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CFH
T A
nnua
l Rep
ort
1
Cana
da-F
rance
-Haw
aii Te
lesco
peAn
nual
Repo
rts20
09 &
201
0
4020
09 &
201
0
Cana
da-F
rance
-Haw
aii T
elesc
ope
65-1
238
Mama
lahoa
Hwy
Kamu
ela, H
I 967
43
Tel (
1) 8
08 8
85-7
944
Fax (
1) 8
08 8
85-7
288
www.
cfht.h
awaii
.edu
CFH
T A
nnua
l Rep
ort
39
Qua
nz S
., G
oldm
an, B
., H
enni
ng, T
., B
rand
ner,
W.,
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row
s, A
., H
ofst
ette
r, L.
W. S
earc
h fo
r Ver
y Lo
w-M
ass
Bro
wn
Dw
arfs
and
Free
-Flo
atin
g P
lane
tary
-Mas
s O
bjec
ts in
Tau
rus.
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24
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thor
s Th
e Ta
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auru
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ork
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r. G
rego
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lman
- H
erzb
erg
Inst
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of A
stro
phys
ics
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Jam
es R
. Gai
nes -
Uni
vers
ity o
f Haw
aii
Dr.
Jean
-Mar
ie H
ameu
ry -
Inst
itut N
atio
nal d
es S
cien
ces d
e l'U
nive
rsD
r. R
ober
t A. M
cLar
en (T
reas
urer
) (20
10-2
011)
- In
stitu
te fo
r Ast
rono
my,
Uni
vers
ity o
f Haw
aii
Dr.
Har
vey
Ric
her -
Dep
artm
ent o
f Phy
sics
& A
stro
nom
y, U
nive
rsity
of B
ritis
h C
olum
bia
Dr.
Gen
eviè
ve S
ouca
il - O
bser
vato
ire M
idi-P
yrén
ées
Scie
ntifi
c A
dvis
ory
Com
mitt
ee -
2010
Dr.
John
Bla
kesl
ee (T
AC
) - D
omin
ion
Ast
roph
ysic
al O
bser
vato
ry, H
erzb
erg
Inst
itute
of A
stro
phys
ics
Dr.
Mar
k C
hun
- Ins
titut
e fo
r Ast
rono
my,
Uni
vers
ity o
f Haw
aii
Dr.
Thie
rry
Con
tini (
TAC
) - L
abor
atoi
re A
stro
phys
ique
de
Toul
ouse
-Tar
bes
Dr.
Pier
re-A
lain
Duc
- Se
rvic
e d'
astro
phys
ique
, CEA
Sac
lay
Dr.
Bre
tt G
ladm
an (C
hair)
(201
0-20
11) -
Dep
t. of
Phy
sics
and
Ast
rono
my,
U. o
f Brit
ish
Col
umbi
aD
r. D
enis
Mou
rard
(Vic
e-C
hair)
(201
0) -
Obs
erva
toire
de
la C
ôte
d’A
zur
Dr.
Cor
alie
Nei
ner (
TAC
) - L
ESIA
, Obs
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toire
de
Paris
Dr.
Dav
id B
. San
ders
(TA
C) -
Inst
itute
for A
stro
nom
y, U
nive
rsity
of H
awai
iD
r. G
regg
A. W
ade
(TA
C) -
Dep
artm
ent o
f Phy
sics
, Roy
al M
ilita
ry C
olle
ge o
f Can
ada
Dr.
Jon
Will
is -
Dep
artm
ent o
f Phy
sics
and
Ast
rono
my,
Uni
vers
ity o
f Vic
toria
CFHT Annual Reports 2009 & 2010C
FHT
Staf
f(on
Dec
31s
t, 20
10)
Aka
na, M
oani
A
dmin
istra
tive
Spec
ialis
tA
rnou
ts, S
téph
ane
Res
iden
t Ast
rono
mer
Arr
uda,
Tys
on
Mec
hani
cal T
echn
icia
nB
abas
, Fer
dina
nd
Ass
ista
nt S
yste
m A
dmin
istra
tor
Bar
il, M
arc
Inst
rum
ent E
ngin
eer
Bar
rick,
Gre
gory
O
ptic
al E
ngin
eer
Bau
man
, Ste
ve
Ope
ratio
ns M
anag
erB
ened
ict,
Tom
In
stru
men
t Spe
cial
ist
Bry
son,
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el-
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09 &
201
0
Dire
ctor
’s M
essa
geTw
o Ye
ars
in O
ne R
epor
t! 20
09 a
nd 2
010
wer
e ve
ry b
usy
inde
ed. M
uch
wor
k w
asac
com
plis
hed
on i
mpo
rtant
in-
hous
e pr
ojec
ts.
Key
dec
isio
ns w
ere
mad
e on
fut
ure
inst
rum
enta
tion.
A w
ell-a
ttend
ed U
sers
’ M
eetin
g w
as o
rgan
ized
for
the
firs
t tim
eou
tsid
e C
anad
a an
d Fr
ance
. The
num
ber o
f sci
entif
ic p
aper
s ba
sed
on C
FHT
data
, as
wel
l as t
heir
impa
ct, k
ept i
ncre
asin
g. A
t the
end
of 2
010,
a n
ew c
omm
unity
dec
ided
tojo
in th
e C
FHT
`oha
na. I
s be
ing
so b
usy
a va
lid e
xcus
e fo
r not
pub
lishi
ng a
n A
nnua
lR
epor
t in
2009
? C
erta
inly
not
! My
apol
ogie
s go
to th
e re
gula
r rea
ders
of t
he A
nnua
lR
epor
t, w
ho m
isse
d on
e ye
ar, h
opin
g th
at th
eir d
isap
poin
tmen
t will
be
com
pens
ated
by
read
ing
this
two-
in-o
ne is
sue
and
the
man
y in
tere
stin
g ne
ws i
t off
ers.
2009
and
201
0 re
pres
ente
d a
perio
d of
tran
sitio
n fo
r CFH
T, fr
om th
e co
mpl
etio
n of
the
Gol
den
Age
Pla
n (G
AP)
to th
e pr
epar
atio
n of
the
CFH
T D
ecad
e Fo
ur (C
D4)
Pla
n. T
heG
AP,
im
plem
ente
d in
200
4 to
cov
er t
he p
erio
d 20
04-2
010,
was
dev
elop
ed a
s a
busi
ness
pla
n an
d a
fram
ewor
k in
whi
ch C
FHT
wou
ld a
ccom
plis
h a
wel
l-def
ined
set
of g
oals
: end
the
GA
P w
ith a
bal
ance
d bu
dget
, con
tain
the
oper
atio
n co
sts a
s muc
h as
poss
ible
, dec
reas
e th
e tim
e lo
st o
n th
e sk
y du
e to
failu
res
whi
le m
aint
aini
ng o
r eve
nim
prov
ing
the
qual
ity o
f ser
vice
s re
nder
ed to
the
user
s of
the
tele
scop
e, a
nd d
evel
opth
e us
ers’
bas
e be
yond
the
CFH
T M
embe
r A
genc
ies
(Can
ada,
Fra
nce,
and
Haw
aii)
thro
ugh
colla
bora
tive
agre
emen
ts w
ith n
ew c
omm
uniti
es. A
t the
ons
et o
f the
GA
P, C
FHT
com
mitt
ed to
reac
hth
ese g
oals
and
the A
genc
ies c
omm
itted
to fo
llow
a fu
ndin
g pl
an w
hich
incl
uded
a re
ason
able
incr
ease
of t
heir
annu
al c
ontri
butio
n to
the
oper
atio
n bu
dget
of t
he o
bser
vato
ry.
The
GA
P is
now
com
plet
ed a
nd a
ll th
e go
als e
stab
lishe
d ba
ck in
200
3/20
04 h
ave
been
reac
hed:
• The
frac
tion
of c
lear
wea
ther
lost
to p
robl
ems h
as b
een
unde
r 2%
for b
oth
2009
and
201
0, e
ven
thou
gh 2
%se
emed
mor
e lik
e a
drea
m th
an a
reac
habl
e ta
rget
six
yea
rs a
go. I
t was
mad
e po
ssib
le th
roug
h th
e am
azin
gw
ork
of a
ll in
volv
ed i
n th
e m
aint
enan
ce o
f th
e ob
serv
ator
y as
a w
hole
(te
lesc
ope,
dom
e, i
nstru
men
ts,
oper
atio
ns, …
) and
by
the
side
eff
ects
of t
he O
bser
vato
ry A
utom
atio
n Pr
ojec
t (O
AP,
see
p. 2
0).
• O
pera
ting
cost
s ha
ve b
een
cont
aine
d as
muc
h as
was
pos
sibl
e w
ithou
t com
prom
isin
g th
e qu
ality
of
the
CFH
T’s
prod
ucts
. Act
ually
, man
y im
prov
emen
ts w
ere
mad
e on
the
way
, fro
m m
ovin
g to
Que
ue S
ervi
ceO
bser
ving
on
the
thre
e m
ain
inst
rum
ents
to c
ontin
uous
ly im
prov
ing
the
qual
ity o
f th
e re
duct
ion
pipe
lines
(suc
h as
I`Iw
i-2 fo
r WIR
Cam
, p.
9) a
nd th
e Ph
ase1
/Pha
se2
proc
ess,
incl
udin
g im
plem
entin
g ne
w m
odes
of
obse
rvat
ions
to e
nhan
ce th
e sc
ient
ific
outc
ome
of th
e ob
serv
ator
y (s
ee fo
r exa
mpl
e th
e St
arin
g M
ode,
p. 1
1).
• Ove
r-su
bscr
iptio
n on
tele
scop
e tim
e, o
ften
calle
d “p
ress
ure”
, is
a m
easu
re o
f how
muc
h th
e te
lesc
ope
is in
dem
and
by it
s use
rs. A
pre
ssur
e of
two
or m
ore
is o
ften
cons
ider
ed h
ealth
y, th
ough
man
y cl
aim
that
it is
mor
eim
porta
nt to
che
ck if
the
obse
rvin
g pr
ogra
ms
sche
dule
d on
the
tele
scop
e ar
e of
goo
d sc
ient
ific
qual
ity. A
tC
FHT,
the
pres
sure
on
norm
al (P
I) p
rogr
ams
mov
ed u
p an
d do
wn
with
the
sche
dulin
g of
Lar
ge P
rogr
ams,
aver
agin
g 2.
6 ov
er th
e du
ratio
n of
the
GA
P an
d 2
over
200
9 an
d 20
10.
• A
ccor
ding
to
the
GA
P go
als,
the
num
ber
of p
ublic
atio
nsba
sed
sign
ifica
ntly
on
CFH
T da
ta w
as to
sta
y ab
ove
50 fo
r its
dura
tion.
As c
an b
e se
en o
nth
e gr
aph
on t
he r
ight
, thi
snu
mbe
r ac
tual
ly i
ncre
ased
dram
atic
ally
, rea
chin
g m
ore
than
120
in 2
010!
In
2009
,on
ly
Kec
k an
d th
e V
LTpu
blis
hed
(per
te
lesc
ope)
mor
e pa
pers
th
an
CFH
T.Q
uant
ity is
def
inite
ly th
ere,
but w
hat a
bout
qua
lity?
The
grap
h on
the
lef
t sh
ows
stat
istic
s (D
. Cra
btre
e, p
riva
te c
omm
unic
atio
n,20
11) o
n a
sim
ple
perf
orm
ance
met
rics:
the
frac
tion
of th
e nu
mbe
r of “
high
impa
ct”
pape
rs o
ver “
low
impa
ct”
ones
for t
he m
ain
obse
rvat
orie
s w
orld
-w
ide.
Her
e, C
FHT
is se
cond
onl
y to
the
Kec
k O
bser
vato
ry.
Chr
istia
n Ve
illet
CFH
TE
xecu
tive
Dire
ctor
CFH
T A
nnua
l Rep
ort
5
• Th
e G
AP
also
incl
uded
goa
ls th
at c
once
rn th
e st
aff
of th
e O
bser
vato
ry, s
uch
as h
igh
staf
f re
tent
ion
as a
mea
sure
men
t of
sta
ff s
atis
fact
ion,
and
a b
ette
r ad
equa
cy o
f th
e st
aff
com
plem
ent
to t
he n
eeds
of
the
Cor
pora
tion.
Sta
ff tu
rnov
er h
as b
een
very
low
in th
e re
cent
yea
rs. E
ach
depa
rture
has
bee
n an
opp
ortu
nity
toas
sess
the
need
for
reh
iring
, eith
er o
n th
e sa
me
job
desc
riptio
n or
ano
ther
one
mor
e cr
itica
l to
the
futu
reop
erat
ion
of th
e ob
serv
ator
y, o
r not
hiri
ng a
t all.
The
staf
f com
plem
ent o
f aro
und
44 p
erso
ns p
roje
cted
for t
heen
d of
201
1, o
nce
OA
P is
fully
ope
ratio
nal (
see
p. 2
3 fo
r det
ails
), in
clud
es n
ine
Res
iden
t Ast
rono
mer
s, am
ong
them
the
Exec
utiv
e D
irect
or a
nd th
e D
irect
or o
f Sci
ence
Ope
ratio
ns. C
FHT
will
then
be
at a
pla
ce a
t whi
chth
e st
aff
will
be
esse
ntia
l fo
r sm
ooth
ope
ratio
ns a
nd a
n ef
ficie
nt p
artic
ipat
ion
in t
he o
ngoi
ng o
r pl
anne
dde
velo
pmen
t of t
he fi
rst h
alf o
f the
new
dec
ade.
The
nint
h C
FHT
Use
rs' M
eetin
g w
as h
eld
in T
aipe
i, Ta
iwan
, in
Nov
embe
r 20
10.
The
Aca
dem
ia S
inic
aIn
stitu
te o
f Ast
rono
my
and
Ast
roph
ysic
s (A
SIA
A) h
oste
d th
e m
eetin
g. It
was
the
first
tim
e th
at C
FHT
held
its tr
ienn
ial U
sers
' Mee
ting
outs
ide
one
of it
s th
ree
mem
ber
natio
ns, a
ckno
wle
dgin
g th
e im
porta
nce
of th
eon
goin
g co
llabo
ratio
n w
ith A
SIA
A, w
hich
sta
rted
in 2
001
and
is n
ow in
its
10th
yea
r. A
s w
ith S
outh
-Kor
eain
the
past
and
with
Bra
zil s
ince
200
9B, s
uch
colla
bora
tions
brin
g to
CFH
T ne
w u
sers
and
man
y op
portu
nitie
sto
gat
her
a w
ider
com
mun
ity a
roun
d sc
ient
ific
proj
ects
as
wel
l as
inst
rum
ent d
esig
n an
d fa
bric
atio
n. T
his
Use
rs' M
eetin
g, n
ickn
amed
"C
FHT
Dec
ade
4", c
ame
afte
r the
cel
ebra
tion
of C
FHT'
s 30
th b
irthd
ay in
200
9,an
d at
a ti
me
whe
n us
ers
and
mem
ber a
genc
ies
wer
e de
finin
g w
ith th
e ob
serv
ator
y its
dev
elop
men
t pla
n fo
r[2
011-
2020
]. N
ew in
stru
men
tatio
n w
as o
ne o
f the
hot
topi
cs o
f the
mee
ting.
The
deve
lopm
ent o
f new
inst
rum
enta
tion
is in
deed
an
impo
rtant
com
pone
nt o
f CD
4. A
t the
end
of 2
010,
two
inst
rum
ents
wer
e se
lect
ed fo
r a P
hase
B: (
1) S
ITEL
LE, a
n im
agin
g FT
S (F
ourie
r Tra
nsfo
rm S
pect
rogr
aph)
base
d on
a p
roto
type
ope
ratio
nal
at M
ont
Még
antic
(Q
uebe
c),
will
be
deve
lope
d an
d fu
nded
mai
nly
onC
anad
ian
fund
s as
a g
uest
ins
trum
ent
(like
ESP
aDO
nS).
(2)
SPIR
ou, a
n ES
PaD
OnS
in
the
near
-IR
, is
asp
ectro
-pol
arim
eter
cov
erin
g th
e ne
ar-I
R (u
p to
K b
and)
, but
aim
ing
also
at p
rovi
ding
hig
h-pr
ecis
ion
(1m
/s)
radi
al v
eloc
ity m
easu
rem
ents
. The
SPI
Rou
team
will
hav
e to
dev
elop
a n
ew M
anag
emen
t Pla
n be
fore
mov
ing
forw
ard
to P
hase
B so
met
ime
in 2
011.
Sad
ly, G
YES
, a w
ide-
field
mul
ti-ob
ject
spec
trogr
aph,
was
not
sele
cted
in sp
ite o
f the
exc
elle
nt w
ork
done
by
an e
nerg
etic
team
whi
ch p
erfo
rmed
a P
hase
A st
artin
g la
te in
the
gam
ean
d w
ithou
t C
FHT’
s su
ppor
t. W
e ar
e ho
pefu
l th
at t
he t
eam
will
fin
d op
portu
nitie
s to
dev
elop
a s
imila
rin
stru
men
t on
anot
her t
eles
cope
. By
the e
nd o
f 201
0, a
deci
sion
abou
t the
futu
re o
f ̀IM
AK
A w
as st
ill p
endi
ng,
as it
s fea
sibi
lity
stud
y w
as n
ot y
et c
ompl
eted
(mor
e on
new
inst
rum
enta
tion
p. 2
4).
Ano
ther
hot
topi
c of
the
Use
rs’
Mee
ting
was
the
futu
re o
f th
e O
bser
vato
ry b
eyon
d 20
20, t
rigge
red
by th
ere
surg
ence
of
the
old
idea
of
repl
acin
g th
e cu
rren
t 3.
6-m
tel
esco
pe b
y a
10-m
ded
icat
ed t
o w
ide-
field
mul
ti-ob
ject
spec
trosc
opy.
Thi
s tim
e, th
e id
ea w
as n
ot ju
st p
rom
oted
by
CFH
T, b
ut a
lso
by o
ne o
f the
CFH
Tco
mm
uniti
es (C
anad
a). N
ickn
amed
NG
CFH
T, th
is p
roje
ct w
ill d
evel
op fu
rther
in 2
011,
hop
eful
ly w
ith m
uch
parti
cipa
tion
from
the
CFH
T pl
ayer
s.
Afte
r inf
orm
al c
onta
cts w
ith C
hine
se c
olle
ague
s fol
low
ed b
y a
tour
of
som
e of t
he m
ain
astro
nom
y in
stitu
tes i
n B
eijin
g, N
anjin
g, an
d Sh
ang-
hai
in t
he s
prin
g of
201
0 an
d m
ore
talk
s w
ith N
AO
C (
Nat
iona
lA
stro
nom
ical
Obs
erva
tory
of
Chi
na)
late
r in
the
year
, Chi
nese
col
-le
ague
s atte
nded
the
Use
rs’ M
eetin
g in
Tai
pei.
An
anno
unce
men
t was
mad
e at
the
end
of
2010
tha
t C
FHT
wou
ld b
e pa
rt of
the
NA
OC
Tele
scop
e A
cces
s Pr
ogra
m (
TAP)
, a
prog
ram
1) t
o al
low
Chi
nese
astr
onom
ers t
o le
ad c
uttin
g-ed
ge o
ptic
al-I
R ob
serv
atio
nal p
rogr
ams,
2) B
uild
the
bas
e of
exp
erie
nced
opt
ical
-IR
obse
rver
s in
Chi
na, 3
)Fa
cilit
ate
colla
bora
tion
betw
een
astr
onom
ers w
ithin
Chi
na, a
nd b
etw
een
astr
onom
ers i
n C
hina
and
thos
e in
the
user
com
mun
ities
of t
eles
cope
s pa
rtic
ipat
ing
in T
AP, 4
) Pro
vide
com
plem
enta
ry o
bser
vatio
nal f
acili
ties
to o
ngoi
ng la
rge
proj
ects
. Bey
ond
CFH
T st
artin
g in
201
1B, T
AP
will
als
o gi
ve a
cces
s to
Pal
omar
Hal
e, th
eM
MT,
and
late
r th
e M
agel
lan
tele
scop
es. T
hrou
gh th
e C
olla
bora
tive
Agr
eem
ent w
ith B
razi
l, B
razi
lian
PIs
used
7 to
8 n
ight
s of
CFH
T tim
e pe
r se
mes
ter
and
a B
razi
lian
Res
iden
t Ast
rono
mer
join
ed th
e as
trono
my
grou
p in
mid
-201
0 (s
ee C
omin
gs a
nd G
oing
, p. 2
9).
Impo
rtant
in-h
ouse
pro
ject
s wer
e co
mpl
eted
in 2
009
and
2010
, suc
h as
the
Mau
na K
ea A
tmos
pher
ic M
onito
r(M
KA
M) o
r the
All-
Sky
Infr
ared
and
Vis
ible
Ana
lyze
r (A
SIV
A),
inst
alle
d an
d m
aint
aine
d by
CFH
T fo
r the
bene
fit o
f all
the
Mau
nake
a O
bser
vato
ries.
`OH
AN
A `I
ki h
ad it
s firs
t frin
ges w
ith th
e `O
HA
NA
inte
rfer
ome-
ter.
The
dom
e ve
ntin
g pr
ojec
t sta
rted
to ta
ke s
hape
, bas
ed o
n an
ext
ensi
ve s
tudy
of
Meg
aPrim
e de
liver
edim
age
qual
ity (m
ore
info
rmat
ion
belo
w).
2009
and
201
0 w
ere
extre
mel
y fr
uitfu
l, th
anks
to a
hig
hly
dedi
cate
d an
d sk
illed
sta
ff a
nd v
ery
supp
ortiv
eco
mm
uniti
es a
nd a
genc
ies.
They
laid
the
grou
nd fo
r yet
ano
ther
dec
ade
of C
FHT’
s exc
elle
nce
at th
e fo
refr
ont
of a
stro
nom
y w
ith e
xciti
ng p
roje
cts f
or it
s mid
-term
futu
re a
nd m
uch
pote
ntia
l for
its f
ifth
deca
de.
CFH
T w
as re
cogn
ized
as o
ne o
f th
e B
est
Pla
ces
to W
ork
in H
a-w
aii
in t
he M
ediu
mC
ompa
nies
cat
egor
y.
The
skyl
ine
of t
heX
ingl
ong
Obs
ervi
ngS
tatio
n of
Nat
iona
lA
stro
nom
ical
Obs
er-
vato
ries,
Chi
nese
Aca
dem
y of
Sci
ence
s.
3620
09 &
201
0
Brid
ge C
.R.,
Car
lber
g, R
. G.;
Sul
livan
, M. T
he C
FHTL
S-D
eep
Cat
alog
of I
nter
actin
g G
alax
ies.
I. M
erge
r Rat
e E
volu
tion
to z
=1.
2. A
pJ 7
09 1
067-
1082
.B
ritav
skiy
N.E
., A
ndrie
vsky
, S. M
., K
orot
in, S
. A.,
Mar
tin, P
. Che
mic
al c
ompo
sitio
n of
sem
i-reg
ular
var
iabl
e gi
ants
. II..
A&
A51
9 id
.A74
.-��I �� �4������������������J���������#����������K����L��+M���.L��5��,��������5�����@������,"�!��1����N55���
in th
e V
505
Sgr
Sys
tem
. AJ
139
2258
-226
8.B
rusa
M.,
Civ
ano,
F.,
Com
astri
, A.,
Miy
aji,
T., S
alva
to, M
., Za
mor
ani,
G.,
Cap
pellu
ti, N
., Fi
ore,
F.,
Has
inge
r, G
., M
aini
eri,
V.
and
57 c
oaut
hors
The
XM
M-N
ewto
n W
ide-
field
Sur
vey
in th
e C
osm
os F
ield
(XM
M-C
OS
MO
S):
Dem
ogra
phy
and
Mul
tiwav
e-le
ngth
Pro
perti
es o
f Obs
cure
d an
d U
nobs
cure
d Lu
min
ous
Act
ive
Gal
actic
Nuc
lei.
ApJ
716
348
-369
.C
abre
ra J
., B
runt
t, H
., O
llivi
er, M
., D
íaz,
R. F
., C
sizm
adia
, Sz.
, Aig
rain
, S.,
Alo
nso,
R.,
Alm
enar
a, J
.-M.,
Auv
ergn
e, M
., B
a-gl
in, A
. and
38
coau
thor
s Tr
ansi
ting
exop
lane
ts fr
om th
e C
oRoT
spa
ce m
issi
on .
XIII
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ilson
G.,
Muz
zin,
A.,
Yee
, H. K
. C.,
Lacy
, M.,
Sur
ace,
J.,;
Gilb
ank,
D.,,
Blin
dert,
K.,
Hoe
kstra
, H.,
Maj
umda
r, S
., D
emar
co,
R. a
nd 3
coa
utho
rs S
pect
rosc
opic
Con
firm
atio
n of
a M
assi
ve R
ed-S
eque
nce-
Sel
ecte
d G
alax
y C
lust
er a
t z =
1.3
4 in
the
SpA
RC
S-S
outh
Clu
ster
Sur
vey.
ApJ
698
194
3-19
50.
CFH
T-ba
sed
refe
reed
pub
licat
ions
- 20
10A
dam
i C.,
Dur
ret,
F., B
enoi
st, C
., C
oupo
n, J
., M
azur
e, A
., M
eneu
x, B
., Ilb
ert,
O.,
Bla
izot
, J.,
Arn
outs
, S.,
Cap
pi, A
., G
arill
i, B
.,G
uenn
ou, L
., Le
brun
, V.,
Lefè
vre,
O.,
Mau
rogo
rdat
o, S
., M
cCra
cken
, H. J
., M
ellie
r, Y
., S
leza
k, E
., Tr
esse
, L.,U
lmer
, M. P
.G
alax
y st
ruct
ure
sear
ches
by
phot
omet
ric re
dshi
fts in
the
CFH
TLS
. A&
A 5
09 A
81.
