# Presentation: 592321

## Lunar Reconnaissance Orbiter: Instrument Suite and Objectives

- R. Vondrak, J. Keller and the LRO Team

- Polar Gateways Arctic Circle Sunrise 2008
- Barrow, Alaska, January 23-29, 2008

## Vision implies extended periods in space and on the Moon

- Unknown terrain, poor maps
- Radiation Environment
-  Long Cold Nights and Warm Days
- Daytime  400 K (266 F)
- Nighttime 100 K (-280 F)
-  Long Way From Home
-  Exploitable Resources?
- - Water
- - Shelter
-  Energy

*Vision* implies extended periods in space and on the Moon

## LRO Objectives

- Safe Landing Sites
- High resolution imagery
- Global geodetic grid
- Topography
- Rock abundances

- Locate potential resources
- Water at the lunar poles?
- Continuous source of solar energy
- Mineralogy

- Space Environment
- Energetic particles
- Neutrons

- New Technology
- Advanced Radar

## LRO Mission Overview

- Launch in late 2008 on a EELV into a direct insertion trajectory to the moon. Co-manifested with LCROSS s/c.
- On-board propulsion system used to capture at the moon, insert into and maintain 50 km mean altitude circular polar orbit.
- 1 year exploration mission followed by handover to NASA Science Mission Directorate.
- Orbiter is 3-axis stabilized, nadir pointed, operates continuously during the primary mission.
- Data products delivered to Planetary Data Systems (PDS) within 6 months of completion of primary mission.

- 4.00 m

- CEM

**LRO**

- 2.25 m Stack CG Height

**L****CROSS**

**Minimum Energy Lunar Transfer**

**Lunar Orbit Insertion Sequence**

**Commissioning Phase, 30 x 216 km Altitude Quasi-Frozen Orbit, Up to 60 Days**

**Polar Mapping Phase, 50 km Altitude Circular Orbit, **
**At least 1 Year**

## 
WAC Design Parameters
Optics (2 lenses) f/5.1 vis., f/8.7 UV
Effective FL 6 mm
FOV 90o
MTF (Nyquist) > 0.5
Electronics 4 circuit boards
Detector Kodak KAI-1001
Pixel format 1024 x 1024
Noise 30 e-
NAC Design Parameters
Optics f/4.5 Maksutov
Effective FL 700 mm
FOV 2.86o (5.67o for both)
MTF (Nyquist) > 0.15
Electronics
Detector Kodak KLI-5001G
Pixel format 1 x 5,000
Noise 100 e-
A/D Converter AD9842A
FPGA Actel RT54SX32-S

**NAC 2**

**WAC**

**NAC 1**

- WAC Design Parameters
- Optics (2 lenses) f/5.1 vis., f/8.7 UV
- Effective FL 6 mm
- FOV 90o
- MTF (Nyquist) > 0.5
- Electronics 4 circuit boards
- Detector Kodak KAI-1001
- Pixel format 1024 x 1024
- Noise 30 e-
- NAC Design Parameters
- Optics f/4.5 Maksutov
- Effective FL 700 mm
- FOV 2.86o (5.67o for both)
- MTF (Nyquist) > 0.15
- Electronics
- Detector Kodak KLI-5001G
- Pixel format 1 x 5,000
- Noise 100 e-
- A/D Converter AD9842A
- FPGA Actel RT54SX32-S

**Lunar Reconnaissance Orbiter Camera (LROC)**Mark Robinson PI, ASU

-      Wide and Narrow Angle Cameras (WAC, NAC)

- MSSS

## LROC Science/Measurement Summary

- Landing site identification and certification, with unambiguous identification of meter-scale hazards.
- Meter-scale mapping of polar regions with continuous illumination.
- Unambiguous mapping of permanent shadows and sunlit regions including illumination movies of the poles.
- Overlapping observations to enable derivation of meter-scale topography.
- Global multispectral imaging to map ilmenite and other minerals.
- Global morphology base map.

- LROC NAC camera will provide 25 x greater resolution than currently available

- 50 cm pixel dimension from 50 km

- Images geodetically tied to LOLA

## National Airport at NAC Resolution

## Lunar Orbiter Laser Altimeter (LOLA)Dave Smith PI, GSFC

**LOLA measures:**
- _RANGE_ to the lunar surface (pulse time-of-flight)
- 	±10cm (flat surface)
- _REFLECTANCE_ of the lunar surface (Rx Energy/Tx Energy)
- 	± 5%
- _SURFACE ROUGHNES_ (spreading of laser pulse)
- 	± 30 cm
- Laser pulse rate 28 Hz, 5 spots => ~ 4 billion measurements in 1 year.

- Detectors (5)
- (2 on reverse side)

- Receiver
- Telescope

- Laser

- Beam
- Expander

- Radiator

## LOLA will Derive an Accurate Global Lunar Reference System

**LOLA will obtain an accuracy base of ~50 meters horizontal (point-to-point) and 0.5 to 1 meter radial**
- Current accuracy ~4 km
**LOLA is a geodetic tool to derive a precise positioning of observed features with a framework (grid) for all LRO Measurements**
- Measure distance from LRO to the surface globally
- Laser ranging from ground station to LRO provides precise orbit determination
- Five laser spots along and across track
- Measure distribution of elevation within laser footprint
- Enhanced surface reflectance (possible water ice on surface)

- Crossovers occur about every 1 km in longitude and 3 deg in latitude at equator

##    
LEND is designed to measure lunar thermal, epithermal and energetic neutrons.

LEND improves spatial resolution for epithermal neutrons from 140km to 10km to locate areas of high hydrogen concentration

