Mars Environmental

ObserverA Scout Mission Concept

Final report25 February 2002

M. Janssen

M. Allen

Concept HistoryA tale of two instruments

May 2001

MAMBOAtmospheric Sounding/ Chemistry On CNES Premier Orbiter

January 2002 Follow-on

MATMOSMars Solar OccultationFTS

MCSIR sounder

MARCISupporting camera

MEO Proposed

US participation to be proposed as

Mission of Opportunity

MEO Scout Concept Study

MOMESMillimeter Spectrometer(US/DLR)

MATMOS

MARCI

MEO Final

MIROSubmillimeter

spectrometer on Rosetta

(US/DLR/French)

ATMOSSolar occultation

FTS onSpace Shuttle

Heritage

MAMBOMillimeter Spectrometer(French/US/DLR)

MOSESSubmm Spectrometer(US/DLR)

MATMOSPrimary Instrumentfor MARVEL Scout

To be proposed as a Scout Mission

Agenda

MEO

MAMBO

MARVEL

Janssen

Janssen

Allen

15 min

15 min

15 min

MEO Science Goals and Objectives

1. Seek evidence of extant life by a uniquely broad and sensitive mapping of the global distribution of atmospheric water (I.A.1).

2. Seek evidence of extant life by an ultra-high sensitivity search for trace atmospheric disequilibrium biosignatures (addresses objectives in I.A.2 by remote means).

3. Determine the oxidation state of the lower atmosphere and surface through highly sensitive global measurements of key trace photochemical oxidized species (II.A.6).

4. Characterize the present Mars climate by acquiring a complete global measurement of the physical state of the atmosphere—temperature and winds—over a wide altitude range and under all atmospheric conditions (II.A.1, IV.A.4).

5. Characterize present Mars climate processes through simultaneous measurements of temperature and water (II.A.1, II.A.3, II.A.4, II.A.5).

6. Determine the composition of surface dust by characterizing the mineralogy of atmospheric dust (addresses aspects of I.A.4, I.C.3, II.B.1, III.A.2, III.A.5).

7. Infer the presence of active volcanism through the detection of trace tectonic-formed gas emissions. (III.A.4)

8. Support the preparation for human exploration through a better understanding of upper atmospheric phenomena relevant to aerobraking and aerocapture (IV.A.4).

LIFE

CLIMATE

GEOLOGY

HUMANEXPLORATION

The Mars Environmental Observer (MEO) concept addresses the key Mars Exploration Program Goals of Life, Climate, Geology, and Human Exploration (MEPAG goals I-IV). MEO Objectives are:

Mission and Flight System Architecture

• Payload mass, power, and viewing requirements are accommodated by Lockheed-Martin Odyssey spacecraft.

• Launched by the Delta 2925 for the 2007 opportunity.

• The limb-sounding and solar occultation observing requirements are satisfied by the sun-synchronous polar orbit.

Parameter Value

Launch Date Sep. 2007 Launch Vehicle Delta 2925 Mission duration 40 mo. Trajectory Type Type II Final Orbit 375 km circ. Inclination 92.9 deg. Local Time Node 3:30 pm

Flight System Element Mass, kg Power, W

Spacecraft (Odyssey) 408 (dry) 366 Launch Vehicle (Delta 2925) 779 (wet) Power Source (GaAs arrays, 475 W) 48.7 41.9

System Estimates System Margins

Payload Mass 68 kg Mass 40 %Payload Power 84 W Power 50 %

MEO Budget

     Phase

A/BPhase

C/DA/B/C/D

TotalPhase E

ProjectTotal

(FY2002$)