Aird
J.,
Nan
dra,
K.,
Laird
, E. S
., G
eorg
akak
is, A
., A
shby
, M. L
. N.,
Bar
mby
, P.,
Coi
l, A
. L.,
Hua
ng, J
.-S.,
Koe
kem
oer,
A. M
.,S
teid
el, C
. C.,
Will
mer
, C. N
. A. T
he e
volu
tion
of th
e ha
rd X
-ray
lum
inos
ity fu
nctio
n of
AG
N. M
NR
AS
401
253
1-25
51.
Als
hino
A.,
Kho
sros
hahi
, H.,
Pon
man
, T.,
Will
is, J
., P
ierr
e, M
., P
acau
d, F
., S
mith
, G.P
. Lum
inos
ity fu
nctio
ns o
f XM
M-L
SS
C1
gala
xy c
lust
ers.
MN
RA
S 4
01 9
41-9
62.
.����,�@���������� ����?�N��-�������(��-��4�B�� ��������.������"������'1����&�&��������5���U@&�������
�1le
cula
r clo
ud. A
&A
515
A75
.A
man
ulla
h R
., Li
dman
, C.,
Rub
in, D
., A
lder
ing,
G.,
Ast
ier,
P.,
Bar
bary
, K.,
Bur
ns, M
. S.;
Con
ley,
A.;
Daw
son,
K. S
.; D
eust
ua,
S. E
. and
36
coau
thor
s S
pect
ra a
nd H
ubbl
e S
pace
Tel
esco
pe L
ight
Cur
ves
of S
ix T
ype
Ia S
uper
nova
e at
0.5
11 <
z <
1.1
2an
d th
e U
nion
2 C
ompi
latio
n. A
pJ 7
16 7
12-7
38.
Ang
lada
-Esc
udé
G.,
Shk
olni
k, E
.L.,
Wei
nber
ger,
A.J
., Th
omps
on, I
.B.,
Osi
p, D
.J.,
Deb
es, J
.H. S
trong
Con
stra
ints
to th
e P
u-ta
tive
Pla
net C
andi
date
aro
und
VB
10
Usi
ng D
oppl
er S
pect
rosc
opy.
ApJ
711
L24
-L29
..������ ��-�����,��*������������������������N�� ���������B�(����������
��������������������S����V���3�#����1
pak,
P. a
nd 2
coa
utho
rs E
nviro
nmen
t of M
AM
BO
Gal
axie
s in
the
CO
SM
OS
Fie
ld. A
pJ 7
08 L
36-L
41.
Ara
vena
M.,
You
nger
, J. D
., Fa
zio,
G. G
., G
urw
ell,
M.,
Esp
ada,
D.,
Ber
told
i, F.
, Cap
ak, P
., W
ilner
, D. I
dent
ifica
tion
of T
wo
Brig
ht z
> 3
Sub
mill
imet
er G
alax
y C
andi
date
s in
the
CO
SM
OS
Fie
ld. A
pJ 7
19 L
15-L
19.
Bel
lini A
., B
edin
, L. R
., P
iotto
, G.,
Sal
aris
, M.,
And
erso
n, J
., B
roca
to, E
., R
agaz
zoni
, R.,
Orto
lani
, S.,
Bon
anos
, A. Z
., P
lata
is,
I. an
d 14
coa
utho
rs T
he e
nd o
f the
whi
te d
war
f coo
ling
sequ
ence
in M
67.
A&
A 5
23 id
.A50
.B
ellin
i A.,
Bed
in, L
. R.,
Pic
hard
o, B
., M
oren
o, E
., A
llen,
C.,
Pio
tto, G
., A
nder
son,
J. A
bsol
ute
prop
er m
otio
n of
the
Gal
actic
open
clu
ster
M 6
7. A
&A
513
id.A
51.
Ben
jam
in J
., va
n W
aerb
eke,
L.,
Mén
ard,
Br.,
Kilb
inge
r, M
. Pho
tom
etric
reds
hifts
: est
imat
ing
thei
r con
tam
inat
ion
and
dist
ribu-
tion
usin
g cl
uste
ring
info
rmat
ion.
MN
RA
S 4
08 1
168-
1180
.B
ielb
y R
.M.,
Fino
guen
ov, A
., Ta
naka
, M.,
McC
rack
en, H
. J.,
Dad
di, E
., H
udel
ot, P
., Ilb
ert,
O.,
Kne
ib, J
. P.,
Le F
èvre
, O.,
Mel
-����� ���,:������������)A��. ���&A�5����,������������4�A����&���,�����������;�;�.9.:HC.DD�
Boh
lend
er D
.A.,
Ric
e, J
. B.,
Hec
hler
, P. D
oppl
er im
agin
g of
the
heliu
m-v
aria
ble
star
a C
enta
uri.
A&
A 5
20 A
44.
Bra
sseu
r C.M
., S
tets
on, P
.B.,
Van
denB
erg,
D.A
., C
asag
rand
e, L
., B
ono,
G.,
Dal
l'Ora
, M. F
iduc
ial S
tella
r Pop
ulat
ion
Se-
quen
ces
for t
he V
JKS
Pho
tom
etric
Sys
tem
. AJ
140
1672
-168
6.
620
09 &
201
0
Goo
d ne
ws
for E
SPaD
OnS
!
E. M
arto
liES
PaD
OnS
is
CFH
T’s
cros
s-di
sper
sed
eche
lle s
pect
ropo
larim
eter
, an
d is
one
of
its 3
mai
n in
stru
men
ts.
Pola
rizat
ion
cros
stal
k ha
d be
en a
n is
sue
sinc
e th
e co
mm
issi
onin
g of
the
inst
rum
ent,
and
star
ted
at a
leve
l of 7
%.
Rep
laci
ng o
ne tr
iple
t len
s dec
reas
ed th
e le
vel o
f cro
ssta
lk to
2-4
%, b
ut it
was
not
unt
il th
e fa
bric
atio
n of
a n
ewtri
plet
(w
ith a
new
des
ign,
new
mat
eria
ls,
and
a ne
w m
echa
nica
l m
ount
not
usi
ng a
ny g
lue
at a
ll),
and
inst
alla
tion
of a
new
AD
C (A
tmos
pher
ic D
ispe
rsio
n C
orre
ctor
) tha
t the
leve
l of c
ross
talk
was
bro
ught
bel
ow1%
, in
Nov
200
9. T
o fu
rther
im
prov
e th
e ov
eral
l pe
rfor
man
ce o
f th
e in
stru
men
t, C
FHT
has
initi
ated
the
DA
NC
E pr
ojec
t, to
repl
ace t
he cu
rren
t EEV
det
ecto
r by
a dee
p-de
plet
ion
devi
ce th
at h
as m
uch
bette
r cos
met
ics,
bette
r QE
and
less
frin
ging
in th
e re
d, a
nd sh
orte
r rea
d tim
e by
usi
ng it
s 2 a
mpl
ifier
s. R
ecen
t on-
sky
test
s with
this
new
dev
ice,
cal
led
Ola
pa,
are
enco
urag
ing.
In
para
llel
with
har
dwar
e im
prov
emen
t, C
FHT
has
also
emba
rked
in th
e O
PER
A p
roje
ct, w
hich
will
off
er E
SPaD
OnS
use
rs a
n op
en-s
ourc
e pi
pelin
e fo
r the
redu
ctio
nof
its d
ata.
Cro
ssta
lkC
ross
talk
is th
e co
ntam
inat
ion
of o
neSt
okes
par
amet
er b
y an
othe
r. In
ES-
PaD
OnS
, cr
osst
alk
is
caus
ed
byst
ress
bire
frin
genc
e in
a tr
iple
t len
s and
in th
e A
DC
. The
evo
lutio
n of
CFH
Tde
velo
pmen
ts to
min
imiz
e th
is p
rob-
lem
is sh
own
on th
e ch
art b
elow
. The
mos
t re
cent
res
ults
of
on-s
ky t
ests
perf
orm
ed w
ith th
e ne
w o
ptic
al e
le-
men
ts in
dica
te a
tota
l cro
ssta
lk b
elow
1% a
s sh
own
in t
he t
able
bel
ow.
Som
e of
the
cros
stal
k le
ft, a
long
with
its v
aria
tion,
is
due
to t
he A
DC
,w
hich
stil
l ex
hibi
ts s
tress
bire
frin
-ge
nce
that
cha
nges
as
func
tion
ofte
lesc
ope’
s po
si-
tion
.
Dan
ce P
roje
ctD
AN
CE
(Dua
l Am
plifi
er N
ew C
CD
for E
SPaD
OnS
) is
one
of C
FHT’
s in
-hou
se in
stru
men
t pro
ject
s th
at a
imto
pro
vide
an im
prov
ed an
d fa
st-
er C
CD
for
ESP
aDO
nS.
The
new
chi
p is
cal
led
Ola
pa a
nd it
has t
he sa
me
phys
ical
cha
ract
er-
istic
s as
the
prev
ious
CC
D, b
utw
ith a
n im
prov
ed p
erfo
rman
cean
d le
ss
over
head
tim
e.
We
have
rece
ntly
per
form
ed la
b an
don
-sky
test
s w
ith O
lapa
, whi
chsh
owed
si
gnifi
cant
im
prov
e-m
ents
like
read
-out
noi
se re
duc-
tion,
bet
ter s
ensi
tivity
in th
e re
d,le
ss f
ringi
ng,
and
fast
er r
ead-
out.
The
com
para
tive
resu
lts b
e-tw
een
Ola
pa a
nd th
e ol
d EE
V1
chip
are
pre
sent
ed o
n th
e le
ftan
d be
low
. Ola
pa is
exp
ecte
d to
be
offe
red,
in
on
e am
plifi
erm
ode,
for s
emes
ter 2
011A
.
CFH
T A
nnua
l Rep
ort
7A th
eore
tical
mod
elfo
r the
glo
win
g pl
as-
ma
in th
e m
agne
to-
sphe
re o
f a m
agne
ticm
assi
ve s
tar.
Cre
dit:
R. T
owns
end.
OPE
RA
Pip
elin
eO
PER
A (
Ope
n-so
urce
Pip
elin
e fo
r ES
PaD
OnS
Red
uctio
n an
d A
naly
sis)
w
ill b
e an
ope
n-so
urce
sof
twar
ere
duct
ion
pipe
line
for E
SPaD
OnS
. The
idea
of O
PER
A is
that
CFH
T w
ill h
ost a
n op
en-s
ourc
e pr
ojec
t to
build
a re
duct
ion
and
anal
ysis
tool
for
ech
elle
spe
ctro
grap
h da
ta, s
uch
as E
SPaD
OnS
. Thi
s w
ill b
e an
alte
rnat
ive
optio
n to
the c
urre
nt sy
stem
, whi
ch is
not
avai
labl
e for
dis
tribu
tion
and
thus
can
not b
e acc
esse
d by
CFH
T us
ers.
With
OPE
RA
, the
scie
ntis
ts w
ill b
e abl
e to
mod
ify an
d bu
ild to
ols t
o co
mpl
emen
t the
stan
dard
redu
ctio
n sy
stem
as w
ell
as t
o tu
ne d
own
the
syst
em f
or t
heir
own
scie
ntifi
c ne
eds.
For
mor
e in
form
atio
n pl
ease
vis
it ou
rso
ucef
orge
pro
ject
site
: http
://so
urce
forg
e.ne
t/pro
ject
s/op
era-
pipe
line/
Mag
netis
m in
Mas
sive
Sta
rs (M
iMeS
)
N. M
anse
tTh
e m
agne
tic fi
elds
of h
ot, h
igh
mas
s st
ars
whi
ch h
ave
initi
alm
asse
s ab
ove
abou
t 8
times
tha
t of
the
sun
are
qua
litat
ivel
ydi
ffer
ent f
rom
thos
e of
coo
l, lo
w-m
ass s
tars
sim
ilar t
o ou
r Sun
.Th
ose
field
s ar
e de
tect
ed in
onl
y a
smal
l fra
ctio
n of
sta
rs, a
ndth
ey a
re st
ruct
ural
ly m
uch
sim
pler
, and
freq
uent
ly m
uch
stro
n-ge
r, th
an th
e fie
lds o
f coo
l sta
rs.
The
Mag
netis
m i
n M
assi
ve S
tars
(M
iMeS
) La
rge
Prog
ram
cond
ucte
d w
ith E
SPaD
OnS
em
ploy
s tw
o st
rate
gies
to
help
impr
ove
our
know
ledg
e of
mag
netic
fie
lds
in m
assi
ve s
tars
.Fi
rst o
f all,
abo
ut h
alf o
f the
obs
ervi
ng ti
me
is s
pent
obs
ervi
ngkn
own
mag
netic
star
s in
deta
il, g
ettin
g sn
apsh
ots o
f the
ir m
ag-
netic
fiel
d st
reng
th a
nd c
onfig
urat
ion.
This
Tar
gete
d C
ompo
nent
of
the
larg
e pr
ogra
m i
s fo
llow
ing
over
2 d
ozen
s sta
rs o
ver t
ime
in o
rder
to g
et h
igh-
prec
isio
n an
dhi
gh-r
esol
utio
n sa
mpl
ing
of th
e ro
tatio
nally
-mod
ulat
ed c
ircul
ar, a
nd s
omet
imes
line
ar, p
olar
izat
ion
line
pro-
3420
09 &
201
0
Lèbr
e A
., P
alac
ios,
A.,
Do
Nas
cim
ento
, J. D
., Jr
., K
onst
antin
ova-
Ant
ova,
R.,
Kol
ev, D
., A
uriè
re, M
., de
Lav
erny
, P.,
de M
e-de
iros,
J. R
. Lith
ium
and
mag
netic
fiel
ds in
gia
nt s
tars
. HD
232
862
: a m
agne
tic a
nd li
thiu
m-r
ich
gian
t Li
thiu
m a
nd m
agne
ticfie
lds
in g
iant
sta
rs. H
D 2
32 8
62: a
mag
netic
and
lith
ium
-ric
h gi
ant.
A&
A 5
04 1
011-
1019
.Lé
ger A
., R
ouan
, D.,
Sch
neid
er, J
., B
arge
, P.,
Frid
lund
, M.,
Sam
uel,
B.,
Olli
vier
, M.,
Gue
nthe
r, E
., D
eleu
il, M
., D
eeg,
H. J
.an
d 15
1 co
auth
ors
Tran
sitin
g ex
opla
nets
from
the
CoR
oT s
pace
mis
sion
. VIII
. CoR
oT-7
b: th
e fir
st s
uper
-Ear
th w
ith m
ea-
sure
d ra
dius
. A&
A 5
06 2
87-3
02.
Li I.
H.,
Yee
, H. K
. C.,
Elli
ngso
n, E
. Ind
ivid
ual a
nd g
roup
gal
axie
s in
CN
OC
1 cl
uste
rs. A
pJ 6
98 8
3-98
.Li
lly S
.J.,
Le B
run,
V.,
Mai
er, C
., M
aini
eri,
V.,M
igno
li, M
., S
code
ggio
, M.,
Zam
oran
i, G
., C
arol
lo, M
., C
ontin
i, T.
, Kne
ib, J
. -P
.an
d 56
coa
utho
rs T
he z
CO
SM
OS
10k
-Brig
ht S
pect
rosc
opic
Sam
ple.
ApJ
S 1
84 2
18-2
29.
Lim
ousi
n M
., C
aban
ac, R
., G
avaz
zi, R
., K
neib
, J.-P
., M
otta
, V.,
Ric
hard
, J.,
Than
javu
r, K
., Fo
ex, G
., P
ello
, R.,
Cra
mpt
on, D
.an
d 14
coa
utho
rs A
new
win
dow
of e
xplo
ratio
n in
the
mas
s sp
ectru
m: s
trong
lens
ing
by g
alax
y gr
oups
in th
e S
L2S
. A&
A 5
0244
5-45
6.Lu
T.,
Gilb
ank,
D.G
., B
alog
h, M
.L.;
Bog
nat,
A. R
ecen
t arr
ival
of f
aint
clu
ster
gal
axie
s on
the
red
sequ
ence
: lum
inos
ity fu
nc-
tions
from
119
deg2
of C
FHTL
S. M
NR
AS
399
185
8-18
76.
Lubi
n L.
M.,
Gal
, R. R
., Le
mau
x, B
. C.,
Koc
evsk
i, D
. D.,
Squ
ires,
G. K
. The
obs
erva
tions
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livan
, M.,
Bro
wn,
E. F
., C
onle
y, A
., Le
Bor
gne,
D.,
Hsi
ao, E
. Y.,
Ast
ier,
P.,
Bal
am, D
., B
alla
nd, C
., B
asa,
S.
and
16 c
oaut
hors
The
effe
ct o
f pro
geni
tor a
ge a
nd m
etal
licity
on
lum
inos
ity a
nd 5
6Ni y
ield
in ty
pe Ia
sup
erno
vae.
ApJ
691
661-
671.
Hue
rtas-
Com
pany
M.,
Foex
, G.,
Sou
cail,
G.,
Pel
ló, R
. The
role
of e
nviro
nmen
t in
the
mor
phol
ogic
al tr
ansf
orm
atio
n of
gal
ax-
ies
in 9
rich
inte
rmed
iate
reds
hift
clus
ters
. A&
A 5
05 8
3-96
.H
uerta
s-C
ompa
ny M
., Ta
sca,
L.,
Rou
an, D
., P
elat
, D.,
Kne
ib, J
. P.,
Le F
èvre
, O.,
Cap
ak, P
., K
arta
ltepe
, J.,
Koe
kem
oer,
A.,
McC
rack
en, H
. J. a
nd 3
coa
utho
rs ro
bust
mor
phol
ogic
al c
lass
ifica
tion
of h
igh-
reds
hift
gala
xies
usi
ng s
uppo
rt ve
ctor
ma-
chin
es o
n se
eing
lim
ited
imag
es.II
. Qua
ntify
ing
mor
phol
ogic
al…
.. A
&A
497
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.H
utch
ings
J.B
., S
chol
z, P
., B
ianc
hi, L
. Env
ironm
ents
of Q
SO
s at
Red
shift
0.9
-1.3
. AJ
137
3533
-354
0.H
wan
g C
.-Y.,
Cha
ng, M
ing-
Yan
A c
atal
og o
f mor
phol
ogic
ally
iden
tifie
d m
ergi
ng g
alax
ies.
ApJ
S 1
81 2
33-2
37.
Ideu
e Y
., N
agao
, T.,
Tani
guch
i, Y
., S
hioy
a, Y
., S
aito
, T.,
Mur
ayam
a, T
., S
asak
i, S
., Tr
ump,
J. R
., K
oeke
moe
r, A
. M.,
Aus
sel,
H. a
nd 7
coa
utho
rs E
nviro
nmen
tal e
ffect
s on
the
star
form
atio
n ac
tivity
in g
alax
ies
at z
sim
e 1.
2 in
the
CO
SM
OS
fiel
d. A
pJ70
0 97
1-97
6.Ilb
ert O
., C
apak
, P.,
Sal
vato
, M.,
Aus
sel,
H.,
McC
rack
en, H
. J.,
San
ders
, D. B
., S
covi
lle, N
., K
arta
ltepe
, J.,
Arn
outs
, S.,
LeFl
oc'h
, E. a
nd 5
3 co
auth
ors
Cos
mos
pho
tom
etric
reds
hifts
with
30-
BA
ND
S fo
r 2-d
eg2.
ApJ
690
123
6-12
49.
Kav
elaa
rs J
.J.,
Jone
s, R
. L.,
Gla
dman
, B. J
., P
etit,
J.-M
., P
arke
r, Jo
el W
m.,
Van
Lae
rhov
en, C
., N
icho
lson
, P.,
Rou
ssel
ot, P
.,S
chol
l, H
., M
ousi
s, O
. and
8 c
oaut
hors
The
Can
ada-
Fran
ce E
clip
tic p
lane
sur
vey—
L3 d
ata
rele
ase:
The
orb
ital s
truct
ure
ofth
e K
uipe
r Bel
t. A
J 13
7 49
17-4
935.
Kilb
inge
r M.,
Ben
abed
, K.,
Guy
, J.,
Ast
ier,
P.,
Tere
no, I
., Fu
, L.,
Wra
ith, D
., C
oupo
n, J
., M
ellie
r, Y
., B
alla
nd, C
. and
8 c
oau-
thor
s D
ark-
ener
gy c
onst
rain
ts a
nd c
orre
latio
ns w
ith s
yste
mat
ics
from
CFH
TLS
wea
k le
nsin
g, S
NLS
sup
erno
vae
Ia a
ndW
MA
P5.
A&
A 4
97 6
77-6
88.
Kor
men
dy J
., Fi
sher
, D.B
., C
orne
ll, M
.E.,
Ben
der,
R. S
truct
ure
and
form
atio
n of
elli
ptic
al a
nd s
pher
oida
l gal
axie
s. A
pJS
182
216-
309.
Laird
E.S
., N
andr
a, K
., G
eorg
akak
is, A
., A
ird, J
. A.,
Bar
mby
, P.,
Con
selic
e, C
. J.,
Coi
l, A
. L.,
Dav
is, M
., Fa
ber,
S. M
., Fa
zio,
G. G
. and
4 c
oaut
hors
AE
GIS
-X: t
he C
hand
ra d
eep
surv
ey o
f the
ext
ende
d gr
oth
strip
. ApJ
S 1
80 1
02-1
16.
Lam
arei
lle F
., B
rinch
man
n, J
., C
ontin
i, T.
, Wal
cher
, C. J
., C
harlo
t, S
., P
érez
-Mon
tero
, E.,
Zam
oran
i, G
., P
ozze
tti, L
., B
olzo
-ne
lla, M
., G
arill
i, B
. and
36
coau
thor
s P
hysi
cal p
rope
rties
of g
alax
ies
and
thei
r evo
lutio
n in
the
VIM
OS
VLT
Dee
p S
urve
y. I.
The
evol
utio
n of
the
mas
s-m
etal
licity
rela
tion
up to
z ~
0.9
. A&
A 4
95 5
3-72
.La
ndst
reet
J.D
., K
upka
, F.,
Ford
, H. A
., O
ffice
r, T.
, Sig
ut, T
. A. A
., S
ilaj,
J., S
trass
er, S
., To
wns
hend
, A. A
tmos
pher
ic v
eloc
ityfie
lds
in te
pid
mai
n se
quen
ce s
tars
. A&
A 5
03 9
73-9
84.
820
09 &
201
0
files
. Th
e in
form
atio
n is
use
d to
rec
onst
ruct
map
s of
the
mag
netic
fiel
d.
The s
econ
d pa
rt of
the L
P is
a Su
rvey
Com
pone
nt w
hich
look
sfo
r pre
viou
sly
unkn
own
mag
netic
mas
sive
star
s fro
m an
initi
allis
t of a
bout
200
star
s.
A l
ittle
ove
r ha
lfway
thr
ough
the
9 s
emes
ter
prog
ram
, th
ein
tern
atio
nal c
olla
bora
tion
has
acqu
ired
over
125
0 hi
gh-r
eso-
lutio
n po
lariz
ed s
pect
ra o
f ab
out
150
indi
vidu
al s
tars
, an
ddi
scov
ered
new
mag
netic
fie
lds
in o
ver
a do
zen
hot
and
mas
sive
sta
rs,
out
of t
he h
undr
ed o
r so
whi
ch h
ave
been
obse
rved
so fa
r. O
ther
not
able
resu
lts in
clud
e th
e de
tect
ion
ofm
agne
tic fi
elds
in th
e 2 m
ost r
apid
ly-r
otat
ing
know
n m
agne
ticst
ars,
whi
ch r
otat
e in
abo
ut o
nly
half
a da
y, a
nd in
the
mos
tm
assi
ve k
now
n m
agne
tic st
ar.
MA
gnet
ic P
roto
star
s an
d Pl
anet
s (M
aPP)
N. M
anse
t
MaP
P (M
Agn
etic
Pro
tost
ars a
nd P
lane
ts) i
s a C
FHT
Larg
e Pro
gram
that
inve
stig
ates
the r
ole o
f mag
netic
fiel
dsin
the
form
atio
n of
sta
rs a
nd p
lane
tary
sys
tem
s, es
peci
ally
sta
rs w
ith a
mas
s si
mila
r to
that
of o
ur S
un. M
aPP
focu
sses
esp
ecia
lly o
n th
e co
re re
gion
s of p
roto
stel
lar a
ccre
tion
disc
s - in
clud
ing
the
new
ly b
orn
star
.
Star
ted
durin
g se
mes
ter
2008
B, t
his
larg
e pr
ogra
m h
asal
read
y fo
llow
ed 1
5 of
the
20 o
r so
you
ng s
tars
on
itslis
t. B
y th
e tim
e it
ends
dur
ing
sem
este
r 20
12B
, al
lta
rget
s w
ill h
ave
been
fol
low
ed c
lose
ly, s
omet
imes
at
two
diff
eren
t epo
chs s
epar
ated
by
a fe
w y
ears
. Typ
ical
-ly
, eac
h st
ar is
obs
erve
d on
e or m
ore t
imes
each
nig
ht fo
r10
-16
cons
ecut
ive
nigh
ts,
with
the
spe
ctro
pola
rimet
erES
PaD
OnS
, allo
win
g as
trono
mer
s to
map
the
mag
netic
field
s as t
he st
ar ro
tate
s on
itsel
f fro
m n
ight
to n
ight
.
