http

://w

ww

.mpi

a.de

/rin

g200

7

Salz

bu

rg

Old

Tow

n

http

://w

ww

.mpi

a.de

/rin

g200

7

SA

LZ

BU

RG

, AU

ST

RIA

- EX

CU

RS

ION

, WE

D, O

CT

31, 1

1:0

0-1

8:3

0H

Main

sig

hts

(fr

om

Wik

iped

ia)

Salz

burg

is a

touris

t favorite

. In a

dditio

n to

Mozart's

birth

pla

ce, o

ther n

ota

ble

pla

ces in

clu

de:

!•!

The w

hole

Old

Tow

n o

f Salz

burg

was n

om

inate

d

as a

World

Herita

ge S

ite in

1996

.

!•!

The b

aro

que a

rchite

ctu

re in

clu

din

g th

e m

any

churc

hes a

re w

orld

fam

ous.

!•!

The S

alz

burg

Cath

edra

l

!•!

The fo

rtress H

ohensalz

burg

on a

hill d

om

inatin

g

the o

ld to

wn is

one o

f the la

rgest c

astle

s in

Euro

pe, w

ith v

iew

s o

ver S

alz

burg

.

!•!

The F

ranzis

kanerc

hurc

h

!•!

The S

t.Pete

r cem

ete

ry

!•!

The N

onnberg

Abbey a

Benedic

tine m

onaste

ry

!•!

The "R

esid

enz" P

ala

ce (th

e m

agnifi

cent fo

rmer

Prin

ce-A

rchbis

hop's

resid

ence)

!•!

Mozart's

Birth

pla

ce

!•!

Mozart's

Resid

ence

!•!

The U

niv

ers

ity C

hurc

h

!•!

The S

iegm

undsto

r (or N

euto

r)

!•!

The G

etre

idegasse

(where

you c

an fi

nd

Mozart"s

birth

pla

ce)

The earlie

st

settle

ments

can

be tra

ced back

about

6500 years

. 2000

years

ago,

vario

us

Celtic

villa

ges in

the a

rea b

ecam

e th

e R

om

an

tow

n o

f Ju

vavu

m. T

he

nam

e S

alz

bu

rg

(“Salt

Castle

”) goes back to

th

e year

696,

when

mis

sio

nary

(S

ain

t) R

ubert a

rrived

in th

e a

rea

and fo

unded th

e B

enedic

tine M

onaste

ry o

f St.

Pete

rs. T

he to

wn

evolv

ed

into

an in

dependent

churc

h sta

te,

rule

d by th

e Arc

hbis

hop.

The

sovere

ign w

as not

only

th

e s

piritu

al

leader

but a

lso

possessed m

any w

orld

ly p

ow

ers

. The

org

anis

atio

n o

f th

e c

ity w

as in

a V

atic

an-lik

e

sty

le and is

w

as not

with

out

a re

ason th

at

Salz

bu

rg w

as re

ferre

d to

as th

e "R

om

e o

f the

North

".

The c

ity o

f Salz

bu

rg

is

nestle

d betw

een th

e

two

m

ou

nta

ins

Ka

pu

zin

erb

erg

an

d

Mö

nch

sb

erg and th

e riv

er

Salz

ach

. It

is a

pic

ture

sque

city

w

ith

sm

all

alle

yw

ays,

qu

ain

t co

lou

rfu

l tow

n h

ou

ses, r

ich c

astle

s

and p

ala

ces, w

ith s

tyle

d g

ard

ens a

nd a

larg

e

num

ber o

f churc

hes a

nd m

onaste

ries.

The F

ortre

ss o

f H

oh

en

salz

bu

rg,

a 9

00 year

old

build

ing,

is consid

ere

d to

be th

e m

ost

well-m

ain

tain

ed M

edie

val F

ortre

ss in

Euro

pe.

St.

Seb

astia

n is

th

e c

ity's

m

ost

impre

ssiv

e

churc

h, b

uilt

in th

e G

oth

ic sty

le, w

ith a

well-

tended cem

ete

ry.

The city

of

Salz

burg

still

dis

pla

ys th

e w

ealth

and

pow

er

of th

e fo

rmer

Arc

hbis

hops,

and

is

to

day

hom

e

to

appro

xim

ate

ly 1

50.0

00 in

habita

nts

.

Salz

bu

rg is

a c

ity o

f m

usic

. It was th

e h

om

e a

nd

birth

pla

ce o

f Wolfg

ang

Am

adeus M

ozart a

nd th

e

mem

oria

l to h

im a

t the S

alz

burg

Mo

zart S

qu

are h

onours

the

city

's m

ost fa

mous s

on. S

alz

burg

has a

lo

ng his

tory

of

bein

g a

popula

r destin

atio

n fo

r m

usic

ians,

harb

oure

d by th

e m

any Arc

hbis

hops’

fondness fo

r m

usic

. This

city

has re

tain

ed

its

charm

and

chara

cte

r th

rough

th

e c

entu

ries.

Today

Salz

burg

is k

now

n fo

r its a

nnual c

ultu

ral F

estiv

al (S

alz

bu

rg

er F

ests

pie

le), w

hic

h o

ffers

a v

arie

ty o

f opera

s, c

oncerts

and

theatric

al p

lays, ra

ngin

g fro

m c

lassic

al to

conte

mpora

ry s

tyle

s. T

he c

ity is

als

o a

very

popula

r pla

ce fo

r m

usic

al o

r theatric

al s

tudie

s, a

nd a

s a

result, m

any s

tudents

from

aro

und th

e

world

enro

l at

one

of

the

m

any

diffe

rent

schools

in

Salz

burg

every

year.

(sourc

e:

http

://w

ww

.abouta

ustria

.org

/capita

ls/s

alz

burg

.htm

)

http://ww

w.m

pia.de/ring2007

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Ringberg W

orkshop 2007 - N

otes

http

://w

ww

.mpi

a.de

/rin

g200

7

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Rin

gber

g W

orks

hop

2007 - N

otes

http

://w

ww

.mpi

a.de

/rin

g200

7

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Rin

gber

g W

orks

hop

Oct

28 - N

ov 2

, 2007

The fi

eld

of

Adapti

ve O

pti

cs (A

O)

for

ast

ronom

y has

matu

red in

re

cent

years

, and

dif

fracti

on-l

imit

ed i

mage r

eso

luti

on i

n t

he n

ear-

infr

are

d s

pectr

al

range i

s n

ow

routi

nely

achie

ved by

most

8-1

0m

cla

ss t

ele

-scopes.

In

ord

er

to w

ork

, adapti

ve opti

cs

needs a

nearb

y re

fere

nce s

tar

that

has

to b

e r

ela

tively

bri

ght,

there

by

lim

itin

g t

he a

rea o

f th

e

sky t

hat

can b

e s

urv

eyed.

To o

verc

om

e t

his

lim

itati

on,

ast

ronom

ers

use

a p

ow

erf

ul

lase

r th

at

cre

ate

s a

n a

rtif

icia

l st

ar

– a s

o c

alled l

ase

r guid

e s

tar

(LG

S)

– w

here

and w

hen t

hey

need it

. The com

bin

ati

on of

both

te

chniq

ues,

LG

S a

nd A

O,

has

opened new

re

searc

h

win

dow

s to

gala

cti

c a

nd e

xtr

agala

cti

c a

stro

nom

y. R

ese

arc

h t

opic

s ra

nge f

rom

the s

tudy

of

bin

ary

bro

wn d

warf

syst

em

s, s

earc

h f

or

exopla

nets

, obse

rvati

ons

of

young,

mass

ive

stars

, st

arb

urs

t clu

sters

, gala

cti

c b

lack h

ole

s and a

cti

ve g

ala

cti

c n

ucle

i, g

ala

xy

clu

sters

as w

ell

as hig

h re

dsh

ift

gala

xie

s, in

clu

din

g th

ose

m

agnif

ied by gra

vit

ati

onal

lensi

ng

eff

ects

.This

work

shop i

s in

tended t

o b

ring t

ogeth

er

scie

nti

sts a

nd e

ngin

eers

work

ing in t

he f

ield

of

Lase

r G

uid

e S

tar

Adapti

ve O

pti

cs.

