measuring the polarization of disk-integrated lunar...
TRANSCRIPT
Au
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umm
er 2
010:
Lab
orat
ory
for
Me
asu
rin
g t
he
po
lari
zati
on
of
dis
k-i
nte
gra
ted
lun
ar
refl
ect
an
ce in
th
e m
idd
le
ult
rav
iole
t
Pa
ige
Ba
ile
y
Ric
e U
niv
ers
ity
Me
nto
rs:
Gre
go
ry H
ols
cla
w a
nd
Ma
rtin
Sn
ow
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Lab
orat
ory
for
Ove
rvie
w
•Background
–Key definitions
–What we were trying to find
•Analysis
–Methods used to address problem
•Conclusions
•Future Steps
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Lab
orat
ory
for
Ove
rvie
w o
f S
OR
CE
•S
OR
CE
= S
OLa
r R
adia
tion
and
Clim
ate
Exp
erim
ent
•S
peci
fical
ly lo
okin
g at
the
dat
a
from
the
the
SO
LSTIC
E
(SO
Lar-S
Tel
lar
Irra
dian
ce
Com
paris
on E
xper
imen
t)
inst
rum
ents
Au
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Lab
orat
ory
for
Mo
tiva
tio
n f
or
SO
RC
E
•N
ASA
-spo
nsor
ed; la
unch
ed in
200
3
•P
rovi
des
mea
sure
men
ts o
f in
com
ing
x-ra
y, u
ltrav
iole
t, vi
sibl
e, n
ear-
infrar
ed, an
d to
tal s
olar
irra
diat
ion.
•Thi
s da
ta a
ddre
sses
long
-ter
m c
limat
e ch
ange
, na
tura
l var
iabi
lity
and
enha
nced
clim
ate
pred
ictio
n, a
nd a
tmos
pher
ic o
zone
and
UV
-B r
adia
tion
•4
inst
rum
ents
: S
pect
ral I
rrad
ianc
e M
onito
r (S
IM), S
olar
Ste
llar
Irra
dian
ce
Com
paris
on E
xper
imen
t (S
OLS
TIC
E), T
otal
Irrad
ianc
e M
onito
r (T
IM),
and
XU
V P
hoto
met
er S
yste
m (
XP
S)
Au
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Lab
orat
ory
for
SO
LS
TIC
E (
A a
nd
B)
•P
urpo
se o
f S
OLS
TIC
E =
one
of
four
inst
rum
ents
on
SO
RC
E
•M
easu
res
the
ultrav
iole
t (fro
m
~115
-310
nm
), w
ith a
2.2
nm
reso
lutio
n in
MU
V (
180-
310
nm)
stel
lar
mod
e an
d 0.
1 nm
reso
lutio
n in
sol
ar m
ode
Au
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orat
ory
for
SO
LS
TIC
E s
et-u
p
•G
ratin
g sp
ectrom
eter
•Fie
ld o
f vi
ew =
~2
degr
ees;
en
tire
moo
n is
sho
wn
•D
etec
tor
is a
pho
tom
ultip
lier
tube
; m
easu
res
one
wav
elen
gth
at a
tim
e by
chan
ging
the
rot
atio
n of
the
gra
ting
–P
lane
wav
es, in
cide
nt o
n th
e gr
atin
g, a
re d
iffra
cted
into
zer
o an
d fir
st o
rder
–R
otat
ing
the
grat
ing
caus
es the
diff
ract
ion
angl
es to
chan
ge
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Lab
orat
ory
for
Inte
rnal
wo
rkin
gs
of
SO
LS
TIC
E
Pla
ne g
ratin
g m
onoc
hrom
ator
des
ign
–us
es o
ne c
onca
ve m
irror
to
col
limat
e an
d fo
cus
the
spec
trum
. O
nly
light
that
leav
es th
egr
atin
g at
the
corr
ect a
ngle
will
pas
s th
roug
h th
e ex
it sl
it.
Au
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Lab
orat
ory
for
Ref
lect
ion
Gra
tin
g, c
td.
Pla
ne w
aves
, in
cide
nt o
n th
e gr
atin
g,
are
diffr
acte
d in
to z
ero
and
first
ord
er
650
nm
400
nm
Zer
o or
der
Rot
atin
g th
e gr
atin
g ca
uses
the
di
ffrac
tion
angl
e to
cha
nge
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orat
ory
for
Orb
it o
f sp
acec
raft
64
5 k
m,
40°
incl
ina
tio
n,
90
min
ro
tati
on
pe
rio
d
* N
OT
E: n
ot to
scale
Au
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Lab
orat
ory
for
Ph
ase
ang
le
•=
0 (ful
l moo
n)
•=
180
(new
moo
n)
•=
-90
(wax
ing
quar
ter)
•=
+90
(wan
ing
quar
ter)
An
gle
MO
ON
Au
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Lab
orat
ory
for
SO
LS
TIC
E L
un
ar
Mea
sure
men
ts•
Rea
sons
why
SO
LSTIC
E lu
nar
mea
sure
men
ts a
re u
niqu
e:
–B
road
pha
se a
ngle
cov
erag
e (0
-170
deg
.)