By
com
parin
g th
e ob
serv
atio
ns a
nd m
aps
of m
agne
ticfie
lds w
ith th
e pre
dict
ions
of n
ew th
eore
tical
mod
els a
ndm
agne
tohy
drod
ynam
ic s
imul
atio
ns,M
aPP
will
ans
wer
seve
ral
maj
or o
pen
ques
tions
on
star
for
mat
ion
and
prod
uce
upda
ted
mod
els
inco
rpor
atin
g th
e ef
fect
of
mag
netic
fie
lds.
Alre
ady,
MaP
P ha
s fo
und
a no
n-st
a-tio
nary
mag
netic
fie
ld c
onfig
urat
ion
on V
2129
Oph
,w
ith c
hang
es n
otic
eabl
e w
ithin
onl
y 4
year
s. Th
e m
ag-
netic
fiel
d is
pol
oida
l and
axi
sym
etric
, and
the
obse
rva-
tions
show
a d
ark
phot
osph
eric
spot
and
a lo
caliz
ed a
rea
of a
ccre
tion-
pow
ered
em
issi
on, i
n ag
reem
ent w
ith r
ecen
t 3D
mag
neto
hydr
odyn
amic
sim
ulat
ions
spe
cific
toth
is st
ar.
Var
iabi
lity
on a
tim
esca
le o
f one
onl
y ye
ar w
as a
lso
obse
rved
on
AA
Tau
, whi
ch a
lso
has
a m
ostly
pol
oida
lm
agne
tic fi
eld.
The
circ
ular
pol
ariz
atio
n da
ta s
ugge
st th
at th
e ac
cret
ing
mat
eria
l in
the
inne
r dis
k re
gion
s is
mos
tly b
eing
exp
elle
d ou
twar
d in
stea
d of
get
ting
to th
e su
rfac
e of
the
star
. Thi
s phe
nom
enon
in th
e en
d sl
ows
dow
n th
e sp
in o
n th
e st
ar.
The
MaP
P La
rge
Prog
ram
is c
onfir
min
g th
at m
agne
tic fi
elds
inde
ed p
lay
a ke
y ro
le in
the
form
atio
n an
d ea
rlyev
olut
ion
of st
ars,
thro
ugh
accr
etio
n an
d ej
ectio
n pr
oces
ses.
Mag
neto
sphe
re o
fth
e cT
TS V
2129
Oph
, ext
rapo
late
dfro
m th
e su
rface
mag
netic
map
de-
rived
from
spe
c-tro
pola
rimet
ry o
fbo
th p
hoto
sphe
riclin
es a
nd a
ccre
tion
prox
ies.
Ope
n an
dcl
osed
fiel
d lin
esar
e in
blu
e an
dw
hite
, res
pect
ivel
y;co
lors
at t
he s
urfa
cede
pict
the
rad
ial
field
com
pone
nt,
with
red
and
blue
corr
espo
ndin
g to
posi
tive
and
nega
-tiv
e po
larit
ies
(from
Don
ati e
t al.
2007
;Ja
rdin
e et
al.i
2008
)
Sig
ma
Ori
E is
ayo
ung
star
with
ave
ry s
trong
mag
net-
ic fi
eld
in a
tilte
ddi
pole
con
figur
a-tio
n. M
ater
ial b
low
naw
ay fr
om th
e st
arin
a w
ind
is c
on-
fined
by
the
mag
-ne
tic fi
eld,
bui
lds
up, a
nd p
erio
dica
llybr
eaks
out
of t
hem
agne
tosp
here
.Th
e m
ass
loss
slow
s do
wn
the
ro-
tatio
n of
the
star
, by
7 m
s pe
r yea
r.
Cre
dit:
R. C
ohen
.
CFH
T A
nnua
l Rep
ort
9
I’iw
i 2,
the
CFH
T da
ta p
roce
ssin
g an
dca
libra
tion
pipe
line
for W
IRC
amK
. Tha
njav
ur, D
. Tee
ple,
C-H
. Yan
, D. D
evos
t, K
. With
ingt
on,
S. A
rnou
ts, a
nd E
. Mar
tioli
1. I
ntro
duct
ion
Dur
ing
sem
este
r 20
10A
, we
upgr
aded
th
e W
IRC
am d
ata
proc
essi
ng a
nd c
alib
ratio
n pi
pelin
e,I’
iwi,
curr
ent
vers
ion
2, w
ith s
igni
fican
t en
hanc
emen
ts t
o th
e da
ta q
ualit
y an
d pr
oces
sing
spe
ed.
Due
to
the
enor
mou
sW
IRC
am d
ata
volu
me,
we
have
repl
aced
the
sequ
entia
l pro
cess
ing
of th
e ea
rlier
pip
elin
e w
ith m
ulti-
mac
hine
para
llel c
ompu
tatio
n to
ach
ieve
a r
educ
tion
~30%
in c
alib
ratio
n an
d da
ta p
roce
ssin
g tim
es, c
ompa
red
to th
eea
rlier
I’iw
i ve
rsio
n. I
’iwi
2 is
driv
en b
y di
stin
ct g
oals
(cr
eatio
n of
eac
h da
ta p
rodu
ct a
nd a
ll as
soci
ated
depe
nden
cies
), an
d th
us in
corp
orat
es in
its d
esig
n th
e im
porta
nt p
rope
rty o
f bei
ng a
ble
to a
bort
and
rest
art t
hepr
oces
s at
any
poi
nt. F
or o
ptim
al n
ear i
nfra
red
(NIR
) sky
est
imat
ion,
in a
dditi
on to
the
stan
dard
dith
er p
atte
rn(D
P),
we
have
inc
orpo
rate
d se
vera
l ne
w s
trate
gies
(N
oddi
ng D
P, W
ide
DP,
Use
r D
P) i
n re
spon
se t
o PI
dem
ands
. Zer
o po
int c
alib
ratio
n is
don
e w
ith b
oth
stan
dard
star
s and
2M
ASS
star
s in
ever
y ca
mer
a ru
n. W
eigh
tm
aps a
nd m
asks
are
gen
erat
ed a
nd u
sed
in th
e re
duct
ions
for e
ach
expo
sure
. Six
dat
a pr
oduc
ts a
nd th
e co
mpl
ete
set o
f cal
ibra
tions
are
dis
tribu
ted
to th
e PI
s in
an e
asy-
to-u
se w
eb in
terf
ace.
Her
e w
e pr
esen
t the
salie
nt fe
atur
esan
d ad
vant
ages
of I
’iwi 2
.
2. D
ata
proc
essi
ng w
ith I
’iwi 2
Each
exp
osur
e of
a P
I pr
ogra
m u
nder
goes
aco
nsis
tent
serie
s of p
roce
ssin
g st
eps,
illus
trate
dw
ith t
he f
low
char
t in
Fig
1.
The
inpu
t ra
wim
age
(*o.
fits)
is fi
rst d
etre
nded
to re
mov
e al
lin
stru
men
tal
sign
atur
es u
sing
the
app
ropr
iate
calib
ratio
ns,
nam
ely
the
mas
ter
twili
ght
flat
field
for t
hat f
ilter
, a d
ark
curr
ent f
ram
e fo
r the
corr
espo
ndin
g ex
posu
re ti
me,
and
a b
ad p
ixel
mas
k to
acc
ount
for c
hip
cosm
etic
s. Th
ree
data
prod
ucts
are
gen
erat
ed a
t thi
s st
ep: (
1) a
mas
kim
age
(*m
.fits
) w
ith a
ll ba
d pi
xels
inc
ludi
ngsa
tura
ted
pixe
ls, a
nd g
uide
sta
r win
dow
s se
t to
zero
, (2)
a w
eigh
t map
(*w
.fits
) to
acco
unt f
orpi
xel
to p
ixel
sen
sitiv
ity v
aria
tions
ref
lect
ing
the
flat
field
, an
d 3.
the
det
rend
ed i
mag
e,(*
s.fits
), w
hich
has
bee
n co
rrec
ted
for
dark
curr
ent,
flat f
ield
ed a
nd m
aske
d fo
r bad
pix
els
(for
illu
stra
tion,
the
se t
hree
dat
a pr
oduc
ts a
resh
own
fram
ed in
yel
low
, mag
enta
and
gre
en in
Fig.
1).
For
the
next
ste
p of
sky
sub
tract
ion,
ana
tura
l seq
uenc
e of
imag
es w
hich
are
with
in a
pred
efin
ed t
ime
win
dow
(no
min
ally
20m
in)
and
spat
ial e
xten
t (la
rge
enou
gh to
avo
id o
ver-
lap
of ex
tend
ed o
bjec
ts) a
re fi
rst i
dent
ified
. The
detre
nded
imag
es o
f th
is n
atur
al s
eque
nce
are
then
med
ian
com
bine
d (w
ith b
ad p
ixel
regi
ons
and
all
obje
cts
mas
ked)
to
cons
truct
the
sky
imag
e, (
*y.fi
ts,
show
n in
a b
lue
fram
e).
The
sky
back
grou
nd i
n ea
ch e
xpos
ure
is t
hen
re-
mov
ed b
y th
e co
rres
pond
ing
sky
imag
e in
the
sky
subt
ract
ion
step
. A fi
rst p
ass a
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n is
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g th
e 2M
ass P
oint
Sou
rce
cata
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It is
impo
rtant
to n
ote
that
onl
y lin
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are
app
lied
and
no p
ixel
resa
mpl
ing
is d
one
durin
g th
e as
trom
etric
calib
ratio
n, in
ord
er to
leav
e th
e flu
x in
eac
h pi
xel u
nalte
red
(in k
eepi
ng w
ith th
e po
licy
adop
ted
at C
FHT)
.
Figu
re 1
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wi 2
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wel
las
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sixd
ata
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long
with
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i-br
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nnua
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31
2009
& 2
010
Fina
ncia
l Res
ourc
esTh
e th
ree
Mem
ber A
genc
ies
supp
orte
d th
e C
FHT
annu
al b
udge
tin
200
9 an
d 20
10 a
s sh
own
in th
e ta
ble
at th
e rig
ht, i
n U
S fu
nds.
Thes
e co
ntrib
utio
ns r
efle
ct a
3%
incr
ease
in 2
009
over
the
prio
rye
ar, a
nd a
4%
incr
ease
in 2
010
over
the
prio
r yea
r, in
acc
orda
nce
with
the
Gol
den
Age
Pla
n.
In 2
009,
und
er a
col
labo
rativ
e ag
reem
ent
with
CFH
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he A
cade
mia
Sin
ica
Inst
itute
of
Ast
rono
my
and
Ast
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s of
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wan
and
the
Bra
zilia
n M
inis
try o
f Sc
ienc
e an
d Te
chno
logy
re
mitt
ed $
557,
452
and
$180
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pect
ivel
y, a
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mbu
rsem
ent f
or c
osts
ass
ocia
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with
its u
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f the
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s. O
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sour
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sus
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acili
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Atm
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Mon
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and
$40,
221
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tere
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allo
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the
area
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ted
inth
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ble
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ft
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rall
in 2
009
and
2010
, res
ourc
es f
rom
all
CFH
T fu
nds
wer
e al
loca
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tego
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of e
xpen
ditu
res
show
n in
the
pie
char
t bel
ow.
Age
ncy
Con
trib
utio
ns20
0920
10N
RC
3,13
6,12
63,
261,
571
CN
RS
3,13
6,12
63,
261,
571
UH
727,
218
756,
308
Tota
l6,
999,
470
7,27
9,45
0
Ope
ratin
g Fu
nd E
xpen
ditu
res
2009
2010
Obs
erva
tory
faci
litie
s an
dop
erat
ions
732,
435
803,
303
Bas
e fa
cilit
ies
and
oper
atio
ns64
8,63
968
7,46
6
Inst
rum
enta
tion
203,
284
86,6
28S
cien
ce66
,670
53,6
01O
utre
ach
84,9
5638
,660
Gen
eral
adm
inis
trativ
eex
pens
es35
6,78
843
3,13
3
Sta
ffing
5,04
1,69
85,
101,
159
Tran
sfer
from
Res
erve
(135
,000
)75
,500
Tota
l O
pera
ting
Fund
Exp
endi
ture
s6,
999,
470
7,27
9,45
0
65.7%
25.8%
6.5%
1.9%
2010
Pe
rso
nn
el
Op
era
tin
g e
xp
en
ses
Inv
est
me
nt
in n
ew
de
ve
lop
me
nts
Inv
est
me
nt
in o
the
r
ass
ets
69.0%
26.6%
2.4%
2.1%
2009
1020
09 &
201
0
Fina
lly, t
he fl
ux in
the
sky
subt
ract
ed im
age
is sc
aled
usi
ng st
anda
rd st
ar z
erop
oint
, and
chi
p-to
-chi
p va
riatio
nsar
e ac
coun
ted
usin
g th
e m
agni
tude
s of
2M
ass
obje
cts
in e
ach
expo
sure
. Th
e as
trom
etric
sol
utio
n an
d th
eze
ropo
int v
alue
s are
pro
vide
d as
fits
hea
der k
eyw
ords
in th
e de
trend
ed, s
ky su
btra
cted
, and
ast
rom
etric
ally
and
phot
omet
rical
ly c
alib
rate
d im
age,
*p.
fits (
show
n in
the
gree
n fr
ame
in F
ig 1
).
3. A
utom
atio
n an
d pa
ralle
l pro
cess
ing
By
inco
rpor
atin
g a
mul
ti-m
achi
ne p
aral
lel
driv
er, I
’iwi 2
aut
omat
es a
nd o
ptim
izes
all
aspe
cts
of W
IRC
am d
ata
proc
essi
ng a
ndca
libra
tion
for m
axim
um th
roug
hput
. Com
-pu
ting
reso
urce
s to
us
e (C
PUs,
stor
age
disk
s, et
c) m
ay b
e ea
sily
set
bas
ed o
n av
ail-
abili
ty.
Eac
h da
ta p
rodu
ct is
crea
ted
in an
indi
vidu
alm
odul
e (a
tom
ical
ly).
Mod
ular
des
ign
per-
mits
the p
roce
ssin
g to
be a
borte
d an
d re
star
t-ed
“cl
eanl
y” -
the
pipe
line,
thou
gh r
unni
ngm
ultip
le p
roce
sses
on
mul
tiple
mac
hine
s,m
ay b
e sa
fely
stop
ped
at a
ny ti
me
(aut
omat
-ic
ally
cle
ans
up i
ncom
plet
e pr
oduc
ts a
ndru
nnin
g pr
oces
ses)
; w
hen
proc
essi
ng r
e-su
mes
, the
pip
elin
e au
tom
atic
ally
pic
ks u
pw
here
it le
ft of
f.
Proc
essi
ng i
s ve
ry f
lexi
ble,
bei
ng a
ble
tore
duce
an
entir
e C
amer
a R
un w
ith a
sin
gle
com
man
d, t
o re
duci
ng a
par
ticul
ar P
I pr
o-gr
am c
ross
ing
mul
tiple
cam
era
runs
, to
redu
cing
a si
ngle
imag
e.
All
proc
essi
ng p
aram
eter
s are
take
n fr
om a
data
base
with
a fle
xibl
e web
inte
rfac
e, sh
own
in F
ig 2
. The
inte
rfac
epe
rmits
eas
y br
owsi
ng o
f da
taba
se t
able
s an
d pr
oces
sed
calib
ratio
ns,
as w
ell
as t
o en
able
/dis
able
use
of
parti
cula
r dat
a. P
roce
ssin
g pa
ram
eter
s may
be
chan
ged
as re
quire
d. T
hum
bnai
ls o
f sci
ence
dat
a pr
oduc
t im
ages
are
also
ava
ilabl
e fo
r qua
lity
eval
uatio
n pu
rpos
es. I
n ad
ditio
n it
is p
ossi
ble
to m
onito
r the
sta
tus
and
gene
rate
repo
rts o
f ong
oing
redu
ctio
ns.
4. P
hoto
met
ric
and
astr
omet
ric
calib
ratio
nsI’
iwi
2co
mpu
tes
phot
omet
-ric
ze
ropo
ints
fo
rea
ch c
am-
era
run
in-
stea
d of
just
on
ceat
the
end
of t
he s
e-m
este
r.A
bsol
ute
zero
poi
nt c
alib
ratio
n is
obt
aine
d us
ing
broa
d an
d na
rrow
ban
d st
anda
rd st
ar o
bser
vatio
ns, o
bser
ved
each
nig
htun
der p
hoto
met
ric c
ondi
tions
. R
elat
ive
zero
poi
nt o
ffse
ts b
etw
een
the
four
CC
D c
hips
(Fig
3a)
are
com
pute
dus
ing
2MA
SS st
ars i
n th
e sta
ndar
d st
ar fi
elds
; we b
oots
trap
avai
labl
e JH
K m
agni
tude
s fro
m th
e 2M
ASS
cata
log
for
the
narr
ow b
and
filte
rs. C
eles
tial c
oord
inat
es o
f 2M
ASS
sta
rs in
eac
h sc
ienc
e im
age
are
used
for
line
aras
trom
etric
cor
rect
ion;
as
a po
licy,
no
pixe
l re-
sam
plin
g is
per
mitt
ed d
urin
g da
ta p
roce
ssin
g. W
ith th
e cu
rren
tal
gorit
hms,
we
estim
ate
~10%
err
or in
pho
tom
etry
, and
< 2
” as
trom
etric
err
or, t
houg
h w
ith tr
ends
acr
oss
the
mos
aic
(Fig
3b)
.
Figu
re 2
��������������� ���
face
to s
how
the
sta-
tus
of p
roce
ssed
prog
ram
s, fo
r mon
itor-
ing
proc
ess
para
me-
ters
, and
bro
wsi
ng o
fda
taba
se ta
bles
, cal
i-br
atio
ns a
nd d
ata
prod
ucts
.
Figu
re 3
a (le
ft)Th
e re
lativ
e ch
ip-to
-ch
ip o
ffset
in p
hoto
-m
etric
zer
opoi
nts
com
pute
d w
ith2M
AS
S c
atal
og.
Fig
ure
3b (r
ight
).Th
e di
strib
utio
n of
as-
trom
etric
err
ors
alon
gth
e ch
ip in
sec
ond
quad
rant
. The
mos
aic
cent
er is
the
top-
left
corn
er.
CFH
T A
nnua
l Rep
ort
11
5. W
eb in
terf
ace
for
PI d
ata
dist
ribu
tion
We
have
des
igne
d an
eas
y-to
-use
web
inte
rfac
e (F
ig 4
) for
the
dist
ribut
ion
of d
ata
prod
ucts
to th
e PI
s. Fo
r eac
hpr
ogra
m, a
pas
swor
d pr
otec
ted
web
page
is c
reat
ed a
nd th
e PI
info
rmed
as s
oon
as th
e ob
serv
atio
ns a
re st
arte
dan
d ra
w fi
les
are
avai
labl
e, w
ith re
gula
r upd
ates
as
the
data
are
pro
cess
ed. O
nce
the
prog
ram
is c
ompl
ete
and
the
data
hav
e be
en fu
lly p
roce
ssed
, the
PI i
s aga
in in
form
ed a
bout
the
data
pro
duct
s rea
dy fo
r dow
nloa
d.
6. S
umm
ary
and
futu
re d
evel
opm
ent
We
have
impl
emen
ted
all t
he m
ajor
upg
rade
s to
I’iw
i 2 in
aut
omat
ion
and
para
llel p
roce
ssin
g, s
ky e
stim
atio
nst
rate
gies
and
zer
o po
int c
alib
ratio
ns. I
t is
curr
ently
und
er p
rodu
ctio
n m
ode
for t
he p
roce
ssin
g an
d re
leas
e of
the
ongo
ing
2011
A P
I dat
a.
Our
I’iw
i 2 e
xper
ienc
e ha
s he
lped
iden
tify
chan
ges
in th
e pr
oces
s w
hich
will
yie
ld fu
rther
boo
st in
spe
ed (e
g,co
llaps
ing
mul
ti-sl
ice
cube
s prio
r to
sky
imag
e co
nstru
ctio
n). T
he c
ompl
ete
IDL
scrip
t will
be
repl
aced
with
aco
mpi
led
prog
ram
min
g la
ngua
ge su
ch a
s C to
gai
n ~1
0x in
crea
se in
spee
d,an
d av
oid
licen
sing
nee
ds. W
e pl
anto
impl
emen
t ase
cond
pas
s of s
ky su
btra
ctio
n us
ing
stac
ked
imag
es o
f the
*p.
fits i
mag
es fo
r con
stru
ctin
g hi
ghS/
N s
ky i
mag
es. B
y m
appi
ng d
isto
rtion
s in
the
WIR
Cam
cam
era
optic
s, w
e ai
m t
o be
tter
char
acte
rize
the
inst
rum
ent w
ith g
ains
in b
oth
flat f
ield
ing
effic
ienc
y an
d in
ast
rom
etric
and
pho
tom
etric
cal
ibra
tions
.
Figu
re 4
A s
ampl
e m
etad
ata
page
use
d fo
r pr
o-ce
ssed
dat
a di
strib
u-tio
n to
PIs
. Eac
h P
I is
prov
ided
with
a u
niqu
eke
y to
acc
ess
thei
rpr
oprie
tary
dat
a.
WIR
Cam
sta
ring
mod
e &
exo
plan
et s
tudi
es
D. D
evos
t
Intr
oduc
tion
Hig
h-pr
ecis
ion
diff
eren
tial p
hoto
met
ry fo
r tim
e-se
ries
obse
rvat
ions
last
ing
up to
sev
eral
hou
rs is
key
for t
hesu
cces
s of
sev
eral
ast
roph
ysic
al p
rogr
ams.
In
the
past
at
the
Can
ada-
Fran
ce-H
awai
i Te
lesc
ope
(CFH
T),
subm
illim
agni
tude
pho
tom
etry
was
ach
ieve
d w
ith a
spec
ializ
ed p
hoto
met
er o
pera
ting
in v
isib
le li
ght m
ount
edin
vis
itor
mod
e (B
iller
es 1
997)
. W
ith Q
ueue
Ser
vice
Obs
erva
tions
(Q
SO; M
artin
200
1) n
ow in
ope
ratio
nal
mos
t all-
year
roun
d, it
bec
ame
appa
rent
that
sim
ilar p
erfo
rman
ces c
ould
be
achi
eved
with
a g
ener
al-p
urpo
sein
stru
men
t suc
h as
WIR
Cam
but
nee
ded
the i
mpl
emen
tatio
n of
a ne
w se
rvic
e mod
e: th
e WIR
Cam
Sta
ring
Mod
e.
The
WIR
Cam
Sta
ring
Mod
e co
nsis
ts in
taki
ng sh
ort e
xpos
ures
usi
ng th
e fu
ll de
tect
or m
osai
c w
hile
gui
ding
toke
ep th
e ta
rget
on
the
sam
e pi
xel o
f the
det
ecto
r, ke
epin
g th
e te
lesc
ope
defo
cuse
d at
a c
onst
ant d
efoc
us a
mou
ntto
pre
vent
satu
ratio
n. T
he c
halle
nges
of t
his o
bser
ving
stra
tegy
are
: 1) G
uidi
ng o
n de
focu
sed
star
s; 2
) Kee
ping
the
defo
cus
amou
nt f
ixed
ove
r th
e en
tire
obse
rvin
g se
quen
ce; 3
) In
tegr
atin
g sp
ecifi
c re
quire
men
ts in
to th
ehi
ghly
aut
omat
ed Q
SO m
odel
, i.e
. pos
ition
ing
the
targ
et a
nd s
ettin
g th
e de
focu
s am
ount
at t
he s
tart
of th
eob
serv
ing
sequ
ence
. Th
e st
arin
g m
ode
with
WIR
Cam
can
thus
obs
erve
a ta
rget
for s
ever
al h
ours
on
the
sam
epi
xels
of
the
arra
y.
This
allo
ws
for
char
acte
rizat
ion
of th
e ph
otom
etric
var
iatio
ns o
f th
e ta
rget
to le
ss th
an0.
02%
, or t
o a
sign
al-to
-Noi
se R
atio
~50
00.
3020
09 &
201
0
KA
RU
N T
HA
NJA
VU
R jo
ined
CFH
T in
Apr
il 20
10 a
s C
anad
ian
Res
iden
tA
stro
nom
er.
He
was
app
oint
ed I
nstru
men
t Sc
ient
ist
for
WIR
cam
. H
ispr
inci
pal r
espo
nsib
ilitie
s ar
e to
pro
vide
PI a
s w
ell a
s in
-hou
se s
uppo
rt fo
ral
l WIR
Cam
rel
ated
sci
ence
issu
es, w
hile
act
ivel
y pa
rtici
patin
g in
que
ueco
ordi
natio
n an
d ot
her
QSO
dut
ies.
