Good afternoon and
welcome to the Webcast about the results of the mission of the Lunar
Crater Observation and Sensing Satellite or LCROSS. We are fortunate
to today to have with us key members of the LCROSS science team.
At the far end of the table we have the principal investigator for
the mission, Dr. Anthony Colaprete, next to him is the astronomer
for the mission, Dr. Diane Wooden, next to me here is planetary
scientist, Dr. Jennifer Heldmann. My name is Brian Day. I was the
education and public outreach lead for the mission.
So this past November we actually had the announcement that water
had been discovered on the Moon by the LCROSS impact. That’s
pretty exciting. We know more now, but perhaps the best thing
to start out with is a little bit of an overview; real quickly,
what were the components of LCROSS and how did it work?
I can take that Brian if you’d like. I just happened
to have a model right here, that’s good! The LCROSS mission
was a secondary mission. It flew with the Lunar Reconnaissance
Orbiter Mission, which is in orbit still now around the Moon,
making lots of measurements, really mapping the Moon at unprecedented
detail, and LCROSS road with it. It was an opportunity; they had
some extra throw capacity/lift capacity to the Moon, meaning the
rocket could carry more than just LRO so NASA wanted to do something
with it. So we came up with this idea of LCROSS. You see in this
model of LCROSS here, LCROSS is technically just this small satellite
rights here, this little spacecraft. It actually connected to
the upper stage of the Centaur of the Atlas V (actually the Atlas
V took both LRO and LCROSS to the Moon) the upper stage or top
part of the rocket had this piece here called the Centaur. The
Centaur is about 12 meters long or so and about 2 ½ meters
wide. It’s a big rocket. It’s mostly fuel tanks with
some large engines on it. Normally this is ditched and it’s
dropped into the ocean, burns up on entry, and is thrown away.
We wanted to hold onto it and use it as an impactor. So we built,
with our colleagues at Northrop Grumman, this small spacecraft.
We called it the shepherding spacecraft because it shepherded
the Centaur around. I held onto it instead of its being thrown
away after it pushed LRO and LCROSS to the moon. We held onto
it for four months as we orbited the Earth. And what we were doing
there was we were drying this thing out, getting it completely
dry, no water in it, no other contaminants as best we could. We
calibrated our instruments; on this spacecraft (LCROSS shepherding
spacecraft) we had a number of instruments and you’ll hear
about the observations from those instruments in a bit, but we
had a variety of cameras, and instruments called spectrometers
on this spacecraft here.
After four months in orbit around Earth, it so happened that
basically the Moon got in our way – Now it was timed just
to do that, and that’s how we actually created the impact.
We timed our orbits around Earth so that as the Moon came around
we came around and met it at the South Pole. What impacted was
this part (the Centaur). About 9 hours before impact, we separated
from it and turned our instruments around to watch. This piece
(Centaur) went into the moon, and came in just like so (this is
not to scale, but the way), and we followed it about 4 behind
it. So both were moving at about 2 ½ kilometers per second.
This impacted the Moon; we observed the impact plume (the ejecta
cloud, vapors and whatnot) and the final crater with this spacecraft
(LCROSS) and it then eventually impacted the Moon as well. So
in a nutshell that was the LCROSS Mission and the hardware involved.
Excellent! So, again, last November we found out water
was observed in that plume that came up, but I think now we have
a better idea of how much, so how much water did come up out of
that impact plume?
Basically, as Dan put it, I think well:
about one us/ one of me -- about 150 kilograms or so in terms
of mass of what we saw in our field of view. That may not seem
like a whole lot, but when you compare it to the amount of dirt
that actually we could see too, it equates to about 5% or so by
weight in terms of mixing ratio. So, how much dirt--there’s
about 5% of the dirt was actually water ice.
a lot more than people think of…
Based on observations
from hydrogen measurements…we’ve never had a measurement
actually of water in on of these craters. So this is the first
real measurement of such. We thought there might be something
like maybe 1%, maybe upwards of about 1 ½ % perhaps. That
assumed that it was evenly distributed in the crater. So we were
excited to see that there was this much water, but maybe not necessarily
So Jen, what else did we find besides water
Jem: We found a lot of different types of ices and what we
call volatiles, which is a fancy science word, and basically,
it just means something, when it’s in the ground on the
Moon in these very cold areas it’s a solid, and then when
it gets into sunlight or it gets warmed up it turns into a gas.
So I think that Diane said it nicely, it’s like something
in your house that starts to smell because there are some vapors
coming off. So that’s what we talk about as volatile. Tony
has some data you might want to show to indicate the different
types of materials that were found.
Sure, we can describe
the spectroscopy of it…That’s one way to go about
it and I think we’ve got that video that I showed you a
bit ago that gives an example of spectroscopy. Maybe Diane, who
is the expert spectroscopist on the team, would like to talk to
Sure, I’d love to. Well, spectroscopy
is a tool where we break the light into its wavelengths, and we
look at how the molecules vibrate. Every molecule and every atom
has its own vibration pattern. Right here we’re seeing the
light curve of how much energy was emitted: First there was a
flash. Actually there was duration where we didn’t see any
light, and then there was a flash and decay, and from that measurement
we know … why don’t you take over here…
This is just showing the ejecta plume as it came up into light.
This is the Cabeus Crater, and we zoom in and this is the ejecta
cloud that we saw at about 20 seconds after impact. That red circle
is the field of view of our spectrometers that are making these
And this is a spectroscopy. So the first thing that we
do is we try to basically add things together and be a geological
sleuth. So here we’re adding water to the continuum of the
sunlight and you see that the upper curve is dropping down, better
matching. Then we add water vapor, and we get a better match.
