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ce P

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Hun

g C

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l Ene

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<~

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g ga

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RA

S 4

02 2

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el-

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ctor

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essa

geTw

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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

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.A74

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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

. CoR

oT-1

3b: a

den

se h

ot J

upite

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trans

it ar

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a s

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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

of r

edsh

ift e

volu

tion

in la

rge-

scal

een

viro

nmen

ts (O

RE

LSE

) sur

vey.

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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.,

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kem

oer,

A.,

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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.,

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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.,

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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.,

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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

stro

met

ric c

alib

ratio

n is

then

app

lied

usin

g th

e 2M

ass P

oint

Sou

rce

cata

log.

It is

impo

rtant

to n

ote

that

onl

y lin

ear s

hifts

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

Flow

cha

rt ill

ustra

ting

the

proc

essi

ng s

teps

used

in Ii

wi 2

, as

wel

las

the

sixd

ata

prod

-uc

ts, a

long

with

cal

i-br

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ns, w

hich

are

dist

ribut

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the

PIs

.

3220

09 &

201

0

CFH

T-ba

sed

refe

reed

pub

licat

ions

- 20

09A

dam

i C.,

Gav

azzi

, R.,

Cui

lland

re, J

. C.,

Dur

ret,

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lber

t, O

., M

azur

e, A

., P

elló

, R.,

Ulm

er, M

. P. O

rient

atio

ns o

f ver

y fa

int

gala

xies

in th

e C

oma

clus

ter.

A&

A 4

93 3

99-4

07.

Ada

mi C

., P

elló

, R.,

Ulm

er, M

. P.,

Cui

lland

re, J

. C.,

Dur

ret,

F., M

azur

e, A

., P

icat

, J. P

., S

chei

degg

er, R

. On

the

natu

re o

f fai

ntlo

w s

urfa

ce b

right

ness

gal

axie

s in

the

Com

a cl

uste

r. A

&A

495

407

-414

.A

dam

i C.,

Le B

run,

V.,

Biv

iano

, A.,

Dur

ret,

F., L

amar

eille

, F.,

Pel

ló, R

., Ilb

ert,

O.,

Maz

ure,

A.,

Trilli

ng, R

., U

lmer

, M. P

. Ver

yde

ep s

pect

rosc

opy

of th

e C

oma

clus

ter l

ine

of s

ight

: exp

lorin

g ne

w te

rrito

ries.

A&

A 5

07 1

225-

1241

.A

gra-

Am

boag

e V

., D

ouga

dos,

C.,

Cab

rit, S

., G

arci

a, P

. J. V

., Fe

rrui

t, P

. [O

I] s

ub-a

rcse

cond

stu

dy o

f a m

icro

jet f

rom

an

in-

term

edia

te m

ass

youn

g st

ar: R

Y T

auri.

A&

A 4

93 1

029-

1041

.A

ngui

ta T

., Fa

ure,

C.,

Kne

ib, J

.-P.,

Wam

bsga

nss,

J.,

Kno

bel,

C.,

Koe

kem

oer,

A. M

.; Li

mou

sin,

M. C

OS

MO

S 5

921+

0638

:ch

arac

teriz

atio

n an

d an

alys

is o

f a n

ew s

trong

gra

vita

tiona

lly le

nsed

AG

N. A

&A

507

35-

46.

Aur

ière

M.,

Wad

e, G

. A.,

Kon

stan

tinov

a-A

ntov

a, R

., C

harb

onne

l, C

., C

atal

a, C

., W

eiss

, W. W

., R

oudi

er, T

., P

etit,

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Don

ati,

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., A

leci

an, E

. and

4 c

oaut

hors

Dis

cove

ry o

f a w

eak

mag

netic

fiel

d in

the

phot

osph

ere

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e si

ngle

gia

nt P

ollu

x. A

&A

504

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237.

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delli

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, Zam

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., B

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chel

li, A

., Tr

esse

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gani

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and

44 c

oaut

hors

The

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DS

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p fie

ld. I

V. R

adio

-opt

ical

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es. A

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ete

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ic S

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OD

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ld1.

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689

687

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.B

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., B

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ilde

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utho

rs O

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e na

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he e

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ctic

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A 4

94 6

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va L

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, Béj

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ó-P

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íaz-

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, J.

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es-C

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e X

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e-fie

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CO

SM

OS

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d. T

he p

oint

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8.C

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nat B

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ontin

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, Le

Fèvr

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., V

erga

ni, D

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., Q

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., Ta

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L.,

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se, L

. Int

egra

l fie

ld s

pec-

trosc

opy

with

SIN

FON

I of V

VD

S g

alax

ies.

I. G

alax

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nam

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mas

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sem

bly

at 1

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z <

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. A&

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., H

ildeb

rand

t, H

., Le

rchs

ter,

M.,

Hud

elot

, P.,

Ben

jam

in, J

., va

n W

aerb

eke,

L.,

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rabb

ack,

T.,

Brim

ioul

le, F

., C

orde

s,O

., D

ietri

ch, J

. P. a

nd 3

coa

utho

rs C

AR

S: t

he C

FHTL

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rchi

ve-R

esea

rch

Sur

vey.

I. F

ive-

band

mul

ti-co

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.de

g. C

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obse

rvat

ions

. A&

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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

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