SPICA Mid-infrared Instrument...
Transcript of SPICA Mid-infrared Instrument...
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SPICA Mid-infrared Instrument (SMI) SPICA Italian Workshop @INAF Headquarters, 4-5 Apr, 2016
H. Kaneda D. Ishihara, S. Oyabu, T. Suzuki, M. Yamagishi, K. Murata (Nagoya Univ),
T. Wada, M. Kawada, N. Isobe, K. Asano (ISAS/JAXA), I. Sakon (Univ of Tokyo),
K. Tsumura (Tohoku Univ), H. Shibai, T. Matsuo (Osaka Univ), the SMI consortium
SMI: SPICA Mid-infrared Instrument by Japanese Consortium
Grating + Si:Sb w/ beam-steering mirror 18 – 36 mm, R = 1200 – 2300, slit: 1’ long
Immersion grating + Si:As 12 – 18 mm, R = 28,000, slit: 4” long
Multi-long-slit prism + Si:Sb w/ slit viewer 17 – 36 mm, R = 50 – 120, slit:10’ long, 4 slits
LRS
MRS
HRS
Three spectroscopic channels:
1/26 AKARI Mid-IR all-sky map
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Why we need SMI, besides JWST/MIRI ?
2/26
R~2000
R~30000 R~2000
10-21
10-20
10-19
10-18
10-17
10-16
Lin
e s
en
sit
ivit
y (
W m
-2, 1
hr,
5 s
)
MRS HRS
JWST/MIRI
JWST/MIRI
Spitzer/IRS
Spitzer/IRS
SAFARI
R=300
10 20 30 40 50
Wavelength (mm)
-21
-20
-19
-18
-17
10 12 14 16 18 20
HRS (R=25000)
TMT (R=120000)
Wavelength(µm)
-16
Log
(Dete
ctio
n lim
it [
W m
-2])
(5s
, 1 h
r)
TMT
HRS
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Why we need SMI, besides JWST/MIRI ?
3/26
10-21
10-20
10-19
10-18
10-17
10-16
Lin
e s
en
sit
ivit
y (
W m
-2, 1
hr,
5 s
)
10 20 30 40 50
Wavelength (mm)
R~2000
R~30000 R~2000
MRS HRS
JWST/MIRI
JWST/MIRI
Spitzer/IRS
Spitzer/IRS
SAFARI
R=300
LRS
R~100
-21
-20
-19
-18
-17
10 12 14 16 18 20
HRS (R=25000)
TMT (R=120000)
Wavelength(µm)
-16
Log
(Dete
ctio
n lim
it [
W m
-2])
(5s
, 1 h
r)
TMT
HRS
Improvements at l > 20 mm
HRS High survey speed
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Why we need SMI, besides JWST/MIRI ?
4/26
20 30 40 50
Wavelength (mm)
R~2000
1020
1021
1022
1023
1024
Fo
V / L
ine
se
ns
itiv
ity (
arc
se
c2 / (
W m
-2))
R~30000
R~2000
MRS
HRS
JWST/MIRI
JWST/MIRI
Spitzer/IRS
Spitzer/IRS
SAFARI
R=300
LRS R~100
1019
10
R~2000
survey speed
FoV / (Line sensitivity)
High
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Si:Sb 1K x 1K
Si:Sb 1K x 1K
Si:Sb 1K x 1K
MRS 18 – 36 μm
Slit-Viewer camera
fore optics
MRS slit
LRS multi-slit
Pick-up
Prism Grating
HRS 12 – 18 μm
LRS 17 – 36 μm
Shutter
Telescope focus
rear optics rear optics
1D beam-steering mirror
34μm band (fixed)
Si:As 1K x 1K
HRS slit
Immersion grating
No moving parts except for a beam-steering mirror and shutter.