In
conj
unct
ion,
Kar
un a
lso
purs
ues
his
scie
nce
inte
rest
s, w
ith re
sear
ch s
pann
ing
a va
riety
of a
stro
phys
ical
are
as e
xten
ding
from
the
early
Uni
vers
e, s
uch
as la
rge
scal
e st
ruct
ure
form
atio
n an
d ga
laxy
evo
lutio
n, to
the
dyna
mic
s of
glo
bula
r cl
uste
rs a
nd h
igh
velo
city
clo
uds
in t
he M
ilky
Way
. Th
ese
expl
orat
ions
of
the
Uni
vers
e co
me
afte
r a
full
care
er a
s a
mec
hani
cal
engi
neer
,sp
ecia
lizin
g fir
st in
com
bust
ion
engi
neer
ing,
and
late
r in
cont
rol s
yste
ms a
nd ro
botic
s.B
orn
and
rais
ed in
a s
mal
l tow
n in
Sou
th In
dia,
Kar
un c
ompl
eted
his
edu
catio
n up
toa
bach
elor
s de
gree
in
mec
hani
cal
engi
neer
ing
ther
e, a
nd w
orke
d as
a p
rofe
ssio
nal
engi
neer
for s
ever
al y
ears
bef
ore
emig
ratin
g to
Can
ada
to p
ursu
e gr
adua
te st
udie
s firs
tin
Rob
otic
s, an
d la
ter i
n A
stro
phys
ics.
His
cur
rent
pos
ition
at C
FHT
prov
ides
him
the
enric
hing
exp
erie
nce
ofw
orki
ng w
ith c
uttin
g-ed
ge te
lesc
ope
tech
nolo
gy w
hile
pon
derin
g on
Nat
ure’
s man
y w
onde
rs in
our
Uni
vers
e.
MA
RY
BET
H L
AY
CH
AC
K l
eft
CFH
T in
Sep
tem
ber
2010
afte
r w
orki
ng f
or C
FHT
for
mor
e th
en 7
yea
rs.
Mar
y B
eth
was
hire
d as
a S
ervi
ce O
bser
ver i
n Ju
ne 2
003.
She
was
an
exce
llent
SO
and
her
kno
wle
dge
of a
stro
nom
y an
d he
r atte
ntio
n to
det
ails
pro
vide
d hi
ghqu
ality
dat
a to
the
CFH
T PI
s. H
er c
ontri
butio
n to
the
Rem
ote
Obs
erve
r tra
inin
g w
as v
ery
impo
rtant
to th
e su
cces
s of
the
prog
ram
and
pla
yed
a m
ajor
rol
e in
the
early
day
s of
OA
P’s
obse
rvin
g si
dede
velo
pmen
t.
Mar
y B
eth
was
als
o le
adin
g th
e O
utre
ach
prog
ram
, mak
ing
sure
that
CFH
T w
as p
rese
nt to
sev
eral
com
mun
ity e
vent
s an
d al
way
s be
ing
a pa
rtici
pant
her
self
to t
hese
eve
nts.
Mar
y B
eth'
s gr
eat
com
mun
icat
ion
skill
s m
akes
her
an
effe
ctiv
e co
mm
unic
ator
of S
cien
ce to
the
publ
ic.
She
was
als
oin
volv
ed o
n se
vera
l oth
er a
spec
ts r
elat
ed to
wor
k pe
rfor
med
at C
FHT;
hel
ping
with
dat
a di
strib
u-tio
ns, w
ith th
e lib
rary
and
with
inst
rum
ent e
xcha
nges
, am
ong
othe
rs.
Mar
y B
eth
has m
oved
to O
ahu
whe
re sh
e ca
n no
w e
njoy
the
big
city
life
and
als
o be
with
her
hus
band
who
star
ted
a la
w c
aree
r.
EDER
MA
RTI
OLI
join
ed C
FHT
as a
Bra
zilia
n re
side
nt a
stro
nom
er in
Sep
-te
mbe
r 20
10.
Eder
rec
eive
d hi
s Ph
D i
n A
stro
phys
ics
from
the
Ins
titut
oN
acio
nal
de P
esqu
isas
Esp
acia
is (
INPE
) w
ith c
olla
bora
tive
perio
d at
the
Uni
vers
ity o
f Tex
as a
t Aus
tin. E
der's
sci
ence
inte
rest
s ar
e co
ncen
trate
d on
opt
ical
and
infr
ared
ast
rono
my.
He
wor
ks o
n th
e de
tect
ion
and
char
acte
rizat
ion
of e
xopl
an-
ets,
brow
n dw
arfs
and
low
-mas
s st
ar c
ompa
nion
s, gr
avita
tiona
l mic
role
nsin
g an
dst
ella
r ac
tivity
. He
perf
orm
ed h
is s
cien
ce u
sing
pho
tom
etry
and
tim
e se
ries,
high
prec
isio
n ra
dial
vel
ocity
with
hig
h re
solu
tion
spec
trosc
opy,
and
nar
row
fie
ld a
s-tro
met
ry w
ith t
he F
ine
Gui
danc
e Se
nsor
s on
HST
, op
tical
int
erfe
rom
etry
and
imag
ing.
Ede
r is
inv
olve
d in
sev
eral
pro
ject
s at
CFH
T an
d m
ainl
y w
orks
on
ESPa
DO
nS. W
elco
me
to C
FHT,
Ede
r!
DA
N S
AB
IN re
tired
in O
ctob
er 2
010,
afte
r 25
year
s of s
ervi
ce a
s CFH
T's m
achi
nist
/ m
echa
nica
lde
sign
er .
His
kno
wle
dge
of th
e m
echa
nica
l sys
tem
s of t
he te
lesc
ope
and
his a
bilit
y to
fabr
icat
ean
d re
pair
prec
isio
n pa
rts a
nd a
ssem
blie
s w
ill b
e gr
eatly
mis
sed.
Dan
's de
parti
ng a
ccom
plis
h-m
ent w
as th
e cr
eatio
n of
a 3
-D c
ompu
ter m
odel
of t
he te
lesc
ope,
dom
e, a
nd b
uild
ing.
Dan
cam
e to
us
from
the
tool
and
die
trad
e as
a m
aste
r m
achi
nist
, but
ove
r th
e ye
ars,
with
his
inte
rest
in d
esig
n, h
ebe
cam
e pr
ofic
ient
in th
e us
e of
mod
ern
com
pute
r des
ign
tool
s, st
artin
g w
ith A
utoC
ad w
hen
it fir
st c
ame
out a
nd m
ost r
ecen
tly w
ith A
utoD
esk
Inve
ntor
.
Am
ong
his
man
y ot
her a
ccom
plis
hmen
ts, D
an d
esig
ned
and
man
aged
the
cons
truct
ion
of th
e th
en n
ewM
egaP
rime
uppe
r end
, and
was
inst
rum
enta
l in
rebu
ildin
g th
e fil
ter a
nd ju
ke b
ox m
echa
nism
s whe
n th
eyfa
iled
cata
stro
phic
ally
in th
e fir
st y
ears
of M
egaC
am o
pera
tions
.
CFH
T A
nnua
l Rep
ort
29
Com
ings
and
Goi
ngs
RA
ECH
EL Z
ELM
AN
left
CFH
T in
Aug
ust 2
009
afte
r bei
ng w
ith u
s fo
r a li
ttle
mor
e th
an 3
yea
rs.
She
was
hire
d as
a S
ervi
ce O
bser
ver a
t CFH
T in
May
200
6.R
acha
el w
as a
con
scie
ntio
us S
O a
nd p
rovi
ded
good
obs
erva
tions
for t
he C
FHT
PIs.
She
also
hel
ped
with
dis
tribu
tions
, alw
ays
striv
ing
to p
rovi
de b
ette
r da
ta to
our
Scie
ntis
ts.
She
did
a go
od j
ob!
Rac
hael
was
als
o in
volv
ed i
n ou
treac
h an
d al
way
sav
aila
ble
to h
elp
with
all
aspe
cts
of C
FHT'
s op
erat
ions
. Rac
hael
and
her
hus
band
hav
em
oved
bac
k to
the
mai
nlan
d to
pur
sue
othe
r int
eres
ts.
LOIC
ALB
ERT
left
CFH
T in
Dec
embe
r 200
9 af
ter a
tenu
re a
s C
anad
ian
Res
iden
t Ast
rono
mer
for
near
ly fi
ve an
d a h
alf y
ears
. He s
tudi
es B
row
n D
war
fs an
d is
hea
vily
invo
lved
in th
e Can
ada F
ranc
eB
row
n D
war
fs S
urve
y. T
his
surv
ey a
ims
at id
entif
ying
ultr
acoo
l bro
wn
dwar
fs (
Y d
war
fs)
and
obta
in a
larg
e sa
mpl
e of
bro
wn
dwar
fs to
trac
e th
eir g
alac
tic d
istri
butio
n. D
urin
g hi
s st
ay a
t CFH
T, L
oïc
was
the
WIR
Cam
Inst
rum
ent S
cien
tist a
nd c
ontri
bute
d si
gnifi
cant
ly to
sev
eral
asp
ects
of t
he in
stru
men
t.H
e al
so w
rote
the
first
ver
sion
of t
he s
cien
ce d
ata
redu
ctio
n pi
pelin
e. M
ost o
f the
sof
twar
e Lo
ïc w
rote
isst
ill in
use
toda
y in
the
seco
nd v
ersi
on o
f the
softw
are.
Loï
c re
mai
ns a
regu
lar u
ser o
f CFH
T an
d re
cent
lyjo
ined
the
Ast
roph
ysic
s gro
up a
t the
Uni
vers
ité d
e M
ontré
al to
wor
k on
the
JWST
gui
ders
.
The
film
was
sho
wn
on f
our
occa
sion
s on
the
Big
Isla
nd in
per
form
ance
thea
ters
off
erin
g a l
arge
scr
een
and
a po
wer
ful s
ound
sys
tem
. The
se s
how
ings
wer
eco
uple
d w
ith s
peci
al a
ftern
oon
sess
ions
for s
choo
ls.
Whi
le th
e fil
m c
reat
or h
ad th
e op
portu
nity
to s
hare
such
form
at w
ith th
e pu
blic
thro
ugho
ut 2
009
(Vic
to-
ria, P
aris
, Pad
ova,
And
orra
, Mau
i), th
e fi
lm w
as a
lso
adop
ted
by v
ario
us g
roup
s inv
olve
d in
the
prom
otio
nof
the
Int
erna
tiona
l Y
ear
of A
stro
nom
y in
Can
ada
and
Fran
ce.
C. V
eille
t gav
e tw
o ta
lks
for t
he O
bser
vato
ry D
irec-
tor’
s Le
ctur
e Se
ries
orga
nize
d on
the
Big
Isl
and.
In
colla
bora
tion
with
Pro
Scie
nce
- Te
Teru
‘Ihi
Ass
oci-
atio
n an
d th
e A
stro
nom
ical
Soc
iety
of T
ahiti
, and
muc
h he
lp fr
om th
e lo
cal D
epar
tmen
t of E
duca
tion,
he
spen
ttw
o w
eeks
vis
iting
mid
dle
and
high
scho
ols,
givi
ng c
onfe
renc
es o
n th
e Is
land
of T
ahiti
and
als
o on
less
vis
ited
isla
nds,
such
as
Rai
atea
and
the
Aus
trale
s (R
urut
u an
d Tu
buai
). Th
is v
isit
has
been
the
maj
or e
vent
of I
YA
inFr
ench
Pol
ynes
ia,
touc
hing
900
stu
dent
s th
roug
h vi
sits
in
clas
s ro
oms
in t
wel
ve d
iffer
ent
scho
ols
(Lyc
éeSa
mue
l Rap
ooto
, Pap
eete
, pic
ture
on
the
left)
, as
wel
l as
univ
ersi
ty-le
vel s
tude
nts
in E
duca
tion.
Tha
nks
tose
ven
conf
eren
ces
orga
nize
d at
the
Uni
vers
ity a
nd in
city
hal
ls in
eve
ry is
land
vis
ited,
C. V
eille
t was
abl
e to
reac
h hu
ndre
ds o
f pe
ople
fro
m t
he g
ener
alpu
blic
. A
ver
y st
rong
sup
port
of t
he l
ocal
med
ia,
incl
udin
g ev
enin
g ne
ws
on l
ocal
TV
chan
nels
(Ta
hiti
Nui
Tel
evis
ion
- pi
ctur
e on
the
right
), he
lped
in
prom
otin
g th
e va
rious
even
ts,
givi
ng a
stro
nom
y an
d C
FHT
a w
ide
expo
sure
in th
e ge
nera
l pub
lic, a
nd a
ctiv
atin
gon
ce m
ore
the
hist
oric
al l
ink
betw
een
Tahi
tian
d th
e H
awai
ian
Isla
nds.
Can
ada P
ost s
elec
ted
CFH
T as
one
of t
he tw
o C
anad
ian
tele
scop
es fe
atur
ed o
n st
amps
issu
ed to
cel
ebra
te IY
A.
In a
dditi
on, t
wo
imag
es m
ade
from
Meg
aCam
dat
a pr
oces
sed
by J
ean-
Cha
rles
Cui
lland
re a
nd C
oelu
m w
ere
used
for t
he st
amps
bac
kgro
und
(see
fron
t cov
er fo
r the
stam
ps, a
nd fr
ont a
nd b
ack
cove
rs fo
r the
imag
es).
Haw
aiia
n St
arlig
ht
J.C
. Cui
lland
re s
ign-
ing
the
DV
D a
fter a
show
ing
in th
e K
ahilu
Thea
tre (W
aim
ea).
The
DV
D h
as b
een
are
al a
sset
for C
FHT
durin
g IY
A.
1220
09 &
201
0
Exo
plan
et c
hara
cter
isat
ion
at C
FHT
The d
isco
very
hun
dred
s of e
xopl
anet
s in
the l
ast 5
yea
rs h
as o
pene
d ne
w av
enue
s of s
cien
tific
dis
cove
ries.
New
tech
niqu
es a
re b
eing
dev
elop
ed to
und
erst
and
the
phys
ics o
f the
se n
ew sy
stem
s. T
rans
it ph
otom
etry
is u
sed
toob
serv
e th
e si
gnal
res
ultin
g fr
om th
e ec
lipse
of
the
seco
ndar
y co
mpo
nent
of
a sy
stem
. Th
e si
gnal
is m
uch
fain
ter
then
that
of
an e
clip
se o
f th
e pr
imar
y an
d th
us m
ore
chal
leng
ing
to o
bser
ve a
nd n
eeds
ver
y pr
ecis
em
easu
rem
ents
.
TrE
S-2b
A te
am fr
om th
e U
nive
r-si
ty o
f Tor
onto
(UT)
tar-
gete
d th
e ec
lipse
of
the
hot
Jupi
ter
TrES
-2b
(Cro
ll et
al 2
010b
) w
ithst
arin
g m
ode
obse
rva-
tions
.
TrES
-2b'
s pr
imar
y ha
s a
Ks
mag
nitu
de o
f 9.
846
and
eclip
sed
the
plan
eton
the
nigh
t of J
une
10 to
June
11
2009
. T
he o
b-se
rvat
ions
wer
e co
nduc
t-ed
for
~3.
5 ho
urs.
The
ther
mal
em
issi
on o
f th
epl
anet
was
det
ecte
d to
a 5
sigm
a le
vel
(Fig
ure
1).
The
obse
rvat
ions
, pr
o-ce
ssin
g an
d an
alys
is o
fth
e da
ta l
ead
to a
stu
n-ni
ng 1
sig
ma
erro
r ba
rson
the
ord
er o
f 0.
012%
.Th
ey c
ombi
ned
thei
r C
FHT
WIR
Cam
dat
a to
pre
viou
s Sp
itzer
/IRA
C d
ata
and
foun
d th
at T
rES-
2b l
ikel
yfe
atur
es a
mod
est r
edis
tribu
tion
of h
eat f
rom
the
nigh
tsid
e to
the
days
ide
of th
e pl
anet
. Th
eir K
s det
ectio
n al
sohe
lped
det
erm
ined
that
the
spec
tral e
nerg
y di
strib
utio
n of
TrE
S-2b
cou
ld b
e fit
by
a bl
ackb
ody
curv
e th
usin
dica
ting
a fa
irly
isot
herm
al d
aysi
de te
mpe
ratu
re st
ruct
ure.
GJ
1214
bSi
nce
then
, the
UT
team
has
per
form
ed o
bser
-va
tions
on
othe
r pla
nets
. Th
e la
test
one
bei
ngG
J 12
14b,
a tr
ansi
ting
exop
lane
t who
se ra
dius
lies
mid
way
bet
wee
n th
at o
f th
e Ea
rth a
ndN
eptu
ne (C
roll
et a
ll 20
11).
For
thes
e ob
serv
a-tio
ns,
they
use
d th
ree
WIR
Cam
ban
ds t
hus
obse
rvin
g th
e br
oad
band
spec
trum
of t
he p
lan-
et in
the
near
-infr
ared
. In
June
and
Aug
ust 2
010,
they
use
d W
IRC
am st
arin
g m
ode
to p
erfo
rm o
bser
vatio
ns in
the
J, K
s and
CH
4On
with
the
goal
of d
eter
min
ing
if G
J121
4b is
a sc
aled
dow
n N
eptu
ne o
r a S
uper
Ear
th.
To d
o th
is, o
ne n
eeds
to d
eter
min
e th
e co
mpo
sitio
n of
the
exop
lane
t's a
tmos
pher
e. A
n at
mos
pher
e do
min
ated
by H
ydro
gen
and
Hel
ium
like
Nep
tune
will
hav
e a
larg
e sc
ale
heig
ht th
us m
akin
g th
e de
tect
ion
of m
olec
ular
spec
ies
like
wat
er a
nd m
etha
ne p
ossi
ble.
On
the
othe
r han
d, a
n at
mos
pher
e lik
e Ea
rth d
omin
ated
by
heav
ier
mol
ecul
es, i
mpl
ies a
low
er sc
ale h
eigh
t whi
ch fl
atte
ns th
e spe
ctra
and
mak
es it
feat
urel
ess w
hen
obse
rved
usi
ngth
is te
chni
que.
Figu
re 2
sho
ws
thei
r re
sults
. T
he l
ines
in
this
plo
t ar
e th
e di
ffer
ent
mod
el a
tmos
pher
es w
hile
the
bla
ckdi
amon
ds a
re th
e W
IRC
am d
ata
poin
ts.
The
othe
r dat
a po
ints
are
from
oth
er o
bser
vatio
ns.
The
WIR
Cam
dat
ase
ems
to i
ndic
ate
that
the
nea
r-in
frar
ed s
pect
rum
of
GJ
1214
b is
not
fea
ture
less
thu
s po
intin
g to
war
d an
atm
osph
ere
with
a lo
w m
olec
ular
wei
ght,
dom
inat
ed b
y H
ydro
gen
and
Hel
ium
, mor
e lik
e N
eptu
ne th
en E
arth
.H
owev
er, t
heir
anal
ysis
can
not r
ule
out t
hat t
he a
tmos
pher
e ha
s a
high
mol
ecul
ar w
eigh
t and
that
ther
e is
abso
rptio
n by
a h
aze
laye
r at h
igh
altit
ude.
Thi
s haz
e co
uld
be m
ade
of su
b-m
icro
n si
ze p
artic
les t
hat a
bsor
bslig
ht fr
om th
e op
tical
up
to 1
mic
rons
thus
flat
teni
ng th
e sp
ectra
in th
e bl
uer p
arts
of t
he n
ear-
infr
ared
spec
trum
and
star
ting
to sh
ow fe
atur
es in
the
CH
4On
and
Ks b
ands
.
Figu
re 1
CFH
T/W
IRC
am K
s-ba
nd p
hoto
met
ry o
fth
e se
cond
ary
eclip
seof
TrE
S-2
b. T
he to
ppa
nel s
how
s th
e un
-bi
nned
lig
htcu
rve,
whi
le th
e pa
nel t
hat i
sth
e se
cond
from
the
top
show
s th
e lig
ht-
curv
e w
ith th
e da
tabi
nned
eve
ry 7
.0 m
in-
utes
. Th
e pa
nel t
hat
is th
e se
cond
from
the
botto
m s
how
s th
ebi
nned
dat
a af
ter t
hesu
btra
ctio
n of
the
best
-fit b
ackg
roun
d,w
hile
the
botto
m p
an-
el s
how
s th
e bi
nned
resi
dual
s fro
m t
hebe
st-fi
t m
odel
. I
nea
ch o
ne o
f the
pan
-el
s th
e be
st-fi
t bes
t-fit
seco
ndar
y ec
lipse
and
back
grou
nd, B
f , is
show
n w
ith th
e re
dlin
e. T
he e
xpec
ted
mid
-sec
onda
ry e
clip
seis
if T
rES
-2b
has
zero
ecce
ntric
ity.
Figu
rean
d ca
ptio
n fro
m C
roll
et a
l (20
10b)
.
Figu
re 2
Tran
sit o
bser
vatio
ns o
fG
J 12
14b.
Bla
ck d
ia-
mon
ds a
re th
e w
eigh
t-ed
mea
n of
WIR
Cam
J- &
Ks-
band
and
CH
4O
n fil
ter d
ata.
Red
diam
onds
are
the
ME
arth
(Cha
rbon
neau
et a
l. 20
09),
and
the
Kitt
-pea
k S
ada
et a
l.(2
010)
tran
sit d
epth
,bl
ue d
iam
onds
are
VLT
/FO
RS
2 po
ints
(Bea
n et
al.
2010
)G
rey
dotte
d cu
rve
line
is G
J 12
14b
atm
o-sp
heric
mod
el, o
rang
ea
sola
r-m
etal
licity
mod
el, c
yan
a so
lar-
met
allic
ity n
o m
etha
nem
odel
(M
iller
-Ric
ci20
10)
for
> 1
m.
For
<1
m, t
he p
re-
dict
ed a
bsop
rtion
iscu
t of t
o si
mul
ate
the
impa
ct o
f put
ativ
e ha
z-es
. Fig
ures
and
cap
-tio
n fro
m C
roll
et a
l(2
011)
.
CFH
T A
nnua
l Rep
ort
13
Con
clus
ion
The
WIR
Cam
sta
ring
mod
e ha
s be
en o
pera
ting
at C
FHT
for
a lit
tle m
ore
then
tw
o ye
ars
and
has
alre
ady
prod
uced
sig
nific
ant s
cien
tific
resu
lts.
Des
pite
the
tech
nica
l cha
lleng
es re
late
d to
the
impl
emen
tatio
n of
this
mod
e of
obs
erva
tion,
subm
illim
agni
tude
pre
cisi
on p
hoto
met
ry o
ver s
ever
al h
ours
of o
bser
ving
can
be
reac
hed
relia
bly
thus
ope
ning
a n
ew w
indo
w o
f sci
entif
ic o
ppor
tuni
ties f
or o
ur o
bser
vato
ry.
Ref
eren
ces
Bea
n, J
.L.,
Kem
pton
, E.M
.-R.,
Hom
eier
, D. 2
010,
Nat
ure,
468
, 669
Bill
eres
, M.,
Font
aine
, G.,
Bra
ssar
d, P
., C
harp
inet
, S.,
Lieb
ert,
J., S
affe
r, R
. A.,
& V
aucl
air,
G. 1
997,
ApJ
L, 4
87, L
81C
harb
onne
au, D
. et a
l. 20
09, N
atur
e, 4
62, 8
91C
roll,
B.,
Alb
ert,
L., L
afre
nier
e, D
., Ja
yaw
ardh
ana,
R.,
& F
ortn
ey, J
. J. 2
010b
, ApJ
, 717
, 108
4C
roll,
B.,
Alb
ert,
L., J
ayaw
ardh
ana,
R.,
Mill
er-R
icci
Kem
pton
, E.,
Fortn
ey, J
.~J.
, Mur
ray,
N.,
& N
eils
on, H
. 201
1, a
rXiv
:110
4.00
11, A
pJ a
ccep
ted.
Mar
tin, P
. 200
1, B
ulle
tin d
'info
rmat
ion
du te
lesc
ope
Can
ada-
Fran
ce-H
awai
i, 43
, 2M
iller
-Ric
ci, E
. & F
ortn
ey, J
.J. 2
010,
ApJ
, 716
, L74
Sad
a, P
.V. e
t al.
2010
, ApJ
, 720
, L21
5
MK
AM
& A
SIVA
MK
AM
(M
auna
Kea
Atm
osph
eric
Mon
itor)
is a
col
labo
rativ
e pr
ojec
t bet
wee
nIf
A, C
FHT
and
W.M
. Kec
k. I
ts g
oal
is to
mak
e av
aila
ble
a se
eing
mon
itor
on th
eC
FHT
site
for
use
by
all
the
obse
rvat
orie
s on
the
sum
mit.
The
pro
ject
is
fund
edth
roug
h in
fras
truct
ure
mon
ey m
anag
ed b
y IF
A a
nd o
pera
ting
fund
s co
me
from
the
parti
cipa
ting
obse
rvat
orie
s. A
fter
mon
ths
of in
tegr
atio
n in
Wai
mea
in 2
009,
it w
asin
stal
led
on t
he c
oncr
ete
pad
of t
he w
eath
er t
ower
, w
hich
was
dis
mou
nted
and
rem
oved
fro
m th
e su
mm
it. I
t ope
rate
d sm
ooth
ly fo
r sev
eral
mon
ths
until
Feb
ruar
y20
10 w
hen
an ic
e sto
rm re
sulte
d in
a ca
tast
roph
ic fa
ilure
of i
ts en
clos
ure.
Ice f
roze
one
of t
wo
mot
ors
whi
ch c
ause
d th
e en
clos
ure
totw
ist a
nd e
vent
ually
a w
eld
on th
e en
clos
ure
tofa
il. T
he e
nclo
sure
was
rep
aire
d in
sho
rt or
der.
The
tele
scop
e az
imut
h en
code
r als
o fa
iled
durin
g th
ispe
riod.