–Ful
l-dis
k m
easu
rem
ent A
alw
ays
obse
rvin
g th
e w
hole
moo
n
–The
luna
r U
V r
efle
ctan
ce is
rel
ativ
ely
unex
plor
ed
–S
ince
the
moo
n an
d th
e su
n w
ere
obse
rved
with
the
sam
e in
stru
men
t,
refle
ctan
ce w
ould
n't de
pend
on
sens
itivi
ty
Au
gu
st 5
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0
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umm
er 2
010:
Lab
orat
ory
for
Qu
esti
on
s to
ad
dre
ss:
Can
we
mea
sure
the
pol
ariz
atio
n of
lu
nar
irrad
ianc
e in
the
ultr
avio
let?
Au
gu
st 5
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010:
Lab
orat
ory
for
Po
lari
zati
on
•D
efin
ition
: the
fra
ctio
nal l
inea
r po
lariz
atio
n of
a b
eam
of lig
ht fro
m a
bod
y
is d
efin
ed a
s:
•W
here
Is
is the
mag
nitu
de o
f th
e be
am w
hich
is o
rient
ed s
uch
that
the
elec
tric
vec
tor
is p
erpe
ndic
ular
to
the
scat
terin
g pl
ane,
and
Ip
is the
mag
nitu
de o
f th
e be
am w
hich
is p
oint
ed w
ith the
ele
ctric
vec
tor
para
llel t
o
the
scat
terin
g pl
ane
•P
olar
izat
ion
rang
es fro
m -
1 to
+1,
with
0 =
unp
olar
ized
ligh
t
ps
ps
bI
I
II
P+−
=
Au
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Lab
orat
ory
for
Ph
oto
met
ry
–The
stu
dy o
f th
e va
riatio
n in
the
brig
htne
ss o
f a
surfac
e or
body
as
a fu
nctio
n of
illu
min
atio
n an
d vi
ewin
g ge
omet
ry
–M
athe
mat
ical
fun
ctio
ns a
re u
sed
to m
odel
thi
s va
riatio
n
–E
ssen
tial f
or in
terc
ompa
ring
the
refle
ctan
ce o
f on
e su
rfac
e
to a
noth
er for
diff
eren
t vi
ewin
g ge
omet
ries
Au
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Lab
orat
ory
for
Sca
tter
ing
Pla
ne
•E
xam
inin
g th
e ge
omet
ry o
f
the
obse
rvat
ions
•D
eriv
ed the
vec
tor
norm
al to
the
scat
terin
g pl
ane
betw
een
the
Sun
-Moo
n-S
OR
CE
(th
e
sour
ce, th
e ta
rget
, an
d th
e
obse
rver
)
•P
olar
izat
ion
rang
es fro
m -
1 to
+1,
with
0 =
unp
olar
ized
ligh
t
Au
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orat
ory
for
EC
I Co
ord
inat
es
•E
arth
-Cen
tere
d In
ertia
l
•O
rigin
al d
ata
prov
ided
vec
tors
for
the
sun,
the
moo
n, a
nd
the
SO
RC
E s
pace
craf
t, bu
t
the
orie
ntat
ions
of th
e ve
ctor
s
wer
e no
t al
igne
d on
sim
ilar
axes
Au
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Lab
orat
ory
for
Ho
w a
re e
ffec
ts m
easu
red
?
•E
ffect
s ar
e m
easu
red
by r
otat
ing
a po
lariz
er w
ith r
espe
ct
to the
sca
tterin
g pl
ane
and
obse
rvin
g ch
ange
s in
mod
ulat
ion
of s
igna
l
•W
ide
rang
e of
pha
se a
ngle
s fo
r a
give
n ro
ll an
gle →
mea
ns w
e ca
n m
easu
re p
olar
izat
ion
Au
gu
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Lab
orat
ory
for
Ro
ll an
gle
fo
r sp
acec
raft
•D
eriv
ed b
y ob
tain
ing
the
cros
s pr
oduc
t of
tw
o ve
ctor
s (s
ame
as p
hase
angl
e)
•W
here
is it
poi
nted
?
–S
pace
craf
t ca
n po
int its
axi
s (a
ny d
irect
ion)
→de
fined
z-a
xis
–S
pace
craf
t ca
n ro
ll ab
out its
z-a
xis
–A
ll po
sitio
ns a
re s
tore
d in
dat
abas
e as
vec
tors
(w
ith d
irect
ion
& m
agni
tude
)
–E
arth
-Cen
tere
d In
ertia
l (E
CI) is
fix
ed w
ith r
espe
ct to
cele
stia
l sph
ere,
i.e.