SMI block diagram
R~2000 R~30000 R~100
5/26
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SMI: Detectors
Si:Sb: 1K x 1K, 2 arrays for LRS, 1 array for MRS
Si:As: 1K x 1K, 1 array for HRS
Si:Sb array: Spitzer/IRS 128 x 128, low QE at > 34 μm
SMI 1024 x 1024, improved QE (planned) 6/26
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SMI: Optical layout
Focus MRS
LRS
Slit-Viewer camera
HRS
Focal plane layout (TBD)
LRS
HRS
MRS
7/26
Focal-plane
Attitude Sensors SAFARI
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(1) Low-resolution spectrometer and camera
10’
12
’
1024 pix
3’
Dark
Dark
Detector: Si:Sb, 1K x 1K multi-slit format (4 long slits)
l/Dl as a function of wavelength Color: difference from slit to slit
Solid or dotted: difference within a slit
R=50
R=120
LRS
Wide FoV (4 slits, slit length 10’)
high continuum sensitivity
~30 mJy (1hr, 5s)
0.7”/pixel
R = 50–120 spectral mapping
10’x10’ slit viewer (34 μm, R = 5)
sensitivity: ~10 mJy (1hr, 5s) 8/26
LRS
Ohyama + 07
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17-36 mm spectroscopy & 34 mm imaging
in parallel
2”
ste
p
AGN@z=1.5
20 30 35 25 λ (mm)
SF@z=1.5
20 30 35 25 λ (mm)
20 30 35 25
SF@z=3
λ (mm)
ste
p
ste
p
10’
LRS Slit viewer
Multi-object
17-36 mm spectra
34 mm (30 – 37 mm)
deep image
Spatial scan with 90 steps (1 step length ~ 2” ~ 0.5 x slit width) produces a spectral map and a broad-band image of 10’ x 12’ area, simultaneously.
30 – 40 mm: unexplored region between Spitzer 24 mm and Herschel 70 mm surveys.
SMI-LRS provides spectroscopic & photometric survey datasets at ~30 – 40 mm.
9/26
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LRS blind survey
Spec
R=1000
20 30 35 25 λ (mm)
R=1000@z=3
~2 hrs / field x 300 fields 1 field = 10’x12’
→ 10 deg2 in ~600 hrs
Follow-up with MRS, if necessary, (and SAFARI).
Cosmological survey with LRS
10 deg2
Multi slit slit size: 10’x3.7”
R = 50 – 120
SPICA/SMI-LRS
PAH galaxies at z > 1
(at z = 2 - 4)
43,000 spectra
(14,000)
MS stars (F, G, K)
(debris disks)
11,000 spectra
(~1000 for >900 zodi.)
3.2°x3.2°
λ (mm) 30 35 25 20
Debris disk
@z=0
10/26
Based on AKARI mid-IR all-sky survey.
20 30 35 25
R=100@z=3
λ (mm)
AGNs at z > 1
102,000 at 34 mm
with slit viewer
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Comparison of spectral mapping efficiency at 25 mm
Multi slit slit size: 10’x3.7”
For the same observational time & the same depth at 25 mm
R = 50 – 120 R = 60 – 120
Spitzer / IRS-LL SPICA/SMI-LRS
slit size: 168”x11”
3.3’x3.3’
R = 2000
JWST / MIRI-MRS
slit size: 7.7”x7.7”
2’x2’
Spec
R=1000
20 30 35 25 λ (mm)
R=1000@z=3
3.2°x3.2°
11/26
20 30 35 25
R=100@z=3
λ (mm)
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PAH bands
gas lines
flu
x (m
Jy)
Star-forming galaxy at z = 3 (1x1012 L
)
Observed wavelength (mm)
6.0 6.6
Tielens 2008
9.0 μm 8.0 7.5 8.5
PAH band diagnostics for distant galaxies