Rep
laci
ng it
was
not
triv
ial a
nd re
quire
ddi
sass
embl
y of
the
tele
scop
e m
ount
in o
rder
to g
ain
acce
ss.T
he M
ASS
unit
over
estim
ated
the
seei
ng w
hen
the
scin
tilla
tion
inde
x is
hig
h (a
kno
wn
issu
e) a
nd n
ew p
roce
ssin
g so
ftwar
e w
ere
obta
ined
to c
orre
ct th
e pr
oble
man
d da
ta v
erifi
ed b
efor
e re
leas
ing
it to
the
com
mun
ity. A
new
wea
ther
arm
for t
he a
nem
omet
er a
nd w
ind
vane
was
des
igne
d, fa
bric
ated
, and
inst
alle
dby
the e
nd o
f 201
0, re
plac
ing
the o
rigin
al o
ne at
the e
nclo
sure
pla
tform
that
had
sign
ifica
nt v
ibra
tion
prob
lem
s. It
is se
en o
n th
e pi
ctur
e on
the
left.
In sp
ite o
f the
se is
sues
, MK
AM
has
succ
essf
ully
ope
rate
d fo
r mor
e th
an a
year
, off
erin
g a l
ong-
awai
ted
prov
ided
the M
auna
kea o
bser
vato
ries a
nd th
eM
auna
kea
Wea
ther
Cen
ter w
ith re
liabl
e se
eing
dat
a
ASI
VA
(All-
Sky
Infr
ared
Vis
ible
Ana
lyze
r) is
a m
ultip
urpo
se v
isib
le a
nd in
frar
ed s
ky im
agin
e an
d an
alys
isin
stru
men
t tha
t will
be u
sed
to o
btai
n a r
eal-t
ime c
ensu
s of t
he cl
ouds
and
wat
er v
apor
stru
ctur
e in
the n
ight
sky.
ASI
VA
is a
n If
A-C
FHT
colla
bora
tion,
dev
elop
ed a
nd o
pera
ted
by C
FHT
for a
ll th
e ob
serv
ator
ies i
n th
e sa
me
way
as
MK
AM
. ASI
VA
has
bee
n in
stal
led
on th
e su
mm
it at
the
end
of 2
010.
Som
e is
sues
with
the
unit
wer
eid
entif
ied
and
addr
esse
d in
the
test
ing
in W
aim
ea p
rior t
o in
stal
latio
n on
the
sum
mit.
The
se in
clud
ed is
sues
with
ser
ial c
omm
unic
atio
ns, t
he h
atch
mot
or c
ontro
ller,
and
wea
ther
proo
fing
of th
e ha
tch.
The
uni
t ran
suc
cess
-fu
lly in
Wai
mea
for 2
wee
ks b
efor
e mov
ing
to th
e sum
mit.
ASI
VA
is u
sing
the
wea
ther
info
rmat
ion
from
the
CFH
T w
eath
er s
yste
m to
aut
omat
ical
lycl
ose
whe
n pr
ecip
itatio
n is
sens
ed. P
relim
inar
y da
ta lo
oks v
ery
prom
isin
g,an
d m
ore
data
will
be
gath
ered
to c
hara
cter
ize
the
inst
rum
ent a
nd p
repa
reth
e us
er i
nter
face
. D
ata
rele
ase
to C
FHT
and
othe
r ob
serv
ator
ies
will
happ
en a
s soo
n as
dat
a ar
e w
ell u
nder
stoo
d an
d th
e sy
stem
is o
pera
tiona
l.
Imag
es re
ceiv
ed fr
omA
SIVA
(IR
, lef
t) an
dth
e A
ll-S
ky O
ptic
alC
amer
a (v
isib
le, r
ight
).Th
e in
frare
d im
age
reve
als
clou
d st
ruct
ure
that
is n
ot e
asily
iden
ti-fie
d in
the
optic
al a
ll-sk
y im
age.
MK
AM
inte
grat
ed in
the
Wai
mea
sho
p.
2820
09 &
201
0
Out
reac
hC
FHT’
s out
reac
h pr
ogra
m h
as b
een
agai
n ve
ry a
ctiv
e, e
mph
asiz
ing
as u
sual
act
iviti
es d
irect
ed to
war
d th
e lo
cal
com
mun
ity, t
hank
s to
the
cont
ribut
ion
of m
any
staf
f mem
bers
. The
sta
ff m
embe
r at t
he h
elm
of t
hese
eff
orts
,M
ary-
Bet
h La
ycha
ck,
depa
rted
in S
epte
mbe
r 20
10.
She
was
rep
lace
d in
thi
s ro
le b
y N
adin
e M
anse
t an
dD
eeD
ee W
arre
n. O
ne p
erso
n w
as n
ot e
noug
h to
take
ove
r Mar
y-B
eth’
s si
gnifi
cant
role
, a tr
ibut
e to
the
maj
orco
ntrib
utio
ns sh
e de
dica
ted
to o
utre
ach
over
the
year
s.
CFH
T pa
rtici
pate
d in
man
y fa
irs a
nd fe
stiv
als:
Oni
zu-
ka D
ay a
t UH
Hilo
, Wes
t Haw
aii I
nter
med
iate
/Hig
hSc
hool
Sci
ence
Fai
r (ju
dgin
g), F
amily
Sci
ence
Day
at
‘Im
iloa,
Eas
t H
awai
i In
term
edia
te/H
igh
Scho
ol S
ci-
ence
Fai
r (ju
dgin
g), G
irl S
cout
s’ W
omen
in S
cien
ceD
ay,
Hea
lthy
Kei
ki F
est
in W
aim
ea,
Ast
ro D
ay i
nH
ilo, G
irls E
xplo
ring
Mat
h an
d Sc
ienc
e D
ay, W
aim
eaC
ount
ry S
choo
l Sc
ienc
e Fa
ir (ju
dgin
g), F
amily
Sci
-en
ce N
ight
at W
aim
ea M
iddl
e Sc
hool
, Sci
ence
Fai
r at
Koh
ala
Mid
dle/
Hig
h Sc
hool
(ju
dgin
g),
and
Fam
ilyA
stro
nom
y N
ight
at t
he K
ona
and
Koh
ala
Libr
arie
s.
Var
ious
vis
its o
f the
hea
dqua
rters
and
the
sum
mit
wer
e or
gani
zed
for g
roup
s and
spec
ial g
uest
s. C
FHT
offe
red
sum
mit
tour
s as s
ilent
auc
tion
item
s at l
ocal
fund
rais
ing
even
ts fo
r sch
ools
and
non
-pro
fit g
roup
s.
Loca
l sc
hool
s w
ere
visi
ted,
brin
ging
ast
rono
my
and
its a
ctor
s in
the
cla
ssro
om. R
esid
ent A
stro
nom
ers
gave
talk
s fo
r the
Uni
vers
e To
nigh
t con
fere
nce
serie
s at t
he H
ale
Poha
ku V
isito
r Sta
tion.
The
first
Sol
ar S
yste
m W
alk
was
org
aniz
ed in
200
9 in
par
tner
ship
with
the
Kec
k O
bser
vato
ry, a
lso
base
d in
Wai
mea
. In
spite
of
the
win
dy a
nd m
isty
wea
ther
, it
was
wel
l-atte
nded
and
app
reci
ated
. CFH
T an
d K
eck
deci
ded
tom
ake
this
an
annu
al e
vent
. The
201
0 ed
ition
was
als
o a
grea
t suc
cess
!
The
tradi
tiona
l CFH
T St
ar G
azin
g Pa
rty, s
ched
uled
to im
med
iate
ly fo
llow
the
Wai
mea
Chr
istm
as P
arad
e, g
ener
ally
hel
d in
the
even
ing
of th
e fir
st S
atur
day
of D
ecem
ber,
gath
ered
aga
in a
goo
d cr
owd.
Whi
le th
e 20
09 p
arty
was
face
d(a
gain
!) w
ith y
et a
noth
er b
out o
f win
dy-m
isty
-clo
udy
Wai
mea
wea
ther
, 201
0w
as b
less
ed w
ith c
lear
ski
es, b
ringi
ng jo
y an
d aw
e to
the
man
y vi
sito
rs o
f all
ages
, as t
he p
ictu
re o
n th
e rig
ht sh
ows.
In a
dditi
on to
its
usua
l out
reac
h ac
tiviti
es,C
FHT
mar
ked
the
Inte
rnat
iona
l Yea
r of A
stro
nom
y (I
YA
2009
) th
roug
h th
e pa
rtici
patio
n of
sta
ff m
embe
rs i
n IY
A a
ctiv
ities
and
the
org
aniz
atio
n of
spe
cial
even
ts.
J.-C
. Cui
lland
re, L
. Bry
son,
M.B
. Lay
chak
and
C. V
eille
t atte
nded
and
spo
ke a
t the
IA
U/U
NES
CO
conf
eren
ce “
The
Rol
e of
Ast
rono
my
in S
ocie
ty a
nd C
ultu
re”,
Janu
ary
19-2
3. In
add
ition
to a
pre
sent
a-tio
n of
the
DV
D “
Haw
aiia
n St
arlig
ht”,
CFH
T of
fere
d its
200
9 C
alen
dar
to a
ll pa
rtici
pant
s. C
FHT
parti
cipa
ted
in th
e “1
00 H
ours
of A
stro
nom
y: L
ive
from
Mau
na K
ea”
and
in th
e B
ig Is
land
Cos
mic
Post
er C
onte
st (j
udgi
ng a
nd p
rizes
). It
also
pro
vide
d th
e B
ig Is
land
IYA
trad
ing
card
s set
four
imag
esan
d se
t up
an e
xhib
ition
of H
awai
ian
Star
light
imag
es a
t the
‘Im
iloa
Cen
ter f
or A
stro
nom
y
D. D
evos
t was
invi
ted
to g
ive
a ta
lk a
t the
Astr
oLab
du
Mon
t Még
antic
in Q
uébe
c, C
anad
a, a
s pa
rt of
a co
nfer
ence
pro
gram
hel
d ev
ery
Satu
rday
in th
e su
mm
er m
onth
s of
200
9. It
was
a g
ood
oppo
rtuni
tyto
talk
abo
ut C
FHT,
its i
nstru
men
ts a
nd it
s man
y sc
ient
ific
cont
ribut
ions
to a
pub
lic th
at is
ofte
ntim
esun
awar
e of
the
invo
lvem
ent o
f Can
ada
in a
n in
tern
atio
nal s
cien
ce p
roje
ct lo
cate
d in
Haw
aii.
The
CFH
T co
-pro
duce
d sc
enic
film
and
DV
D "
Haw
aiia
n St
arlig
ht"
(Exp
lorin
g th
e U
nive
rse
from
Mau
na K
ea)
was
a s
olid
veh
icle
for
the
prom
otio
n of
the
tele
scop
e du
ring
the
Inte
rnat
iona
l Yea
r of
Ast
rono
my.
The
film
was
pre
sent
ed o
n se
vera
l occ
asio
ns in
lect
ure
halls
and
per
form
ance
thea
ters
,al
way
s fre
e of
cha
rge
for t
he a
udie
nce.
Jean
-Cha
rles C
uilla
ndre
, the
CFH
T as
trono
mer
who
cre
ated
the
piec
e, in
trodu
ced
the
film
by
givi
ng a
sho
rt le
ctur
e de
scrib
ing
the
stor
y of
the
tele
scop
e an
d ho
w th
efil
m w
as c
reat
ed o
ver s
even
yea
rs. A
pop
ular
que
stio
ns a
nd a
nsw
ers s
egm
ent f
ollo
wed
the
scre
enin
g.
GEM
SM
ary
Bet
h L
aych
ack
at th
e 20
09 G
irls
Ex-
plor
ing
Mat
hs a
ndS
cien
ce D
ay .
CFH
T A
nnua
l Rep
ort
27
Dom
e Ve
ntin
gSi
nce
mid
-200
3 an
d fo
r man
y ye
ars,
Meg
aCam
has
bee
n us
edby
the
CFH
T Le
gacy
Sur
vey,
fol
low
ed b
y a
few
Lar
ge P
ro-
gram
s, as
wel
l as h
undr
eds o
f PI p
rogr
ams.
As a
ll im
ages
hav
ebe
en p
re-p
roce
ssed
in-
hous
e, C
FHT
has
at i
ts d
ispo
sal
anam
azin
g da
taba
se o
f de
liver
ed i
mag
e qu
ality
(IQ
) w
ith,
for
each
dat
a po
int,
a w
ealth
of
info
rmat
ion
on e
nviro
nmen
t pa-
ram
eter
s. Th
is d
ata
was
tho
roug
hly
anal
yzed
, re
sulti
ng i
nm
any
grap
hs li
ke th
e on
e sh
own
on th
e le
ft, w
hich
pro
vide
dva
luab
le h
ints
on
how
to im
prov
e the
imag
e qua
lity
seen
by
the
inst
rum
ents
.
With
the
stro
ng su
spic
ion
that
the
lack
of p
rope
r ven
ting
of th
edo
me
was
deg
radi
ng th
e ou
tsid
e se
eing
, it w
as d
ecid
ed b
y th
een
d of
200
9 to
star
t an
in-h
ouse
pro
ject
, dom
e ve
ntin
g, fu
nded
usin
g C
FHT’
s Dev
elop
men
t Fun
d an
d ai
min
g at
(1) c
onfir
min
g th
roug
h ap
prop
riate
stud
ies t
he v
alue
of v
entin
gth
e do
me
alre
ady
reco
gniz
ed th
roug
h M
egaC
am IQ
stu
dies
, and
(2) d
esig
ning
and
impl
emen
ting
vent
s on
the
dom
e. T
he c
urre
nt sc
hedu
le c
alls
for a
com
plet
ion
of th
e en
tire
proj
ect b
efor
e th
e en
d of
201
3.
A c
ompu
ter m
odel
of t
he te
lesc
ope
and
its e
nclo
sure
wer
e co
m-
plet
ed a
t th
e en
d of
the
sum
mer
201
0 by
CFH
T’s
mec
hani
cal
desi
gner
jus
t pr
ior
to h
is r
etire
men
t. Th
e m
odel
is
com
plet
ely
artic
ulat
ed, a
llow
ing
dom
e ro
tatio
n, d
ome
shut
ter
open
ing
and
clos
ing
and
tele
scop
e m
otio
ns in
Dec
linat
ion
and
Hou
r A
ngle
.Th
e m
odel
was
use
d to
gen
erat
e th
ree
cand
idat
e ve
nt g
eom
etrie
s,on
e of
whi
ch is
sho
wn
on th
e le
ft. T
he c
ompu
ter m
odel
s of
the
dom
e an
d te
lesc
ope
have
bee
n pr
ovid
ed to
the
NO
AO
and
Tai
-w
an C
FD g
roup
s w
ho a
re c
urre
ntly
wor
king
up
com
pute
r CFD
mod
els t
o sh
ow a
ir flo
w a
nd fl
ushi
ng a
ssoc
iate
d w
ith th
e ve
nts a
tva
rious
win
d-to
-dom
e sl
it or
ient
atio
ns.
As
a co
nseq
uenc
e of
adv
ice
from
flu
iddy
nam
ics
labs
, it w
as d
ecid
ed to
und
er-
take
wat
er tu
nnel
test
s at
the
Uni
vers
ityof
Was
hing
ton
as a
sta
rting
poi
nt f
orun
ders
tand
ing
air f
low
in a
nd a
roun
d th
eC
FHT
dom
e.A
terr
ain
mod
el o
f the
sum
-m
it ar
ea w
as fa
bric
ated
ove
r the
sum
mer
, a d
etai
led
phys
ical
mod
el o
f the
tele
scop
e at
160:
1 sc
ale w
as fa
bric
ated
from
the c
ompu
ter m
odel
by
a com
mer
cial
ster
eo li
thog
raph
yho
use
and
a tra
nspa
rent
acr
ylic
mod
el o
f the
dom
e ha
s bee
n st
arte
d in
-hou
se. A
n im
age
of th
e m
odel
, ass
embl
ed w
ith a
pap
er m
ocku
p of
the
low
er b
uild
ing,
is s
how
n on
the
right
. W
ater
tun
nel
test
s ar
e sc
hedu
led
for
the
first
hal
f of
201
1 at
Uni
vers
ity o
fW
ashi
ngto
n an
d w
ind
test
s in
Taiw
an in
sum
mer
201
1.
In p
aral
lel
with
the
dom
e ve
ntin
gpr
ojec
t, a
ther
mal
ass
aypr
ogra
m w
as in
itiat
ed to
iden
tify
heat
sou
rces
in a
nd a
roun
dth
e C
FHT
dom
e. O
n th
e le
ft is
a s
ampl
e IR
imag
e of
the
PLC
cabi
nets
us
ed
for
Meg
aPrim
e w
hen
inst
orag
e, ta
ken
with
aFL
IR S
C62
0 ca
mer
abo
rrow
ed f
rom
IfA
.N
ight
-tim
e ai
rpla
nefli
ghts
ove
r the
sum
-m
it ca
ptur
ed
wid
ervi
ews
of t
he d
ome
and
surr
ound
ing
area
. The
vie
w o
n th
e rig
ht sh
ows t
he b
uild
ing
wak
evo
rtice
s. M
itiga
ting
heat
sou
rces
in
the
dom
e an
d bu
ildin
g ar
e an
impo
rtant
com
plem
ent t
o th
e do
me
vent
ing
proj
ect.
Meg
aCam
IQ v
ersu
ssl
it to
win
d an
gle
IQ is
sig
nific
antly
bet
-te
r whe
n th
e sl
it is
orie
nted
at 4
5º fr
omth
e w
ind,
thus
allo
w-
ing
a st
rong
flus
hing
of th
e do
me.
1420
09 &
201
0
Clo
sing
the
CFH
TLS
The
last
imag
es ta
ken
for t
he C
FHT
Lega
cy S
urve
y w
ere
take
n in
ear
ly 2
009.
Nea
rly tw
o ye
ars
late
r, m
any
resu
lts h
ave
been
alre
ady
publ
ishe
d, e
ven
thou
gh th
e fin
al p
ublic
rele
ase
is sc
hedu
led
for m
id-2
011.
The
SNLS
3rd
yea
r sam
ple
The
Supe
rNov
a Le
gacy
Sur
vey
team
has
upd
ated
thei
r con
stra
ints
on
cosm
olog
ical
par
amet
ers
base
d on
thei
r3-
year
sam
ple.
It in
clud
es 2
52 h
igh
reds
hift
Type
Ia su
pern
ovae
up
to z
=1.1
, fo
ur ti
mes
larg
er th
an th
e or
igin
alSN
LS p
aper
by
Ast
ier e
t al.
(200
6).
The
new
ana
lysi
s in
clud
e a
com
plet
e ch
arac
teriz
atio
n of
the
syst
emat
icun
certa
intie
s w
hich
app
ear
to b
e du
e fir
st to
the
calib
ratio
n of
the
four
CFH
TLS
field
s a
nd n
ext t
o th
e m
odel
ing
of th
e SN
ligh
t cur
ves.
The
cons
train
ts o
n th
e co
smol
ogic
al p
aram
eter
s ba
sed
on th
e SN
LS s
ampl
eal
one
are
pres
ente
d in
Guy
et a
l. (2
010,
see
Fi
g 1,
left
) a
nd le
ad to
�M
=0.2
11 +
/-0.0
34(s
tat)+
/-0.0
69(s
ys).
By
com
bini
ng t
heSN
LS 3
yr
sam
ple
with
lo
wer
-z
and
high
er-z
sa
mpl
es,
Con
ley
et
al.
(201
1)
gi
ves
aco
nstra
int
on
the
dark
ene
rgy
equa
-tio
n of
sta
te
pa-
ram
eter
��������
+0.1
6/-0
.20
(sta
t)+0.
07/-0
.14
(sys
)
cons
iste
ntw
ith a
cos
mol
ogi-
cal c
onst
ant.
Prog
enito
rs o
f Typ
e Ia
Sup
erno
vae
?SN
e Ia a
re w
idel
y be
lieve
d to
be e
xplo
sion
of w
hite
dw
arfs
(WD
)w
hose
mas
s has
gro
wn
by a
ccre
tion
to t
he C
hand
rase
khar
mas
s.W
D w
ith a
n ev
olvi
ng b
inar
y st
ar i
s th
e a
ccep
ted
prog
enito
rsc
enar
io a
nd th
e pr
esen
ce o
f SN
e Ia
in
evol
ved
gala
xies
, dom
i-na
ted
by o
ld lo
w m
ass
star
s, su
ppor
ts th
is p
ictu
re.
The
incr
ease
of S
Ne s
ampl
e and
the i
dent
ifica
tion
of th
eir h
ost g
alax
ies,
allo
ws
us t
o ch
arac
teriz
e th
e oc
curr
ence
s of
SN
e Ia
with
the
ste
llar
activ
ity o
f the
ir ho
sts.
By
usin
g SN
LS d
ata,
Sul
livan
et al
. (20
06)
have
con
firm
ed r
ecen
t cl
aim
s th
at t
he r
ate
of S
Ne
Ia d
epen
dsst
rong
ly o
n th
e ga
laxy
type
s. A
n in
crea
se o
f a fa
ctor
10
of t
hem
ass
norm
aliz
ed S
N I
a ra
te f
rom
pas
sive
gal
axy
to a
ctiv
e st
ar-
form
ing
gala
xies
is
obse
rved
(as
illu
stra
ted
in F
ig 2
, bo
ttom
pane
ls).
Pritc
het e
t al.
(200
8) h
ave
mod
eled
the
WD
form
atio
n ra
te fo
r a la
rge
varie
ty o
f gal
axy
activ
ities
and
foun
dth
at t
he W
D r
ate
mat
ches
the
SN
e Ia
rat
e if
an e
ffic
ienc
y (W
D e
xplo
ding
as
SN I
a) o
f 1%
is
assu
med
,in
depe
nden
tly o
f the
gal
axy
star
form
atio
n hi
stor
y.
Sinc
e lo
w m
ass
prog
enito
rs a
re e
xpec
ted
to h
ave
low
erco
nver
sion
eff
icie
ncie
s th
an h
igh-
mas
s pr
ogen
itors
, th
e st
anda
rd p
roge
nito
r sc
enar
io o
f on
e W
D w
ith a
nev
olvi
ng b
inar
y co
mpa
nion
will
be
less
eff
icie
nt w
hen
dom
inat
ed b
y lo
w m
ass
star
sys
tem
s as
in t
he c
ase
ofev
olve
d ga
laxi
es. T
here
fore
oth
er p
roge
nito
r sce
nario
s are
requ
ired
to re
prod
uce
the
cons
tant
eff
icie
ncy
of 1
%ov
er a
ll ga
laxy
type
s.
Fig
1 (L
eft)
68%
con
fiden
ce le
vels
���������
M) b
ased
on
2lig
ht c
urve
s fitt
ers (
red,
blue
) and
the
com
bina
-tio
n of
the
tw
o (th
ick
line)
. Ast
ier’
s re
sult
issh
own
as d
otte
d lin
e.Fr
om G
uy et
al.
(201
0).
Fig
1 (R
ight
)
Con
stra
int
on���
M)
assu
min
g a
fla
t un
i-ve
rse
and
incl
udin
g al
lth
e sy
stem
atic
s. Fr
omC
onle
y et
al.
(201
1).
Fig
268
% c
onfid
ence
leve
ls����������
M) b
ased
on
2lig
ht c
urve
s fit
ters
(re
d,bl
ue)
and
the
com
bina
-tio
n of
th
e tw
o (th
ick
line)
. A
stie
r’s r
esul
t is
show
n as
dot
ted
line.
From
Guy
et a
l. (2
010)
.
CFH
T A
nnua
l Rep
ort
15
The
rate
of S
Ne
core
col
laps
e
Usi
ng th
e 3yr
SN
LS sa
mpl
e, B
azin
et al
. (20
09) h
ave d
eter
min
ed th
e rat
e of c
ore c
olla
pse S
Ne a
t <z>
~0.3
. Thi
sra
te is
diff
icul
t to
mea
sure
due
to th
eir f
aint
mag
nitu
de d
istri
butio
n, 1
.5 m
ag fa
inte
r tha
n th
eir s
iste
rs S
Ne
Ia.
The
auth
ors
used
a s
ampl
e of
SN
e de
tect
ed d
own
to i
~24,
and
cla
ssifi
ed t
hem
acc
ordi
ng t
o th
eir
dist
inct
ive
light
cur
ves b
y m
akin
g us
e of
the
pho-
tom
etric
reds
hift
mea
sure
d by
Ilbe
rt et
al (
2006
).Th
ey id
entif
ied
117
SNcc
with
z<0
.4 a
nd d
eriv
eda
SN
core
co
llaps
e ra
te
of
1.42
±0
.3
(sta
t)±0
.3(s
ys) 1
0-4 y
r-1h-1
Mpc
-3 ,w
hich
is a
fact
or 4
.5hi
gher
than
for S
N Ia
type
.
Sinc
e th
e pr
ogen
itors
of c
ore
colla
pse
supe
rnov
aear
e be
lieve
d to
be
shor
t-liv
ed m
assi
ve s
tars
, thi
sra
te m
ust r
efle
ct th
e re
dshi
ft ev
olut
ion
of th
e co
s-m
ic s
tar
form
atio
n ra
te. T
he c
urre
nt r
esul
t co
m-
bine
d w
ith p
revi
ous
stud
ies
show
s a
reds
hift
evol
utio
n in
goo
d ag
reem
ent
with
the
exp
ecte
dev
olut
ion
of th
e co
smic
SFR
in (1
+z)3.
6 .
Gal
axy
mer
ger r
ate
up to
z~1
.2
Gal
axy
inte
ract
ions
are
a n
at-
ural
ing
redi
ent
of t
he h
iera
r-ch
ical
ga
laxy
fo
rmat
ion
scen
ario
and
can
pla
y a
key
role
in
our
unde
rsta
ndin
g of
the
glob
al d
eclin
e of
the
star
form
atio
n ac
tivity
with
cos
-m
ic ti
me.