Then we add some more volatile materials including methanol and
C2H2, and we get a best match. So we have primarily water and
water ice. But we also have more volatile materials of methanol
and formaldehyde and C2H4. This is very exciting because we never
imagined we would see these materials besides water. This is a
part what we call the curtain phase where the light is not evolving
as bright and Tony can describe the figure here.
did with that spectroscopy you just saw is we can monitor these
species over time and see how they’re changing, and that
figure you just saw in animation was basically how water vapor
was evolving after the impact. In this figure right her you can
see it’s relatively low. What we’re looking at here
is the depth of one of those features and the spectrum, and the
color of light: where there’s water it’s absorbing
or eating away a bit of the light, and if we measure how deep
that bite is, that’s what shown here and you can see that
red line indicates where the impact was relative in time. Before
it’s relatively flat, around zero. After it rises quite
quickly and it kind of holds steadily over the entire four minute
period as we observe the ejecta plume. So, this is how we can
determine what’s in a cloud and how much there is and how
it’s evolving over time. The rest of this video basically
shows the final evolution of the light plume. One of the interesting
things, Brian, is that we did actually fly through the ejecta
cloud in the very end with the spacecraft, and we were able to
detect that ejecta cloud in our instruments, which is really exciting.
That is exciting, to actually have the spacecraft flying
through this cloud of debris, and when you think of that Centaur
that created that cloud of debris, sometimes its fun to think
of it as something approaching the size of a school bus, but a
school bus moving at 5600 miles an hour. This becomes a fun job!
So it sounds like basically the spectrometers on board the spacecraft
broke up the light from that cloud into a series of rainbow colors
that actually had the fingerprints, if you will, of all the chemicals
that were in that cloud, and then the job that you did was kind
of like putting together a puzzle. You take the known patterns
of existing chemicals and you fit them together to match the pattern
that we saw from the spacecraft. Is that how it worked?
That’s right and the finger prints that we saw were not
only of water vapor and water ice (icy grains like little tiny
ice particles) but we also saw molecules much more complex than
what we thought we were going to see, and those molecules are
fairly common in comets.
Wow. So what do the chemicals that were detected tell
us about where the ice and the volatiles came from? Did they originate
on the Moon? Or did the come from somewhere else?
take that one. From the abundances that we saw, well, we saw molecules
that were very similar to comets. Comets are very good, over the
last billion years, comets hit the Moon and the materials would
have migrated and gotten stuck in these very cold regions on the
poles of the Moon where it’s very cold. We hit the south
pole, but it’s true of the north pole also that the sunlight
never reaches those craters and so the energy is very, very minimal
and they get very, very cold, so anything that gets there sticks
and stays. So over the last billion years comets could have hit
anywhere on the Moon and those materials would have created a
little vapor cloud and the vapor would have hopped and finally
gotten into those. So it’s like an attic where the last
billion years of what’s been happening we can see what’s
But the surprise is that the amounts of molecules that
we saw compared to water were higher than what we see in comets.
We came to think that maybe these molecules are actually forming
in those really cold regions.
So there’s actual active
chemistry going on, on the surface of the Moon?
cold regions, over a long time scale.
Another cincher for that
idea was the Lunar Reconnaissance Orbiter, which was the satellite
attached to here that is orbiting the Moon, they saw at the impact,
molecular hydrogen and carbon monoxide and those two molecules
are really volatile. Molecular hydrogen is enough to put up airships.
So molecular hydrogen would probably not stay around for more
than about a million years at the temperature of the cold craters
(40 degrees Kelvin). So we know that the material had to have
been made there. It’s really exciting that we discovered
that on the cold airless body of the Moon, the very harsh environment
there actually might be a nurturing place for molecules that are
important for life.
Wow. That is exciting. One of the things,
Tony, that you became kind of famous for before the impact, was
describing how the water ice on the Moon might be distributed.
I think you used the analogy: smooth style peanut butter versus
chunky style peanut butter, so whether the water ice was evenly
distributed or located in clumps. What did we find? Do we have
an answer to that question?
We’re one step closer
to maybe understanding the complexity of the question, which is
a good way to say: We know for sure now you can’t just say
its this way or that way. I think what we’ve learned is
that there’s a complexity to the Moon now and in particular
complexity to the water cycle on the Moon that we never appreciated
a couple of years ago. Where we hit we saw as I mentioned, about
5% water. If you took the remote sensing data, the data from the
spacecraft in orbit that tell us how much hydrogen there is (a
part of water – water is 2 hydrogen atoms and 1 oxygen atom
combined), from orbit we can measure where the hydrogen is, but
there’s other things that contain hydrogen and the area
over which you measure is very broad, so it’s kind of averaged
or smoothed out. So when we were thinking about LCROSS, one of
the tests we wanted to make was exactly what you just described:
is it uniformly distributed or is it in patches, in pockets. I
always think about food, so I use the peanut butter analogy; but
another analogy is it a thin frosting, (there I am thinking about
food again) like a thin layer of frost or is it ice cubes in the
dirt? And if you take our observation, with the latest neutron
data (the neutron data is what determines how much hydrogen there
is) it points to the chunky model being preferred. There are other
observations that support this idea. What we’ve learned
about some of the craters is that a lot of the craters at the
poles are extremely cold, but a lot of these extremely cold craters
don’t show signs of hydrogen from orbit. So it’s not
just good enough to be cold, to retain water ice or other hydrogen-bearing
species. There are some other observations from radar that also
suggest some areas perhaps that have slabs of ice in them. Other
observations show large veneers of very small amounts of water
even in sunlight. So what we’re learning is, you can’t
generalize the Moon, just like you couldn’t generalize the
Earth and say it’s this way and only this way. There’s
everything from, I think, the very thin, uniform veneers to blocks
of ice, perhaps. And LCROSS hit in one of those places where it
was rather enhanced.
