smart-x · configuration • no extendable optical bench • m tot < 4,000 kg (including 30%...
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SMART-X
Aim at a mission more compelling than IXO:
• with significant cost savings
• and big science gains via achieving Chandra-like angular resolution.
team at SAO, PSU, MIT, GSFC, MSFC, JHU, Stanford, U.Waterloo,Rutgers, NIST, Dartmouth
Approved for public release, distribution unlimited
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Configuration
• No extendable optical bench
• M tot < 4,000 kg (including 30% growth contingency)
• ATLAS V–541 launch to L2; throw weight > 5,000 kg, 28% margin for SMART-X
• Parameters very similar to Chandra and AXSIO
Approved for public release, distribution unlimited
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Configuration
• 5×5′ microcalorimeter with 1″ pixels (XMIS)
• 22×22′ CMOS imager with 0.33″ pixels (APSI)
• insertable CAT gratings with R = 5000 (CATGS)
• f =10 m, ⌀ = 3 m mirrors with 0.5″ HPD resolution
and Aeff = 2.3 m2 at 1 keV
Approved for public release, distribution unlimited
![Page 4: SMART-X · Configuration • No extendable optical bench • M tot < 4,000 kg (including 30% growth contingency) • ATLAS V–541 launch to L2; throw weight > 5,000 kg, 28%](https://reader033.vdocuments.us/reader033/viewer/2022042313/5edc0cddad6a402d66668cdb/html5/thumbnails/4.jpg)
Performance
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IXO Science
✓ What Happens Close to a Black Hole? time-resolved Fe-K line spectra for 5–10 AGNs
✓ How does matter behave at high ρ?✓ high-res spectroscopy- no timing for 106 cnt/s sources
✓ When and How Did SMBHs Grow?
✓ BH spins in ~40 low-z AGNs- (little area at E >10 keV)
✓ BH spins for brightest z=3 AGNs
✓ Observations of BHs to z=10 found in other wavebands or in SMART-X surveys
z = 10,MBH = 3� 10
8M�,
L
x
= 3� 1044 erg/s
NH = 1.5� 1024 cm�2
NH = 0
10.5 2 510−6
10−5
10−4
10−3
0.01
0.1
norm
aliz
ed c
ount
s s−
1 keV
−1
Energy (keV)
data and folded model
alexey 19−Oct−2011 17:55
z = 3LX = 10
45 erg/sEWrel = 160 eV
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SMART-X projections for high-z AGNs
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IXO Science
✓ How does Large Scale Structure Evolve?
✓ Precision Cosmology using ~1000 eRosita/ WFXT clusters:Δγ = ± 0.02, Δw ≃ ± 0.02
✓ Detection of WHIM in absorption (2× IXO efficiency)
✓ Connection between SMBH and LSS
✓ Exquisite data on groups and clusters to high-z
✓ Spatially-resolved turbulence measurements
✓ High-res spectroscopy of AGN outflows,galaxy winds
2x4 arcsec diameterextraction region
Energy (keV)4.4 4.5 4.6 4.7 4.80
0.5
1
1.5
2
Flux
(10!
" ph/
cm#/
s/ke
V)
Perseus@z=0.5Fe K, 300 ksec
ThermalOnly
Best-$t: 350±50km/s
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SMART-X/XMIS simulation of Perseus-like clusters at z = 0.5
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Adjustable mirrors
• make segments for ~7″ mirror quality (AXSIO-like), deposit PZT & electrodes
• mount, calibrate and determine required piezo voltages on the ground, using available optical interferometry
• apply voltage to correct the figure when in orbit (low power)
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Adjustable mirrors: analytic modelingFinite element analysis of 410×205mm conical elements with 20×20 piezo adjusters, 10+2 point mount:
• correction works for generic low-f distortions (e.g., gravity release)
• up to 5% errors on correction coefficients can be tolerated
50 100 150 200
-0.20
-0.15
-0.10
-0.05
0.00
0.05
0.10
z@mmD
slopeerror@arcsecD
Residual Slope Center Strip, Primary, 1g
Simulations of 1-g gravity release correction — an order of magnitude reduction in slope error
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• PZT film successfully deposited and energized. ~500 ppm strain required, 700 –900 ppm obtained;
• Deposition on Corning Eagle glass
• PZT lifetime, stability, repeatability studies on-going
“first move” measurement: 60×60mm, ~2μm displacement
Adjustable mirrors: current state
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PZT deposition on D263 vs Corning Eagle
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Adjustable mirrors: current state
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Corning Eagle glass, single cell energized, 690ppm strain
• PZT film successfully deposited and energized. ~500 ppm strain required, 700 –900 ppm obtained;
• Deposition on Corning Eagle glass
• PZT lifetime, stability, repeatability studies on-going
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Adjustable mirrors: development plan
• $45M, 7-yr development program (SAO, GSFC, PSU, MSFC, Industry)
• TRL6 by 2019 through a rocket flight
Approved for public release, distribution unlimited
ID Task Name
1 PZT Development
2 Extend to conical mirrors
3 Optimize Influence Function
4 Improve mid frequency figure
5 Flight-like Alignment and Mounting
6 Sounding Rocket Program
7 Sounding Rocket Launch
8 Metrology development
9 Lifetime testing
10 Technology Readiness Level
SAO, PSU
SAO, PSU, Industry, GSFC,
SAO, PSU, MSFC
SAO, GSFC
SAO, GSFC, Industry
SAO, MIT, PSU, MSFC, GSFC
10/2
SAO, Industry
SAO, MSFC, PS
TRL 2 TRL 3 TRL 6TRL 5TRL4
2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 41 2012 2013 2014 2015 2016 2017 2018 2019 2020
Task
Split
Progress
Milestone
Summary
Project Summary
External Tasks
External Milestone
Deadline
Page 1
Project: Smart-X Tech Development - Date: Mon 12/12/11
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Science instruments status
• CATGS — see Bautz et al.,Heilmann et al.