N
umer
ous
stud
ies
have
es
timat
ed
the
reds
hift
evol
utio
n of
the
mer
ger
rate
prov
idin
g hi
ghly
di
scre
pant
resu
lts f
rom
no
evol
utio
n to
stro
ng e
volu
tion
yiel
ding
to
an a
mbi
guou
s co
ntrib
utio
n of
the
mer
ger r
ate
in th
e de
clin
eof
the
SFR
.
The
disc
repa
ncy
refle
cts
mai
nly
the
dive
rse
defin
ition
sof
a m
erge
r sy
stem
and
the
adop
ted
mer
ger t
imes
cale
. By
usin
g th
e 4
CFH
TLS
deep
fiel
ds, B
ridge
et a
l. (2
010)
hav
e de
velo
ped
a ne
w c
lass
ifica
tion
of m
ajor
mer
gers
base
d on
the
pres
ence
of t
idal
tails
and
brid
ges (
a cl
ear s
igna
ture
of i
nter
actio
n), w
hich
exp
loits
the
low
surf
ace
brig
htne
ss re
ache
d by
the
i ban
d C
FHTL
S da
ta. T
hey
iden
tifie
d a
tota
l of 1
600
mer
ging
gal
axie
s up
to z
=1.2
.Th
e m
erge
r fr
actio
n in
crea
ses
from
4.3
% a
t z=
0.3
to 1
9% a
t z~
1, i
mpl
ying
an
evol
utio
n of
(1+
z)m
, w
ithm
=2.2
5±0.
24, s
trong
ly s
uppo
rtive
of
an e
volv
ing
frac
tion
of th
e ga
laxy
mer
gers
with
tim
e.
By
split
ting
inst
ella
r mas
s, th
ey fo
und
an h
ighe
r mer
ger f
ract
ion
for l
ess
mas
sive
gal
axie
s (M
~1010
Mo)
, con
sist
ent w
ith th
ega
laxy
ass
embl
y do
wns
izin
g pi
ctur
e. F
inal
ly th
ey fo
und
that
inte
ract
ing
gala
xies
hav
e SF
R tw
ice
high
er th
anno
n in
tera
ctin
g fie
ld g
alax
ies,
sugg
estin
g th
at th
e de
clin
e of
the
mer
ger r
ate
is o
ne o
f the
con
tribu
tors
to th
ede
clin
e of
the
SFR
.
Fig
3Th
e m
easu
red
rate
of
SN
cor
e-co
llaps
e as
afu
nctio
n of
reds
hift.
The
solid
line
sho
ws
anev
olut
ion
prop
ortio
nal
to th
e ev
olut
ion
of th
eco
smic
SFR
. (fro
m B
a-zi
n et
al.,
200
9).
Fig
4E
volu
tion
of th
e M
erge
rra
te a
s a
func
tion
ofre
dshi
ft fo
r gal
axy
with
M>1
09.5
Mo
(b
lack
squa
res)
. Fr
om B
ridge
et a
l. (2
010)
.
2620
09 &
201
0
surv
eys
to id
entif
y th
e tru
e pl
anet
s am
ong
the
cand
idat
es th
ey w
illdi
scov
er.
The
seco
nd m
ain
goal
is to
exp
lore
the
impa
ct o
f mag
netic
fiel
ds o
nst
ar a
nd p
lane
t fo
rmat
ion,
by
dete
ctin
g m
agne
tic f
ield
s of
var
ious
type
s of
you
ng s
tella
r ob
ject
s (e
.g.
youn
g FU
Or-
like
prot
oste
llar
accr
etio
n di
scs,
clas
sica
l T T
auri
star
s) a
nd b
y ch
arac
teriz
ing
thei
rla
rge-
scal
e to
polo
gies
. SP
IRou
will
als
o in
vest
igat
e th
e po
tent
ial
pres
ence
of g
iant
pla
nets
in th
e in
ner r
egio
ns o
f pro
tost
ella
r acc
retio
ndi
scs
and
thei
r re
latio
n w
ith d
isc
mag
netic
fie
lds.
Such
stu
dies
will
stro
ngly
am
plify
the
initi
al e
xplo
ratio
n su
rvey
pre
sent
ly c
arrie
d ou
tin
the
visi
ble
by th
e M
aPP
(Mag
netic
Pro
tost
ars
and
Plan
ets)
CFH
TLa
rge
Prog
ram
(LP
) . I
t will
als
o id
eally
com
plem
ent t
he d
ata
that
ALM
A w
ill st
art c
olle
ctin
g so
on o
n ou
ter a
ccre
tion
disc
s and
den
se p
re-s
tella
r cor
es.
SPIR
ou w
ill a
lso
be a
ble
to ta
ckle
man
y ot
her e
xciti
ng re
sear
ch to
pics
in s
tella
r phy
sics
(e.g
. dyn
amo
of fu
llyco
nvec
tive
star
s, w
eath
er p
atte
rns
at t
he s
urfa
ces
of b
row
n dw
arfs
), in
pla
neta
ry p
hysi
cs (
e.g.
win
ds a
ndch
emis
try o
f sol
ar-s
yste
m p
lane
t atm
osph
eres
) gal
actic
phy
sics
(e.g
. ste
llar a
rche
olog
y) as
wel
l as i
n ex
traga
lac-
tic a
stro
nom
y.
`IM
AK
AFo
llow
ing
a se
ries o
f hig
hly
succ
essf
ul w
ide-
field
imag
ers,
`IM
AK
A is
pro
posi
ng a
n in
stru
men
t whi
ch w
ill n
otco
mpe
te w
ith th
e ne
w g
ener
atio
n of
imag
ers l
ike
Hyp
er-S
uprim
e-C
am, t
he D
ark
Ener
gy C
amer
a, o
r ulti
mat
ely
LSST
in te
rm o
f fie
ld si
ze. I
nste
ad, i
t will
focu
s on
one
of th
e un
ique
cha
ract
eris
tics o
f the
sky
over
Mau
nake
a:its
turb
ulen
ce p
rofil
e, p
artic
ular
ly su
ited
to G
roun
d La
yer A
dapt
ive
Opt
ics a
pplic
atio
ns. T
he b
est i
mag
e qu
ality
on a
wid
e-fie
ld o
f vie
w is
the
mai
n dr
iver
for ‘
IMA
KA
.
The
scie
nce
requ
irem
ents
of `
IMA
KA
inde
ed re
flect
this
driv
er:
• Fie
ld o
f Vie
w a
s lar
ge a
s pos
sibl
e, w
ith a
goa
l of 1
º dia
met
er• I
mag
e R
esol
utio
n 0.
3 h
(med
ian
seei
ng, r
-ban
d)• S
ensi
tivity
/Lim
iting
Mag
nitu
de•�
mag
� 1
over
Meg
aCam
at a
ll w
avel
engt
hs (m
edia
n se
eing
)• S
pect
ral C
over
age/
Res
olut
ion
[340
nm-1
100n
m] (
at le
ast g
rizY
)
In o
rder
to m
eet t
hese
requ
irem
ents
, `IM
AK
A w
ill b
enef
it fr
om th
eim
prov
emen
ts b
roug
ht b
y th
e Dom
e Ven
ting
Proj
ect (
see n
ext p
age)
and
from
a n
ovel
app
roac
h br
ingi
ng to
geth
er G
LAO
and
OTC
CD
s(o
rthog
onal
tra
nsfe
r C
CD
s).
The
GLA
O c
ompo
nent
will
hav
e~2
0x20
act
uato
rs, u
sing
~6
NG
S (n
atur
al g
uide
sta
rs)
on a
bout
1º
diam
eter
fiel
d, y
ield
ing
a sk
y co
vera
ge >
95%
ulti
mat
ely
limite
d by
free
-see
ing.
On
the
OTC
CD
sid
e, 1
00-1
50 T
ip/T
ilt n
atur
al g
uide
star
s of
mag
nitu
de r<
~14.
5 (s
ky c
over
age
~ 50
% a
t the
NG
P) w
illbe
use
d. T
he sp
ectra
l cov
erag
e w
ill b
e [4
00-1
10nm
].
Tech
nica
l cha
lleng
es a
re n
umer
ous
for
this
pro
ject
: the
siz
e of
the
optic
s m
akes
the
inst
rum
ent b
ut b
ig a
ndhe
avy
for a
prim
e-fo
cus s
etup
, and
wou
ld re
quire
impo
rtant
cha
nges
at t
he C
asse
grai
n fo
cus.
The
iden
tific
atio
nof
an
optic
al d
esig
n pr
ovid
ing
in th
e re
al w
orld
the
requ
ired
perf
orm
ance
s is
not
cle
ar e
ither
. All
thes
e is
sues
will
hav
e to
be
addr
esse
d ul
timat
ely
in a
Pha
se A
if th
e pr
ojec
t mov
es a
head
in m
id 2
011.
Scie
nce
goal
s ar
e nu
mer
ous,
but s
ome
coul
d be
cha
lleng
ed b
y th
e ch
arac
teris
tics
of th
e PS
F (p
oint
spr
ead
func
tion)
del
iver
ed b
y th
e G
LAO
cor
rect
ions
and
by
its c
hang
ing
natu
re w
ith th
e lo
catio
n of
the
guid
es s
tars
diff
eren
t fro
m a
fiel
d to
ano
ther
. At t
his
poin
t, it
seem
s po
ssib
le to
add
ress
thes
e is
sues
but
mor
e si
mul
atio
nw
ork
is n
eede
d, h
elpe
d by
on-
site
GLA
O te
sts.
Ass
umin
g a
reso
lutio
n of
0.3
” in
r (f
ull-w
idth
hal
f-m
ax) u
nder
med
ian
seei
ng c
ondi
tions
, a d
epth
of r
= 2
6.5
can
be re
ache
d in
1 h
our (
5 ),
and
a fie
ld o
f at l
east
0.6
squ
are
degr
ee, `
IMA
KA
wou
ld b
e in
stru
men
tal t
o th
e fu
ture
of C
FHT
rese
arch
ion
the
Kui
per B
elt
as w
ell a
s to
a w
ide
rang
e of
app
licat
ions
such
as r
esol
ved
stel
lar p
opul
atio
ns, g
alax
y fo
rmat
ion,
or c
osm
olog
y. D
etai
led
dyna
mic
alst
udie
s in
glo
bula
r cl
uste
rs c
ould
inc
lude
sea
rch
for
inte
rmed
iate
mas
s bl
ack
hole
s, dy
nam
ical
sig
natu
rem
etal
licity
var
iatio
ns, s
tella
r orb
its an
d ev
apor
atio
n ra
te. S
imila
r stu
dies
in o
pen
clus
ters
coul
d al
low
to se
para
tecl
uste
r fr
om f
ield
, br
ingi
ng i
nfor
mat
ion
on a
ges
and
star
for
mat
ion
hist
ory,
and
tac
kle
prob
lem
s lik
e th
eun
iver
salit
y of
the
IMF,
its
rela
tions
hip
with
met
allic
ity. B
eyon
d ou
r G
alax
y, `
IMA
KA
cou
ld o
bser
ve R
edG
iant
s out
to 1
0 M
pc, l
ocat
ing
stel
lar s
tream
s, br
ingi
ng c
lues
to g
alax
y fo
rmat
ion
and
test
the�C
DM
mod
el.
Pola
rimet
ric m
odul
eba
selin
e de
sign
The
desi
gn fo
llow
s th
eco
ncep
t suc
cess
fully
used
for E
SP
aDO
nS.
How
goo
d an
IQ?
Pre
limin
ary
sim
ula-
tions
of `
IMA
KA
imag
equ
ality
pro
babi
lity
dist
ribut
ion
CFH
T A
nnua
l Rep
ort
25
SITE
LLE
SITE
LLE
is a
n im
agin
g FT
S (F
ourie
r Tr
ansf
orm
Spe
ctro
grap
h) b
ased
on
the
sam
e co
ncep
t as
SpIO
MM
, an
inst
rum
ent
inst
alle
d on
the
Mon
t M
égan
tic t
eles
cope
. Th
e fig
ures
on
the
right
out
line
the
desi
gn o
f th
ein
stru
men
t: at
its
core
is a
n in
terf
erom
eter
with
a f
rictio
n-le
ss s
can
and
tip-ti
lt m
echa
nism
bas
ed o
n fo
rmer
Mar
s-m
issi
on in
stru
men
t des
ign
mad
e by
AB
B-B
aum
en, w
hich
is th
e m
ain
SITE
LLE
cont
ract
or.
SITE
LLE
scie
nce
goal
s co
ver a
wid
e ra
nge
of fi
elds
, tha
nks
to th
e si
ze o
f its
fiel
d (1
2’x1
2’),
its w
ide
spec
tral
cove
rage
[35
0nm
-900
nm],
good
spa
tial
imag
e sa
mpl
ing
(035
”/pi
xel),
and
spe
ctra
l re
solu
tion
(fro
m 1
to
~20,
000)
. Am
ong
the
man
y to
pics
its s
cien
ce c
ase
addr
ess,
one
can
cite
:• G
alac
tic n
ebul
ae a
roun
d ev
olve
d st
ars (
PN, W
R, L
BV
s)• G
alac
tic H
II re
gion
s: te
mpe
ratu
re fl
uctu
atio
ns, i
nter
nal s
truct
ure,
loca
l enr
ichm
ent,
…• A
bund
ance
dis
tribu
tion
in n
earb
y sp
iral g
alax
ies
• Sta
r-fo
rmat
ion
rate
at d
iffer
ent r
eshi
fts• L
yman
-����������
Com
pare
d to
SpI
OM
M a
t Mon
t Még
antic
, SIT
ELLE
at C
FHT
will
be
65 (
15)
times
bet
ter
at 3
70nm
(65
0)re
spec
tivel
y.
SPIR
ouSP
IRou
, an
nea
r-in
frar
ed s
pect
ro-p
olar
imet
er,
was
pro
pose
d by
Jea
n-Fr
anço
is D
onat
i(I
RA
P, T
oulo
use)
. It i
s a n
atur
al ex
tens
ion
of th
e vis
ible
spec
tro-p
olar
imet
ESP
aDO
nS to
the
near
-IR
. ESP
aDO
nS is
cur
rent
ly o
ne o
f the
thre
e m
ain
CFH
T in
stru
men
ts, u
sed
for t
wo
very
succ
essf
ul L
arge
Pro
gram
s as
wel
l as
by m
any
PIs.
SPIR
ou w
ill b
e un
ique
not
onl
y as
IRsp
ectro
-pol
arim
eter
; it w
ill a
lso
offe
r the
pos
sibi
lity
of m
easu
ring
radi
al v
eloc
ity a
ccur
acy,
open
ing
the
poss
ibili
ty o
f Ear
th-s
ize
extra
sola
r pla
nets
aro
und
M-d
war
f sta
rs.
The
scie
nce
requ
irem
ents
of t
he in
stru
men
ts, a
t the
end
of t
he P
hase
A a
reas
follo
win
g:•
Spec
tral
dom
ain:
0.9
8-2.
4μm
(w
/ fu
ll co
vera
ge u
p to
at
leas
t 2μ
m)
spec
tral r
esol
utio
n >
50,0
00 (7
0,00
0 if
poss
ible
)• R
adia
l vel
ocity
acc
urac
y <
1m/s
• S/N
=150
per
3km
/s p
ixel
in 1
hr @
J=12
& K
=11
• Th
erm
al in
stru
men
t bac
kgro
und
< sk
y ba
ckgr
ound
, ie
J>15
.5, H
>13.
5,K
>13.
0• A
ll po
lariz
atio
n st
ates
acc
essi
ble
with
>99
% e
ffic
ienc
y an
d <1
% c
ross
talk
over
full
spec
tral d
omai
n
SPIR
ou p
lans
to e
ssen
tially
con
cent
rate
on
two
mai
n sc
ient
ific
goal
s. Th
efir
st o
ne i
s to
sea
rch
for
and
char
acte
rize
habi
tabl
e ex
o-Ea
rths
orbi
ting
low
-mas
s an
d ve
ry l
ow m
ass
star
s us
ing
high
-pre
cisi
on r
adia
l ve
loci
tysp
ectro
scop
ic m
easu
rem
ents
. Thi
s sea
rch
will
exp
and
the
initi
al, e
xplo
rato
-ry
stud
ies b
eing
car
ried
out n
ow w
ith v
isib
le in
stru
men
ts a
nd w
ill su
rvey
inpa
rticu
lar l
arge
sam
ples
of s
tars
(e.g
. lat
e-M
dw
arfs
) out
of r
each
of e
xist
ing
inst
rum
ents
. SPI
Rou
will
als
o w
ork
in c
lose
col
labo
ratio
n w
ith s
pace
- and
gro
und-
bas
ed p
hoto
met
ric tr
ansi
t
SITE
LLE
Prel
imin
ary
Des
ign
On
the
left,
the
over
all
inst
rum
ent,
as it
will
be
mou
nted
on
the
Cas
segr
ain
bonn
ette
.
On
the
right
, the
inte
r-fe
rom
eter
and
the
two
cam
era
ports
.
SPIR
ou s
pect
rogr
ahpr
elim
inar
y de
sign
© E
ditio
ns D
upui
s
1620
09 &
201
0
Gal
axy
stru
ctur
es in
the
CFH
TLS
Clu
ster
’s c
ount
s is a
n al
tern
ativ
e m
etho
d to
con
stra
in th
e co
smol
ogic
al p
aram
eter
s but
has
bee
n la
rgel
y lim
ited
by e
ither
a s
mal
l red
shift
regi
me
or a
sm
all a
rea.
The
CFH
TLS
prov
ides
a m
ajor
ste
p fo
rwar
d to
con
tribu
te in
this
dom
ain.
By
usin
g th
e C
FHTL
S-T0
004
data
rele
ase,
Ada
mi e
t al (
2010
) hav
e an
alyz
ed 2
.5 d
eg2 i
n th
e C
FHTL
S D
eep
and
28 d
eg2 i
n th
e C
FHTL
S W
ide
field
tode
tect
mas
sive
stru
ctur
es u
p to
reds
hift
z~1.
5 - 1
.2. T
hey
mak
e us
e of
the
pho-
tom
etric
re
dshi
fts
from
Ilb
ert
el
al(2
006)
and
Cou
pon
et al
(200
9) d
own
toi=
25 a
nd 2
3 re
spec
tivel
y.
They
con
-st
ruct
edth
e ga
laxy
den
sity
map
s in
narr
ow
phot
omet
ric
reds
hift
slic
es���������������������� �� �������!���"
ous d
etec
tion
thre
shol
d (s
ee F
ig b
elow
).Th
ey e
nd u
p w
ith a
list
of 1
200
cand
i-da
tes c
lust
ers i
ncre
asin
g by
a si
gnifi
cant
num
ber p
revi
ous c
lust
er d
etec
tions
.
In o
rder
to
asse
ss t
he v
alid
ity o
f th
eir
dete
ctio
n ra
tes,
they
hav
e te
sted
the
irm
etho
d ag
ains
t the
Mill
enni
um s
imul
a-tio
n an
d th
ey a
lso
perf
orm
ed a
clu
ster
-in
g an
alys
is w
hich
app
ears
con
sist
ent
with
hig
h re
dshi
ft cl
uste
rs m
easu
re-
men
ts. T
hese
res
ults
rep
rese
nt th
e fir
stst
ep o
f thi
s ana
lysi
s. A
val
idat
ion
and
anac
cura
te m
ass
dete
rmin
atio
n ar
e no
wre
quire
d to
pro
vide
cos
mol
ogic
al c
on-
stra
ints
.
Fig
5 E
xam
ple
of t
wo
clus
-te
r de
tect
ions
with
S/N
~6 i
n th
e de
nsity
map
of t
he C
FHTL
S-D
2at
z~0
.65-
0.75
. Fro
mA
dam
i et a
l . (2
010)
.
`OH
AN
A-`
Iki
`OH
AN
A-`
Iki i
s a
pair
of tw
o sm
all t
eles
cope
s (o
ne th
em is
sho
wn
on th
erig
ht)
used
to
feed
the
OH
AN
A f
iber
s to
tes
t th
e be
am-c
ombi
ning
and
frin
ge tr
acki
ng a
bilit
y of
the
OH
AN
A d
elay
-line
and
bea
m c
ombi
ner p
rior
to c
omm
issi
onin
g w
ith th
e C
FHT
and
Gem
ini t
eles
cope
s. Fo
llow
ing
the
com
plet
ion
of th
e de
lay-
line
inst
alla
tion
and
in in
itial
test
ing
in th
e sp
ring
of 2
009,
eff
orts
of
the
OH
AN
A te
am f
or th
e re
st o
f 20
09 a
nd 2
010
have
been
aim
ed at
obt
aini
ng in
tern
al fr
inge
s with
the 3
00 m
inte
rfer
omet
er in
put
fiber
s and
then
to o
btai
n fr
inge
s on-
sky
with
the
`OH
AN
A-`
Iki t
eles
cope
s.
Inte
rnal
frin
ges
with
the
inte
rfer
omet
er s
et u
p w
ere
first
obt
aine
d in
Apr
il20
10 u
sing
the
shor
t (10
m)
J-ba
nd f
iber
s. V
ibra
tion
of th
e fib
ers
was
apr
oble
m, p
artic
ular
ly w
ith th
e m
ulti-
pass
set
up re
quire
d fo
r aut
o-co
llim
a-tio
n fr
inge
s.
At
the
end
ofA
pril
2010
, the
seco
nd `
OH
A-
NA
-`Ik
i te
lesc
ope
was
com
mis
sion
ed. D
urin
g th
eJu
ne ru
n at
tem
pts w
ere
mad
e to
obt
ain
frin
ges w
ithth
e `O
HA
NA
-`Ik
i te
lesc
opes
on
the
star
Ant
ares
.Fr
inge
s on
-sky
wer
e ob
tain
ed a
t th
e en
d of
Jun
eal
thou
gh th
e fib
er in
ject
ion
was
sub-
optim
al an
d th
efr
inge
s w
ere
very
noi
sy.
Cha
sing
vib
ratio
ns a
ndm
ore
obse
rvat
ions
are
sche
dule
d fo
r 201
1.
`OH
AN
A-`I
kiD
iffer
ence
in th
e si
gnal
betw
een
the
two
re-
com
bina
tion
path
s of
the
inte
rfero
met
er o
nth
e st
ar A
ntar
es in
J-
band
.
CFH
T A
nnua
l Rep
ort
17
Cos
mol
ogy
Com
ing
Clo
ser
Alan
W. M
cCon
nach
ie a
nd T
he P
an-A
ndro
med
a Ar
chae
olog
ical
Sur
vey
A m
atte
r of
sca
leW
hen
astro
nom
ers
thin
k “c
osm
olog
y”, t
he A
ndro
med
a G
alax
y (M
31) p
roba
bly
isn’
t at t
he to
p of
the
list o
fob
ject
s the
y ar
e th
inki
ng a
bout
. Rat
her,
high
reds
hift
gala
xies
, the
cos
mic
mic
row
ave
back
grou
nd, l
arge
-sca
lest
ruct
ures
, sup
erno
vae
expl
osio
ns in
dis
tant
gal
axie
s…th
e lis
t con
tinue
s. O
n th
ese
larg
est s
cale
s, th
e su
cces
s of
the p
reva
iling
cosm
olog
ical
par
adig
m -
Lam
bda-
Col
d D
ark
Mat
ter (#
CD
M)
- is
impr
essi
ve, a
nd is
now
pos
ing
fasc
inat
ing
ques
tions
rega
rdin
g th
e na
ture
of d
ark
mat
ter a
nd d
ark
ener
gy. T
he d
evel
opm
ent o
f an
appa
rent
lyro
bust
mod
el fo
r the
bro
ad ev
olut
ion
of th
e Uni
vers
e mea
ns at
tent
ion
is n
ow sh
iftin
g to
how
bar
yoni
c stru
ctur
es–
star
s an
d ga
laxi
es –
form
with
in th
at m
odel
. And
a d
etai
led
mod
el o
f how
indi
vidu
al g
alax
ies
form
requ
ires
a de
taile
d un
ders
tand
ing
of th
e st
ruct
ure
and
cont
ent o
f ind
ivid
ual g
alax
ies…
A p
re-h
isto
ry“N
ear-
field
cos
mol
ogy”
is n
ot, d
espi
te c
laim
s to
the
cont
rary
, a n
ew fi
eld,
but
rath
er th
e re
-em
erge
nce
of a
fiel
dth
at fo
r a lo
ng ti
me
form
ed th
e ba
sis o
f ga
laxy
form
atio
n an
d ev
olut
ion.
Tw
o cl
assi
c pa
pers
in th
e Si
xtie
s and
Seve
ntie
s pr
ovid
ed, w
ith s
pect
acul
ar s
ucce
ss,
exac
tly th
e ty
pe o
f res
ult t
hat m
oder
n-da
y ne
ar-f
ield
cos
mol
o-gi
sts d
ream
of.