20 30 40 50 100 200
12/26
1x1012 L
at z = 3, R=50
1x1012 L
at z = 3, R=50
SF100%
AGN50+SF50
Not only detection, but characterization
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PAH bands
gas lines
flu
x (m
Jy)
Star-forming galaxy at z = 3 (1x1012 L
)
Observed wavelength (mm)
6.0 6.6
Tielens 2008
9.0 μm 8.0 7.5 8.5
Not only detection, but characterization
Organic matter & ice in the early Universe
20 30 40 50 100 200
13/26
l (μm)
- z = 5
Flu
x (μ
Jy)
- z = 7
20 40 60 80 100 200
High-z star-forming galaxies (2x1013 L
)
SMI (R=50, 10 hrs, 5s)
JWST / MIRI (R=50, 10 hrs, 5σ)
SAFARI (R=50, 10 hrs, 5s)
Simulated spectra based on AKARI M82 (Yamagishi + 13) + ISO (Spoon + 03)
H2O ice
CO2 ice
C-H sp3
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- 250 K - 200 K - 150 K
Flu
x (
Jy)
λ (mm)
Ldisk/L★=10-7
SMI -LRS JWST/MIRI LRS
For 200 K disks: Fdisk/F★ at 20 mm = ~6 x Fdisk/F★ at 10 mm
Faint debris disks, vital debris disks
(SPICA’s advantage over JWST)
Debris
of 1 Zodi.
Dis
k flu
x (
mJy
)
stellar continuum (∝ λ-2) subtracted
λ (mm)
Dolomite, 1 mm
Posch+07
Calcite, 1 mm
Posch+07
16σ 12σ
λ (mm) λ (mm)
CaCO3 MgCa(CO3)2
(pixel-by-pixel cal. using our Zodi.)
Low-T, link to water, atmosphere and life. e.g., Halevy et al. 2011
Challenges to Zodi analogs
Search for vital minerals in a large sample
Sys. Error = 0%, 1 zodi. , 1hr. 1 mm amorphous forsterite
(Jager 2003)
~30σ detection
Sys. Error = 0.1%, 5 zodi. , 1hr. 1 mm amorphous forsterite
(Jager 2003)
~10σ detection
G2V at 10 pc; 6,000 K → 400 mJy at 20 mm
~36 times more photons needed at 10 mm.
14/26
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Spectral diagnosis of Galactic filaments
15/26
Miville-Deschenes + 10, Ward-Thompson + 10, Men’shchikov + 10, Andre + 10
Polaris - Herschel/SPIRE 250 mm
20 30 Wavelength (mm)
R~100 (Spitzer/IRS LL)
1 deg
Fast spectral mapping of large areas
with the tracers of PDRs, ionized
gases, shocks. (thanks to pointing
reconstruction with the slit viewer).
PAH17
[SIII]18
H2S(0)
[SIII]33
[SiII]
35
Multi slit slit size: 10’x3.7”
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Detector: 1 Si:Sb, 1K x 1K Echelle format
Beam steering
mirror
Detector
Focus
Telescope
focus
l/Dl
R=1200
R=2300
(2) Mid-resolution spectrometer
MRS
wide FoV (slit length 60”
+ beam steering mirror)
high line sensitivity
~4 x10-20 W/m2 (1 hr, 5s)
good spectral resolution
R = 1200 – 2300
spectral mapping
16/26
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slit size
slit size
slit size
slit size: 60” x 3.7”, R = 1200 – 2300 spatial resolution: 3.7” @35 mm
20 30 35 25 λ (mm)
slit size : 168” x 11”, R = 60 – 120 spatial resolution: 11” @35 mm
Spitzer / IRS-LL
slit size : 22” x 11”, R = 600 spatial resolution: 11” @35 mm
Spitzer / IRS-LH
SPICA / SMI-MRS
20 30 35 25 λ (mm)
20 30 35 25 λ (mm)
For the same observational time & the same depth at 35 mm
Comparison of spectral mapping efficiency at 35 mm
