La lecture à portée de main
Découvre YouScribe en t'inscrivant gratuitement
Je m'inscrisDécouvre YouScribe en t'inscrivant gratuitement
Je m'inscrisDescription
Sujets
Informations
Publié par | ruprecht-karls-universitat_heidelberg |
Publié le | 01 janvier 2010 |
Nombre de lectures | 8 |
Langue | English |
Poids de l'ouvrage | 3 Mo |
Extrait
Natural
Dissertation
Or
submitted
v
to
of
the
ard
Com
orn
bined
th
F
aculties
Put
of
y
the
Natale
Natural
Caserta,
Sciences
examination:
and
,
Mathematics
Do
of
of
the
Sciences
Rup
forw
erto{Carola{Univ
b
ersit
Gio
y
anni
of
b
Heidelb
in:
erg,
Italy
German
al
y
16
for
July
the
2010
degreeW
Dust
ervisor:
emission
F
and
T
Star
Hofmann
formation
Boulanger
in
the
Prof.
Stephan's
erner
Quin
Prof.
tet
rancois
Sup
group
Dr.
of
hard
galaxies
us
Referees:Spitzer
the
Understanding
with
the
formation
in
ell
distribution
medium
ered
(IGM)
w
gas
the
oling
X-ra
pro
through
whic
y
h
o
are
no
b
to
p
fuel
study
star
onen
formation
group
in
tted
galaxies,
main
and
elucidate
the
to
eect
fraction
of
from
galaxy{galaxy
map
and
dust
galaxy{IGM
y
in
and
whic
e
h
separate
mo
in
dify
at
stellar
a
and
for
gas
luminous
distributions
dust
of
o
galaxies
in
the
groups
emission
and
onen
is
sho
vital
p
to
AH
photons.
mo
y
dels
photons,
of
with
galaxy
on
formation
e
and
ev
is
olution.
ered
The
b
Stephan's
plasma
Quin
Applying
tet
el
(SQ)
to
maps,
group
v
of
able
galaxies
dieren
is
dust
a
group
natural
their
lab
as
oratory
MIR
for
elengths.
studying
rev
these
rst
phenomena
of
b
extended
ecause
of
the
not
galaxies
main
of
of
this
and
group
with
are
halo
hea
W
vily
inferred
in
ectral
this
b
the
et
emission
w
of
een
in
k,
h
other
w
and
and
with
taking
the
t
group
and
IGM.
and
F
bining
urthermore
dust
its
o
y
y
deriv
allo
SED
ws
UV
to
observ
study
GALEX
the
SQ,
details
the
of
(SFR)
the
dust
in
emission
p
phenomena,
w
whic
b
h
are
et
b
een
eliev
particles
ed
dust.
to
a
b
v
e
tting
m
hnique
uc
the
h
FIR
more
w
ha
in
e
the
een
early
to
univ
the
erse,
t
and
of
its
emission
this
on
and
the
erform
sky
photometry
p
FIR
ermits
w
studies
as
of
w
diuse
v
Our
onen
has
ts
ealed
asso
the
time
with
the
a
group
and
IGM.
In
t
this
infrared
thesis
emission,
w
e
the
presen
b
t
dies
an
the
analysis
galaxies,
of
roughly
a
t
the
e
y
set
of
of
group.
MIR/FIR
e
observ
the
a-
dust
tions
sp
of
energy
Stephan's
of
Quin
extended
tet,
and
tak
other
en
infrared
with
the
ts
Spitzer
SQ,
Space
the
Observ
atory
.
to
The
the
emission
hanisms
seen
o
at
ering
these
dust
w
P
a
emission,
v
in
elengths
is
dust
pro
heating
heating
b
UV
y
dust
Com
particles
the
and
of
luminosit
b
p
e
w
used
b
to
UV
trace
as
star
ed
formation
the
ev
tting,
en
the
ts,
luminosit
A
GN
ed
activit
the
y
FUV
and
of
also
w
hot
estimated
gas
star
rate
oling,
for
in
h
the
emit-
oling
4
ting
b
th
k,
us
where
pro
in
viding
f
a
e
gas
of
ur
star
die
formation
w
in
un
SQ
Studie
em
A
bracing
a
obscured
SQ
and
sho
unobscured
dust
a
onen
Zusammenfassung
ts.
The
v
total
Mediums
SFR
teraktionen
of
v
SQ
eine
is
hselwirk
7
dieser
:
dem
5
the
M
of