Olin
Egg
en, D
onal
d Ly
nden
-Bel
l and
Ala
n Sa
ndag
e, in
196
2, n
otic
ed th
at 2
21st
ars i
n th
e so
lar
neig
hbor
hood
exh
ibite
d a
corr
elat
ion
betw
een
thei
r dy
nam
ical
and
che
mic
al p
rope
rties
. Fr
om t
his,
they
deve
lope
d a
mod
el fo
r the
form
atio
n of
the
Gal
axy
from
a c
olla
psin
g ga
s-cl
oud
that
suc
cess
fully
repr
oduc
edth
e ob
serv
ed c
hem
o-dy
nam
ical
cor
rela
tions
. Som
e 16
yea
rs la
ter,
Leon
ard
Sear
le a
nd R
ober
t Zin
n pr
esen
ted
an a
naly
sis
of th
e st
ella
r po
pula
tions
of
Gal
actic
glo
bula
r cl
uste
rs, w
here
they
sho
wed
that
the
mos
t dis
tant
clus
ters
wer
e co
nsis
tent
with
exh
ibiti
ng a
bro
ad r
ange
in
ages
, in
con
trast
to
thei
r m
ore
tight
ly b
ound
coun
terp
arts
. Fro
m th
is, t
hey
sugg
este
d th
at th
ese o
uter
clus
ters
had
bee
n ac
cret
ed in
to th
e Gal
axy
from
exte
rnal
syst
ems o
ver a
n ex
tend
ed p
erio
d of
tim
e. N
owad
ays,
both
the
colla
pse
mod
el a
nd th
e ac
cret
ion
mod
el a
re k
eyco
mpo
nent
s of g
alax
y fo
rmat
ion
theo
ry.
Too
ls o
f the
trad
eW
hile
par
t of t
he re
ason
that
nea
r fie
ld c
osm
olog
y ha
s bee
n re
born
can
be
trace
d to
adv
ance
s in
our c
osm
olog
-ic
al u
nder
stan
ding
(and
per
haps
app
reci
atio
n) o
f gal
axie
s, th
at is
but
hal
f of t
he s
tory
. The
big
ger h
alf r
elat
esto
our
obs
erva
tiona
l cap
abili
ties.
Gal
axie
s ar
e bi
g, w
hich
mea
ns n
earb
y ga
laxi
es a
re b
ig in
an
appa
rent
sen
seto
o. S
o fie
lds
of v
iew
bec
ome
very
impo
rtant
. A c
ompr
ehen
sive
vie
w o
f our
ow
n G
alax
y re
quire
s su
rvey
ing
the
entir
e sk
y; th
e fa
mou
s di
sk o
f the
And
rom
eda
gala
xy s
pans
mor
e th
an fo
ur ti
mes
the
diam
eter
of t
he fu
llM
oon;
eve
n a
dwar
f gal
axy
like
Forn
ax o
r Scu
lpto
r is o
f the
sam
e ap
pare
nt si
ze –
if n
ot b
igge
r! –
than
the
full
Moo
n. B
ut c
ombi
ne th
eir s
ize
with
the
fact
sta
rs in
oth
er g
alax
ies
(or t
he o
uter
par
ts o
f our
Gal
axy)
are
fain
t,an
d yo
u co
me
up w
ith th
e ne
ed fo
r a te
lesc
ope
with
a la
rge
aper
ture
and
a b
ig fi
eld
of v
iew
.
Ente
r the
Can
ada-
Fran
ce-H
awai
i tel
esco
pe.
PAnd
AS
A n
atur
al c
onse
quen
ce o
f gal
axy
form
atio
n in
the
hier
arch
ical#
CD
M p
arad
igm
is th
at a
typi
cal g
alax
y lik
e th
eM
ilky
Way
or A
ndro
med
a w
ill a
ccre
te h
undr
eds o
f sm
alle
r dar
k m
atte
r clu
mps
, aki
n to
the
idea
s pro
pose
d by
Sear
le a
nd Z
inn.
Not
all
thes
e cl
umps
are
exp
ecte
d to
con
tain
star
s, bu
t tho
se th
at d
o w
ill d
epos
it th
ose
star
s in
the
surr
ound
ings
of t
he g
alax
y, p
rodu
cing
pot
entia
lly th
e en
tire
stel
lar h
alo
of th
e ga
laxy
. Dyn
amic
al ti
mes
inth
e ou
ter h
alo
are
long
, and
man
y ac
cret
ed su
bstru
ctur
es w
ill su
rviv
e to
the
pres
ent w
ithou
t bei
ng to
tally
tida
llydi
srup
ted.
The
ir nu
mbe
r, sp
atia
l dis
tribu
tion
and
mor
phol
ogy
prov
ides
test
s of
stru
ctur
e fo
rmat
ion
on s
mal
lsc
ales
; the
met
al-c
onte
nt a
nd a
ges o
f the
ir st
ella
r pop
ulat
ions
reve
al h
ow st
ar fo
rmat
ion
proc
eeds
at e
arly
tim
esan
d in
the
leas
t lum
inou
s gal
axie
s in
the
Uni
vers
e. In
shor
t, on
e can
dec
onst
ruct
a ga
laxy
on
a sta
r-by
-sta
r bas
is,
and
so re
cons
truct
its f
orm
atio
n.
The
Pan-
And
rom
eda
Arc
haeo
logi
cal S
urve
y –
one
of th
e la
rge
prog
ram
s th
at h
as ju
st c
ompl
eted
its
prim
ary
obse
rvat
ions
on
the
CFH
T -
is d
esig
ned
to s
earc
h fo
r the
se “
relic
s” o
f the
gal
axy
form
atio
n pr
oces
s - f
ossi
l
2420
09 &
201
0
New
Inst
rum
ents
Two
year
s of
dev
elop
men
t in
a nu
tshe
llFo
llow
ing
the
call
for
idea
s fo
r ne
w in
stru
men
ts f
or 2
013
and
beyo
nd, t
he s
ubm
issi
on o
f fo
ur c
once
pts
ofin
stru
men
ts a
nd t
heir
revi
ew b
y C
FHT
and
its S
cien
tific
Adv
isor
y C
ounc
il (S
AC
), th
e B
oard
of
Dire
ctor
sde
cide
d at
its 2
008
fall
mee
ting
to m
ove
one
inst
rum
ent,
SPIR
ou, t
o a
Phas
e A
stud
y to
be
com
plet
ed m
id-2
01an
d to
sup
port
furth
er s
tudi
es o
n th
e `I
MA
KA
con
cept
. The
pro
pose
rs o
f a th
ird in
stru
men
t, SI
TELL
E, w
ere
enco
urag
ed to
seek
app
ropr
iate
fund
ing
and
deve
lop
SITE
LLE
as g
uest
inst
rum
ent i
n co
llabo
ratio
n w
ith C
FHT
staf
f. A
four
th in
stru
men
t, G
YES
, joi
ned
the
gam
e at
the
end
of 2
009,
dec
idin
g to
pre
pare
a P
hase
A st
udy
afte
rin
itiat
ing
cont
act w
ith C
FHT
early
that
yea
r. A
fter
revi
sing
the
Phas
e A
sch
edul
e fo
r bo
th p
roje
cts,
revi
ewpr
ojec
ts w
ere
held
for
bot
h G
YES
and
SPI
Rou
at
CFH
T in
Oct
ober
201
0, w
ith t
he a
ssis
tanc
e of
ext
erna
lre
view
ers.
The
revi
ew c
omm
ittee
s co
nclu
ded
in b
oth
case
s th
at th
e in
stru
men
t con
cept
s w
ere
very
inte
rest
ing
as w
ell a
s qu
ite c
halle
ngin
g. I
n sp
ite o
f th
eir
Phas
e A
not
bei
ng f
ully
com
plet
ed, G
YES
and
SPI
Rou
wer
eco
nsid
ered
stud
ied
wel
l eno
ugh
to m
ove
ahea
d. C
lear
adv
ice
and
guid
ance
on
step
s to
be ta
ken
prio
r to
the
real
star
t of a
Pha
se B
wer
e al
so g
iven
by
the
revi
ewer
s. It
was
then
up
to th
e Sc
ient
ific
Adv
isor
y C
omm
ittee
whi
chfo
llow
ed im
med
iate
ly th
e U
sers
’ Mee
ting
to c
hoos
e be
twee
n th
em. S
AC
reco
mm
ende
d to
the
Boa
rd to
favo
rSP
IRou
ove
r G
YES
, a r
ecom
men
datio
n th
e B
oard
end
orse
d. S
PIR
ou w
ill m
ove
to P
hase
B in
201
1, a
fter
am
anda
tory
reor
gani
zatio
n of
its M
anag
emen
t Pla
n.
Mea
nwhi
le, t
he C
anad
ian
SITE
LLE
team
mov
ed fo
rwar
d fu
ndin
g-w
ise,
as r
eque
sted
by
the
Boa
rd a
t the
end
of
2008
, sec
urin
g th
e fu
ndin
g of
the
inst
rum
ent t
hrou
gh a
CFI
gra
nt. C
FHT
help
ed a
n ea
rly st
art o
f the
pro
ject
by
prov
idin
g se
ed f
undi
ng w
hile
Uni
vers
ité L
aval
aw
aite
d th
e av
aila
bilit
y of
CFI
fun
ding
, ena
blin
g th
e m
ain
cont
ract
or fo
r the
inst
rum
ent,
AB
B-B
aum
en, t
o m
ove
forw
ard.
Follo
win
g a
first
feas
ibili
ty st
udy
repo
rt pr
esen
ted
to S
AC
in M
ay 2
010,
the
`IM
AK
A te
am c
ontin
ued
to w
ork
and
mor
e si
mul
atio
n st
udie
s con
clud
ed th
at th
e pe
rfor
man
ces o
f the
inst
rum
ent w
ere
pote
ntia
lly n
ot a
s goo
d as
prev
ious
ly th
ough
t, le
adin
g to
a lo
w-k
ey p
rese
ntat
ion
at th
e U
sers
’ Mee
ting
and
mor
e w
ork
to b
e do
ne. T
heB
oard
ackn
owle
dged
the
situ
atio
n by
aski
ng fo
r a n
ew F
easi
bilit
y St
udy
Rep
ort t
o be
pre
sent
ed at
the M
ay 2
011
SAC
mee
ting.
GY
ESG
YES
was
pro
pose
d by
a te
am le
d at
Par
is O
bser
vato
ry (G
EPI)
by
Pier
carlo
Bon
ifaci
o. T
he in
stru
men
t is
a50
0-fib
ers
wid
e-fie
ld m
ulti-
obje
ct s
pect
rogr
aph
to b
e in
stal
led
at th
e pr
ime
focu
s of
CFH
T, u
sing
the
“old
”C
FHT
wid
e-fie
ld c
orre
ctor
whi
ch u
sed
to b
e in
the
prim
e-fo
cus
cage
and
fed
the
wid
e-fie
ld im
ager
s fr
om p
hoto
grap
hic
plat
es u
p to
CFH
12K
. It o
ffer
s a
reso
lutio
n of
arou
nd 3
0,00
0 in
two
spec
tral r
ange
s [39
0nm
-450
nm] a
nd [5
87nm
-673
nm].
The p
relim
-in
ary
desi
gn o
f the
fibe
r pos
ition
er is
bas
ed o
n th
e A
AO
2dF
pos
ition
er d
esig
n.
GY
ES m
ain
scie
ntifi
c go
als a
re re
late
d to
the
kine
mat
ic st
ruct
ure
and
chem
ical
labe
ling
of st
ars i
n ou
r Gal
axy,
par
tly a
s a fo
llow
-up
of th
e G
aia
mis
sion
:•
Thin
dis
c -
thic
k di
sc:
che
mic
al d
isse
ctio
n of
the
dis
c an
d id
entif
icat
ion
of s
ub-
stru
ctur
es, m
easu
re o
f the
leve
l of h
omog
enei
ty o
f the
elem
ents
in v
ario
us en
viro
nmen
ts(a
rms /
inte
r-ar
ms,
oute
r dis
c, b
ar, e
tc.),
int
erfa
ce o
f the
thic
k di
sk w
ith th
e th
in d
isc
atth
e m
etal
-ric
h en
d an
d th
e ha
lo o
n th
e m
etal
-poo
r sid
e.• B
ulge
: D
etai
led
anal
ysis
of t
he b
ulge
& c
onst
rain
ts o
n th
e bu
lge
form
atio
n sc
enar
ios,
unpr
eced
ente
d co
mbi
natio
n of
kin
emat
ics w
ith a
bund
ance
ratio
s ([�
/Fe]
)•
Hal
o: d
etai
led
abun
danc
e ra
tios
of m
ore
than
10,
000
halo
sta
rs a
nd c
hem
ical
evo
lutio
n of
the
early
gal
axy,
sear
ch fo
r ver
y-m
etal
-poo
r sta
rs w
ith [F
e/H
] <-4
Muc
h m
ore
can
be d
one
with
such
an
inst
rum
ent!
Her
e ar
e a
few
of t
he o
ther
app
licat
ions
of G
YES
:• H
ot S
tars
and
ISM
: B
/Be
star
s & A
/Ap
star
s and
map
ping
of t
he IS
M• P
ulsa
ting
Star
s: C
ephe
ids,
äScu
ti: P
-L re
latio
n an
d g
alac
tic g
radi
ents
• O
pen
Clu
ster
s (1
90 t
arge
ts f
or G
YES
): a
ge-m
etal
licity
rel
atio
n &
che
mic
al h
isto
ry o
f th
e th
in d
isk
and
chem
ical
cha
ract
eriz
atio
n of
new
OC
s ide
ntifi
ed b
y G
aia
• Glo
bula
r Clu
ster
s (49
targ
ets f
or G
YES
): in
tern
al d
ynam
ics &
mul
tiple
stel
lar p
opul
atio
ns id
entif
icat
ion
Spec
trog
raph
base
line
desi
gnTw
o A
rms
(blu
e an
dre
d) w
ith a
VP
H a
nd a
cam
eara
for e
ach.
CFH
T A
nnua
l Rep
ort
23
Que
ued
Serv
ice
Obs
ervi
ng a
t CFH
T: T
wo
year
s of
tran
sitio
nTh
e m
ain
goal
of t
he O
bser
vato
ry A
utom
atio
n Pr
ojec
t was
to b
ring
mod
ifica
tions
and
impr
ovem
ents
to C
FHT'
ssy
stem
s so
that
onl
y on
e per
son
coul
d op
erat
e the
tele
scop
e and
inst
rum
ent r
emot
ely
from
CFH
T's h
eadq
uarte
rsin
Wai
mea
.
Sinc
e its
firs
t lig
ht in
197
9, C
FHT
has
been
ope
ratin
g un
der t
he C
lass
ical
obs
ervi
ng m
ode.
Thi
s m
ode
is s
till
used
a fe
w n
ight
s per
yea
r. In
Cla
ssic
al o
bser
ving
mod
e fr
om th
e su
mm
it of
Mau
nake
a, tw
o pe
ople
are
requ
ired
to b
e pr
esen
t tog
ethe
r for
safe
ty re
ason
s. A
Tel
esco
pe O
pera
tor a
nd o
ne o
r mor
e vi
sitin
g as
trono
mer
s pe
rfor
mth
e ob
serv
atio
ns.
A l
ittle
ove
r 10
yea
rs a
go, o
n Ja
nuar
y 29
, 200
1, C
FHT
reac
hed
a m
ilest
one
with
its
firs
t Q
ueue
d Se
rvic
eO
bser
vatio
ns. U
nder
this
obs
ervi
ng m
ode,
the
Obs
ervi
ng A
ssis
tant
(O
A)
perf
orm
s th
e du
ties
of a
tele
scop
eop
erat
or w
hile
the
Serv
ice
Obs
erve
r (SO
), es
sent
ially
take
s the
role
of t
he v
isiti
ng a
stro
nom
er.
The
SOs a
re h
ired
and
train
ed b
y C
FHT
to o
pera
te in
stru
men
ts, d
eter
min
e w
hich
obs
erva
tion
to c
arry
out
bas
edon
prio
ritie
s and
sky
cond
ition
s, an
d pe
rfor
m th
e da
ta a
cqui
sitio
n an
d pr
elim
inar
y qu
ality
ass
essm
ent.
By
2008
,C
FHT
had
its th
ree m
ain
inst
rum
ents
ope
rate
d un
der t
he Q
SO m
ode.
CFH
T w
ill p
erfo
rm it
s firs
t rem
ote q
ueue
dse
rvic
e ob
serv
atio
ns i
n ea
rly 2
011,
with
no
pers
onne
l at
the
sum
mit
and
only
one
Rem
ote
Obs
erve
r (R
O)
perf
orm
ing
all
the
nece
ssar
y du
ties f
rom
the
CFH
T he
adqu
arte
rs in
Wai
mea
.
In o
rder
to e
nsur
e an
eff
icie
nt a
nd sm
ooth
tran
sitio
n fr
om a
2-p
erso
n on
-site
ope
ratio
n to
a si
ngle
-per
son
rem
ote
oper
atio
n, a
trai
ning
pro
gram
was
car
eful
ly d
esig
ned.
Afte
r def
inin
g th
e go
als
of th
e tra
inin
g, O
As
and
SOs
com
plet
ed m
odul
es c
over
ing
ever
y as
pect
of
tele
scop
e co
ntro
l, do
me
and
win
dscr
een
oper
atio
n, w
eath
erm
onito
ring,
inst
rum
ent f
unct
iona
lity
and
oper
atio
n, e
valu
atio
n of
scie
ntifi
c pr
ogra
ms,
astro
nom
ical
tech
niqu
es,
prin
cipl
es o
f QSO
as u
sed
at C
FHT,
dat
a qu
ality
eva
luat
ion,
etc
. Afte
r tw
o ye
ars,
four
can
dida
tes w
ere
hire
d as
CFH
T's R
emot
e O
bser
vers
.
In W
aim
ea
The
rem
ote
obse
rv-
ing
room
is r
eady
!Th
e en
viro
nmen
t is
very
sim
ilar
to th
esu
mm
it se
tup.
The
2-sc
reen
and
4-
scre
en p
anel
s on
the
left
take
car
e of
the
cont
rol o
f the
sum
mit
faci
lity
and
of th
e in
-st
rum
ent,
whi
le th
ene
xt tw
o sc
reen
s on
the
desk
are
use
d fo
rth
e co
ntro
l of t
he te
le-
scop
e.
At t
he s
umm
it
In t
he o
bser
ving
room
, the
left
desk
(2-
and
4-sc
reen
pan
els)
are
for t
he S
O, a
ndth
e rig
ht d
esk
is fo
rth
e O
A, o
pera
ting
the
tele
scop
e. T
he e
nvi-
ronm
ent h
as b
een
mod
ified
to h
andl
ere
mot
e op
erat
ions
:ha
nds
on m
ice
orke
yboa
rds
only
!
1820
09 &
201
0
sign
atur
es o
f th
e ch
emic
al a
nd d
ynam
ical
orig
ins
of s
tella
r po
pula
tions
pre
sent
in
the
obse
rved
pos
ition
s,ve
loci
ties a
nd c
olor
s of s
tars
- in
the
clos
est g
iant
gal
axy
to u
s, A
ndro
med
a.
And
rom
eda
is, i
n m
any
way
s, an
ide
al t
arge
t th
at n
eatly
com
plim
ents
sim
ilar
stud
ies
of o
ur o
wn
Gal
axy.
Whe
reas
the
prec
isio
n an
d de
tail
of o
bser
vatio
ns th
at c
an b
e ob
tain
ed fo
r the
Milk
y W
ay w
ill a
lway
s su
rpas
sth
ose
poss
ible
for e
xtra
-gal
actic
targ
ets,
a cl
ear p
anor
amic
vie
w is
una
ttain
able
due
to o
ur a
wkw
ard
view
ing
angl
e, e
xtin
ctio
n, c
row
ding
, and
the
vast
are
a th
at m
ust b
e su
rvey
ed. N
o su
ch p
robl
ems
exis
t for
And
rom
eda,
and
indi
vidu
al st
ars c
an st
ill b
e re
solv
ed a
nd a
naly
zed,
alb
eit a
t a lo
wer
sign
al-to
-noi
se.
PAnd
AS
has o
bser
ved
near
ly 4
00 sq
uare
deg
rees
of s
ky in
the v
icin
ity o
f the
And
rom
eda G
alax
y, an
d its
nea
rby
neig
hbor
, the
Tria
ngul
um G
alax
y (s
epar
ated
by
15 d
egre
es in
pro
ject
ion,
or a
bout
225
kpc)
. Obs
erva
tions
are
cond
ucte
d in
the
g an
d i f
ilter
s, fo
r a to
tal o
f 145
0 se
cond
s in
eac
h. T
he re
sulti
ng o
bser
vatio
ns a
re g
ener
ally
suff
icie
nt to
reac
h S/
N=1
0 fo
r poi
nt so
urce
s at g
=25.
5 an
d i=
24.5
. Rel
ativ
e to
M31
, the
y re
solv
e st
ars i
n th
e to
pse
vera
l mag
nitu
des o
f the
red
gian
t bra
nch.
Inde
ed, a
s of t
he e
nd o
f S09
B, m
ore
than
30
mill
ion
stel
lar s
ourc
esar
e re
solv
ed in
PA
ndA
S da
ta.
Une
arth
ing
foss
ils o
f for
mat
ion
Figu
re 1
sho
ws
the
spat
ial d
ensi
ty d
is-
tribu
tion
of
red
gian
t br
anch
st
ars
acro
ss th
e PA
ndA
S a
rea,
a c
onve
nien
tpr
oxy
for
the
light
dis
tribu
tion
whe
nde
alin
g w
ith v
ery
fain
t stru
ctur
es. T
hesh
eer s
cale
of t
his
imag
e - a
nd th
e fa
ctth
at it
isn’
t em
pty!
- is
sur
pris
ing.
The
mai
n di
sk o
f M
31 is
incl
uded
for s
cale
,an
d th
e pr
esen
ce o
f st
ruct
ures
at
all
mor
e th
an 1
0 de
gree
s fr
om th
e ce
nter
of M
31 is
a s
tartl
ing
visu
al c
onfir
ma-
tion
of th
e va
st (a
nd g
ener
ally
una
ppre
-ci
ated
) sca
le o
f gal
axie
s.
And
wha
t of t
he st
ruct
ures
them
selv
es?
A p
leth
ora
of e
xten
ded
stre
ams,
loop
s,cl
umps
and
blo
bs c
over
the
entir
e m
ap,
exte
ndin
g ou
t to
proj
ecte
d ra
dii i
n ex
-ce
ss o
f 13
0kpc
(>2
0 sc
ale
leng
ths)
.M
any
indi
vidu
alst
ruct
ures
, suc
h as
the
larg
e lo
op in
the
north
-wes
t, ar
e gr
eate
rth
an 1
00kp
c in
ext
ent.
And
per
haps
mos
t stri
king
of a
ll is
the
num
ber o
f hig
hlig
hted
, con
cent
rate
d, s
tella
r ove
r-de
nsiti
es: t
hese
are
dw
arf g
alax
ysa
telli
tes
of M
31/M
33, t
he v
ast m
ajor
ity o
f whi
ch w
ere
unkn
own
prio
r to
thes
e ob
serv
atio
ns: s
o fa
r, 19
new
dwar
f gal
axie
s hav
e be
en u
ncov
ered
by
PAnd
AS,
with
mor
e lik
ely
to b
e di
scov
ered
.
One
of
the
mos
tun
expe
cted
ea
rlyre
sults
from
PA
n-dA
S in
volv
ed th
efa
int,
exte
nded
,st
ruct
ure
sur-
roun
ding
the
disk
of M
33. A
naly
sis
sugg
ests
tha
t it
isa
resu
lt of
a p
revi
-ou
s in
tera
ctio
nw
ith M
31 a
s M
33or
bits
aro
und
itsm
ore
mas
sive
com
pani
on.
This
findi
ng
fits
with
seve
ral o
ther
pie
c-es
of
circ
umst
an-
Figu
re 1
A ta
ngen
t pla
ne p
ro-
ject
ion
of th
e sp
atia
lde
nsity
dis
tribu
tion
ofre
d gi
ant b
ranc
h st
ars
acro
ss th
e P
And
AS
area
(as
of th
e en
d of
S09
B) a
con
veni
ent
prox
y fo
r the
ligh
t dis
-tri
butio
n w
hen
deal
ing
with
ver
y fa
int s
truc-
ture
s. T
he o
uter
mos
tci
rcle
cor
resp
onds
to a
proj
ecte
d ra
dius
from
M31
of 1
50kp
c. S
mal
lci
rcle
s hi
ghlig
ht d
war
fga
laxy
com
pani
ons
toM
31 a
nd M
33. R
edci
rcle
s hi
ghlig
ht n
ewdw
arfs
dis
cove
red
with
in th
e pa
st y
ear
(Ric
hard
son
et a
l.20
11, A
pJ, i
n pr
ess)
.
Figu
re 2
Pro
ject
ion
of th
e or
bit
of M
33 a
nd M
31 th
atbe
st re
prod
uces
the
exte
nded
stru
ctur
esu
rrou
ndin
g th
e di
skof
M33
firs
t obs
erve
din
the
PA
ndA
S d
ata-
set,
show
ing
the
rela
-tiv
e po
sitio
n of
the
gala
xies
as
a fu
nctio
nof
tim
e in
thei
r orb
it.Th
e rig
ht p
anel
sho
ws
the
sim
ulat
ed s
tella
rsu
rface
brig
htne
ssdi
strib
utio
n of
the
M33
dis
k at
the
pres
-en
t day
, whi
ch c
lose
lym
atch
es th
e ob
serv
a-tio
ns (M
cCon
nach
ieet
al.
2009
, Nat
ure,
461,
66)
.
CFH
T A
nnua
l Rep
ort
19
tial e
vide
nce,
in p
artic
ular
pec
ulia
ritie
s in
the
dyna
mic
s of
var
ious
trac
ers
in M
33 th
at u
ntil
now
hav
e de
fied
sim
ple
expl
anat
ion.
