Meixner Margaret · 2019-03-12 · 3/8/19 Meixner -Dusting the Universe. Origins accesses H 2O lines 0 5 10 15 20 25 30 OSriTgins ALMA BinsofGasTemperature,Eu/k(K) JWST 3/8/19. Water

Margaret MeixnerSpace Telescope Science Institute

Johns Hopkins University

For the Origins STDT study team

http://origins.ipac.caltech.eduhttps://asd.gsfc.nasa.gov/firs/

@NASAOriginsTele

https://asd.gsfc.nasa.gov/firs/

Large Mission Studies for 2020 Decadal survey

Lynx X-ray Surveyor Habitable Exoplanet Observatory LUVOIR

Study Chairs:Feryal Ozel (U. Arizona)Alexey Vikhilin (CfA)

Study Chairs:Sara Seager (MIT)Scott Gaudi (OSU)

Study Chairs:Debra Fischer (Yale)Brad Peterson (OSU)

Origins Space Telescope

Study Chairs:Margaret Meixner (STScI/JHU)Asantha Cooray (UC Irvine)

3/8/19 Meixner - Dusting the Universe

Through the Astrophysics Roadmap, the community expressed interest in a “Far-IR Surveyor” mission.

asd.gsfc.nasa.gov/firs/team/

The Origins Science and Technology Definition Team from community directs the Decadal mission concept study.

From the community, by the community, and

for the community

Guest Observers will use Origins to make transformative discoveries.


3/8/19

origins.ipac.caltech.eduThe Origins Space Telescope is a community-led mission concept study sponsored by NASA in preparation for the 2020 Astronomy and Astrophysics Decadal Survey.

DISCOVERY SPACE OF ORIGINS

By obtaining precise mid-infrared transmission and emission spectra, Origins will assess the habitability of nearby exoplanets and search for signs of life.

Do planets orbiting M-dwarf stars support life?

ARE WE ALONE?

With sensitive and high-resolution far-IR spectroscopy Origins will illuminate the path of water and its abundance to determine the availability of water for habitable planets.

How do the conditions for habitability develop during the process of planet formation?

HOW DID WE GET HERE?

Using sensitive spectroscopic capabilities of a cold telescope in the infrared, Origins will measure properties of star-formation and growing black holes in galaxies across all epochs in the Universe.

How do galaxies form stars, make metals, and grow their central supermassive black holes from reionization to today?

HOW DOES THE UNIVERSE WORK?

Fromfirst starsto life

SCIEN

CE D

RIVER

S FOR

MISSIO

N D

ESIGN

Top science drivers for Origins mission design


Origins accesses H2O lines

0

5

10

15

20

25

30ALMAOSTOrigins

Bins of Gas Temperature, Eu/k (K)

JWST

3/8/19

Water and disk masses across all evolutionary stages

• Detect nearly the entire rotational spectrum of water in 1000 planet-forming disks to reveal the trail of life’s ingredients.

• Use the ground-state line of deuterated hydrogen (HD) to determine the planet-forming mass in protoplanetary disks.

• Measure the D/H ratio in over 100 comets to understand the delivery of water to our own inhabited planet. 3/8/19 Meixner - Dusting the Universe

Do planets orbiting M-dwarfs support life?

• Assess the habitability of nearby exoplanets and search for signs of life.

• Constrain the presence of bio-indicators (H2O and CO2) and biosignatures (O3, N2O and CH4) in rocky planets transiting M dwarfs.

• Answer the age-old question of "Are we alone?"



origins.ipac.caltech.eduThe Origins Space Telescope is a community-led mission concept study sponsored by NASA in preparation for the 2020 Astronomy and Astrophysics Decadal Survey.

DISCOVERY SPACE OF ORIGINS

By obtaining precise mid-infrared transmission and emission spectra, Origins will assess the habitability of nearby exoplanets and search for signs of life.

Do planets orbiting M-dwarf stars support life?

ARE WE ALONE?

With sensitive and high-resolution far-IR spectroscopy Origins will illuminate the path of water and its abundance to determine the availability of water for habitable planets.

How do the conditions for habitability develop during the process of planet formation?

HOW DID WE GET HERE?