The a

ims

of

this

meeti

ng c

an b

e s

um

mari

sed in t

he f

ollow

ing p

oin

ts:

The p

urp

ose

of

LG

S-A

O i

s to

wid

en th

e r

ange a

nd i

ncre

ase

th

e i

mpact

of

ast

rophysi

cs

that

is p

oss

ible

w

ith a

dapti

ve o

pti

cs.

There

fore

, w

e a

sk:

for

what

scie

nce are

LG

S-A

O

syst

em

s bein

g u

sed?

•Evalu

ati

on a

nd d

iscuss

ion o

f th

e f

irst

scie

nce r

esu

lts o

bta

ined f

rom

LG

S-A

O s

yst

em

s. I

n

part

icula

r: G

ala

cti

c cente

r and A

GN

, gala

cti

c and extr

a-g

ala

cti

c st

ar

form

ati

on,

sola

r sy

stem

obje

cts

, bro

wn d

warf

s, g

ala

xie

s and c

osm

olo

gy.

• L

GS-A

O sy

stem

s are

desi

gned to

pro

duce hig

h Str

ehl

rati

os

and dif

fracti

on lim

ited

obse

rvati

ons

over

most

of

the s

ky.

Are

the s

yst

em

s livin

g u

p t

o t

hese

expecta

tions?

• T

he f

irst

genera

tion o

f LG

S s

yst

em

s on 3

-m c

lass

tele

scopes (

at

the L

ick O

bse

rvato

ry,

and a

t Cala

r Alt

o,

the M

PIA

/M

PE s

yst

em

) w

ere

dif

ficult

to u

se;

the n

ew

genera

tion o

n 8

- to

10-m

cla

ss te

lesc

opes a

re si

gnif

icantl

y bett

er.

Are

w

e now

confi

dent

that

LG

S-A

O

could

becom

e part

of

the st

andard

obse

rvin

g p

rocedure

, as

is e

nvis

aged fo

r th

e n

ext

genera

tion o

f extr

em

ely

larg

e t

ele

scopes?

• H

ave L

GS-A

O s

yst

em

s b

een e

mplo

yed i

n n

ovel

meth

ods

of

obse

rvin

g (

e.g

. if

there

is n

o

natu

ral st

ar

for

tip-t

ilt

com

pensa

tion)?

Have t

hese

been s

uccess

ful?

• K

now

ledge o

f th

e P

oin

t Spre

ad Functi

on is

of

cru

cia

l im

port

ance f

or

extr

acti

ng t

he

most

info

rmati

on f

rom

the d

ata

. W

hat

pro

gre

ss h

as b

een m

ade i

n d

ete

rmin

ing t

his

for

LG

S-A

O (

eit

her

em

pir

ically t

hro

ugh a

ddit

ional obse

rvati

ons

or

via

modellin

g)?

• W

hat

less

ons have been le

arn

ed eit

her

in th

e desi

gn or

opera

tion of

the LG

S-A

O

syst

em

s th

at

should

be b

orn

e in m

ind w

hen d

esi

gnin

g f

utu

re s

yst

em

s fo

r ELT

s?

Scope o

f th

e w

ork

shop:

http://ww

w.m

pia.de/ring2007

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Lodgin

g (2

5 O

cto

ber 2

007)

Durin

g th

e w

ork

shop w

eek a

ll partic

ipants w

ill have ro

om

s eith

er in

the c

astle

itself o

r in o

ne

of th

e

neig

hbourin

g h

ote

ls. All p

artic

ipants w

ho c

annot sta

y o

vern

ight a

t the c

astle

will b

e in

form

ed u

ntil

Septe

mber 2

1, 2

007 in

ord

er to

make th

eir o

wn re

serv

atio

n in

the h

ote

l Park

resid

enz o

r a h

ote

l of

their c

hoic

e.

A b

lock re

serv

atio

n o

f 20 d

ouble

room

s (cate

gory

"Delu

xe") h

as b

een

arra

nged fo

r work

shop

partic

ipants in

the h

ote

l Park

resid

enz (w

ww

.park

resid

enz.c

om

, em

ail: in

fo@

park

resid

enz.c

om

). The

blo

ck re

serv

atio

n is v

alild

until S

epte

mber 2

6, 2

007.

Pric

e p

er ro

om

and

day in

clu

din

g a

"Vita

l" bre

akfa

st buffe

t is 135,0

0 E

uro

(one p

erso

n) o

r 163,0

0 E

uro

(two p

erso

ns).

A sh

uttle

serv

ice to

the c

astle

(confe

rence

locatio

n) w

ill be a

vaila

ble

in th

e m

orn

ing a

t 8:4

5am

and

in th

e e

venin

g a

fter d

inner. P

artic

ipants lo

dgin

g o

utsid

e th

e c

astle

can

have lu

nch (1

0,0

0 E

uro

) and

din

ner (1

3,0

0 E

uro

) at th

e c

onfe

rence site

.

The e

arlie

st check-in

at th

e R

ingberg

castle

hote

l is on S

unday, O

ct 2

8, a

t 16:0

0 h

ours (4

pm

).

You h

ave to

leave y

our ro

om

at th

e la

test u

ntil 9

:00 h

ours (9

am

) on F

riday, N

ov 2

. This a

llow

s the

castle

managem

ent to

pre

pare

for th

e n

ext c

onfe

rence.

The c

onfe

rence w

ill end a

t 14:0

0 h

ours (2

pm

) afte

r Lunch.

Ple

ase

note

that E

uro

pe w

ill switc

h fro

m su

mm

er to

win

ter tim

e o

n O

ct 2

8 a

t 3am

.

If you n

eed

furth

er in

form

atio

n o

r help

ple

ase

conta

ct th

e L

OC

via

em

ail to

ring2007@

mpia

.de

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - P

rogra

mme (v0

71025)

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Monday, O

ct 29

9:0

0 A

rrival and R

egistration

10:3

0 C

offee10:5

0 W

elcom

e, O

pen

ing

11:0

0 L

GS

-AO

Intro

(1a - ch

air: Fra

nço

is Rig

au

t) E

SO ad

aptive o

ptics ro

adm

ap an

d p

lan fo

r ELT

- Norbert H

ubin

Com

mon-u

ser and E

xperim

ental L

aser Guid

e Star AO

at the W

illiam H

erschel Telesco

pe - T

im M

orris

Overview

of th

e curren

t ESO

activities on L

aser Guid

e Stars for A

dap

tive Optics - R

onald Holzlöhner

12:3

0 Lunch

14:0

0 G

ala

ctic

Nu

cle

ii (1b - ch

air Cla

ire M

ax

) B

ringin

g our G

alaxy's Su

perm

assive Black H

ole an

d its E

nvirons in

to Fo

cus w

ith LG

S AO

- Andrea

Ghez H

igh an

gular reso

lutio

n o

bservatio

ns o

f the G

alactic Cen

ter at the V

LT w

ith LG

S-AO

- Thom

as Ott

Detectin

g superm

assive black h

oles in

pseu

dobulges an

d lo

w-m

ass bulges w

ith LG

S-AO

- Nina N

ovak15:3

0 C

offee16:0

0 L

GS

Te

ch

niq

ue

s an

d O

ptim

izatio

ns (1

c - chair N

orb

ert H

ub

in)

Can

laser beaco

ns b

e used

as guid

e stars? - Erez R

ibak C

om

pen

sation o

f ELT

LG

S WFSs fo

r variations o

f sodiu

m layer - G

len Herriot

Increasin

g the retu

rn fl

ux fro

m so

diu

m gu

ide star lasers- E

d Kibblew

hite O

ptim

ization o

f a LG

S support w

avefront co

rrector - D

iethard Peter18:3

0 D

inner

Tuesday, Oct 3

09:0

0 H

igh

-z U

niv

erse

(2a - ch

air An

dre

a G

he

z)

OSIR

IS: Early Scien

ce from

the K

eck LG

SAO

Integral Field

Spectro

graph - Jam

es Larkin M

odelin

g the d

ynam

ics of h

igh red

shift galax

ies with

SINFO

NI an

d L

GS - G

iovanni Cresci

High

redsh

ift science w

ith A

dap

tive Optics: H

ighligh

ts from

the SIN

S survey - N

atasha Förster-Schreiber10:3

0 C

offee11:0

0 A

O-P

SF

(2b - ch

air Ed

Kib

ble

wh

ite)