17/26
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Major gas lines and dust bands for SMI & SAFARI
[OIII] 88.4 μm SF ne~103 cm-3
metallicity
[NII] 121.7 μm SF ne~102 cm-3
[OI] 145.5 μm PDR nH [CII] 157.7 μm PDR NH
[NII] 205.2 μm SF ne~102 cm-3
Molecular gas lines indicator purpose
H2 12.3, 17.0, 28.2 mm PDR/ C-shock
NH2 outflow
HD 19, 23, 28, 38, 56, 112 μm
MC/PDR CO-dark gas tracer
OH 53, 84, 119, 163 μm
PDR/ C-shock
outflow
High-J CO C-shock/AGN
H2O 17.8, 18.7,, mm SF
Dust band indicator purpose
H2O ice 44, 62 mm PDR/MC crystallinity
Crystalline silicate 24 –
69 mm
PDR/MC/
CSM/SNR
mineralogy, crystallinity temperature
graphite 30 μm PDR/XDR crystallinity
PAH 12.7, 13.5, 14.2,
15.9, 17, 18.9 μm
PDR
FeO 20 μm SNR
MgS 30 μm CSM/SNR
Carbonate 20-100 mm
Full gas & dust spectral diagnostics
is applied to studies of nearby Universe. 18/26
Atomic gas line indicator purpose
[NeII] 12.8 μm, [NeIII] 15.6 μm
SF ionization temperature
[SIII] 18.7 μm SF ne~104 cm-3
[ArIII] 21.8 μm SF ne~105 cm-3 (w JWST)
[FeIII] 22.9 μm J-shock temperature
[NeV] 24.3 μm AGN
[OIV] 25.9 μm AGN
[FeII] 26.0 μm J-shock
[SIII] 33.5 μm SF ne~104 cm-3
[SiII] 34.8 μm J-shock/PDR
[NeIII] 36.0 μm SF ne~105 cm-3
(w JWST)
[OIII] 51.8 μm SF ne~103 cm-3
metallicity
[NIII] 57.3 μm SF metallicity
[OI] 63.2 μm PDR/C-shock nH
Red: covered by SMI
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Revealing local relationship of SF activity with metal- dust enrichment and AGN through spectral mapping
19/26
Tremblay 16 (ALMA) Star-formation rate : [OI]+[CII], [OIII], MIR-FIR Black hole accretion rate : [NeV], [OIV] Metallicity : [NIII]/[OIII], [NeII]/Hua Total gas mass: dark gas (HD, [CII]) + radio (HI, CO) Gas density, T, radiation, shock : lines Dust mass, T, composition : continuum, bands
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1K x 1K
Echelle format
slit length ~4”
very high line sensitivity
~1 x10-20 W/m2 (1 hr, 5s)
high spectral resolution
R = 28,000
Continuous coverage from 12.1 to
17.3 mm, plus partial coverage up to
18.9 mm for H2O 17.77 & 18.66 mm.
Detector: 1 Si:As 1K x 1K
CdZnTe immersion Grating
Detector
Cross disperser
Fore-optics Focus
l/Dl
77th order, 18.6618μm
81th order, 17.7665μm
118th order, 12.1442μm
85th order, 17.0813μm
(3) High-resolution spectrometer
m=118
m=77
R=28,000
l (mm)
Spec
tral
res
olv
ing
po
wer
Ikeda et al. 2015 Applied Optics 54, 5193
HRS
20/26
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1 10 100 0
0.2
0.4
0.6
0.8
1e-18
1e-16
1e-14
1e-12
1e-10
1e-08
1e-06
0.0001
0.01
Snow line and its 3-D geometry
Heig
ht
/ R
adiu
s
H2O
abundan
ce
Flu
x d
ensi
ty (
mJy
) 3
2
1
0
-40 40-20 200Velocity (km s-1)
18.7 mm H2O line
A = 1.69x10-2 s-1
Disk radius (AU)
outer disk snow line
17.8 mm H2O line, A = 2.91x10-3 s-1
HRS can separate
the snow line (red)
from the
contribution
of the outer disk
surface (blue).
