spectroscopic sensitivity
Roelfsema+2018
Circinus
SED ~2 orders of scaled to mag better 12 LIR=10 L⦿
Note that D=3.5m Herschel has already hit the sky confusion limit in imaging at >100 μm. Current Status & Next Steps Current Status & Next Steps
• In May 2018, SPICA was selected as one of the three M5 mission candidates out of 25 proposals. The other two are Theseus (high energy transient survey) and EnVision (Venus orbiter). Current Status & Next Steps
• In May 2018, SPICA was selected as one of the three M5 mission candidates out of 25 proposals. The other two are Theseus (high energy transient survey) and EnVision (Venus orbiter).
• The SPICA consortium is actively working together to define the mission design and prepare the final ESA M5 proposal. Current Status & Next Steps
• In May 2018, SPICA was selected as one of the three M5 mission candidates out of 25 proposals. The other two are Theseus (high energy transient survey) and EnVision (Venus orbiter).
• The SPICA consortium is actively working together to define the mission design and prepare the final ESA M5 proposal.
• The final M5 review will take place in April 2021 ➜ Next 1.5 years is critical for the preparation of a successful proposal! Current Status & Next Steps
• In May 2018, SPICA was selected as one of the three M5 mission candidates out of 25 proposals. The other two are Theseus (high energy transient survey) and EnVision (Venus orbiter).
• The SPICA consortium is actively working together to define the mission design and prepare the final ESA M5 proposal.
• The final M5 review will take place in April 2021 ➜ Next 1.5 years is critical for the preparation of a successful proposal!
• SPICA Science Study Team is expected to send out an announcement to the world-wide community soon, soliciting participation of interested researchers. SAFARI SPICA Far-IR Instrument
• PI: Peter Roelfsema (SRON, The Netherlands)
• Single-object spectrometer covering 35-230 μm with 4 bands (31-56, 54-89, 87-143, & 140-230 μm)
• LR mode: R~300, 5x10-20 Wm-2 (5σ, 1 hr)
• HR mode:
• With a Martin-Puplett interferometer inserted in front of the spectrometer.
• R~11000@35 μm ➜ R~1500@230 μm SMI SPICA Mid-IR Instrument
• PI: Hidehiro Kaneda (Nagoya University, Japan)
• LR spectroscopy (more later)
• R=50-120, 17-36 μm, with prism
• Four 600”x3.6” slits
• Covers 12’x10’ in 90 2” steps
• 34 μm (R=5) imaging with the slit-viewer camera, 12’x10'
• MR: R=2000,18-36 μm, 60”x3.7” slit
• HR: R=28000,12-18 μm, 4”x1.7” slit B-BOP (Previously known as POL)
• PI: Marc Sauvage (CEA, France)
• Far-IR Polarimetric camera
• 110, 220, 350 um, 160”x160”
Taurus B211 filaments (SPIRE 250 μm; Planck B-field) Mission Operation
• 0.5 yr for commissioning
• Nominal mission (2.5 yrs)
• <40% GT
• Extended mission (+2 yrs)
• <10% GT
• Observing time open to the world-wide community
• Data proprietary period = 1 yr SPICA White Papers
• PASA Collection: Exploring Astronomical Evolution with SPICA
1. SPICA Mission (Roelfsema+2018)
2. Extragalactic science overview (Spinoglio+2017)
3. SMI low-resolution spectroscopic survey (Kaneda+2017)
4. SMI 34 um imaging survey (Gruppioni+2017)
5. Rise of metals and dust (Fernandez-Ontiveros+2017)
6. Molecular inflows/outflows (Gonzalez-Alfonso+2017)
7. Nearby galaxies (van der Tak+2018)
8. SAFARI high-z (z>5) science (Egami+2018)
9. B-BOP polarimetric camera (Andre+2019, submitted) Extragalactic Reference Surveys
1. SAFARI spectroscopic survey
2. SMI spectroscopic survey
3. SAFARI 34 μm imaging survey
4. SAFARI spectroscopy at z>5 1. SAFARI Survey
MCG-3-34-64 (nearby active galaxy) 12 Spectra scaled to LIR=10 L⦿
• Obtain SAFARI low-resolution spectra (R~300; 35-230 μm) of ~1,000 galaxies up to z~4 in 2000 hours.
• Should be able to sample 12 LIR=10 L⦿ galaxies up to z~3.