The Po

int Sp

read Fu

nctio

n o

f a Laser G

uid

e Star Adap

tive Optics System

- Matthew

Britton

Gettin

g Lucky w

ith (L

GS) A

O: 2

X H

ST reso

lutio

n in

the visib

le - Nicholas Law

LGS-A

O w

ithout tip

-tilt - Ric D

avies12:3

0 Lunch

14:0

0 P

SF

Fittin

g D

iscu

ssion

+ P

oste

r T

alk

s (2c - ch

air Wo

lfgan

g B

ran

dn

er) - A

ndersen

, R

ajagopal, ... (5

min

) 15:3

0 P

oste

r V

iew

ing

+ C

offee16:0

0 H

igh

-z U

niv

erse

- cont’d

(2d - ch

air Masa

no

ri Iye

) M

ass-Metallicity R

elation an

d D

ynam

ical Mass o

f Galax

ies at z>3 - Filippo M

annucci Star Fo

rmin

g Galax

ies in th

e Early U

niverse: Sp

atially Reso

lved Sp

ectrosco

py with

Keck LG

S AO

- Shelley W

right C

AT

S observatio

ns o

f 11 C

han

dra so

urces in

GO

OD

S-S at z~1 u

sing K

eck LGSA

O - M

ark Am

mons

18:3

0 D

inner

Sunday, O

ct 28

16:0

0 to

22:0

0 A

rrival18:3

0 W

elc

om

e re

ce

ptio

n. Italian

Buffet.

http

://w

ww

.mpi

a.de

/rin

g200

7

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Tra

vel

Info

rmati

on

(24

Octo

ber

2007)

Co

min

g t

o G

erm

any

is

usu

ally

ver

y e

asy

, fr

om

mo

st c

ou

ntr

ies

no

vis

a i

s re

qu

ired

, ju

st a

pas

spo

rt w

ill

do

.N

ever

thel

ess

ple

ase

do

ub

le c

hec

k.

All

par

tici

pan

ts a

rriv

ing

via

air

pla

ne s

ho

uld

tra

vel

to

Mu

nic

h a

irp

ort

. F

rom

th

e a

irp

ort

, M

un

ich

an

d R

ing

ber

gC

astl

e ca

n b

e r

each

ed v

ia p

ub

lic

tran

spo

rtat

ion

(~

10

0 k

m).

Fo

r th

e c

ity

of

Mu

nic

h t

ran

spo

rtat

ion

ser

vic

es(c

om

mu

ter

trai

ns,

un

der

gro

un

d t

rain

s, b

uss

es)

are p

rov

ided

by

th

e M

VV

.

Ho

w t

o r

each

Rin

gb

erg

Ca

stle

by

pu

bli

c t

ran

spo

rta

tio

n

Fro

m M

un

ich

air

po

rt t

ake e

ith

er t

he "

S-B

ahn

" o

r th

e L

uft

han

sa A

irp

ort

Sh

utt

le b

us

and

go

to

th

e m

ain

sta

tio

n i

nM

un

ich

("H

aup

tbah

nh

of"

). B

oth

op

tio

ns

wil

l ta

ke a

rou

nd

40

min

ute

s. I

f y

ou

go

wit

h t

he S

-Bah

n t

ry t

o g

et a

"Bay

ern

Tic

ket

Sin

gle

" (1

9 E

uro

s),

wh

ich

is

val

id f

or

on

e p

erso

n f

or

the w

ho

le d

ay i

n B

avar

ia -

it

wil

l th

us

be

val

id a

lso

in

th

e t

rain

fro

m M

un

ich

to

Rin

gb

erg

. Y

ou

nee

d t

o v

alid

ate t

he t

ick

et u

sin

g t

he s

mal

l b

lue m

ach

ines

as

yo

u e

nte

r th

e S

-bah

n s

tati

on

. G

oin

g w

ith

th

e s

hu

ttle

bu

s w

ill

cost

yo

u 1

0 E

uro

(p

ayab

le t

o t

he d

riv

er),

an

d y

ou

wil

ln

eed

an

oth

er t

ick

et f

or

the t

rain

fro

m M

un

ich

to

Rin

gb

erg

. A

tax

i co

sts

aro

un

d 6

0 E

uro

fro

m t

he a

irp

ort

to

th

ece

ntr

al s

tati

on

.

Fro

m M

un

ich

cen

tral

sta

tio

n t

o R

ing

ber

g y

ou

hav

e t

o t

ake t

he B

ayri

sch

e O

ber

lan

db

ahn

, n

ick

nam

ed "

BO

B".

It

leav

es f

rom

tra

cks

27

to

36

, at

th

e n

ort

her

n s

ide o

f th

e s

tati

on

. T

he

ver

y l

ast

trai

n l

eav

es s

ho

rtly

bef

ore

mid

nig

ht.

Th

e ti

cket

off

ice i

s lo

cate

d c

lose

to

th

ese

trac

ks

and

no

t in

th

e m

ain

hal

l o

f th

e s

tati

on

. If

yo

u a

lrea

dy

hav

e a

"Bay

ern

Tic

ket

Sin

gle

" y

ou

do

no

t n

eed

to

go

to

th

e t

ick

et o

ffic

e a

nd

can

go

dir

ectl

y t

o t

he t

rain

. T

he

"BO

B"

trai

ns

are c

om

po

sed

ou

t o

f se

ver

al c

ars.

No

t al

l w

ill

go

to

"T

eger

nse

e"

sin

ce t

he t

rain

s ar

e s

pli

t o

n t

hei

r w

ay s

ou

th.

So

wat

ch o

ut

that

yo

u g

et o

n t

he r

igh

t ca

r. G

o w

ith

th

e "

BO

B"

to t

he f

inal

sta

tio

n "

Teg

ern

see".

Tra

vel

tim

e: R

ou

gh

lyo

ne

ho

ur.

BO

B t

imet

able

: S

atu

rday

s/S

un

day

s/H

oli

day

s, w

ork

ing

day

s.

If n

o s

pec

ial

arra

ng

emen

t w

as m

ade,

yo

u s

ho

uld

tak

e a

tax

i at

Teg

ern

see m

ain

sta

tio

n t

o "

Sch

loss

Rin

gb

erg

". T

he

pri

ce f

or

the t

axi

to R

ing

ber

g C

astl

e sh

ou

ld b

e l

ess

than

20

Eu

ros.

Ph

on

e n

um

ber

s to

cal

l a

cab

at

Teg

ern

see m

ain

stat

ion

are

:

Tax

i T

ag u

nd

Nac

ht:

Tel

efo

n:

+4

98

02

2 2

01

1

Tax

i T

hel

en:

Tel

efo

n:

+4

98

02

2 3

03

0 o

der

+4

91

71

38

62

00

4

Tax

i C

om

pan

y:

Tel

efo

n:

+4

98

02

2 9

94

45

T

axi

Sie

fert

: T

elef

on

: +

49

80

22

27

18

18

T

axi-

Sta

nd

Bad

Wie

ssee

: T

elef

on

: +

49

80

22

81

03

1

Tax

i S

eid

ler:

Tel

efo

n:

+4

91

71

45

20

42

0

Tax

iver

ein

igu

ng

Teg

ern

seer

Tal

: T

elef

on

: +

49

80

22

20

11

T

axi

Sei

dl:

Tel

efo

n:

+4

98

02

9 1

24

9

Tax

i E

cker

t: T

elef

on

: +

49

17

1 7

75

73

86

T

axi

Wo

lfg

er:

Tel

efo

n:

+4

98

02

2 6

58

00

Ph

on

e n

um

ber

of

Rin

gb

erg

Ca

stle

: +

49

80

22

/27

90

Fo

r th

ose

wh

o s

tay

ov

ern

igh

t in

th

e h

ote

l P

ark

resi

den

z l

eav

e B

OB

at

the s

tati

on

"G

mu

nd

" an

d t

ake a

tax

i (~

15

Eu

ro)

to t

he h

ote

l. Y

ou

can

als

o a

sk t

he h

ote

l fo

r a

sh

utt

le t

axi.

Yo

u a

lso

mig

ht

wan

t to

ch

eck

th

e r

esp

ecti

ve

sect

ion

of

the R

ing

ber

g C

astl

e w

ebp

age.