Using sensitive spectroscopic capabilities of a cold telescope in the infrared, Origins will measure properties of star-formation and growing black holes in galaxies across all epochs in the Universe.

How do galaxies form stars, make metals, and grow their central supermassive black holes from reionization to today?

HOW DOES THE UNIVERSE WORK?

Fromfirst starsto life

SCIEN

CE D

RIVER

S FOR

MISSIO

N D

ESIGN


Origins Observatory level parameters Mission Parameter Value Telescope aperture diameter 5.9 m Telescope area 25 m2

Telescope Temperature 4.5 K Telescope & instruments cooled by Cryo-coolers Diffraction limit 30 µm Wavelength coverage 2.8-590 µm Maximum scanning speed 60² per second Launch year 2035 Launch vehicle Large vehicle: SLS Block I or

Space-X BFR Orbit Sun-Earth L2 Lifetime requirement 5 years Propellent lifetime requirement 10 years

Origins: minimal deployments, Spitzer-like architecture


4.5 K

40 K

80 K

220 K

3 10 100 600

10-1

10-2

100

101

102

103

104

105

106

107

Wavelength (microns)

Astro

nomi

cal +

Teles

cope

Bac

kgrou

nd (M

Jy/sr

)

The importance of being cold

3/8/19

Origins OSS(4.5°K)

Herschel PACS

Herschel SPIRE SOFIA FIFI-L S

Wavelength (µm)

Sensitivity Increases

Spectral line sensitivity

5σ 1

-hou

r Sen

sitiv

ity (W

/m2 ) 10-17

10-18

10-19

10-20

10-21

30 100 500

(80°K)

(80°K)(220°K)

Hubble Telescope optical (2.4m)

76 m = x1000 increase in sensitivity

Transformational gains because Origins is cold (4.5 K) with sensitive detectors


Summary of instrument capabilities Instrument/Mode Wavelength (µm) Field of View Spectral Resolution

(R=l/Dl) Sensitivity, 5s in 1 hr

Origins Survey Spectrometer (OSS) Grating, 6 bands simultaneously

25¾590 µm simultaneously

6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm

High Resolution w/Fourier Transform Spectrometer (FTS)

25¾590 µm Total range scanned by FTS

Slit: 20² ´ 2.7 to 20² ´ 20² <43,000 ´ [112 µm/l] tunable w/FTS scan length

7.4 ´ 10-21 W m-2 @ 200 µm

Ultra-High-resolution w/ Fabry-Perot

100¾200 µm Select lines

One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm

Far-infared Imager Polarimeter (FIP) Pointed images 50 or 250 µm

(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy

Survey mapping 50 or 250 µm (selectable)

60² per second scan rate, with above FOVs

3.3 Confusion limit 50 µm: 120 nJy 250 µm: 1.1 mJy

Polarimetry 50 or 250 µm (selectable)

50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 0.1% in linear/circular polarization, ±1° angle

Mid-Infrared Spectrometer Camera Transit Spectrometer (MISC-TRA) Ultra-Stable Spectroscopy

2.8¾20 µm in 3 simultaneous bands

2.8-10.5 µm: 2.5² radius 10.5-20 µm: 1.7² radius

2.8-10.5 µm: 50-100 10.5-20 µm: 165-295

K~10.8 mag M-type star SNR/sqrt(h) > 12,900 @ 3.3 µm with 85 transits


Table 2 summarizes the calculated heat load and available lift with the cooler for each of these stages. Akey advantage of the ADR approach is the high Carnot e�ciency, and the CADR heat rejection is a negligibleterm in the 4 K budget even though it is designed to provide 100% lift margin at all of its actively cooled stages.The 4 K situation is more challenging relative to our adopted allocation from the observatory, and remainsan area of study. 4 K houses the first stage low-noise amplifier, and the 0.5 mW in the table corresponds tocommercially-available amplifiers operating up to 8 GHz, but we expect that improvements in amplifier powerdissipation should be possible. Of course, a straightforward descope to ease this aspect is to simply not operateall 6 bands simultaneously. (Parasitic conduction in harnesses are book-kept at observatory level, but are muchsmaller than the amplifier dissipation.)

