LPOD: 'a wetter hole' for LCROSS

Cabeus: On initial examination, a section of earth-bound radar maps of the far southern hemisphere of the Moon, from Goldstone or Arecebo, shows the target zone for LCROSS, Oct. 9. Mission planners at NASA Ames have changed course from Cabeus A to Cabeus "proper" and are sticking with the choice of a target at a surprisingly higher latitude than LCROSS fans had long expected. Their reason for the choice is to make observations from Earth of the resulting plume easier (and for a longer period of time in the 100 seconds after the impacts) and recent verification by LRO instruments of "the strongest signature for hydrogen anywhere on the Moon" as originally mapped by the neutron spectrograph on-board Lunar Prospector in 1998. [Charles Wood, Lunar Picture of the Day (LPOD), via NASA-LCROSS Observation Campaign]

When Charles Wood lends his noted expertise to any earth-bound lunar observation exercise, particularly when he devotes a daily update to his prestigious Lunar Picture of the Day (LPOD) website to the subject area, then what is known about the target in question (and what we think we know) are covered, definitively.

"Nine days from now the Lunar Crater Observing and Sensing Satellite (LCROSS) will impact the Moon, aiming at a new target. On September 11 NASA announced that the site selected in the attempt for a positive identification of water would be a small crater on the rim of Cabeus A, informally labelled A1. But although "A1" usually means "the very best", that target seemed to not be the best and LPOD recommended that a larger crater with a higher chance of success be targeted. Now NASA has just announced that they have changed the LCROSS target, not to the LPOD recommended Cabeus B but to Cabeus itself. This is a great improvement, made in response to new topographic data from the Lunar Reconnaissance Orbiter and continuing analysis of existing Kaguya, Chandrayaan-1 and Lunar Prospector data..."

Read the Sept. 30 LPOD, HERE.

Deep Impact identifies water on the surface

Since successfully carrying out its spectacular impact experiment at comet Tempel 1 on July 4, 2005, the Deep Impact spacecraft has been on an extended mission, called Epoxi, which culminates in a flyby of comet Hartley 2 on November 4, 2010. En route to the second comet, the spacecraft observed the moon for calibration purposes on several occasions. In June 2009, the northern polar regions were observed and detailed measurements of light from the regions, called spectra, were collected (blue and cyan). These data unambiguously show the signature of water and hydroxyl (hashed regions). The water signature varies in strength; in particular, data acquired over the warm equator in December 2007 have a distinct but weaker signature (purple). [NASA/JPL-Caltech/University of Maryland]

Lunar Weather: many miles wide, 2 mm deep

Chart highlighting the calibration observations by Deep Impact of the northern polar regions of the moon on June 9. At left is a reference albedo map from Clementine while the other images are different representations of Deep Impact data, including measurements of brightness, temperature, and the strength of a signature for water and hydroxyl. The water signature varies significantly across the lunar surface but, while the strength of the water signature is not correlated with any terrain type it is highly dependent on temperature. Since successfully carrying out a spectacular impact experiment on comet Tempel 1 July 4, 2005, Deep Impact spacecraft has been on an extended mission, called "EPOXI," which will culminate in a flyby of comet Hartley 2 on November 4 2010. The spacecraft observed the moon for calibration purposes on several occasions en route to its second cometary encounter. [NASA/JPL-Caltech/University of Maryland]

Short-range 'lunar hydrology'

Observations from NASA's Deep Impact mission of the moon's north pole June 2 and 9, 2009 revealed changes in the amounts of water and hydroxyl. In the week between these datasets, the moon rotated 90 degrees. A volcanic mare terrain (labeled 'M') is observed in the morning on June 2 and at local noon by June 9 and a highland unit ('H') begins at noon and rotates to evening by June 9. Deep Impact observed a significant change in the strength of a water and hydroxyl signature as the moon rotated around. The highland unit has a weaker signal near noon (red) and a stronger signal by evening (blue). Taken together the data show a "systematic" change in water loss from morning to noon, recovery in the afternoon and return to "steady state" by evening. This daytime cycle suggests that hydrogen ions in the solar wind may be a source for re-hydration. [NASA/JPL-Caltech/University of Maryland]

NASA instruments reveal water molecules in lunar surface

Minerally-bound water in the ejecta blanket of a fresh crater (less than 100 million years old) as detected in 1,000 gigabytes of data collected by NASA's 3M spectrograph as it flew aboard the Indian Space Research Organisation (ISRO) lunar orbiter Chandrayaan-1. A simular image was built showing hydroxels that was not spread from the point of impact in all direction, as is the water-bearing materials, showing that the hydroxel-bearing minerals were likely to have been excavated from some depth.