Con

tact

ph

on

e n

um

ber

s:

Ste

fan H

ipple

r (c

ell

phone)

: +

49 (

0)

176 2

33 9

7516

Wolf

gan

g B

randner

(ce

ll p

hone)

:+49 (

0)

151 1

07 1

3266

http

://w

ww

.mpi

a.de

/rin

g200

7

Thu

rsda

y, N

ov 1

9:0

0 R

eso

lve

d S

tell

ar P

op

ula

tio

ns

(4a

- ch

air

Han

s-W

alt

er R

ix)

Pro

per

Motions

of G

alac

tic

Com

pac

t O

bje

cts

- Brian

Cam

eron

The

orb

ital

motion o

f th

e A

rches

clu

ster

fro

m K

eck

LG

S- a

nd V

LT N

GS-

AO

obse

rvat

ions

- And

rea

Stol

te

Bulg

e an

d d

isk

fiel

ds

in M

31 w

ith t

he

ALT

AIR

AO

sys

tem

and N

IRI on G

emin

i N

ort

h -

Knu

t O

lsen

10:3

0 C

offe

e11:0

0 L

GS

Up

gra

de

s an

d O

pe

rati

on

s (4

b -

chai

r A

nd

reas

Gli

nd

em

an

n)

Upgr

ades

to t

he

puls

ed s

um

fre

quen

cy las

er o

per

ated

on t

he

5m

at

Pal

om

ar -

Ed

Kib

blew

hite

SuPy:

sci

ence

cas

es for

the

infr

ared

tip

-tilt

sen

sor

for

the

Subar

u las

er s

yste

m -

Miw

a G

oto

The

Par

anal

/VLT

AO

Fac

ility

- S

ylva

in O

bert

i12:3

0 L

unch

14:0

0 L

GS

Op

era

tio

ns

(cont’d

) +

Dis

cu

ssio

n (

4c

- ch

air

Ere

z R

ibak

) L

GS-

AO

at

the

VLT

, com

mis

sionin

g re

port

- M

arku

s K

asper

SIN

FON

I an

d L

GS

at t

he

VLT

, com

mis

sionin

g re

port

- S

tefa

n St

röbe

le (

10 m

in)

Kec

k LG

S A

O e

xper

ience

- R

andy

Cam

pbe

ll G

emin

i LG

S A

O e

xper

ience

- F

ranç

ois

Rig

aut

(5m

in)

Im

pro

ving

the

Sky

Cove

rage

of th

e G

emin

i LG

S A

O s

yste

m -

Dav

id A

nder

sen

(5m

in)

15:3

0 P

ost

er V

iew

ing +

Cof

fee

16:0

0 M

ilk

y W

ay &

Be

yo

nd

(4d -

chai

r M

iwa G

oto

) K

eck

/ O

SIR

IS L

GSA

O O

bse

rvat

ions

of th

e Eje

cta

from

the

Cla

ssic

al N

ova

, V723 C

as -

Ran

dy C

ampbe

ll U

sing

LGS

AO

to S

tudy

Stel

lar

and G

as K

inem

atic

s in

the

Cen

tral

100 p

c of A

GN

- E

rin

Hic

ks A

O Im

agin

g an

d S

pec

trosc

opy

of N

GC

6240 -

Cla

ire

Max

Dee

p v

iew

of th

e A

rp 2

99 inte

ract

ing

syst

em w

ith A

ltai

r-LG

S -

Dam

ien

Gra

tado

ur18:3

0 D

inne

r

Rin

gber

g W

orks

hop

2007 - Pro

gra

mme (

v071025)

Ast

ron

omy

wit

h L

GS

AO

Frid

ay, N

ov 2

9:0

0 S

ola

r S

yst

em

(5a

- ch

air

Mark

us

Kasp

er)

Applic

atio

ns

of LG

S-A

O t

o S

ola

r Sy

stem

Sci

ence

s -

Chr

isto

phe

Dum

as A

O Im

agin

g of G

iant

Pla

net

s usi

ng

LG

S -

Imke

de

Pate

r

Sea

rchin

g an

d C

har

acte

rizi

ng

Multip

le T

roja

n A

ster

oid

s W

ith L

GS

AO

Sys

tem

s -

Fran

ck M

arch

is10:3

0 C

offe

e11:0

0 L

BT

LG

S (

5b -

chai

r R

ic D

avie

s)

Las

er G

uid

e St

ars

for

the

LBT

- S

ebas

tian

Rab

ien

What

's t

he

bes

t LG

S upgr

ade

for

LIN

C-N

IRVA

NA

? -

Wol

fgan

g G

ässler

LB

T L

GS

syst

em: fi

rst

sim

ula

tion r

esults

and s

enso

r optica

l des

ign -

Lor

enzo

Bus

oni /

Enr

ico

Pinn

a S

cien

ce P

ersp

ective

s fo

r Lu

cife

r an

d L

GSA

O a

t LB

T -

And

reas

Qui

rren

bach

12:3

0 L

unch

14:0

0 E

nd

of

Wo

rksh

op

Wed

nesd

ay, O

ct 3

19:0

0 B

row

n D

warfs

(3a

- ch

air

Imk

e d

e P

ate

r)