6. DETECTOR AND READOUT APPROACH

Detectors which are capable of taking advantage of the low-background space environment must be substantiallymore sensitive than any that have been used scientifically to date (Figure 7), and beyond what is required foreven the most extreme instruments in ground-based or sub-orbital platforms. Furthermore, the OSS has a total

B4

B6

B2

B5

B1

B3OST FSM

B6FoldB6Col B6Slit

Interferometer

Etalon position

OST FSM

Figure 5. Configuration of the OSS with the OST telescope. Right-hand panels are zoomed views of left hand panels.Grating modules are arrayed in a plane which is approximately orthogonal to the plane of the interferometer bench, sotwo views are provided with the telescope, they di↵er by a rotation about the telescope boresight. Top shows the showsthe 6 grating spectrometer bands, with notional enclosure. A polarizing grid picks o↵ on polarization and sends it downto illuminate bands 1, 3 and 5. Bands 2, 4, 6 couple to the transmitted beam via reflective dichroic filters. The entranceto band 6 is the natural telescope focus position. Bottom shows the interferometer bench and the full extent of the band6 collimator.

OSS: Key Features-Multiband coverage:25-590 micron -fast mapping of reasonable areas-Continuum and lines together -multiple resolutions: 300, 3x104,2x105


OSS Optical / Functional Block Diagram

• Single long slit on the sky which couples all 6 bands

• Each with 3 grating bands coupling the same position.

• FTS engaged when desired -- serves small sub-field only

TelBeam-steerin

g mirror

B4: 119-208

B5: 200-350

B6: 335-588

B1: 25-44

B2: 42-74

B3: 71-124

R=300 Grating Modules

Interferometer engaged via sliding mirrors intercepting beam. M2

Interferometer

D

D D

Interferometer has long scanning stage. M1

Etalon has fine scanning stage. M3

Etalon carriage slides in and out of interferometer beam. M4

Etalon

D

Pol. Grid

Red boxes are mechanisms.

(D=dichroic beamsplitter)






6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295






6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295



FIP Key Features:simple, robust instrumentlarge discovery space50 or 250 micronsLarge area (100 to 1000 deg2) surveyspolarizationbest for variability studiesprovide pictures for PRHelp align telescope


Instruments Mounted to Backplane

4.5KBaffle/Barrel

4.5KZone

35KZone (Passively cooled)

263K-313KZone

ADR cooler

35K Enclosure

Fore

O

ptic

s (M

6.M

7)

FIP Enclosure

4.5KCold Tip

Cryocoolers

Blue Det(50/250 µm)

120 x 120 0.5 mm

pixels

Preamp x8

FIP Instrument Electronics R

FFPE & Bias

BoxMEB

ADRC

Sunshields

HEMT x 8

Launch Lock

HWP

(3

mod

es)

Filter

POM

0.6K

50mK

Power

RS-422

SpW

LDF-V (2-Pos)“Barrel Mechanism”

FIP: Block diagram






6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295






6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295


MISC-TRA: Transit Spectrometer ModuleKey Features

No moving partsDensified pupil opticsUltra-stable, 5 ppmHigh precision spectrophotometryR~50-300Whole band pass of interest simultaneously (2.8-20 microns)


MISC: Transit Spectrometer Module





6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295


3/8/19

3/8/19

3/8/19

2025 2026 2027 2028 2029 2030 2031 2032 2033 2034 2035JFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASONDJFMAMJ JASOND

Primary Critical Path

Funded Sched.Margin

Environmental Tests

TRL

2/11/19

Project Phases

Mission Milestones

Telescope Assembly (Includes Qual Unit)