SMI-HRS can reveal snow line and its 3-D geometry by velocity-resolved spectroscopy of multiple H2O lines with different Einstein A-coefficients.
21/26
Flu
x d
ensi
ty (
mJy
)
Velocity (km s-1)
3
2
1
0 0 20 40 -20 -40
1 M star at 140 pc
Base on disk
models from
Notsu, Nomura
+ 2016a, b
R = 28,000
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JWST/MIRI (R=3,000) SPICA/SMI-HRS (R=28,000)
Characteristics of planetary atmosphere depend on the C/O ratio of the gas at a formation site. → CO2 & H2O in the atmosphere of exoplanets to be studied by JWST.
The HRS range of 12–18 mm contains numerous emission bands of major C-bearing molecules. Carr & Najita 2011 ApJ 733, 102
R=3,000
Velocity-resolved H2O, OH, HCN, CO2, C2H2 lines → C/O ratio distribution at <~1–2 AU in disks
T=300 K, LTE
13.9 14.0 14.1 Wavelength (mm)
13.9 14.0 14.1 Wavelength (mm)
Not only
de-blending,
but also
resolving
molecular bands
Chemistry in proto-planetary disks
22/26
By M. Takami
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Current status of SPICA in Japan
23/26
Evaluations and Reviews International Science Preview (Paris, July 2015)
Mission Definition Review (MDR) was held by ISAS’s Space Science Advisory Committee (Sep - Nov 2015) → passed
New SPICA is now in phase A1 (“project preparation”).
Science Council of Japan In Master Plan for Big Project 2017, SPICA is recommended by
Astronomy/Astrophysics Division as a highest-priority project.
SPICA Special Session in ASJ meeting 16 Mar 2016, >250 participants,
talks: H. Shibai, HK, P. Roelfsema, E. Egami, H. Nomura
SMI technical meeting 29 Mar 2016, 35 participants from the SMI university consortium
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H H H
H
O D H
20 30 40
Si O
O O
Mg
O
HRS
12 14 16 18 λ (μm)
17.2 17.3
20 40 60 λ (μm)
IR spectroscopy
“Enrichment of the Universe with metal and dust leading to the formation of habitable worlds”
24/26
SPICA science program for JAXA MDR
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Enrichment of the Universe with metal and dust leading to the formation of habitable worlds
Metal and dust enrichment through galaxy evolution
Planetary formation to habitable systems
Debris disks to solar system Spatially-resolved,
high-z analogs or relics
Over the peak of the cosmic star-formation history
Beyond the peak, first mineral, aromatics
Nearby galaxies, including high-z
analogs
Interplay with dust-obscured AGNs
The peak of the cosmic star formation history
and beyond
Roles of SMI in the SPICA science program
Changes of mineral and ice properties in disks
Gas dissipation in proto-planetary disks
25/26
Spectral mapping with MRS
AGN Outflows with HRS
Cosmological surveys with LRS
+ follow-up with MRS
Mineralogy with LRS
+ follow-up with MRS
Resolving gas Kepler motion
with HRS
Tracing the gas, ice, and dust evolution
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AKARI Mid-IR all-sky map
Summary
SMI has three spectroscopic channels: (1) LRS (17–36 mm, R~100) w/ slit-viewer camera (34 mm) 10’-long, 4 slits. Spitzer/IRS-LL-like with higher mapping speed.
(2) MRS (18–36 mm, R~2000) 1’-long with beam-steering mirror. IRS-LH-like with better mapping.
(3) HRS (12–18 mm, R~30000). 4”-long with beam-steering mirror. Unique (↔ JWST/MIRI R~2000)
26/26
High-speed dust-band mapping
High-sensitivity multi-purpose spectral mapping
High-resolution molecular-gas spectroscopy