Usi
ng a
ll th
ese
obse
rvat
iona
l co
nstra
ints
, we
have
bee
n ab
le t
o re
cons
truct
the
orb
ital
hist
ory
of M
33 a
nd M
31, a
nd ti
med
thei
r mos
t rec
ent e
ncou
nter
to h
ave
been
som
e 2.
5 G
yrs a
go (F
igur
e 2)
.
Not
all
of th
e ob
ject
s we
dete
ct a
re v
isib
le in
thes
e m
aps.
Glo
bula
r clu
ster
s, lo
ng re
gard
ed a
s ste
llar p
opul
atio
nbe
acon
s, ar
e pr
esen
t to
o. F
igur
e 3
show
s a
colle
ctio
n of
the
se o
bjec
ts,
exac
tly 1
00 o
f w
hich
hav
e be
endi
scov
ered
in re
cent
yea
rs as
a re
sult
of th
is an
d re
late
d su
rvey
s. A
ll of
the d
isco
verie
s hav
e bee
n at
radi
i gre
ater
than
1 d
egre
e fr
om M
31; t
hat i
s, no
t lik
ely
asso
ciat
ed w
ith th
e di
sk. P
rior t
o th
is w
ork,
onl
y 3
clus
ters
wer
ekn
own
to l
ie b
eyon
d 30
kpc,
whe
reas
now
the
re a
re 7
9 kn
own
clus
ters
. Of
thes
e, 1
5 lie
at
proj
ecte
d ra
dii
betw
een
85 –
145
kpc
. Thi
s is a
virt
ually
une
xplo
red
regi
on in
any
spira
l gal
axy,
and
the
Milk
y W
ay h
as o
nly
2 kn
own
clus
ters
at c
ompa
rabl
e ra
dii.
A b
eaut
iful v
erifi
catio
n of
the
Sear
lean
d Zi
nn s
cena
rio h
as b
een
mad
epo
ssib
le
with
th
ese
disc
over
ies.
Whe
n th
e sp
atia
l di
strib
utio
n of
all
the
oute
r cl
uste
rs a
re c
ompa
red
toth
e sp
atia
l dis
tribu
tion
of st
ella
r sub
-st
ruct
ures
, a cl
ear c
orre
latio
n is
pre
s-en
t – c
lust
ers
are
pref
eren
tially
see
nw
here
ver a
stel
lar s
tream
is d
etec
ted
(inde
ed,
ofte
n “c
hain
s” o
f cl
uste
rsst
retc
h al
ong
the
stel
lar f
eatu
re; F
ig-
ure
3), a
nd c
lust
ers a
re p
refe
rent
ially
abse
nt in
are
as w
ith n
o st
ella
r su
b-st
ruct
ures
. Thi
s is a
rgua
bly
the
mos
tdi
rect
– a
nd v
isua
l – c
onfir
mat
ion
ofth
e ex
traga
lact
ic o
rigin
of m
any
out-
er h
alo
glob
ular
clu
ster
s si
nce
the
idea
was
firs
t pro
pose
d ba
ck in
197
8.
To
infin
ity!
With
the
com
plet
ion
of d
ata
colle
ctio
n in
S10
B, w
ork
with
in P
And
AS
is n
ow fo
cusi
ng o
n th
e fin
al q
uant
itativ
em
easu
rem
ents
of t
he s
patia
l dis
tribu
tion,
mor
phol
ogy
and
popu
latio
ns o
f the
ste
llar h
alo,
its
subs
truct
ure,
the
dwar
f ga
laxi
es a
nd t
he g
lobu
lar
clus
ters
. A
sig
nific
ant
num
ber
of f
ollo
w-u
p ob
serv
atio
ns o
n C
FHT,
the
KPN
O-4
m, W
HT,
Sub
aru,
Gem
ini a
nd K
eck
have
take
n pl
ace
too,
that
con
cent
rate
on
deep
er o
bser
vatio
ns,
blue
r and
redd
er b
ands
, as w
ell a
s spe
ctro
scop
y of
clu
ster
s and
indi
vidu
al re
d gi
ant b
ranc
h st
ars.
The
latte
r has
prov
en p
artic
ular
ly in
tere
stin
g, b
ut is
fund
amen
tally
lim
ited
by th
e re
lativ
ely
smal
l fie
ld o
f vie
w o
f the
pre
sent
gene
ratio
n of
mul
ti-ob
ject
spe
ctro
grap
hs, s
uch
that
the
ultim
ate
goal
of o
btai
ning
che
mo-
dyna
mic
al in
form
a-tio
n fo
r eve
ry b
right
star
acr
oss t
he P
And
AS
area
is st
ill so
me
way
off
. But
CFH
T/M
egaC
am h
as e
nsur
ed th
atPA
ndA
S w
ill li
kely
rem
ain
one
of th
e m
ost p
ower
ful d
atas
ets f
or a
ddre
ssin
g th
e pr
oper
ties o
f ste
llar h
alos
and
for
com
paris
on to
cos
mol
ogic
al s
imul
atio
ns o
f ga
laxy
for
mat
ion
for
the
fore
seea
ble
futu
re. A
nd it
s no
t jus
tw
ithin
the
PAnd
AS
cons
ortiu
m th
at th
e ne
w fe
w y
ears
will
pro
ve in
tere
stin
g. N
ear-
field
cos
mol
ogy
is e
nter
ing
a de
cade
that
pro
mis
es to
be
exce
ptio
nally
rich
.
As
wel
l as
the
(po
inte
d) w
ide
field
im
agin
g ca
pabi
litie
s pr
esen
ted
by C
FHT/
Meg
aCam
, an
d im
min
ently
Suba
ru/H
SC, t
he 3
PI s
urve
y of
PS1
will
pre
sent
a d
eep
view
of
the
Milk
y W
ay th
at w
ill p
robe
the
stel
lar
popu
latio
ns o
f the
Milk
y W
ay h
alo
and
shou
ld in
prin
cipl
e de
tect
the
fain
test
gal
axie
s eve
r fou
nd. I
n th
e so
uth,
SkyM
appe
r will
like
wis
e ch
art t
he sk
y, a
lbei
t not
as
deep
as P
anST
AR
RS,
and
at t
he e
nd o
f the
dec
ade
LSST
will
pre
sent
the
deep
est a
nd m
ost c
ompr
ehen
sive
pho
tom
etric
vie
w y
et o
f the
hal
o of
the
Milk
y W
ay, w
ith th
eab
ility
to e
xam
ine
the
stel
lar p
opul
atio
ns o
f the
Gal
axy
out t
o th
e eq
uiva
lent
radi
i pro
bed
in M
31 b
y PA
ndA
S.
But
as g
reat
as t
hese
pho
tom
etric
surv
eys w
ill b
e, th
e im
med
iate
futu
re is
ast
rom
etric
, with
the
adve
nt o
f GA
IAin
201
2. W
ith it
s abi
lity
to m
easu
re th
ree
dim
ensi
onal
pos
ition
s and
vel
ociti
es fo
r all
star
s with
V<2
0, a
s wel
las
det
aile
d ch
emic
al a
bund
ance
ana
lysi
s of a
ll st
ars w
ith V
<12,
it w
ill e
nabl
e fu
ll ch
emo-
dyna
mic
al se
para
tion
of t
he n
earb
y G
alax
y us
ing
all
6 ph
ase-
spac
e co
ordi
nate
s an
d m
ulti-
elem
ent
abun
danc
es. A
stro
nom
ers
are
abou
t to
dig
up a
trea
sure
che
st o
f fos
sils
to p
robe
the
hist
ory
of o
ur G
alax
y.
In sh
ort,
cosm
olog
y is
onc
e ag
ain
com
ing
clos
er…
Figu
re 3
Left.
, a s
elec
tion
of th
e10
0 ne
w M
31 g
lobu
lar
clus
ters
tha
t ha
vebe
en d
isco
vere
d in
this
and
rela
ted
sur-
veys
, all
at ra
dii g
reat
-er
than
1 d
egre
e fro
mM
31. R
ight
, a s
egm
ent
of th
e P
And
AS
map
show
ing
the
posi
tions
of g
lobu
lar
clus
ters
rela
tive
to th
e st
ella
rst
ruct
ures
. The
out
er-
mos
t clu
ster
s sh
ow a
strik
ing
posi
tiona
l cor
-re
latio
n w
ith th
e st
ella
rst
ream
s. T
his
impl
ies
that
the
se c
lust
ers
wer
e on
ce a
ssoc
iate
dw
ith th
e pr
ogen
itors
of
the
stre
ams,
and
are
thus
ext
raga
lact
ic in
orig
in (M
acke
y et
al.
2010
, ApJ
, 717
, L11
).
2220
09 &
201
0
On
the
softw
are
side
, the
cho
ice
was
mad
e to
cen
traliz
e th
e co
ntro
l int
o a
sing
le s
oftw
are
com
pone
nt, w
hich
sim
plifi
es th
e bu
sine
ss r
ules
and
the
inte
ract
ions
bet
wee
n sy
stem
s. Th
ree
cont
rol m
odes
(Su
mm
it, S
tand
by,
Wai
mea
) he
lp m
oder
ate
the
exec
utio
n of
the
com
man
ds a
nd i
nsur
e th
at a
ctio
ns c
anno
t be
“ac
cide
ntal
ly”
initi
ated
rem
otel
y. T
he o
vera
ll ar
chite
ctur
e is
out
lined
in th
e gr
aph
belo
w.
In d
evel
opin
g th
e G
raph
ical
Use
r In
terf
aces
(G
UIs
) fo
r al
l the
sub
-sy
stem
s to
be
rem
otel
y op
erat
ed, m
uch
atte
ntio
n w
as g
iven
to d
eliv
-er
ing
a co
nsis
tent
look
and
feel
, fro
m o
peni
ng th
e sh
utte
r to
mov
ing
the
win
dscr
een,
ope
ning
the
mirr
or, c
heck
ing
the
door
s on
the
dom
eflo
or o
r con
trolli
ng th
e lo
uver
s.
An
auto
nom
ous c
losi
ng p
roce
dure
has
bee
n im
plem
ente
d, w
hich
will
park
the
tele
scop
e, tu
rn th
e te
lesc
ope
hydr
aulic
s off
, clo
se th
e m
irror
cove
rs a
nd th
e do
me
shut
ter.
In o
rder
to p
rote
ct th
e ob
serv
ator
y, su
chan
aut
onom
ous
clos
ing
is tr
igge
red
whe
n ce
rtain
con
ditio
ns a
re m
et,
like
high
hum
idity
, pre
cipi
tatio
n, h
igh
win
d, o
r day
time.
Los
ing
the
conn
ectio
n be
twee
n W
aim
ea a
nd th
e su
mm
it is
not
eno
ugh
to s
hut-
dow
n th
e fa
cilit
y im
med
iate
ly. H
owev
er, a
fter a
giv
en ti
me
with
out
conn
ectio
n (c
urre
ntly
set a
t 15
min
), an
auto
nom
ous c
losi
ng se
quen
cew
ill b
e au
tom
atic
ally
gen
erat
ed.
Ano
ther
impo
rtant
pro
ject
, rel
ated
to O
AP,
is m
ovin
g th
e do
me
from
hydr
aulic
driv
es to
elec
tric m
otor
s. Im
plem
enta
tion
has b
egun
and
the
syst
em w
ill li
kely
be
in p
lace
in e
arly
Spr
ing
2011
. In
addi
tion
tosi
gnifi
cant
sav
ings
in
ener
gy c
onsu
mpt
ion,
the
new
sys
tem
will
elim
inat
e th
e ris
k of
leak
s re
late
d to
the
dom
e m
otio
n. It
will
leav
e on
ly th
e te
lesc
ope
as a
pot
entia
l sou
rce
ofoi
l lea
k, fo
r whi
ch p
rote
ctio
n m
easu
res h
ave
been
take
n to
avo
id a
ny sp
ill in
the
envi
ronm
ent (
soil
unde
rnea
thth
e bu
ildin
g or
out
side
).
All
the
chan
ges
and
addi
tions
mad
e to
ena
ble
CFH
T to
ope
rate
rem
otel
y ha
ve b
een
incr
emen
tally
inte
grat
eddu
ring
obse
rvin
g fr
om th
e su
mm
it. T
heir
impl
emen
tatio
n di
d no
t cau
se a
ny lo
ss o
f ob
serv
ing
time
and
will
ultim
atel
y al
low
a sm
ooth
tran
sitio
n to
rem
ote
obse
rvin
g m
ode.
The
impa
ct o
f OA
P on
the
oper
atio
nal r
elia
bilit
y of
the
entir
e fa
cilit
y ha
s al
read
y be
en s
igni
fican
t. Th
anks
toan
impr
oved
mon
itorin
g of
the
sum
mit
sub-
syst
ems a
nd to
the
ease
of r
emot
e ac
cess
to m
ost o
f the
par
amet
ers,
prev
entio
n of
fai
lure
s an
d re
mot
e di
agno
stic
hav
e m
ade
a su
bsta
ntia
l di
ffer
ence
on
the
dow
n-tim
e of
the
tele
scop
e an
d its
inst
rum
enta
tion.
The
am
ount
of t
ime
lost
to te
chni
cal p
robl
ems,
whi
ch is
now
wel
l bel
ow 2
%of
the
clea
r w
eath
er o
bser
ving
tim
e, d
emon
stra
tes
an e
xcel
lent
rel
iabi
lity
for
an o
ld f
acili
ty e
quip
ped
with
com
plex
hig
h-te
ch in
stru
men
tatio
n. L
ast,
but n
ot le
ast,
the
tech
nica
l sta
ff is
alre
ady
enjo
ying
a w
elco
me
pea
ceof
min
d, a
s a re
sult
of th
e re
mot
e se
nsin
g ca
pabi
litie
s off
ered
by
the
Obs
erva
tory
Aut
omat
ion
Proj
ect..
GU
I win
dow
sA
typi
cal G
UI w
indo
w,
show
ing
the
tele
scop
eflo
or a
nd th
e st
atus
of
the
door
s. N
o re
dsh
ould
be
seen
in
nigh
t- tim
e op
erat
ion.
CFH
T A
nnua
l Rep
ort
21
�W
inds
cree
n m
onito
ring
and
rem
ote
cont
rol i
mpl
emen
tatio
n�
Rem
ote
oper
atio
ns ro
om U
PS u
pgra
de�
End-
to-e
nd te
stin
g of
all
tech
nica
l req
uire
men
ts�
Rev
iew
of r
emot
e op
erat
ing
proc
edur
esM
onito
ring
the
envi
ronm
ent
isan
othe
r ar
ea w
here
bei
ng a
way
from
the
sum
mit
repr
esen
ts d
if-fic
ultie
s: it
is n
ot e
asy
to re
plac
eal
l th
e in
form
atio
n an
obs
erve
rca
n gr
asp
from
sim
ply
wal
king
out
on t
he c
atw
alk!
Rel
iabl
yse
nsin
g th
e te
mpe
ratu
re, h
umid
-ity
, win
d, p
reci
pita
tion
(rai
n or
snow
) ca
n be
don
e th
roug
h th
eim
plem
enta
tion
of ro
bust
wea
th-
er
sens
ing
inst
rum
ents
w
ithen
ough
re
dund
ancy
to
av
oid
fals
e al
arm
s or
mis
s ba
d co
ndi-
tions
. The
nig
ht v
isio
n go
ggle
sus
ed to
che
ck fa
int c
loud
s co
m-
ing
from
afa
r ha
ve t
o be
re-
plac
ed w
ith lo
w li
ght c
amer
as. A
good
com
plem
ent i
s an
infr
ared
all-s
ky
cam
era
to
dete
ct
the
clou
d co
ver,
ASI
VA
, no
w i
n-st
alle
d by
CFH
T at
the
sum
mit
for t
he b
enef
it of
all t
he o
bser
va-
torie
s. Sk
ypro
be, u
sed
for y
ears
,is
one
mor
e im
porta
nt p
iece
of o
bser
vatio
n to
che
ck th
e ex
tinct
ion
of th
e sk
y w
here
the
tele
scop
e is
poi
ntin
g.
As
vario
us m
aint
enan
ce a
nd i
mpr
ovem
ent
wor
k is
don
e du
ring
the
day
on t
he d
ome,
the
tel
esco
pe,
the
inst
rum
ents
and
the
vario
us su
bsys
tem
s of t
he o
bser
ving
env
ironm
ent,
it is
par
amou
nt to
ass
ure
that
the
faci
lity
is le
ft re
ady
for
nigh
t rem
ote
oper
atio
n. A
sim
ple
stat
us s
cree
n is
inst
alle
d cl
ose
to th
e su
mm
it fr
ont d
oor
build
ing,
pro
vidi
ng i
n on
e gl
ance
the
app
ropr
iate
inf
orm
atio
n on
all
the
syst
ems
criti
cal
to t
he r
emot
eob
serv
atio
ns fr
om W
aim
ea. B
elow
is a
snap
shot
of h
ow th
is st
atus
scre
en w
ill lo
ok li
ke o
nce
rem
ote
oper
atio
nsw
ill b
e C
FHT’
s re
gula
r mod
e of
obs
ervi
ng.
Figu
re 1
Rep
laci
ng th
e ey
esan
d ea
rs o
f the
Ob-
serv
ing
Ass
ista
nt is
one
of th
e ke
y-co
mpo
-ne
nts
of th
e O
AP
env
i-ro
nmen
t. Fi
xed
orre
mot
ely
cont
rolle
dca
mer
as a
t stra
tegi
clo
catio
ns o
ffer e
noug
hin
form
atio
n fo
r a c
lose
look
at
the
criti
cal
com
pone
nts
of t
heob
serv
ator
y an
d fo
rw
ell-i
nfor
med
dec
i-si
ons
from
rem
ote
lo-
catio
n (fr
om t
heW
aim
ea h
eadq
uarte
rsto
mob
ile d
evic
es).
2020
09 &
201
0
Obs
erva
tory
Aut
omat
ion
Proj
ect:
Tow
ard
Rem
ote
Ope
ratio
nO
AP
(the
Obs
erva
tory
Aut
omat
ion
Proj
ect)
has
been
the
maj
or in
-hou
se p
roje
ct c
arrie
d ou
t by
the
staf
f ove
r20
09-2
010,
follo
win
g on
e ye
ar o
f bra
inst
orm
ing
and
plan
ning
. Whi
le “
OA
P” su
gges
ts a
full
auto
mat
ion
of th
eob
serv
ator
y op
erat
ion,
the
goal
of t
he fi
rst p
hase
of O
AP
near
ing
com
plet
ion
by th
e en
d of
201
0 is
to a
llow
rem
ote
oper
atio
n at
nig
ht w
ithou
t any
one
at th
e su
mm
it.
Whe
n Se
rvic
e Obs
erve
rs (S
Os)
took
ove
r the
obs
erva
tions
in th
e ear
ly d
ays o
f QSO
(Que
ue S
ervi
ce O
bser
ving
),th
e ob
serv
ator
y st
ill re
quire
d an
Obs
ervi
ng A
ssis
tant
(OA
) to
man
the
tele
scop
e an
d th
e ov
eral
l fac
ility
whi
leth
e SO
per
form
ed th
e ob
serv
atio
ns. W
ith in
crea
sed
com
pute
rized
ass
ista
nce
adde
d to
the
QSO
mod
e, s
uch
asan
aut
omat
ic s
lew
of t
he te
lesc
ope
once
an
obse
rvat
ion
is s
elec
ted,
or a
utom
atic
fiel
d ac
quis
ition
and
gui
ding
setti
ng o
nce
on a
targ
et, t
he r
ole
of th
e O
A b
ecam
e lim
ited
to r
eady
ing
the
obse
rvat
ory
for
obse
rvin
g at
the
begi
nnin
g of
the
nigh
t and
clo
sing
and
secu
ring
it at
the
end
of th
e ni
ght.
Dur
ing
the
obse
rvin
g its
elf,
the
OA
’sro
le w
as m
ainl
y to
int
erve
ne a
nd a
ssis
t in
cas
e of
pro
blem
s. It
beca
me
clea
r th
at a
sin
gle
pers
on,
with
appr
opria
te t
rain
ing,
cou
ld a
ctua
lly h
andl
e bo
th t
he S
O a
nd O
A d
utie
s. Th
is w
ould
red
uce
the
man
pow
erne
eded
for o
bser
ving
, the
refo
re in
crea
sing
the
effic
ienc
y of
the
oper
atio
ns o
f the
obs
erva
tory
. Unf
ortu
nate
ly, a
tsi
tes l
ike
Mau
nake
a, re
mot
enes
s and
alti
tude
man
date
s for
the
pers
onne
l saf
ety
requ
irem
ent t
o ha
ve a
t lea
st tw
ope
ople
pre
sent
in th
e bu
ildin
g at
any
giv
en ti
me.
In o
rder
to re
ally
impr
ove
the
oper
atio
nal e
ffic
ienc
y of
the
obse
rvat
ory,
we
had
to th
ink
abou
t not
bei
ng a
t the
tele
scop
e an
ymor
e du
ring
obse
rvin
g!
Ret
rofit
ting
an o
ld fa
cilit
y lik
e C
FHT
to e
nabl
e its
rem
ote
oper
atio
n is
not
a si
mpl
e en
deav
or: a
fter a
ll, w
e ar
eta
lkin
g ab
out a
tele
scop
e w
ith a
250
-ton
mov
ing
mas
s , o
r a
580-
ton
dom
e, w
ith th
eir
hydr
aulic
driv
es a
ndhi
gh-p
ress
ure
oil r
unni
ng fr
om th
e ba
sem
ent t
o th
e do
me
floor
, hun
dred
s of
met
ers
of h
oses
car
ryin
g gl
ycol
runn
ing
all o
ver t
he te
lesc
ope
and
its in
stru
men
tatio
n. Is
it re
ally
feas
ible
to re
plac
e al
l the
han
ds-o
n m
onito
ring
carr
ied
out
by a
n O
A a
nd a
ll th
e m
anua
l in
terv
entio
ns a
per
son
coul
d do
at
nigh
t by
rem
otel
y-co
ntro
lled
func
tions
acc
essi
ble
on a
scre
en a
nd th
roug
h th
e cl
ick
of a
mou
se?
Act
ually
, not
onl
y it
is f
easi
ble,
but
it b
rings
muc
h m
ore
than
just
the
poss
ibili
ty o
f re
mot
ely
oper
atin
g th
efa
cilit
y! A
n ex
ampl
e: A
n ol
d-st
yle
dial
gau
ge, l
ooke
d at
by
the
OA
to c
heck
if a
pre
ssur
e is
nom
inal
at t
hebe
ginn
ing
of th
e ni
ght,
has t
o be
repl
aced
by
a se
nsor
rem
otel
y ac
cess
ible
. It o
pens
the
poss
ibili
ty o
f con
tinuo
usco
ntro
l of
the
pre
ssur
e th
roug
h a
scrip
t re
adin
g th
e va
lue,
sen
ding
a w
arni
ng w
hen
sign
ifica
nt i
ncre
ase,
decr
ease
, or
chan
ge r
ate,
are
det
ecte
d, th
eref
ore
prev
entin
g a
failu
re b
efor
e it
occu
rs!
Add
to th
e sc
ript a
nau
tom
atic
not
ifica
tion
thro
ugh
text
mes
sage
s on
smar
t pho
nes,
writ
e as
man
y sc
ripts
for a
s man
y se
nsor
s as y
oude
em n
eces
sary
for s
afe
oper
atio
ns, a
nd y
ou e
nd u
p w
ith te
chni
cal s
taff
mad
e aw
are
in a
dvan
ce o
f pot
entia
lfa
ilure
s: t
he o
pera
tions
mov
e fr
om f
ight
ing
fires
to
wel
l-inf
orm
ed p
reve
ntiv
e m
aint
enan
ce a
nd p
reem
ptiv
eac
tions
.
The
follo
win
g ite
ms o
utlin
e so
me
of th
e va
rious
sub-
proj
ects
rela
ted
to th
e w
hole
OA
P.�
New
mon
itorin
g an
d re
mot
e co
ntro
l of t
he te
lesc
ope
hydr
aulic
syst
em�
Mon
itorin
g of
per
sonn
el e
ntry
to th
e 5th
floo
r (a
safe
ty is
sue)
�Se
nsin
g th
e lo
catio
n of
the
sola
r sai
l�
Sens
ing
the
loca
tion
of th
e m
irror
coo
ling
duct
�N
ew m
onito
ring
capa
bilit
ies f
or th
e se
cond
ary
mirr
or su
ppor
t sys
tem
�C
oord
inat
ed a
lert
syst
em th
at in
clud
es sl
ew to
nes,
pop-
up m
essa
ges,
war
ning
s, al
erts
, and
bro
adca
sted
mes
sage
s in
the
dom
e an
d th
e re
mot
e op
erat
ions
room
�M
onito
ring
of th
e su
mm
it U
PS(s
)�
Rem
oval
of t
he te
lesc
ope
key
�In
stal
latio
n of
a li
ght s
ourc
e by
one
of t
he c
atw
alk
cam
eras
to a
ssis
t in
mon
itorin
g th
e en
viro
nmen
tal
cond
ition
s (fo
g de
tect
ion)
�Im
plem
enta
tion
of a
n au
tono
mou
s shu
tdow
n pr
otoc
ol�
Add
ition
al fu
nctio
nalit
y in
the
OA
P C
ontro
l GU
I�
Mod
ifica
tions
to th
e su
mm
it co
ntro
l roo
m a
nd th
e re
mot
e op
erat
ions
room
�Su
mm
it fir
e al
arm
syst
em u
pgra
de
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