sta
rs
are
iner
tial t
arge
ts
Au
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Lab
orat
ory
for
Bro
ad r
ang
e o
f p
has
e an
gle
s
Au
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010:
Lab
orat
ory
for
Alb
edo
at
250n
m v
s. r
oll
ang
le
Au
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Lab
orat
ory
for
Wh
y w
avel
eng
ths
wer
e ch
ose
n
Pol
ariz
er a
t 25
0 (s
ensi
tive
to p
olar
izat
ion
at lo
nger
wav
elen
gths
)
No
spec
tral
line
s @
195
(do
esn'
t m
atte
r w
hat ro
ll an
gle
is)
Au
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Lab
orat
ory
for
Rat
io a
t 25
0 n
m a
nd
195
nm
Sun
's s
pect
rum
is n
orm
aliz
ed w
ith a
Gau
ssia
n fit
Rat
io o
f sun
vs.
moo
n is
the
refle
ctan
ce
Ang
les
wer
e ch
osen
bec
ause
the
inst
rum
ent i
s se
nsiti
ve to
pol
ariz
atio
n at
250
nm, a
nd n
ot a
t 195
nm
Au
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Lab
orat
ory
for
Wh
at w
e ex
pec
ted
to
fin
d
•S
OLS
TIC
E is
a w
eak
pola
rizer
, an
d th
e pl
ots
of r
efle
ctan
ce v
s. r
oll a
ngle
shou
ld s
how
var
iatio
n if
ther
e is
a d
etec
tabl
e po
lariz
atio
n ef
fect
•The
slo
pe o
f th
e lin
e is
a m
easu
rem
ent of
the
mag
nitu
de o
f po
lariz
atio
n;
that
slo
pe is
the
n pl
otte
d ag
ains
t ph
ase
angl
e
•M
alus
's L
aw =
sta
tes
that
whe
n a
perfec
t po
lariz
er is
pla
ced
in a
pola
rized
bea
m o
f lig
ht, th
e in
tens
ity (
I) is
giv
en b
y:
•W
here
Im
= in
itial
inte
nsity
, an
d th
eta
is the
ang
le b
etw
een
the
light
's
initi
al p
olar
izat
ion
dire
ctio
n an
d th
e ax
is o
f th
e po
lariz
er
Au
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orat
ory
for
Lu
nar
po
lari
zati
on
•N
early
all
airle
ss s
olar
sy
stem
bod
ies
exhi
bit t
his
shap
e of
po
lariz
atio
n re
spon
se [H
apke
, 199
3].
•T
he c
urve
s ar
e ch
arac
teriz
ed b
y a
few
obv
ious
pa
ram
eter
s (P
is p
olar
izat
ion,
V is
ph
ase
angl
e):
•P
max
, Vm
ax•
Pm
in, V
min
•V
i(in
vers
ion
angl
e)•
h i(s
lope
at i
nver
sion
an
gle)
•T
his
show
s th
at th
e m
agni
tude
of t
he p
olar
izat
ion
is
inve
rsel
y pr
opor
tiona
l to
the
albe
do
(thu
s, th
e da
rk m
are
exhi
bit a
larg
e po
lariz
atio
n).
Au
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orat
ory
for
Wh
at w
e fo
un
d...
at
firs
t
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Lab
orat
ory
for
Red
uci
ng
un
cert
ain
ty o
f sl
op
e
•S
ince
rol
l ang
le d
ata
poin
ts s
houl
d th
eore
tical
ly b
e m
irror
ed a
cros
s
the
90 d
egre
e m
ark,
a c
omm
and
was
inpu
t to
ref
lect
and
com
bine
the
two
bran
ches
(do
ublin
g th
e da
ta, an
d ho
pefu
lly r
educ
ing
the
nois
e)
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orat
ory
for
Dat
a fi
lter
ing
•Filt
ered
out
liers
Apo
ints
gre
ater
tha
n 2
sigm
a from
the
mea
n
•Filt
ered
obv
ious
ly s
uspi
ciou
s da
ta
•Trie
d pa
rsin
g va
rious
inte
rval
s of
deg
rees
for
the
x-a
xis
(10
degr
ee in
terv
als,
20
degr
ees,
30
degr
ees,
etc
.)
•P
erce
ntag
e of
pol
ariz
atio
n
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orat
ory
for
Exa
mp
les
of
filt
erin
g
Pha
se a
ngle
from
0 to
10
Pha
se a
ngle
from
10
to
20
Ro
ll an
gle
vs.
Alb
edo
at
250
nm
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Lab
orat
ory
for
Res
ult
s: S
lop
e vs
. Ph
ase
An
gle
Au
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Lab
orat
ory
for
Qu
esti
on
s
Au
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Lab
orat
ory
for
Ack
no
wle
dg
men
ts
•Tha
nks
so m
uch
to LASP
and
the NSF
for
givi
ng m
e th
e
oppo
rtun
ity to
com
e do
res
earc
h at
Bou
lder
thi
s su
mm
er, to
Aet
na in
sura
nce
for
havi
ng d
octo
rs to
give
me
mon
o m
eds
(eve
n
in C
olor
ado)
-an
d, e
spec
ially
, Marty and Greg
for
bein
g
such
aw
esom
e m
ento
rs. H
uge
than
ks to Erin,a
nd to
all o
f
you guys
for
mak
ing
this
an
awes
ome
sum
mer
.