A K

eck

Lase

r G

uid

e St

ar A

dap

tive

Optics

Stu

dy

of V

ery

Low

Mas

s B

inar

ies: C

onst

rain

ing

Evo

lutionar

y M

odel

s w

ith N

ew D

ynam

ical

Mas

ses

- Q

uinn

Kon

opac

ky A

stro

met

ric

monitori

ng

of bin

ary

bro

wn d

war

fs w

ith P

AR

SEC

- M

icae

la S

tum

pf

Bin

ary

Bro

wn D

war

fs fro

m K

eck

LG

S A

O -

Mik

e Li

u10:3

0 C

offe

e11:0

0 t

o 1

8:3

0 E

xcu

rsio

n t

o S

alz

bu

rg18:4

5 C

on

fere

nce

Din

ne

r -

Bav

aria

n B

uffe

t

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

http://ww

w.m

pia.de/ring2007

Last n

am

e First n

am

e Institu

tion

Ageo

rges N

ancy E

SO

Santia

go d

e Chile

Am

mons M

ark U

C S

anta

Cru

z

Andersen

David

NR

C-H

IA V

ictoria

Bra

ndner W

olfg

ang M

PIA

Heid

elberg

Britto

n M

atth

ew C

altech

Pasa

den

a

Buso

ni L

oren

zo O

bserva

tory o

f Arcetri

Cam

eron B

rian C

altech

Pasa

den

a

Cam

pbell R

andy K

eck Observa

tory H

aw

aii

Cresci G

iova

nni M

PE

Garch

ing

Davies R

ic MP

E G

arch

ing

De P

ater Im

ke UC

Berkeley

Dum

as C

hristo

phe E

SO

Santia

go d

e Chile

Egner S

ebastia

n M

PIA

Heid

elberg

Eisen

hauer F

rank M

PE

Garch

ing

Förster S

chreib

er Nata

scha M

PE

Garch

ing

Gässler W

olfg

ang M

PIA

Heid

elberg

Gen

zel Rein

hard

MP

E G

arch

ing

Ghez A

ndrea

UC

Los A

ngeles

Glin

dem

ann A

ndrea

s ESO

Garch

ing

Goodsa

ll Tim

Dep

t. of A

strophysics O

xford

Goto

Miw

a M

PIA

Heid

elberg

Gra

ham

Jam

es UC

Berkeley

Gra

tadour D

am

ien G

emin

i La S

erena

Hastie M

ora

g M

MT

Observa

tory A

rizona

Hen

nin

g T

hom

as M

PIA

Heid

elberg

Herrio

t Glen

NR

C-H

IA V

ictoria

Hicks E

rin M

PE

Garch

ing

Hip

pler S

tefan M

PIA

Heid

elberg

Holzlö

hner R

onald

ESO

Garch

ing

Hubin

Norb

ert ESO

Garch

ing

Iye Masa

nori N

AO

Tokio

Kasp

er Marku

s ESO

Garch

ing

Kib

blew

hite E

dw

ard

Univ. o

f Chica

go

Konopacky Q

uin

n U

C L

os A

ngeles

Last n

am

e First n

am

e Institu

tion

Larkin

Jam

es UC

Los A

ngeles

Law

Nich

ola

s Caltech

Pasa

den

a

Liu

Mich

ael IfA

Honolu

lu

Mannucci F

ilippo IN

AF

-IRA

Arcetri

March

is Fra

nck U

C B

erkeley / SE

TI

Max C

laire U

C S

anta

Cru

z

Morris T

im U

niversity o

f Durh

am

Myers R

ichard

University o

f Durh

am

Now

ak N

ina M

PE

Garch

ing

Oberti S

ylvain

ESO

Garch

ing

Olsen

Knut N

OA

O T

ucso

n

Ott T

hom

as M

PE

Garch

ing

Pasq

uin

i Luca

ESO

Garch

ing

Peter D

iethard

MP

IA H

eidelb

erg

Pin

na E

nrico

Observa

tory o

f Arcetri

Quirren

bach

Andrea

s LSW

Heid

elberg

Rabien

Seb

astia

n M

PE

Garch

ing

Raja

gopal Ja

yadev C

TIO

/NO

AO

La

Seren

a

Rib

ak E

rez Tech

nio

n H

aifa

Rid

gw

ay S

usa

n C

TIO

/NO

AO

La S

erena

Rig

aut F

ranço

is Gem

ini O

bserva

tory H

ilo

Rix H

ans-W

alter M

PIA

Heid

elberg

Rocca

taglia

ta V

eronica

MP

IA H

eidelb

erg

Salin

ari P

iero IN

AF

Firen

ze

Sch

wab C

hristia

n Z

AH

/LSW

Heid

elberg

Sim

ard

Luc N

RC

-HIA

Victo

ria

Sto

lte Andrea

UC

Los A

ngeles

Strö

bele S

tefan E

SO

Garch

ing

Stu

mpf M

icaela

MP

IA H

eidelb

erg

Tacco

ni-G

arm

an L

ow

ell ESO

Garch

ing

Wrig

ht S

helley U

C L

os A

ngeles

Zin

necker H

ans A

IP P

otsd

am

Ringberg W

orkshop 2007 - P

artic

ipants (v0

71025)

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - P

oste

rs (v071025)

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Impro

ving th

e Sky Coverage o

f the G

emin

i LG

S AO

system - D

avid Andersen

A Laser G

uid

e Star h

as been

successfu

lly dep

loyed

on G

emin

i-North fo

r use w

ith th

e A

ltair Adap

tive O

ptics

(AO

) system.

The sky

coverage

of th

e G

emin

i AO

system is

limited

, how

ever, by th

e relatively sm

all patro

l field availab

le fo

r the N

atural G

uid

e Star (N

GS) tip

-tilt (T/T

) wavefro

nt sen

sor (W

FS). At th

e request o

f the G

emin

i directo

r and

the G

emin

i Adap

tive O

ptics Scien

ce W

orkin

g Gro

up (G

AO

SWG

), we h

ave explo

red th

e possib

ility of re-co

nfigu

ring th

e N

IRI o

n-in

strum

ent W

FS to o

perate as a n

ear-infrared

T/T

pro

be

over

a larger

FOV

(u

p

to

60

arcsec in

diam

eter), findin

g th

at su

bstan

tial im

pro

vemen

ts in sky co

verage are possib

le, u

p to

almost 6

0%

at the N

orth

Galactic Po

le.

First PAR

SEC

/LIDA

R m

esosp

heric So

diu

m p

rofiles ab

ove P

aranal - Stefan

Hip

pler et al.

We rep

ort o

n fi

rst measu

remen

ts of th

e meso

spheric So

diu

m layer u

sing PA

RSE

C/LID

AR

at the E

SO V

LT.

Physical O

ptics Sim

ulatio

n o

f LG

S Pro

pagatio

n -

Ronald H

olzlöhner

We rep

ort o

n physical o

ptics sim

ulatio

ns o

f LGS p

ropagatio

n an

d im

aging in th

e p

lanned

G

RA

AL

wavefro

nt

senso

r (WFS).

We m

odel

differen

t launch

telesco

pes

(LTS)

with

realistic

aberratio

ns, th

e tu

rbulen

t atmosp

here

, a sodiu

m layer o

f finite

thickn

ess, the

dow

nlin

k p

ropagatio

n o

f the retu

rn ligh

t, the V

LT, and fi

nally th

e 7

x7 N

AC

O o

r 40x40

GR

AA

L WFS. W

e stu

dy b

oth

long-ex

posu

re an

d in

stantan

eous im

ages and co

mpute

spot

size statistics. T

he resu

lts agree

with

observatio

n an

d en

able

us

to o

ptim

ize th

e LT

S diam

eter and d

evise design

rules.

Poster Sessions: Tu, Th 1

5:3

0-1

6:0

0h

http

://w

ww

.mpi

a.de

/rin

g200

7

Rin

gber

g W

orks

hop

2007 - Abstra

cts

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Mat

thia

s Tec

za/T

im G

oods

all: T

he

Oxfo

rd S

WIF

T inte

gral

fiel

d s

pec

trogr

aph

We

pre

sent

the d

esig

n a

nd l

abora

tory

tes

t re

sults

of

the

Oxfo

rd S

WIF

T in

tegr

al fi

eld

spec

trogr

aph, a

ded

icat

ed I

and

z ban

d in

stru

men

t (0

.65

mic

ron -

1.0

mic

ron a

t R

~4000),

des

igned

to b

e u

sed

in c

onju

nct

ion

with t

he P

alom

ar l

aser

guid

e s

tar

adap

tive

optics

sy

stem

(P

ALA

O,

and

its

pla

nned

upgr

ade

PALM

3k)

. SW

IFT

si

multan

eousl

y pro

vides

sp

ectr

a of

~4000 s

pat

ial

elem

ents

, ar

range

d in

a

rect

angu

lar

fiel

d-o

f-vi

ew of

44 ! 89

pix

els.

It h

as t

hre

e on-t

he-

fly

sele

ctab

le p

ixel

sca

les

of

0.2

35",

0.1

6"

and 0

.08". It

build

s on

two r

ecen

t dev

elopm

ents

(i)

the i

mpro

ved a

bili

ty o

f se

cond

gener

atio

n a

dap

tive

optics

sy

stem

s to

corr

ect

for

atm

osp

her

ic t

urb

ule

nce

at

wav

elen

gths

less

than

or

equal

to

1

mic

ron, an

d (ii)

the a

vaila

bili

ty o

f C

CD

arr

ay d

etec

tors

with

hig

h quan

tum

effi

cien

cy a

t ve

ry r

ed w

avel

engt

hs

(clo

se t

o t

he

silic

on b

and

edge

). C

om

bin

ing

thes

e w

ith a

sta

te-o

f-th

e-ar

t in

tegr

al fi

eld

unit d

esig

n usi

ng

an a

ll-gl

ass

imag

e s

licer

, SW

IFT

's d

esig

n p

rovi

des

ve

ry h

igh

thro

ugh

put

and low

sca

tter

ed l

ight.

The im

age s

licer

and m

ost

of

the

optics

are

finis

hed

while

the m

echan

ics

is c

urr

ently

in its

man

ufa

cturi

ng

phas

e."

Inte

grat

ion

will

sta

rt

in S

epte

mber

2007 w

ith

test

sta

rtin

g in

Jan

uar

y 2008 a

nd

com

mis

sionin

g an

d fi

rst

light

in

spri

ng

2008.

She

lley W

righ

t: St

ar F

orm

ing

Gal

axie

s in

the

Ear

ly U

niv

erse

: Spat

ially

Res

olv

ed

Spec

trosc

opy

with K

eck

LGS

AO

will

pre

sent

resu

lts

of

an o

n-g

oin

g st

udy

of

the d

ynam

ics

of

hig

h-r

edsh

ift s

tar

form

ing

gala

xie

s at

su

b-k

ilopar

sec

scal

es.

Obse

rvat

ions

wer

e

mad

e

usi

ng

the

inte

gral

fiel

d

spec

trogr

aph

(IFS

) O

SIR

IS a

nd

the

Kec

k La

ser

Guid

e S

tar

Adap

tive

O

ptics

(L

GSA

O)

syst

em. F

or

six z

~1.5

gal

axie

s I w

ill p

rese

nt

reso

lved

H-a

lpha

kinem

atic

s w

ithin

the c

entr

al

arcs

econd

at

0.1

" re

solu

tion.