Let’s talk a little more about
the nature of the ground that got hit by LCROSS. You mentioned
already that it’s probably 5% by weight water ice, but there
were a lot of other volatiles there, so how would you describe
the nature of the ground that we actually impacted?
been described in a lot of ways actually, and we were surprised
by this, but certainly fluffy.
Diane: Fairy castle-like?
Fairy castle-like, yea, and the reason we say that is, we measured
the flash of the impact. The flash is a part of the impact that
comes out first. The flash, and it happens when all of that dirt
and structure from the crashing impactor compress and rub against
each other and create heat. You mentioned that we were a fast
impactor; we were actually really slow compared to a natural impactor.
Meteorites striking the Moon hit ten times faster easily than
what we hit, and so the same sized impactor, a natural asteroid
impactor would have to be the size of a lemon to generate the
same kind of energy we generated with this big rocket. When those
things hit that fast, they create a bright flash of visible light,
white light. We didn’t see that, and what we saw was a very
delayed thermal flash, so we got temperatures up to about 1000
degrees Kelvin, or so. We saw that. But it was delayed from the
initial impact time. So what that means to us is we hit into something
that was really fluffy, fairy “castle-ish”, and with
all these volatiles you might imagine it could be like what’s
called it hoarfrost, I don’t know if anyone is familiar
with hoarfrost but if you live in areas that have very cool mornings
and you get a lot of water vapor in there you can have water vapor
freeze and create this very light fluffy matrix. Maybe that’s
something akin to what we hit.
Is that like when you walk across it, it goes crunch,
Yes, with a lot of empty space between all
So 5% of that was water ice. But then there’s
all this other stuff mixed in. How much of that was ice of some
sort, do we think?
Tony: Diane, do you want to take that? Diane:
I think that we decided about 1/3 of it – frozen volatiles,
icy stuff. Tony: And those are the things we could see. LCROSS
was very specifically designed to look for water, because it was
a strategic resource mission for NASA. It really begs the question:
What all is in there? You know, if we had better instruments,
the right kind of instruments to look beyond what we could see,
wonder what else is in there?
Some people might ask, “Well,
I can imagine what ice is, water ice, and ice cubes, but what
other kind of ices?” Well, I know one of them that we often
see is dry ice. Like when we’re trying to make a real scary
(we just had Halloween), a big scary, you know, fog or something,
that’s another kind, that’s frozen carbon dioxide,
and so that’s another kind of ice. And if you ever have
a chance to crush it with a hammer, it’s not as solid as
water ice, so it’s kind of an example of how fluffy friable
that is and mix that with dirt, let’s call it lunar soil – it’s
not the same as Earth dirt, but lunar soil, and you’re basically
going to get a fluffy structure. This is really exciting for us
because we really thought it was just maybe a thin layer of powder
on something solid.
Right, you bring up a good point, I
know Jen, you’ve got a lot of experience digging in frozen
debris in Antarctica, and if you put a little bit, even 5% water
ice in the dirt, it gets pretty firm pretty quick.
very hard! So what we’re finding on the Moon is very different
from what we find near the poles of the Earth, because when you
get water ice in dirt, like Tony said, it’s very hard, but
that’s not what we’re seeing here on the Moon. So
its surprising that we’ve all looked at the moon, at night,
and seen it up in the sky, and you think you know what it is and
then we send this mission to the poles, and then we realize, Wow,
there’s a lot more that we don’t know and we’re
surprised about still.
So it sounds like there was a good
place chosen to go. This crater, Cabeus, sounds to be a very interesting
target. How is Cabeus special? What makes it different than, say,
other areas on the Moon, where maybe the Apollo astronauts went?
What is so different about Cabeus?
If we look at the Moon globe we have here, the Apollo astronauts – the
Moon spins on its axis, pretty slowly and it’s pretty much
straight up and down, the Moon doesn’t tilt too much, so
it’s like this, and the Apollo astronauts mostly went towards
the equator, so in this part of the Moon. LCROSS went to the South
Pole, so way down here. The poles are very, very special on the
Moon: because there’s not much tilt there, the sunlight
comes in at a very low angle and some of these craters near the
poles of the Moon, there’s no sunlight that’s getting
in there for a billion years or more. So if there’s no sunlight
that’s reaching there, no direct sunlight, it’s very,
very cold. And so that’s why we were interested in going
there, because it’s very, very cold, and like Diane and
Tony told you, once you have ices and volatiles that get trapped
in these what we call “cold traps” the stuff stays
there for a long time. And so that’s what we wanted to go
And then also another thing about this particular
Cabeus Crater near the South Pole, as Tony mentioned, we were
looking at hydrogen, because we have maps of hydrogen, and we
know that water ice is H2O, which has two hydrogen in it, and
so we wanted to go somewhere where there was a high hydrogen signal,
and that happens to be in the Cabeus region as well. So there
are a lot of reasons why we picked Cabeus to go to. And, we haven’t
really explored the poles very much before because it’s
hard. Imagine you’re working, there’s no sunlight,
it’s completely dark. It’s really, really hard to
There’s one more reason, Jen, which is that
Cabeus is actually not as close to the pole as other regions that
show excess hydrogen, so we had a little bit better chance of
knowing more about it from Earth’s radar as you’ve
already mentioned. And also we were hoping that we would be able
to see the plume from Earth-based telescopes, because we would
have to be peering over a fairly big mountaintop in front, but
we would be looking grazingly in at a crater that wasn’t
really right at the poles.
