mpia.de/ring2007 :// · number of churches and monasteries. the church, ortress hohensalzburg, a y...
TRANSCRIPT
-
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
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Garch
ing
Iye Masa
nori N
AO
Tokio
Kasp
er Marku
s ESO
Garch
ing
Kib
blew
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dw
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Univ. o
f Chica
go
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ngeles
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Los A
ngeles
Law
Nich
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s Caltech
Pasa
den
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Mich
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Honolu
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Mannucci F
ilippo IN
AF
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Arcetri
March
is Fra
nck U
C B
erkeley / SE
TI
Max C
laire U
C S
anta
Cru
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Morris T
im U
niversity o
f Durh
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Myers R
ichard
University o
f Durh
am
Now
ak N
ina M
PE
Garch
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Oberti S
ylvain
ESO
Garch
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Olsen
Knut N
OA
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ucso
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Ott T
hom
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PE
Garch
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Pasq
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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
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Rabien
Seb
astia
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PE
Garch
ing
Raja
gopal Ja
yadev C
TIO
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AO
La
Seren
a
Rib
ak E
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aifa
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gw
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usa
n C
TIO
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AO
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erena
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aut F
ranço
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ini O
bserva
tory H
ilo
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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
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eidelb
erg
Tacco
ni-G
arm
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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