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

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

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

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Performance

Approved for public release, distribution unlimited

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

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

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

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

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

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)

Approved for public release, distribution unlimited

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

Approved for public release, distribution unlimited

CDFS, Chandra, 4 Msec, 16′×16′

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