So that’s again very interesting
in that we had this place that was far enough away from the pole
that we were hoping to get a good view, but that it was this very,
very fluffy ground that we hit, so when the Centaur hit, instead
of bursting into a big fireball on the surface, what happened?
It went cush!
It went cush! That’s a good way
to put it. It went cush. The other thing to keep in mind is the
Centaur was a giant empty thermos if you will. They’re big
tanks, they’re empty, so this, while it’s big and
it’s heavy, it’s mostly hollow, so it’s really
low density, so we had a very unique impact – very much
not like a normal, natural impact. And luckily we had a co-investigator
who worked here at NASA Ames, doing experiments at the vertical
gun to test out exactly what happened, but when you have this
low density impactor, impacting into a low density fluff you just
get all this compaction, everything: this crumples, the ground
compresses; and actually what happened was that this penetrated,
we think, deep into that fluff and created a vacuum, a pocket
behind it if you will, and that creates a cavitation; everything
races in behind it to fill in, and that created a jet, if you
will, of debris that went straight up, a very thin but fast debris
cloud that went up as high as 10 or 15 kilometers, so ten miles
up – almost straight up, very narrow cloud. They’ve
been able to reproduce that in the lab doing similar shots. So,
this was an experiment in a lot of ways. We had to make do with
what we had, the space junk that we were otherwise utilizing and
went to someplace that we’d never been before. So it was
full of surprises. That’s for sure.
We’ve still got hot enough to melt glass—I
think about 1000 Kelvin, is about 1300 degrees Celsius, which
is about the temperature that you might be able to melt glass
or blow glass. I just want to make sure they understand, we got
hot, but just not that hot.
A normal, natural impact would
get 6,000 degrees or so or 5000 degrees. We only got to a 1000.
So, we’ve already shown pictures of the plume, and
I think what you were saying Tony, is that you had some part of
the plume that went straight up very narrow, but there’s
another part that went out like a blanket and that most of what
you saw in that picture was that blanket part, but because we
saw material so late, even as late as a few seconds before we
impacted, that’s this material that went straight up really
far distance and then came down. It took a long time to go up
and down. That’s why it was still there when we actually
flew through it.
And a pencil is an excellent analog because
it was pencil thin. That jet that shoots straight up can be very,
very narrow, maybe just a degree or two or three. Jen?
to three degrees.
So the big question then, based on what
you were able to measure in the plume coming out, can you make
an estimate as to how much water ice there is in these dark areas
or around the dark areas of the Moon?
as I mentioned, what we learned is it’s not the same anywhere – it’s
certainly variable, so there needs to be a lot more work that
takes into consideration the new observations from LRO (The Lunar
Reconnaissance Orbiter) of hydrogen, of temperature, topography.
There’s an instrument called LAMP (Lyman-alpha spectrometer).
It looks at starlight and how starlight reflects off of the surface
of the Moon, and it’s going to give us some clues as to
how this hydrogen is distributed. So it’s going to take
time for us to really reassess how much water is on the Moon.
In the past we have kind of naively, or just because of lack of
data, simply said, “Hey, you have this much dark shadowed
area. If it’s at 1%, you have this much water.” Now
we know, well just being dark and shadowed is not a sure thing
for water ice, and it’s not 1%. Some places are 5%; some
may even be more than that. They might be like I said, blocks
of ice. So it’s going to take some time to really assess
things like that. Now, that said, the area where we hit in Cabeus,
the cold area (we hit a place on Cabeus that was particularly
cold – less than 40 Kelvin)….
How does that compare to like, say the surface of Pluto?
It is as cold or colder than the calculated surface temperatures
of Pluto. So the Moon is, as the lead for the instrument that
measured it put it, Dave Page at UCLA; he said, “As of now,
there is no other place in the solar system with a temperature
as cold as the Moon estimated.” Now we have not measured
Pluto yet. We’ve calculated it. We did the same thing for
the Moon: we calculated and found out we were off by factors of
2 in terms of how cold it was. So it remains to be seen, but as
of now, the Moon holds the record for the coldest measured place
in the solar system. It’s colder than the moons of Saturn,
which we have measured the temperatures – that’s why
I bring that up. But if you took that area where we impacted and
you said, OK, in a 5-kilometer radius around our impact site,
let’s say there’s 5% water ice there. It’s about
the same as what we saw in a 5-kilometer radius around us. Then
in the top meter of dirt you’d have about a billion gallons
of water at 5%. It’s not insignificant; it’s quite
So there could be a lot of water there on the Moon.
Did you know Brian that water is really expensive to transport
to the Moon?
That’s probably one of the main reasons
that we were interested in finding water on the Moon, right? How
much does it cost to get say a gallon of water from the surface
of the Earth to the surface of the Moon?
Well, since we’ve
never done it, we don’t know exactly, but I think I’ve
It’s on the order of $100,000 per gallon.