"The moon continues to surprise us," said Dr. Carle Peiters, principle investigator for the American-made 3M experiment on-board India's Chandrayaan lunar orbier. "Widespread water has been detected on the surface of the Moon."

Instruments aboard three spacecraft reveal water molecules in amounts greater than predicted.
Hydroxyl (OH) - molecules consisting of one oxygen and one hydrogen atom was also was found in the lunar soil, in greater abundance. The findings were published in Thursday's edition of the journal Science.

NASA's Moon Mineralogy Mapper, or "M3," instrument reported the observations. M3 was carried into space on Oct. 22, 2008 aboard the Indian Space Research Organization (ISRO) Chandrayaan-1 lunar orbiter. A more robust but very similar instrument, the Mini-RF mapper, is now operating on NASA's Lunar Reconnaissance Orbiter (LRO).

Data from the Visual and Infrared Mapping Spectrometer (VIMS) on Cassini spacecraft and the High-Resolution Infrared Imaging Spectrometer on NASA's EPOXI (AKA "Deep Impact") contributed to confirmation of the findings.

"Water ice on the moon has been something of a holy grail for lunar scientists for a very long time," said Jim Green, director of the Planetary Science Division at NASA Headquarters in Washington.

From lunar orbit M3's state-of-the-art spectrometer measured light reflecting off the moon's surface at IR wavelengths and revealed "a new level of detail in surface composition," according to NASA.

"When the M3 science team analyzed data from the instrument, they found the wavelengths of light being absorbed were consistent with the absorption patterns for water molecules and hydroxyl.

"For silicate bodies, such features are typically attributed to water and hydroxyl-bearing materials," said Carle Pieters, M3's principal investigator from Brown University. "When we say 'water on the moon,' we mean molecules of water and hydroxyl that interact with molecules of rock and dust specifically in the top couple of millimeters of the moon's surface. "

Whether this water is a result of solar wind interaction, out-gassing, cometary impacts, a combination of all of these and other lunar exospheric dynamics is not yet understood.

The M3 team found water molecules and hydroxyl at diverse areas of the sunlit region of the moon's surface, but the water signature appeared stronger at the moon's higher latitudes. Water molecules and hydroxyl previously were suspected in data from a Cassini flyby of the moon in 1999, but the findings were not published until now.

Roger Clark of the USGS, and a member also of the Cassini and 3M teams said the finding was not detected previously because removal of spurious detections of water is very much a part of the calibration process. Cassini was switched on during its fly-by of the Moon in November 1999 as calibration began and was immediately switched off until the vehicle approached Saturn. in 2004. Detection of a lunar water signature in the Cassini data was not apparent until 2008, after four years in Saturnian orbit.

"The data from Cassini's VIMS instrument and M3 closely agree," said Clark. "We see both water and hydroxyl." While the abundances and ratios are not precisely known, as much as 1,000 parts per million could be in the lunar soil. "To put that into perspective, if you harvested one ton of the top layer of the moon's surface, you could get as much as 32 ounces of water."

For additional confirmation, scientists turned to the "EPOXI" mission (AKA 'Deep Impact") and calibration data collected while it flew as close as 8 million kms from the moon in 2008 and June 2009 (on its way to a November 2010 encounter with comet Hartley 2).

That spacecraft confirmed the VIMS and M3 findings and expanded on them. "With our extended spectral range and views over the north pole, we were able to explore the distribution of both water and hydroxyl as a function of temperature, latitude, composition, and time of day," said Jessica Sunshine of the University of Maryland.

Sunshine is EPOXI's deputy principal investigator and also a scientist on the M3 team. "Our analysis unequivocally confirms the presence of these molecules on the moon's surface and reveals that the entire surface appears to be hydrated during at least some portion of the lunar day."

Because the EPOXI data in June 2008 were collected on two occassions, several days apart, Sunshine said, it was possible to see a stronger water signature at sunrise that dissipated at Noon and reaccumulated in the afternoon, before local sunset.

Meanwhile, ahead of the LCROSS impact on October 9, NASA is excited by the possibility of understanding lunar hydrology as a function of depth, as the impactor excavates as much as a meter deep into Cabeus A.