Kin

emat

ics,

dis

k m

odel

ing,

m

erge

r sc

enar

ios,

m

ass

dis

trib

utions,

sta

r fo

rmat

ion r

ates

, an

d m

etal

licity

for

each

gal

axy

will

be

dis

cuss

ed.

In

additio

n, I

will

dis

cuss

our

exper

ience

usi

ng

an L

GSA

O s

yste

m c

ouple

d w

ith

an I

FS o

n

fain

t ex

trag

alac

tic

targ

ets.

Hig

hlig

hte

d sh

all be

issu

es o

f LG

SAO

acq

uis

itio

n o

f fa

int

tip-t

ilt

star

s w

ith

a sm

all

IFS

fiel

d o

f vi

ew, PSF

est

imat

ion

for

an I

FS, bea

m s

mea

ring

effe

cts

on

morp

holo

gy a

nd k

inem

atic

s, a

nd futu

re d

irec

tions.

http

://w

ww

.mpi

a.de

/rin

g200

7

Rin

gber

g W

orks

hop

2007 - Posters

(v0

71025)

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

A L

GS

WFS

tes

t ben

ch d

emonst

rato

r fo

r T

MT

- O

livie

r La

rdie

re, G

lenn

H

erriot

Lase

r G

uid

e S

tars

(LG

S) a

llow

, in

theo

ry, a

full

sky

cove

rage

. H

ow

ever

LG

S h

ave t

hei

r ow

n lim

itat

ions.

In p

articu

lar,

for

the N

a LG

Ss, t

he a

rtifi

cial

sta

r is

elo

nga

ted d

ue t

o t

he

Na

laye

r th

ickn

ess,

and

the t

empora

l an

d sp

atia

l va

riab

ility

of

the N

a at

om

den

sity

in

duce

s ch

angi

ng

wav

efro

nt

mea

sure

men

t er

rors

. In

the fra

mew

ork

of

the T

hir

ty-M

eter

-Te

lesc

ope p

roje

ct (

TM

T), t

he A

O-L

ab o

f th

e U

niv

ersi

ty o

f V

icto

ria

is b

uild

ing

a LG

S-si

mula

tor

test

bed

in o

rder

to

ass

ess

the p

erfo

rman

ce o

f w

avef

ront

sensi

ng

algo

rith

ms

when

usi

ng

Na

LGSs

. The d

esig

n of

this

ben

ch i

s pre

sente

d, as

wel

l as

firs

t la

bora

tory

im

ages

obta

ined

for

a 30x30 S

H-W

FS in t

he

TM

T c

ase. T

his

ben

ch i

s not

limited

to

SH

-W

FS,

but

can s

erve

as

a LG

S-si

mula

tor

test

bed

to a

ny oth

er L

GS-

AO

pro

ject

s fo

r w

hic

h N

a la

yer

fluct

uat

ions

can b

e an

iss

ue.

A lunar

sci

ntillo

met

er t

o m

easu

re g

round-lay

er s

eein

g -

Jaya

dev

Raj

agop

al

New

tec

hniq

ues

lik

e LG

S-A

O r

equir

e a

det

aile

d kn

ow

ledge

of

the t

urb

ule

nce

pro

file

. T

he

inte

nsi

ty o

f G

round

Laye

r (G

L) tu

rbule

nce

det

erm

ines

th

e g

ain e

xpec

ted f

rom

gr

ound-lay

er A

O,

while

its

th

ickn

ess

defi

nes

th

e si

ze of

the

com

pen

sate

d fiel

d. T

he

exte

nt

of

the

turb

ule

nce

in t

he

firs

t fe

w m

etre

s is a

lso

im

port

ant

in d

eter

min

ing

the

optim

um

hei

ght

of

futu

re d

om

es, e

spec

ially

for

Anta

rctic

site

s w

her

e t

he

GL is

stro

ng.

A

sim

ple

and

accu

rate

way

for

det

erm

inin

g th

e G

L tu

rbule

nce

is

by

mea

suri

ng

sola

r an

d

lunar

sci

ntilla

tion. W

e pre

sent

a new

lunar

sci

ntillo

met

er, "L

uSc

i". R

obust

met

hods

for

pro

file

res

tora

tion, i

nco

rpora

ting

effe

cts

of

lunar

phas

es, a

re d

evel

oped

and fi

rst

test

s of

the

tech

niq

ue

are

des

crib

ed.

Post

er S

ession

s: Tu

, Th

15:3

0-1

6:0

0h

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - A

bstra

cts

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Andrea Stolte: T

he o

rbital m

otio

n o

f the A

rches clu

ster from

Keck L

GS-A

O

and V

LT N

GS-A

O o

bservatio

ns

The ex

cellent astro

metric accu

racy of ~

1 m

illiarcsecond p

rovid

ed b

y adap

tive o

ptics (A

O)

observatio

ns

allow

ed us to

measu

re th

e pro

per m

otio

n o

f the G

alactic center A

rches

cluster.

Com

bin

ing

Keck/N

IRC

2

LGS-A

O

and

VLT

N

AO

S/CO

NIC

A

NG

S-AO

observatio

ns, w

e h

ave m

easured

the p

roper m

otio

n o

f the A

rches w

ith resp

ect to th

e su

rroundin

g field p

opulatio

n to

212 +

/- 20 km

/s. The p

roper m

otio

n m

easurem

ent, w

hen

co

mbin

ed with th

e kn

ow

n radial velo

city of th

e cluster, yield

s a first estim

ate of 2

32 +

/- 22 km

/s for th

e 3

D sp

ace m

otio

n o

f the A

rches in

the G

alactic center p

oten

tial. I will

discu

ss the im

plicatio

ns o

f the large velo

city of th

e cluster in

view o

f possib

le form

ation

scenario

s of yo

ung, m

assive clusters in

a den

se environm

ent su

ch as th

e cen

ter of o

ur

Galax

y.

Stefan Ströbele: SINFO

NI &

LGSF co

mm

issionin

g

Micaela Stum

pf: Astro

metric m

onito

ring o

f bin

ary bro

wn d

warfs w

ith PA

RSE

C

Since

their d

etection B

row

n Dw

arfs have

always b

een o

f special in

terest, but th

e ab

sence

of a clear m

ass-lum

inosity relatio

n m

akes it hard to

determ

ine th

eir physical p

roperties

and to

test theo

ries of fo

rmatio

n p

rocesses, in

ner stru

cture an

d atmosp

heres. Sp

atially reso

lved

bro

wn

dw

arf bin

aries pro

vide

the

uniq

ue

opportu

nity

to

determ

ine

the

dyn

amical m

asses of th

e b

inary co

mponen

ts indep

enden

tly from

theo

retical models. W

e now

presen

t high

-resolu

tion m

ulti-ep

och E

SO/V

LT N

GS an

d LGS A

O o

bservatio

ns o

f the

orb

ital motio

n o

f the b

ench

mark b

row

n d

warf b

inary K

elu 1

AB

. The o

bservatio

ns are

part o

f our astro

metric m

onito

ring p

rogram

of b

inary b

row

n d

warfs w

ith relatively sh

ort

orb

ital perio

ds. W

e carry out fi

tting o

f the o

rbital p

arameters fo

r Kelu 1 an

d d

erive a first

dyn

amical m

ass estimate o

f the b

inary. In ad

ditio

n w

e p

resent th

e fi

rst spatially reso

lved H

+K

-ban

d sp

ectra for th

e b

inary

EpsIn

di B

C ach

ieved with PA

RSE

C w

hich

pro

vide th

e m

ost reliab

le w

ay for sp

ectral classificatio

n in

the N

IR, as w

ell as com

parin

g them

with

the

existin

g resolved

H-b

and sp

ectra from

NA

CO

. These resu

lts will h

elp to

impro

ve th

e understan

din

g of th

e physical p

arameters o

f bro

wn d

warfs an

d to ad

just th

e theo

ry of

their evo

lutio

n an

d im

pro

ve the in

terpretatio

n o

f the o

bservatio

ns o

f bro

wn d

warfs.