That’s for a single gallon, and if some of our students
out there some day might be living and working on the surface
of the Moon, just think of that: that’s for one gallon of
water. You’d probably want a whole lot more than one gallon
of water if you’re living and working on the Moon. Water’s
important not just for drinking, but breaking apart the constituent
hydrogen and oxygen; oxygen you need to breathe – that’s
something that you’ll really, really want to do if you’re
living and working on the Moon. So water’s clearly a very
valuable substance, and having found it in such large quantities
on the Moon, that’s exciting. But that brings up another
really important question: How has our view of the Moon changed?
If you look at how we understood the Moon to be before the LCROSS
mission, and now we look at our understanding of Moon, after the
LCROSS mission, how has that view of the Moon changed?
Before LCROSS we pretty much thought that the Moon was dry,
not much water, and then we sent LCROSS, and we found that there’s
all of this water ice near the poles of the Moon. So we completely
changed our view of the Moon: we went from this dry, barren world
to all of a sudden a place that has vast amounts of water near
the poles. So that, in itself, is interesting. So we’re
having to rewrite the textbooks. The things that you learn in
school are changing because of these missions where we go and
explore these places where we haven’t been before.
also very exiting too because now, as Diane and Tony were talking
about, we found all these other molecules and all these other
types of ices in the permanently shadowed region. We didn’t
know that those were there before. Now we’re trying to figure
out how they got there: was it comet impacts, asteroid impacts,
and as we’re learning it’s probably a whole combination
of a bunch of different things – a lot of impacts, and also
active chemistry going on on the Moon to form these molecules.
So now we think there’s an active chemistry cycle that is
going on here as well. And then there’s been some other
observations of other water across the Moon and what we call OH
(hydroxyl). Now we’re talking about a lunar hydrology cycle,
which we would never have talked about just a few years ago. Before
we sent some of these missions. So our whole understanding of
the Moon is changing based on this new data and based on this
exploration, which is one of the really exciting parts about doing
one of these missions – learning these new things.
Wow Jen, you did a great job of summarizing. I’ll just highlight
a couple of the things you said, which was in the weeks before
LCROSS we found out that there was OH, which is a part of water
H2O, so that’s like HOH. It’s just the OH part we
saw in the rocks on the Moon, and we didn’t realize so clearly
until we hit with LCROSS that there’s water in the form
of water, not just water bound in the rocks. So that’s one
really important thing and the idea that all the Moon, on the
poles of the Moon, it is so cold and so dark (or the fact that
it’s dark means it’s so cold) is that there’s
actually possible molecule formation. Before this time, we only
though those molecules would form in very early stages, before
suns and solar systems formed in very cold, dense dark clouds;
those are the kind of clouds that obscure the stars along the
Milky Way. We thought that that kind of molecule formation happened
maybe in the outer regions of our early protoplanetary disk, beyond
where Pluto formed, primarily in the dark clouds out of which
new suns formed. But here, we’ve discovered that perhaps,
those same kind of molecules might be forming on a body somewhat
close to our sun in a fairly harsh environment of the strong solar
wind, and this is really amazing, because those molecules, if
they get evaporated by impacts, which happen all the time, they
could become part of other aspects of the Moon, or perhaps incorporated
into rocks. It could be delivered by small lunar meteorites to
the surface of the Earth. It’s really amazing to discover
that chemistry that we thought only happened in really early conditions,
more than 5 billion years ago, in a cold black cloud, before our
sun was born actually is happening on our Moon, so close to home.
So, maybe I’ll pass the ball…
know how I could actually add much to that. I think maybe Jen
you said it, we rewrote some textbooks. It reminds me of a story
that one of our engineers told us, Steve Board, who said that
his daughter had a quiz and part of the quiz was basically, Which
of these bodies in the solar system has no water? The Moon was
on there and Steve’s like, What do I do here? Do I tell
my daughter to know the answer is: Yes, the Moon has water, when
they were expecting a “No” of course. So it just goes
to show, our thinking about the Moon in the last two or three
years because of the literal armada of space traffic that have
been there from all sorts of countries: Japan, China, India, the
United States has revealed this world that is right there next
to us that still remains to be explored. We’ve been to the
Moon near the equator with the Apollo missions. The poles of the
Moon are an entirely new world, and they’re as rich and
as diverse as any part of the world, Earth. So that for me has
been the most exciting aspect of the results of the past few years.
If you could compare where we hit to any places here on
Earth, what kind of water concentration would that compare to?
On average, the Sahara Desert has about 2 – 3% in
the top meter or so. It’s got a little more water down below,
as you might imagine, but that’s one number that I found
in the literature was about 2-3% on average for the Sahara Desert.
There is a place on the Moon wetter than a place on Earth, which
is kind of neat. Kind of amazing, actually.
So were do
we go from here? What’s our next step?
Tony: One of our
next steps is to understand further this water cycle. Jen mentioned
and Diane too that there’s OH and water in sunlit parts
of the Moon, and that a lot of the things we see trapped in the
cold traps, these cold places, are potentially from impacts occurring
elsewhere and processes occurring elsewhere on the Moon and those
things, those impacts, for example, or chemical processes, causing
a migration of materials to these cold traps.
mission called LADEE (Lunar Atmospheric Dust Environment Explorer)
will be launched by NASA in a couple of years and its purpose
is to study the very tenuous atmosphere of the Moon. There is
an atmosphere on the Moon, it’s really an exosphere, meaning
the poor little molecules never really see each other, and in
an atmosphere they’ll bump into each other and can say hi.