Spinoglio+2017 Line Detectabilities
Spinoglio+2017 2. SMI Survey
PAH mapper
• Wide - 10 deg2, 600 hrs, Texp=90s
• ~5x104 PAH galaxies at z>1 (~104 13 at 2 • ~2x105 AGN (z>1) at 34 μm • >1x104 spectra for main- sequence F, G, K stars. • 1x103 debris disks Deep z=3 12 LIR=10 L⦿ • Deep - 1 deg2, 600 hrs, Texp=1170s Kaneda+2017 3. SMI 34 μm Imaging Survey • Confusion limit is lower at 34 μm due to smaller beam (~ 9 μJy, 5 σ) ➜ can penetrate deeper. • At higher redshift, 34 μm samples the trough between stellar and dust SEDs ➜ sensitive to AGN. SMI 34 um Gruppioni+2017 4. SAFARI spectroscopy at z>5 Egami+2018 13 Discoveries of Hyper-Luminous (LIR>10 L⦿) Dusty Star-Forming Galaxies (DSFGs) at z>5 Lensed DSFGs at z=5-6 DSFG = Dusty Star-Forming Galaxy Simulated SAFARI spectra using template SED/spectra for local IR-luminous galaxies Low-Metallicity Galaxies at z=8? Rest Wavelength (µm) Rest Wavelength (µm) 6 7 8 9 10 20 6 7 8 9 10 20 3.0 3.0 13 13 (B) Haro11 SED at z=8 (LIR=2´10 Lô) (C) IIZw40 SED at z=8 (LIR=2´10 Lô) 2.5 0.6 2.5 0.6 [S III] 0.5 Weak PAHs 0.5 No PAHs 2.0 0.4 0-0 S(5) 0-0 S(3) 2.0 0.4 0-0 S(5) 0-0 S(3) 0-0 S(4) [Ne III] 0-0 S(4) 0.3 0.3 [S III] 1.5 0.2 1.5 0.2 [Ne III] 0.1 0.1 1.0 0.0 1.0 0.0 50 60 70 80 90 100 110 120 50 60 70 80 90 100 110 120 Flux density (mJy) PAH Flux density (mJy) 11.3 [S IV] [Ne II] 0.5 PAH [S IV] [Ne II] 0.5 PAH 7.7 PAH + 6.2 8.6 PAH 12.7 0.0 0.0 40 50 60 70 80 90 100 200 40 50 60 70 80 90 100 200 Observed Wavelength (µm) Observed Wavelength (µm) Simulated SAFARI spectra using local blue compact dwarf (BCD) SED + mid-IR spectra Silicate Mineralogy (Li’s talk) z>5 Quasars Egami+2018 Xie, Li, & Hao (2017) Molecular Hydrogen (H2) Emission ⬇ ⬇⬇ ⬇ ⬇ Can SPICA detect H2 emission from metal-free (Pop III) forming galaxies? First Stars, Dust, & Galaxies See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission • First dust See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission • First dust • Formed in the explosions of pair-instability SNe (= Pop III SNe with M~140-260 M⦿) and possibly emits strong quartz (SiO2) emission (9, 12.4, and 21.5 μm). See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission • First dust • Formed in the explosions of pair-instability SNe (= Pop III SNe with M~140-260 M⦿) and possibly emits strong quartz (SiO2) emission (9, 12.4, and 21.5 μm). • First galaxies See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission • First dust • Formed in the explosions of pair-instability SNe (= Pop III SNe with M~140-260 M⦿) and possibly emits strong quartz (SiO2) emission (9, 12.4, and 21.5 μm). • First galaxies 8 • Formed in atomic cooling halos (e.g., Mh>10 M⦿ at z~10) cooling via H2 and Lyα emission (mid-IR fine-structure lines become important for 2nd-generation galaxies). See Egami+2019 for more discussion and references First Stars, Dust, & Galaxies • First stars 6 • Formed in dark-matter minihalos (Mh~10 M⦿) at z~20-30 cooling via H2 emission • First dust ➜ Next frontier! • Formed in the explosions of pair-instability SNe (= Pop III SNe with M~140-260 M⦿) and possibly emits strong quartz (SiO2) emission (9, 12.4, and 21.5 μm). • First galaxies 8 Far-IR• Formed spectroscopy in atomic cooling halos is essential (e.g., Mh>10 for M⦿ atprobing z~10) cooling via H2 and Lyα emission (mid-IR fine-structure lines become theimportant first-generation for 2nd-generation objects galaxies). See Egami+2019 for more discussion and references Summary • With its large (D=2.5m) cold (< 8K) telescope and sensitive/versatile instruments, SPICA will go ~100x deeper in mid-/far-IR spectroscopy. • SPICA project is now in the critical phase of mission definition/ preparation toward the final ESA M5 selection in 2 years. • US is now an official member of the SAFARI consortium (US lead: Matt Bradford@Caltech/JPL) • There is a significant amount of dialogue between the SPICA and OST teams to take advantage of the expertise in both communities. • We are creating a mailing list for the US SPICA/SAFARI team; Send email to [email protected] if you’re interested. • SPICA collaboration will also be opened up to the world-wide community soon, so stay tuned!