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - A

bstra

cts

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Mark A

mm

ons: CA

TS o

bservatio

ns o

f 11 C

han

dra so

urces in

GO

OD

S-S at z~

1 u

sing K

eck LGSA

O

The C

enter fo

r Adap

tive O

ptics (C

fAO

) Treasury Su

rvey (CA

TS) is co

llecting n

ear-IR

imagin

g and sp

ectrosco

py of A

GN

and h

igh-red

shift galax

ies in several regio

ns o

f the

sky, inclu

din

g GO

OD

S, EG

S, and C

OSM

OS, to

take ad

vantage o

f the p

resence

of o

ther

deep

datasets in

these

regions." R

ecently, C

AT

S h

as observed 1

1 C

han

dra so

urces (1

0

AG

N) at z ~

1 in

the G

OO

DS-So

uth

field

with th

e laser guid

e star adap

tive o

ptics

(LGSA

O) system

at Keck

Observato

ry." We co

mbin

e th

is K‚ b

and im

aging w

ith A

CS

imagin

g in th

e B

, V, I, and z b

ands to

obtain m

ulti-co

lor im

aging at a sp

atial resolu

tion

better th

an 80 m

as in all ban

ds." W

e attem

pt to

remove cen

tral optical p

oin

t sources

from

the o

ptical A

GN

usin

g the G

ALFIT

(Peng et al. 2

002) ro

utin

e." W

e fi

t Bru

zual &

C

harlo

t (2003) tau

-models to

the resid

uals an

d fi

nd yo

ung, d

usty stellar p

opulatio

ns in

th

e cen

tral 1-2

kpc (th

e mean

central o

ptical d

epth

at rest-frame 5

00 n

m is 4

-5)." W

e co

mpare

the age

gradien

ts in th

ese A

GN

to a fi

eld sam

ple

. I will also

high

light o

ther

recent resu

lts from

the C

AT

S su

rvey, inclu

din

g measu

remen

ts of th

e H

-ban

d fl

ux o

f a z =

1.3 su

pern

ova an

d OSIR

IS o

bservatio

ns o

f z~1 A

GN

and LIR

GS." I w

ill specifi

cally co

ncen

trate o

n resu

lts that are

unobtain

able w

ith any o

ther in

strum

entatio

n to d

isplay

the p

ow

er of th

e new

suite o

f laser guid

e star adap

tive optics system

s.

Matthew

Britton: T

he Po

int Sp

read Fu

nctio

n o

f a Laser Guid

e Star Adap

tive O

ptics System

The p

oin

t spread fu

nctio

n (PSF) o

f a single

conju

gate ad

aptive

optics system

varies in

field

lo

cation

due

to an

isoplan

atism." Tem

poral

variability

in th

e PSF

arises

as th

e atm

osp

heric tu

rbulen

ce pro

file

evolves in

time." T

his evo

lutio

n of th

e PSF

in both

time

and fi

eld lo

cation co

mplicates th

e interp

retation o

f observatio

ns acq

uired

with

adap

tive optics system

s." Recen

tly, measu

remen

ts from

turb

ulen

ce m

onito

ring eq

uip

men

t have

been u

sed in su

ccessfully p

redictin

g the P

SF evolu

tion o

f a natu

ral guid

e star adap

tive optics system

s." This p

resentatio

n will d

iscuss p

rosp

ects for ap

plyin

g this tech

niq

ue to

laser gu

ide star ad

aptive o

ptics system

s.

Lorenzo Busoni: L

BT

LG

S system: fi

rst simulatio

ns resu

lts and sen

sor o

ptical

design

http

://w

ww

.mpi

a.de

/rin

g200

7

Rin

gber

g W

orks

hop

2007 - Abstra

cts

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

And

reas

Qui

rren

bach

: Sci

ence

Per

spec

tive

s fo

r Lu

cife

r an

d L

GSA

O a

t LB

T

Seb

astia

n Rab

ien:

Las

er G

uid

e St

ars

for

the

LBT

Ere

z Rib

ak: C

an las

er b

eaco

ns

be

use

d a

s gu

ide

star

s?

We

hav

e ad

opte

d LI

DA

Rs

as b

eaco

ns

for

adap

tive

optics

, and

indee

d t

hey

funct

ion q

uite

wel

l. H

ow

ever

, w

hen

the

tele

scope g

row

s big

ger

and

the b

eam

ret

urn

too

wea

k, w

e d

o

wis

h for

som

ethin

g bet

ter, s

om

ethin

g w

ithout

spot

elonga

tion, a

guid

e s

tar

that

does

not

requir

e fa

st s

hutt

ers

and c

om

ple

x d

etec

tors

. The

pri

ce t

o p

ay,

it s

eem

s, i

s in

com

ple

x

optics

, so

me o

f it

at

the t

ransm

itting

and

som

e at

the r

ecei

ving

end. U

sing

idea

s fr

om

oth

er fi

elds

of

optics

, it

mig

ht

be p

oss

ible

to

ove

rcom

e so

me o

f th

e lim

itat

ions

pose

d b

y th

e p

ure

, nar

row

las

er b

eam

s now

em

plo

yed. I

f su

cces

sful,

we w

ill a

chie

ve a

wid

e a

rtifi

cial

as

teri

sm w

hic

h w

ill al

low

us

to se

par

ate

atm

osp

her

ic la

yers

usi

ng

sim

ple

wav

e fr

ont

senso

rs.

http

://w

ww

.mpi

a.de

/rin

g200

7

Rin

gber

g W

orks

hop

2007 - Abstra

cts

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Brian

Cam

eron

: Pro

per

Motions

of G

alac

tic

Com

pac

t O

bje

cts

It i

s now

ge

ner

ally

ap

pre

ciat

ed t

hat

th

e s

pac

e v

eloci

ties

of

com

pac

t obje

cts

(puls

ars,

m

agnet

ars,

LM

XB

s an

d H

MX

Bs)

dir

ectly

info

rm u

s as

to

thei

r ori

gins

and c

onst

rain

thei

r lif

etim

es. H

ere, w

e w

ill r

eport

on a

pro

gram

to

mea

sure

the p

roper

motions

of

Gal

actic

com

pac

t obje

cts

usi

ng

the

LG

S-A

O s

yste

m o

n th

e K

eck I

I te

lesc

ope. W

e w

ill a

lso

dis

cuss

th

e lim

its

of

ground-b

ased

ast

rom

etry

with a

dap

tive

optics

and

consi

der

the im

plic

atio

ns

of th

is w

ork

for

the

des

ign o

f fu

ture

adap

tive

optics

sys

tem

s.

Ran

dy C

ampb

ell:

Kec

k /

OSI

RIS

LG

SAO

Obse

rvat

ions

of th

e Eje

cta

from

the

Cla

ssic

al N

ova

, V723 C

as

We

pre

sent

the s

pat

ially

res

olv

ed v

eloci

ty s

truct

ure

of

the V

723 C

as n

ova

shel

l obse

rved

at

thre

e ep

och

s: 1

3 S

ep 2

005, 3

1 A

ug

2006, a

nd"

3 Se

p 2

007. S

trong

coro

nal

em

issi

on li

nes

of

[Si

VI]

," [

Al

IX], a

nd

[CaV

III]

ar

e pre

sent

in th

e ex

pan

din

g sh

ell.

The co

ntinuum

-su

btr

acte

d dat

a cu

bes

re

veal

the

morp

holo

gy of

the n

ova

sh

ell

in 3

dim

ensi

ons.

The

diff

eren

t sp

ecie

s of

emis

sion l

ines

are

inhom

oge

neo

us

and a

rise

fro

m d

istinct

reg

ions

of

the e

ject

a. T

he e

mis

sion h

as a

n el

lipso

idal

shap

e in

the c

ase

of

the [

Al IX

] fe

ature

and h

as

radia

lly s

ymm

etri

c to

rus

shap

e w

ith p

ola

r kn

ots

in t

he

case

of [S

i VI]

and [

CaV

III]

lin

es. W

e m

easu

re

a nea

r-co

nst

ant

expan

sion

velo

city

w

ith

the

multi-ep

och

obse

rvat

ions

and

det

erm

ine a

dis

tance

to

the

syst

em u

sing

expan

sion

par

alla

x. O

ur

dat

a sh

ow

that

rec

ent

nova

e a

re idea

l su

bje

cts

for

the

unpre

ceden

ted s

pat

ial re

solu

tion

in t

he

infr

ared

pro

vided

by

OSI

RIS

with L

GSA

O o

n K

eck

II.