On the Moon there’s so few of them that as they leave the
surface they may never see another one again. That’s really
a sad life, but it’s a critical life, because those individual
molecules, as Diane put it, opting around on the Moon may be part
of the process, they’ve certainly got to be part of the
process of accumulating these ices and other things at the poles,
so LADEE will study that and will study dust potentially lifts
off the surface and migrates around the Moon as well, so that’s
one extra piece of the puzzle that we’ll be studying soon.
Excellent. Now I believe Linda Conrad has some questions
that you, our viewers have been sending in.
You guys are
doing an excellent job of answering the questions before you get
them, but just to mention, our friend from India, Dibyendu because
he’s been on for several hours and it’s after midnight
there, he asked: I want to know the details about the South Pole
of the Moon where ice is found. You’ve pretty well covered
it, but maybe you want to put a cap on it.
A polar cap? Sorry!
If you went back to the image of the
dust cloud in that animation, that’s one place we can start.
There’s a good deal of material online that you can find
if you go to the www.nasa.gov/mission_pages/lcross <http://www.nasa.gov/mission_pages/lcross> webpage
under the media tab there’s a headline there about a media
briefing, if you click to read more you can see details from all
the investigators who contributed recently papers in the magazine
SCIENCE, which detail specifically the Cabeus region, which is
shown here. So Cabeus is that large crater that you see right
in the middle. It’s about 84 and a half degrees south, so
it’s about five degrees off the South Pole of the Moon.
For those of you who are enthusiasts, Shackleton is another famous
crater at the South Pole. It’s almost right at the pole.
This crater is about 100 or so kilometers across. It’s very
old and degraded. You can see it’s not particularly round
anymore, and it’s been beat up pretty bad – that shows
its age. It’s probably about three, three and a half, three
point eight billion years old. The large ridge, that hill there,
M-1 that was the bane of many ground-based observers, is actually
part of the outer ejecta ring from the Aechin Basin impact, which
is on the other side of the South Pole. So this is a very old,
heavily eroded part of the Moon. It is on the Earth side (the
Earth would be up in this image, or in the direction of Earth.)
Now where we impacted was right next to that little dimple on
the upper left hand corner. There’s a little dimple there,
a large crater, and we impacted just to the inside of that where
it was very, very cold.
But more information specifically on the
details can be found at the LCROSS website online at NASA, but
also at some of the individual missions who were observing, in
particular if you go to the LROC website (that’s LROC: the
Lunar Reconnaissance Orbiter Camera - http://lroc.sese.asu.edu/).
They’ve got a beautiful mosaic of the South Pole of the
Moon at 400-meter resolution, and other instruments are the Lunar
Laser Altimeter (LOLA) has beautiful digital elevation maps of
the South Pole of the Moon. All of this is public information
now, and that’s one of the great things about these NASA
missions, is they are required to provide their data to the public.
All of the LCROSS data is actually online too if you go to the
Planetary Data System and search LCROSS you can find all the LCROSS
data, all of our image data and spectral data are located there.
You know, Tony, I also saw a really great image on the
Astronomy Picture of the Day, in about the last week. It was a
wonderful composite. It showed sort of a candy cane stick-up of
the pole and the whole Cabeus region in a sort of 3-d projection
with the colors: blue for where there’s hydrogen excess and a little
bit or a squirrelly line showing where the permanently shadowed
region is, and that came out of the science articles that were
released, so if people don’t have access to the science
articles, then, after they’ve looked at the NASA site, that
a wonderful kind of global view. Tony That’s a very nice
picture that the LEND team (the Lunar Exploration Neutron Detector
Team) put together with LOLA, so it’s an excellent image.
So again if you look at the archive section of Astronomy
Picture of the Day, you’ll be able to see some of our best
imagery so far of the terrain near the South Pole of the Moon.
A question here from Owens: Would there have been a better
place to land so that we could have seen the flash?
take that, because I’m the astronomer.
And you were
up there observing it.
Diane: And I was up there observing it
-- I led four international teams at some of the biggest telescopes
on Mauna Kea. The reason we went to Cabeus was the high hydrogen
content that was located by the Lunar Reconnaissance Orbiter,
LEND instrument on that spacecraft before we hit. We had the option
of pointing in several different regions, up to a few weeks before
impact. It was a hard decision; I had many conversations with
Tony about “There’s a big mountain in the way,” but
it was very important that we went to a place that was hydrogen
rich. We had discussed about going to a couple of other regions
at about that same latitude, and they would have been easier to
see from Earth, but since we haven’t been there, to impact,
to really understand what’s there, it’s possible that
the richness of what we discovered would not have been so great
if we chosen to really push towards Earth based observations.
So I think that the plume that we saw and the camera was very
diffuse that you saw in the imager earlier in the broadcast, or
that you can see on the lcross.arc.nasa.gov <http://lcross.arc.nasa.gov> website.
That same image is available. Yes, we could have gone to a bunch
of different locations, but we chose a location with the best
chance of observing water, and we did see water. And I think that
that’s where the ground observers were challenged and yet,
I’m really very happy that we went there.