• XMIS — some areas of development are specific to SMART-X (4×4 or 5×5 Hydras, more pixels, energy vs. spatial resolution trade-off)
• APSI — straightforward development, but funding needed (see D. Burrows talk):
- small pixel size + large depth- thin filter without hydrocarbon- fast readout + large arrays
Results for 3×3 Hydra (65 μm absorbers vs. 46μm for SMART-X)
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Cost
• Use AXSIO as a basis
• Add knowns and unknowns (conservatively)(e.g., 2× cost of module facilities, 50% instead of 30% reserves for mirror production)
• Δ from AXSIO = $430M$170M (mirrors) + $188M (instruments & spacecraft systems) + $52M (integration & test) + $20M (Atlas V-541)
• End-to-end cost = $2,328M
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High-resolution spectroscopy
• Gas outflows in AGNs and starbursts
• Spectroscopy / tomography of slightly extended sources
• Active stars
Bondi radius in NGC3115
5 10 15 20Wavelength (Angstroms)
0
200
400
600
800
C
ou
nts
O VII
O V
III
O V
II
Fe
XV
II
Fe
XV
II
O V
III
Ne IX
Ne
X
Ne X
Fe
XX
IIN
e I
X
Ne
X
Mg
XI
Mg
XII
Si X
III
Si X
IVObservation
Shock Model
Coronal Model
Trumpler 14, Chandra X-ray spectral diagnostic of TW Hydrae with Chandra (Brickhouse et al ’10)
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Black holes and LSS from z = 6 to the present
Springel et al. 2005 simulations — dark matter density
“!rst quasar” at z=6 “nursing home” at z=0
M87, Chandra, 1” pixels
XMIS, z = 0, 300 ks
GasT = 1.4 keV
HaloLX = 5� 10
43 erg/sT = 2 keVr = 45kpc = 8��
1 100.2 0.5 2 510
!6
10
!5
10
!4
10
!3
0.0
10
.1
no
rma
lize
d c
ou
nts
s!
1 k
eV
!1
Energy (keV)
data and folded model
alexey 18!Oct!2011 17:15
10.5 2 510
!3
0.0
10
.11
no
rma
lize
d c
ou
nts
s!
1 k
eV
!1
Energy (keV)
data and folded model
alexey 18!Oct!2011 18:03
APSI, z = 6, 300 ksec
QSOL
x
= 1045 erg/s
XMIS, z = 0, 300 ksec
Jet + gasT = 1.2 keV
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T = 0.7 keVv = �400 km/s
50 kpc
T = 0.5 keVv = +400 km/s
10.5 210
!4
10
!3
0.0
10.1
110
norm
aliz
ed c
ounts
s!
1 k
eV
!1
Energy (keV)
data and folded model
alexey 18!Oct!2011 21:35
NGC 1961, XMIS, 300 ksec
NGC 1961, Chandra
HST+ALMA, z=0
Galaxy and star formation
Subaru, z=3C
old accretion
Ly-α
Hot halos
SMART-X
• Observations of hot halos around SFR≳30 M⊙/yr galaxies at z ~ 2.5
• Detailed study of hot phase at z = 0
• Star-forming regions in the MW
Star
s, du
st,m
olec
ular
gas
optic
al, I
R, A
LMA
, eVL
AKeres et al. simulations
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Surveys
• Vs. Chandra:50× soft-band throughput, 98× grasp,more uniform PSF (4″ HPD at 10′),same particle background
• Deep Field South depth in 80 ksec,10 deg2 to this depth = 8 Msec program
• 4 Msec ⇒ fmin = 3×10–19 erg s–1
cm–2, Lmin = 3.3×1041 erg s–1 at z = 10
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CDFS, Chandra, 4 Msec, 16′×16′
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Imaging time-domain X-ray astronomy
• Evolution of SNRs (Cas-A)
• Cooling of neutron stars
• Light echos from Sgr A*
• Long-term evolution of jets (M87), repeated Deep Field observations
• SN 1987A
Cas-A
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SMART-X• Chandra’s angular resolution,
0.5″
• with 30× effective area
• and state-of-the-art science instruments
• for $2.3B
Needs funding for mirror technology program
Springel et al. 2005 simulations — dark matter density
“!rst quasar” at z=6 “nursing home” at z=0
M87, Chandra, 1” pixels
XMIS, z = 0, 300 ks
GasT = 1.4 keV
HaloLX = 5� 10
43 erg/sT = 2 keVr = 45kpc = 8��
1 100.2 0.5 2 510
!6
10
!5
10
!4
10
!3
0.0
10
.1
no
rma
lize
d c
ou
nts
s!
1 k
eV
!1
Energy (keV)
data and folded model
alexey 18!Oct!2011 17:15
10.5 2 510
!3
0.0
10
.11
no
rma
lize
d c
ou
nts
s!
1 k
eV
!1
Energy (keV)
data and folded model
alexey 18!Oct!2011 18:03
APSI, z = 6, 300 ksec
QSOL
x
= 1045 erg/s
XMIS, z = 0, 300 ksec
Jet + gasT = 1.2 keV
Approved for public release, distribution unlimited