LEND footprint smaller than the Permanently Shadowed Regions of interest

Improves sensitivity of measurements in cold spots

Enables site selection

- LEND is designed to measure lunar thermal, epithermal and energetic neutrons.
- LEND improves spatial resolution for epithermal neutrons from 140km to 10km to locate areas of high hydrogen concentration
- LEND footprint smaller than the Permanently Shadowed Regions of interest
- Improves sensitivity of measurements in cold spots
- Enables site selection

- South Pole

- White areas represent permanently shadowed regions as determined from ground based radar and overlaid on Lunar Prospector hydrogen concentrations

***LEND footprint***

**Lunar Exploration Neutron Detector (LEND)**Igor Mitrofanov PI, IKI

## LEND Science Overview

**LEND collimated sensors CSETN1-4 and SHEN detect epithermal neutrons and high energy neutrons with high angular resolution to test water ice deposit on the surface**

***epithermal neutrons***

**LEND Science Overview**
**                               ****and Theory of Operations**

***high energy neutrons***

**SHEN**

**CSHEN 1**

**CSHEN 3**

## Lyman-Alpha Mapping Project (LAMP)

- Alan Stern PI, SwRI
- Randy Gladstone (SwRI), Acting PI

_**LAMP (with LTS):**_
**5.3 kg, 4.6 W**
**0.2o×6.0o slit**
**520-1800 ****Å**** passband**
**20 Å** **point source**
-      **spectral** **resolution**

## LAMP Science/Measurement Summary

- LAMP will be used to identify and localize exposed water frost in PSRs
- LAMP will provide landform mapping (using Ly albedos) in and around the permanently shadowed regions (PSRs) of the lunar surface.
- LAMP will demonstrate the feasibility of using starlight and UV sky-glow for future night time and PSR surface mission applications.
- LAMP will Assay the Lunar Atmosphere and Its Variability** **

**LAMP Science/Measurement Summary**

## Diviner Lunar Radiometer (DLRE)

**Elevation Rotation Axis**

**Azimuth Rotation Axis**

**Solar Cal Target**

**Telescopes**

**Diviner Lunar Radiometer (DLRE)**
- David Paige PI, UCLA

- Close copy of JPL’s Mars Climate Sounder (MCS) Instrument on MRO
- 9-channel infrared radiometer 40K – 400K temperature range
- 21 pixel continuous pushbroom mapping with ~300 m spatial resolution and 3.15 km swath width at 50 km altitude
- Azimuth and elevation pointing for off-nadir observations and calibration

## Diviner Investigation Goals

**Diviner Investigation Goals**

- Clementine LWIR Daytime Thermal Image (200m /pixel)

- Lunar day, night and polar temperatures

- Characterize the moon’s surface thermal environment
- Daytime
- Nighttime
- Polar
- Map surface properties
- Bulk thermal properties (from surface temperature variations)
- Rock abundance and roughness (from fractional coverage of warm and cold material)
- Silicate mineralogy (8 micron thermal emission feature)
- Characterize polar cold traps
- Map cold-trap locations
- Determine cold-trap depths
- Assess lunar water ice resources (using Diviner data in conjunction with topographic data and models)

## GCR flux is low-level but continuous and has weak solar cycle dependence 
Intense SEPs (>10 MeV p+) are episodic and approximately follow the solar cycle
SEP event occurrence varies with the solar cycle in anti-phase with weaker galactic cosmic ray fluxes

- GCR flux is low-level but continuous and has weak solar cycle dependence
- Intense SEPs (>10 MeV p+) are episodic and approximately follow the solar cycle
- SEP event occurrence varies with the solar cycle in anti-phase with weaker galactic cosmic ray fluxes

- _(plot courtesy R. Mewaldt, Cal Tech)_

**SEP events**

**Solar**
**Minimum**

- At solar minimum:
- Min SEP occurrence
- Max GCR flux

## Cosmic Ray Telescope for the Effects of Radiation (CRaTER)Harlan Spence PI, Boston University

- Cosmic Ray Telescope for the Effects of Radiation (CRaTER)Harlan Spence PI, Boston University

## CRaTER Instrument

- CRaTER will measure the Linear Energy Transfer (LET) spectra behind tissue equivalent plastic (TEP)
- LET spectra is the missing link connecting Galactic Cosmic Rays and Solar Energetic Particles to potential tissue damage

- _Characteristics_
- Nadir FOV: 75°, Zenith FOV: 35°
- Avg. Orbital Power Allocation: 9.0 W
- Mass Allocation: 6.36 kg
- Daily Data Volume: 7.8 Gbits (Flare)
- Data Collection: Full Orbit (113 minutes)
- Inst. Daily Operations: Autonomous

- CRaTER Telescope

- TEP

- Thin & Thick Pairs
- of Si Detectors

## Mini-RF Lunar Demonstrations

- Chandrayaan-1

- Lunar Reconnaissance Orbiter (LRO)

- Chandrayaan-1

- LRO

- SAR Imaging (Monostatic and Bistatic)

- Monostatic imaging in S-band to locate and resolve ice deposits on the Moon.
- Communications Demonstrations
- Component Qualification

- Monostatic imaging in S-band and X-band to validate ice deposits discoveries on the Moon
- X-Band Comm Demo

- Coordinated, bistatic imaging in S-band, to be compatible with the Chandrayaan-1 and LRO spacecraft, can unambiguously resolve ice deposits on the Moon
- Other Coordinated Tech Demos: e.g ranging, rendezvous, gravity

- Miniature Radio Frequency Demonstration Project (Mini-RF)
- Stewart Nozette PI,

## Summary

- LRO launch:			October 2008
- 7 Instruments:		LOLA, LEND, LROC, 				LAMP, DLRE, CRaTER, 				Mini-RF
- Orbit:				Polar                          				Mean altitude 50 km
- Mission length:		1 year Exploration          				+ ? years Science

## Slide 21