And I can
add to that, that we got as many eyes on it, different eyes on
it, everything from the Hubble Space Telescope, to orbiting satellites
(Jen Heldmann was actually the coordinator of all these assets
and there were what, 30ish or more. And we had LRO. We had hoped
to have Chandrayaan, the Indian spacecraft observing, but it was
lost just a month before impact – we were really disappointed,
saddened by that. One of the reasons we had so many things looking
was because this was an experiment. We’ve never crashed
the empty upper stage of a rocket into the Moon at the Southern
Pole into the permanently dark crater, and so we did the best
we could beforehand to predict what would happen, and as Diane
said, we had to go someplace that was relevant to the goals of
the mission, and that was a very difficult decision for all of
us to make – to pull away from our best Earth-observing
assets, because we had lined up such fantastic teams, but if we
had impacted where there was no hydrogen, as it turned out, that
would have been maybe a nice show for some Earth-based observers,
and we might have learned something about impacts and things like
that, but it wouldn’t have addressed the principal question,
which is: What is that hydrogen? That’s what we had to go
after, so that’s why we went deep into a crater. I remember
honestly when LCROSS first started, four odd years ago, we were
talking about all the various craters on the Moon’s poles
to go to, and I said to the team, “We are never going into
Cabeus. It’s too big a hole and it’s got a big mountain
between it and Earth.” And, in the end, it was the one place
that had the most hydrogen, was the most compelling in terms of
relevance, and so we had to go there.
And there were a couple of detections from ground-based
observatories. Kitt Peak Observatory in Arizona and McDonald Observatory
observed sodium, so they saw some of the gases that were coming
out from the impact.
Likewise HST has tentative detection
of hydroxyl, as well.
So that’s the Hubble Space
That was very exciting, Jen, because it was
really a team effort by many astronomers at many different observatories
and you coordinated it all and had us all knowing exactly what
was happening as the spacecraft was coming down, and Rosemary
Killen who led the Kitt Peak Observations, she was observing at
the impact site where many of us were, and didn’t see anything
initially, and moved her spectrometer to look just off the limb
of the Moon and then discovered a very bright emission. So by
being a very good experimentalist, she saw the material that went
up, that was hot, that went up really fast. And that was a really
great discovery. We’ve known that there’s sodium in
the exosphere of the Moon, but to see so much of it released by
an impact is very exciting.
A question here from Westhill
High School: Was the amount of water found expected, and also,
are there other locations on the Moon where water can be found?
I can take that. The water, as I mentioned earlier, was
maybe higher than some would have expected if you assumed a uniform
distribution. And others would argue that it’s completely
reasonable to have that kind of concentration. One of the things
it tells us is that the water is not nice and uniform, but it
is probably concentrated in pockets. Some people believed that
this was the case. Other people thought it would be much more
uniform. So, I wouldn’t say that it was unexpected. We went
in with kind of an attitude that it was going to help to determine,
at least where we impacted, which it was: either uniform or concentrated,
but we weren’t particularly surprised.
you want to say something about the fact that they’re seeing
water in areas where there’s sunlight?
seeing hydrogen. That’s one of the other interesting discoveries
from LRO, is that the neutron spectrometer appears to detect hydrogen
enhancement in areas where there is not permanent shadow, but,
what we call “temporarily lit regions,” so there’s
a permafrost if you get below the top layer of soil (and I just
mean 5 or 10 centimeters) the temperatures can be very cold. It’s
because the lunar dirt is such a good insulator (it doesn’t
conduct heat), and so if it only gets sunlight for a few days
out of the day (Earth days) then at ten centimeters down, you’re
at minus 200 degrees centigrade, and water can be stable. So there
is this potential that in areas that are not permanently shadowed,
you can have water just underneath the surface.
you saying that because the soil is fluffy, there could be ice,
excuse me, there could be hydrogen there, and that maybe the soils
fluffy because there’s ice there?
We don’t know.
We don’t know if it’s the same in the sunlight. Where
we hit it was 40 degree Kelvin, and the top surface could be very
different from where it gets some sunlight. So what we found is,
it really gets to the question: Where else could you find water?” Well,
we’re thinking now that there could be permafrost below
the surface that really extends to a wide area of the Moon that
could potentially be holding water ice. We just don’t know.
We can’t tell for sure. LCROSS sampled one place so it really
begs the question about going back and sampling some other places.
There are a lot of favorite moments from a mission like
this, but one of my favorite moments I remember in a news interview
before the impact: a reporter asking Tony, “What do you
expect?” And Tony’s answer was: “I expect to
be surprised.” That’s kind of one of the beauties
of carrying out an experiment like this, because if what you find
is exactly what you thought you were going to find, you haven’t
necessarily learned a whole lot. But then, when things come out
that surprise you, that’s a really excellent opportunity
to do some learning.
We went to a completely uncharted place,
part of the Moon we’d never been before, can’t see,
haven’t explored. It was really terra incognita, both the
impact, the place, everything. That’s why we looked at it
in so many different ways, and we tried to keep our eyes wide
opened because we knew that if we thought we knew just exactly
what was going to happen we’d probably be wrong and miss
something. So we tried to come in as open to any possibility as
We have a couple more here on the Moon. Since
we feel now that the Moon was probably part of Earth at one time,
is it possible that the water being found on the Moon now was
actually from the Earth at the time of impact or breaking off
from the Earth?
That’s a good question.
Jen to Diane:
You had comments on that.
Well, I think Tony was saying
that it’s a part per million; tens of parts per million,
so that’s less than a tenth or a hundredth of percent of
water has been found in the rocks; tiny vesicles vacuum with water
inside of them in the samples that were brought back by the astronauts.
And these were reported in the 1970s, and had brought some skepticism
to the origin. But since we now see OH (that’s a part or
water we talked about before), the OH in the rocks, more of this
has been discussed about how volcanism on the Moon could have
brought some of the water in the rocks that originated from Earth
when the Moon was ripped off by a big impact and formed from mantle
material of the Earth, that that water could actually be part
of the rocks. But it’s such a low concentration; you can’t
really say that that water in the rocks is the water that we saw
in the LCROSS, because the reservoirs just don’t add up.