Gio

vann

i Cre

sci:

Model

ing

the

dyn

amic

s of hig

h r

edsh

ift g

alax

ies

with S

INFO

NI

and L

GS

In t

he f

ram

ework

of

the

SIN

S s

urv

ey w

e hav

e obse

rved

~35

hig

h-z

sta

r-fo

rmin

g ga

laxie

s,

sele

cted

in a

var

iety

of

way

s. O

ur

SIN

FON

I in

tegr

al fi

eld d

ata

pro

vide

spat

ially

-res

olv

ed

info

rmat

ion o

n t

he d

ynam

ics,

ste

llar

popula

tions,

met

allic

itie

s, a

nd i

oniz

atio

n st

ate

of

the

gas

on t

ypic

al r

esolv

ed s

cale

s of

1.5

-4 k

pc

from

res

t-fr

ame o

ptica

l sp

ectr

al d

iagn

ost

ics.

T

hes

e" u

niq

ue d

ata

pro

vide t

he p

oss

ibili

ty t

o s

tudy

the r

elat

ion b

etw

een t

he

dyn

amic

al

and

stel

lar

mas

s, th

at

is

of"

fundam

enta

l im

port

ance

to

our

under

stan

din

g of

the

dim

ensi

ons

of th

e hal

o a

nd t

he

evolu

tionar

y st

age

of th

e ga

laxie

s, a

nd it

is d

irec

tly

linke

d t

o c

osm

olo

gica

l si

mula

tions.

We p

rese

nt

the fi

rst

resu

lts

in t

his

dir

ection

from

a

robust

dyn

amic

al !

2 fi

ttin

g of

the o

bse

rved

vel

oci

ty a

nd v

eloci

ty d

isper

sion fi

elds

with

suitab

le r

ota

ting

dis

ks m

odel

s, a

nd d

iscu

ss t

he im

plic

atio

ns

on t

he b

aryo

nic

conte

nt

and

on t

he

dyn

amic

al e

volu

tionar

y st

ate

of th

e ga

laxie

s.

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - A

bstra

cts

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Knut O

lsen: H an

d K

observatio

ns o

f the b

ulge an

d d

isk of M

31 w

ith th

e A

LTA

IR ad

aptive o

ptics system

and N

IRI o

n G

emin

i North

These

are th

e h

ighest reso

lutio

n and d

eepest n

ear-infrared

observatio

ns o

btain

ed to d

ate of th

e in

ner regio

ns o

f M31 an

d d

emonstrate th

e p

rom

ise of gro

und-b

ased ad

aptive o

ptics

for stu

dyin

g the cro

wded

regions o

f nearby galax

ies. We h

ave com

bin

ed o

ur o

bservatio

ns

with

previo

usly

publish

ed

Hubble

Space

Telescope

Near-In

frared

Cam

era an

d M

ulti-

Object Sp

ectrom

eter observatio

ns o

f nin

e M

31 fi

elds an

d h

ave d

erived the co

arse star

form

ation histo

ries of

M31's

bulge

and

inner d

isk. From

fits

to th

e M

_K

lu

min

osity

functio

ns, w

e fi

nd th

e stellar populatio

n m

ix o

f the b

ulge an

d in

ner d

isk to

be d

om

inated

by o

ld, n

early solar-m

etallicity stars. The o

ld p

opulatio

ns, w

hich

we d

efine as h

aving age

>~

6 Gyr, in

deed d

om

inate

the star fo

rmatio

n h

istories at all rad

ii indep

enden

t of th

e relative

contrib

utio

ns o

f bulge an

d d

isk stars." In o

ur least cro

wded d

isk fi

eld, w

e see th

e clear sign

ature o

f the 1

0-kp

c ring, w

ith ~

30%

of th

e stellar m

ass havin

g form

ed ~250 M

yr ago

, superp

osed o

n an

old

metal-p

oor p

opulatio

n." O

ur resu

lts suggest th

at M31 acq

uired

a stab

le disk a lo

ng tim

e ago.

Thom

as Ott: H

igh an

gular reso

lutio

n o

bservatio

ns o

f the G

alactic Cen

ter at th

e VLT

with

LGS-A

O

Imagin

g observatio

ns o

f the G

alactic Cen

ter at the d

iffraction lim

it of th

e V

LT are d

one

regularly. T

han

ks to th

e infrared

wavefro

nt sen

sor o

f the N

AO

S ad

aptive o

ptics system

, th

ese o

bservatio

ns d

on't n

eed th

e assistan

ce o

f a laser guid

e star, sin

ce usin

g the b

right

infrared

so

urce

IRS7

fo

r w

avefront

sensin

g is

straightfo

rward

. T

he

integral

field

sp

ectrom

eter SINFO

NI, h

ow

ever, is only eq

uip

ped

with an

optical w

avefront sen

sor. H

ere w

e presen

t first o

bservatio

ns w

ith LG

S-AO

and co

mpare th

em w

ith p

revious resu

lts.

Diethard Peter: O

ptim

ization o

f a LG

S support w

avefront co

rrector

Based

on

measu

remen

ts perfo

rmed

with

th

e

pyramid

in

frared

wavefro

nt

senso

r PY

RA

MIR

on th

e 3

.5 m telesco

pe o

n C

alar Alto

we d

iscuss th

e design o

f a supportin

g low

ord

er wavefro

nt co

rrector fo

r LG

S-AO

observatio

n. T

he q

uestio

n o

f the sen

sor typ

e (SH

S or pyram

id) is ad

dressed as w

ell as the n

um

ber o

f mode su

bject to

the co

rrection o

f th

e supportin

g system.

http://ww

w.m

pia.de/ring2007

Ringberg W

orkshop 2007 - A

bstra

cts

Astro

nom

y with

Laser Guid

e Star Adap

tive Optics

Ric D

avies: LGS-A

O w

ithout tip

-tilt

Imke de Pater: A

O Im

aging o

f Gian

t Plan

ets usin

g LGS

The gian

t plan

ets Jupiter an

d Satu

rn have b

een im

aged in

detail b

y various sp

acecraft, and

by H

ST. These

images, as w

ell as num

erous am

ateur im

ages, show

that th

e atmosp

heres

are very dyn

amic. H

ow

ever, in ord

er to q

uan

tify such d

ynam

ics, one n

eeds to

determ

ine

the velo

city field

s in these

atmosp

heres to

a high

precisio

n. T

his can

only b

e done via

images at h

igh sp

atial resolu

tion, w

hich

histo

rically could o

nly b

e done w

ith sp

acecraft and

HST. W

ith A

O b

eing availab

le at large

telescopes, in

prin

ciple su

ch p

rojects can b

e done

from

the gro

und. In

July 2

006 th

e new

Red

Oval o

n Jupiter w

as passin

g Great R

ed Sp

ot, an

even

t we tried

to im

age w

ith the W

.M. K

eck o

bservato

ry usin

g LGSA

O. A

lthough th

e LGS

part d

id n

ot w

ork, w

e w

ill show

som

e resu

lts and h

ope to

stimulate

discu

ssions o

f how

best to

do

this. O

ther p

rojects w

hich

would

be en

abled u

sing LG

SAO

on Ju

piter/Satu

rn is im

aging o

f their rin

g systems an

d au

rora.

Christophe D

umas: A

pplicatio

ns o

f LGS-A

O to

Solar System

Sciences

I will p

resent an

overview

of LG

S-AO

applicatio

ns to

the stu

dy o

f solar system

bodies,

with

a particu

lar emphasis to

ward

s the cap

abilities o

ffered by th

e n

ewly co

mm

issioned

LG

S system at th

e V

LT-Yepun. SIN

FON

I-LGS o

bservatio

nal resu

lts of th

e tran

snep

tunian

object 2

003 E

L61 an

d its system

of satellites w

ill be d

iscussed

.

http

://w

ww

.mpi

a.de

/rin

g200

7

Rin

gber

g W

orks

hop

2007 - Abstra

cts

Ast

ronom

y w

ith L

aser

Guid

e St

ar A

dap

tive

Optics

Tim

Mor

ris: C

om

mon-u

ser

and E

xper

imen

tal Las

er G

uid

e St

ar A

O a

t th

e W

illia

m H

ersc

hel

Tel

esco

pe

The

Will

iam

H

ersc

hel

Tel

esco

pe (W

HT