  Total Project Costs ($M) $34.3M $261.2M $295.5M $43.8M $339.3M

1.0 Project Management $1.1M $7.5M $8.6M $5.4M $14.0M

1.1   Project Manager & Staff $0.5M $3.2M $3.6M $2.6M $6.2M

1.2 Launch Approval   $0.1M $0.1M   $0.1M

1.3 Planetary Protection Approval   $0.1M $0.1M   $0.1M

1.4 Education & Public Outreach $0.1M $0.8M $0.9M $2.5M $3.4M

1.5   Mission Assurance $0.6M $3.3M $3.9M $0.3M $4.2M

2.0 Science Team $0.6M $4.2M $4.8M $5.4M $10.2M

3.0 Mission Design & Project Engineering $0.3M $2.7M $3.0M   $3.0M

4.0 Instruments $19.4M $32.9M $52.2M   $52.2M

5.0 Spacecraft $5.5M $110.1M $115.6M   $115.6M

6.0 Mission Operations & Development $0.6M $5.2M $5.8M $27.3M $33.0M

7.0 Reserves $6.9M $31.9M $38.8M $5.7M $44.5M

8.0 Launch Vehicle   $66.8M $66.8M   $66.8M

Mission costs with full (MATMOS, MOMES, MARCI) instrument complement

200 MHz

330.6 GHz 345.8 GHz325.2 GHz

12CO

200 MHz 200 MHz

13COH216O

•Advantages over IR: Insensitive to dust presenceDoppler windsHigh H2O sensitivity

•Temperature and Water Vapor will be profiled using limb (shown) and nadir sounding in CO and H2O lines

•Winds will be profiled by limb sounding CO

•Atmospheric chemistry involving H2O2, O3,

HDO, CO, will also be addressed

Atmospheric Sounding with MAMBO

Tangent altitude = 10 km

Spectrometer width

Mars Zonal Wind Simulation for Northern Sosltice

Figure from Conway Leovy (Nature Insight 412, 6843,245-249(2001))-derived from GCM of Haberle et al., J. Geophys. Res. 102, 13301-13311 (1993)

Westward wind, m/sec Eastward wind, m/sec

80S 60 40 20 0 20 40 60 80NLatitude

Retrieval Error, m/s

Alti

tude

, km

Wind Retrieval

Winds along the line of sight will be measured from the Doppler shift of CO lines in the limb-sounding mode. 12CO and 13CO lines allow a wide altitude range to be covered in the atmosphere.

The weighting function for the measurement is narrow in the limb sounding mode and the vertical resolution is set by the beamwidth on the limb (~10 km).

Nominal receiver performance with 10-sec integration time/point allows the determination of wind velocity profiles to better than 10 m/s over a large altitude range.

12CO

13CO

Lines with widths from 1 to 200 MHz are measured at 100 KHz resolution.

cut for weighting function

MAMBO CollaborationWork Agreement

Calibration Load 1st LO

Scan Mechanism

23-cm Off-AxisAntenna

335 GHz Receiver

PowerProcessor

HKP USO

Receiver

Backend

IF ProcessorFrequencySynthesizer

Chirp TransformSpectrometer

PowerProcessor

CP

UE

lect

roni

csIn

terf

ace

S/C

Dat

a B

us

S/C

Pow

er B

usS

igna

l

US

French

German

•MAMBO will be built as an international collaboration.

•A working agreement has been negotiated that minimizes interface complexity and plays to the respective strengths of the partners.

MAMBO US ComponentScience Team

Mike Janssen (lead)

Mark Allen

Gordon Chin

Todd Clancy

Margaret Frerking

Sam Gulkis

Mark Gurwell

Bob Haberle

Mark Richardson

Yuk Yung

JPL

JPL

GSFC

U. Colo

JPL

JPL

Harvard

ARC

Caltech

Caltech

The US MAMBO science team comes from a variety of universities and NASA centers, and brings world-class expertise in all aspects of the investigation: instrumentation, remote sensing, atmospheric dynamics and chemistry

MAMBO US Component Rationale

• Continues international collaboration on heterodyne spectroscopy - this time with French lead

• US responsibility for subsystem complements limited French workforce & experience

• Choice of radiometer backend provides well-defined interface and minimizes risk, travel, ITAR issues, etc.

• Backend experience will be valuable for future instruments• We have found no significant descope options that appear

viable. Possibilities are being explored:– Swedish collaborators assume backend delivery

responsibility, or– French contract to industry for this

US role would be questionable in these cases

MAMBO US Component Budget

02 0403 05 06 07 08 09 10 11

7

6

5

4

3

2

1

0

Schedule of Deliverables

STM

EM

FM

Co

st/F

Y,

M$

FYSchedule Key

Subsystem design and fab at JPL

Delivery to LERMA (French)

Support integration at LERMA

Delivery to CNES (from draft AO)

Budget Key and Summary

Hardware $15.8 MReserves $4.8 M

Science $4.8 M

Total $25.4M

Note: 3%/yr inflation assumed (NASA model)

launch

Phase B