You have 600 times the amount, if my math is correct, 600 times
the amount of concentration that we saw in LCROSS versus what
is known to be in rocks due to the material that was there originally
from its formation.
So we’re talking about different sources of water.
We’re talking about water inside the Moon, incorporated
into the rocks that might have come from that early separation
of the Earth and the Moon. But then we’ve got these big
concentrations of water ice at the poles that probably came from
somewhere entirely different.
That’s right and your point again that we said it was water
ice; we actually saw ice particles, and those ice particles have
to be fairly pure to have lasted for four minutes. If you mix
ice with dirt, the sunlight is absorbed more easily, warms up
the particle, and that ice turns into water vapor. So the fact
that there’s ice particles, that’s very different
than water being in the rock.
The Moon has a very complicated
story to tell, and water on the Moon seems to be coming from:
maybe some of it came from early stages when it separated from
the Earth, but a lot of it is coming from comets,
water rich asteroids…
…and maybe even the
solar wind, the hydrogen streaming from the sun. So the Moon’s
a complicated place. It has a much more dynamically interesting
story to tell than perhaps we had thought.
One point along
those lines is: What I’ve really been inspired by in the
last number of years is where we are discovering water, active
water systems, and these kind of chemistries that we’re
talked about on the Moon, Enceladus in Saturn; we see geysers
coming from its South Pole. The entire E ring of Saturn is made
of water ice crystals coming out of the moon Enceladus. That’s
incredible! It’s probably, in my mind, the greatest discovery
in the last ten years, or fifty years. A few weeks ago when we
were at a scientific meeting, and they were showing the composition
or some of the other things they were seeing in that ice, it looked
a lot like the ice stuff that we saw on LCROSS. And now at Mercury,
we have a spacecraft getting to Mercury, the Messenger spacecraft,
they’ve been finding some interesting things at Mercury.
It’s long been speculated that the poles of Mercury have,
in their craters, just like the Moon, water ice. We suspect this
from radar. So we’re seeing this trend, this thread that
ties the entire solar system together, and it’s what we’re
finding in these dark craters of the Moon.
I have several questions that have come in relating to
the saying, “Where there is water there is life.” When
searching for water, are we also looking for organisms or life?
I know that Jen has thought about this.
thing to keep in mind is that these places near the pole of the
Moon that we’re talking about…since we’ve told you
that you don’t get direct sunlight there, they’re
extremely cold: near absolute zero, 40 Kelvin – that’s
really, really cold. That’s too cold for any life, as we
know it, and life as we know it on Earth, requires liquid water.
We’re not talking about liquid water near the poles of the
Moon, because it’s too cold. It’s frozen, so we’re
talking about very, very cold frozen water. So it’s very
difficult: we’re not looking for life right now near the
poles of the Moon. It’s just too cold, there’s not
liquid water. But like Diane was talking about, there’s
some chemistry going on there that’s very, very interesting
that can be creating the types of molecules that are precursors
So what’s so important about liquid water
We know that all life forms on Earth require it.
We haven’t found any form of life, anywhere on Earth that
doesn’t need some liquid water. Some need very small amounts
of liquid water, but they have to have liquid water, and it’s
just too cold by the poles of the Moon to have it.
is either solid or vapor on the Moon in the poles.
My favorite question is always: “Do you like your
job as a scientist, and what can a sixth grade student do now
to prepare for a life in aerospace and science engineering?
I think it’s safe to say that we all like our jobs.
It’s pretty fun. We get the chance to answer
really interesting science questions. We get to explore places.
I mean, our job is to explore the Moon. How cool is that! So that’s
pretty fun. For starting in sixth grade, one thing you can do
is come to Webcasts like this. That’s great so you can learn
more about: What is NASA doing? What are other countries doing?
What are we learning about space? What do we know about the planets?
And I would say, going to your local science museums, going to
the planetarium, going to astronomy star parties, if you’re
interested in that, reading books from the library, all sorts
of things like that. Do you guys have other suggestions?
We all know that math and physics will become part of your daily
tools when you’re a scientist, and I love my job. But I
think it’s also very important to develop tools of critical
thinking. So that it’s not just the knowledge, but it’s
how we think. It’s how we think as a team. It was together
that we came up with these ideas about what must be happening
on the poles of the Moon, by brainstorming. Just keep in mind
that it’s important to always bring your attention to everything
that you do and see.
I know we’re short on time, but
just to emphasize those two point that I think are really important
is that teamwork, that getting involved with groups, doing the
kinds of things that we do in groups is what makes a great scientist
and a great engineer. Nobody does this alone. It takes a huge
team effort, and that’s important: Get involved in groups.
Well, I think that that probably a good note to end on
there. I will point out that what has happened here is: It looks
like we’ve gained an entirely new view of the Moon. The
Moon is something very different than we thought it to be. But
in answering some of these initial questions from LCROSS, it sounds
like what you’ve done is raised a large number of new questions.
So what that means is, there is a vast new area of exploration
that is going to be available to our next generation of explorers.
We have a team here that is doing some amazing work, but they
are raising new questions that we’re going to need a new
generation of people to answer, and we’re looking forward
to seeing the answers that you, the next generation of explorers,
come up with.
I want to thank our team of scientists here who’ve
done such a wonderful job of the LCROSS mission. Again: Tony Colaprete,
Diane Wooden, and Jennifer Heldmann. Thank you all, and thank
you for joining us.