FAR-IR Imager Polarimeter (FIP) Instrument

Mid-Infrared Imager, Spectrometer (MISC) Instrument

OST Survey Spectrometer (OSS) Instrument

Cryocooler Assy

Sun Shields

CPM Integration & Test

Spacecraft Bus

Observatory Integration & Test

Launch Operations

Launch Vehicle

Ground System

Phase A Phase B

1/4

KDP-B

Phase C

12/6

KDP-C

Phase D

2/23

KDP-D

3/19

KDP-E

Phase E / Ops

6/2Award 12/14SRR 11/1PDR 6/24CDR 1/20SIR

5/25

Delta SIR

8/7

PSR 4/13 LRD

Phase A Prelim Design3/2

SRRPDR5/3

Detail Design, LL Procurement

CDR1/17

Fab, Assy, Test Integration3/3

PER 55 days

To CPM I&T

TRL-5Phase A Prelim Design

SRR6/15

TRL-6

PDR10/13

Detail Design Fab, Assy, Test

CDR2/14 98 days

To CPM I&T

TRL-5Phase A

7/16

SRR

Prelim DesignTRL-6

Detail Design

PDR 11/10

Fab, Assy, Test3/14

CDR 98 days

To CPM I&T


SRR8/17

TRL-6Detail Design

PDR 12/7

Fab, Assy, TestCDR4/18

28 days

To CPM I&T


SRR7/6

TRL-6

PDR 10/25

Detail Design Fab, Assy, TestCDR2/20

98 days

To CPM I&T

Phase A Prelim DesignSRR7/21

Detail DesignPDR11/30

CDR4/11

Fab, Assy, Test

98 days

To CPM I&T

SIR1/20

6/11

PERShip to

JSC 94 days

Ready for Observatory

Phase A Prelim Design7/1

SRR

Detail Design7/12

PDR

4/17

CDR

Fab, Assy, TestPER4/21

98 days

Ready for Observatory

5/25SIR

10/4

PER

Shipto JSC

PSR

120 days

Ready for Launch Site

Unpack

12 days

4/13 Launch

LV Study9/11

LSTO

Preliminary Studies

LV Selection

LV Development & Preparation

Phase A4/5

SRR

1/15

PDR

3/15

CDR

4/22

MOR

10/12

FOR 1/19

ORR

Primary Critical Path

Funded Sched.Margin

Environmental Tests

TRL

ORIGINS Space Telescope Master Schedule

Total schedule margin required216 days vs 254 planned

Origins Mission Development Schedule


Technology Tall Poll, 2021-2027: Detectors, detectors, detectors

Transition-Edge Sensed(TES) Bolometers

Microwave kinetic Inductance Detectors (MKIDs)

HgCdTe arraysSi:As arrays


Technology Tall Poll, 2021-2027: Detectors, detectors, detectors

Transition-Edge Sensed(TES) Bolometers

Microwave kinetic Inductance Detectors (MKIDs)

HgCdTe arraysSi:As arrays

State of the Art: >50 ppm

Need to achieve: 5 ppm

3/8/19

Technology: Cryocoolers, thanks JWST

NGAS JWST/MIRICreare

SHI Hitomi/SXS

Ball 10 K

Lockheed ACTDP

Observatory temps: 4.5 KFIR detectors: <50 mK


Origins Report Schedule• Decadal Science White papers: due Monday

March 11 – mention Origins capabilities• April 26 – Draft Report to NASA HQ for review• August – Report to NASA HQ for final delivery to

pass onto National Academy of Sciences Decadal study

• To Learn more: – https://origins.ipac.caltech.edu– https://asd.gsfc.nasa.gov/firs/


https://origins.ipac.caltech.edu/

https://asd.gsfc.nasa.gov/firs/

3/8/19





6 Slits: 2.7¢ ´ 1.4² to 14¢ ´ 20²

> 300 3.7´ 10-21 W m-2 @ 200 µm




7.4 ´ 10-21 W m-2 @ 200 µm



One beam: 6.7² 325,000 ´ [112 µm/l]

~2.8 ´ 10-19 W m-2 @ 200 µm


(selectable) 50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢

3.3 50 µm: 0.9 µJy 250 µm: 2.5 µJy





50 µm: 3.6¢´2.5¢ 250 µm: 13.5¢´9¢





2.8-10.5 µm: 50-100 10.5-20 µm: 165-295


Instrument Focal Plane


MISC: Transit Spectrometer Module 2.8-20 microns


Documents

Meixner Margaret · 2019-03-12 · 3/8/19 Meixner -Dusting the Universe. Origins accesses H 2O lines 0 5 10 15 20 25 30 OSriTgins ALMA BinsofGasTemperature,Eu/k(K) JWST 3/8/19. Water