EUCLID
Euclid
On
behalf
of
Isobel
Hook
Thanks
to
Euclid
team
(especially
Bruno
and
Stephen
in
the
audience)
Euclid
background
•  Part
of
the
ESA
cosmic
visions
M‐class
(~450Meuros)
selecHon
process
with
launch
in
2018
•  Only
truly
extragalacHc
mission
in
process
(except
SPICA
which
is
joint
JAXA
mission)
•  SubmiRed
yellow
book
late
last
year
and
await
final
decision
in
February
•  ~3
missions
go
into
a
18
month
definiHon
phase
with
2M‐class
missions
being
selected
Euclid
in
a
nutshell
•  Euclid
is
a
cosmology
mission
using
BAO
and
WL
as
its
primary
probes.
•  Wide‐field
imaging
over
20000
sq
degs
to
R+I+Z=24
and
J,H,K
photometry.
•  Slitless
spectroscopy
over
same
area
to
H~19.5
with
70M
galaxies
and
sample
19Gpc3
•  ~1%
precision
in
cosmological
parameters,
test
GR
on
large
scales
to
2%
•  Awesome
legacy
value
including
possible
galacHc
surveys
and
planet
searches
(hRp://arxiv.org/abs/
1001.3349)
•  122
page
YB
at
hRp://arxiv.org/abs/0912.0914
JDEM
•  Presently
part
of
the
Decadal
Review
process
in
the
USA
(~summer
reporHng).
Includes
detailed
cost
and
schedule
informaHon
•  Three
mission
concepts
(SNAP,
ADEPT
and
DESTINY).
Some
discussions
of
merging
these
•  A
year
ago,
embryonic
discussions
of
IDECS
–
those
are
frozen
because
of
CV
and
Decadal
•  JDEM
could
be
a
stronger
mission
for
transients
Supernovae
with
Euclid
Isobel
Hook
University
of
Oxford
and
INAF
(Obs.
Roma)
Thanks
to
R.
Nichol,
M.
Della
Valle,
F.
Mannucci,
A.
Goobar,
P.
AsHer,
B.
Leibundgut,
A.
Ealet
Euclid
Conference
17‐18
Nov
2009
Finding
&
Using
Supernovae
•  Need
to
know
for
each
SN
–  Type
–  Redshin
–  For
cosmology:
distance
(from
corrected
peak
magnitude)
•  in
turn
requires
colours
and
good
sampling
of
the
lightcurve
Example images from the
High-z team (Schmidt et al)
Example
spectrum
and
mulH‐colour
light‐curve
from
SNLS
Parameters
of
a
Euclid
SN
survey
(i)
Imaging
•  Deep
survey
(repeat
observaHons)
–  Lightcurves
in
J,
H,
K,
(R+I+Z)
–  photo‐zs
for
most
host
galaxies
–  spaHal
locaHon
of
the
SN
within
its
host
•  Details
TBD
(matched
to
primary
science
requirements)
–  FOV
>
40
sq
deg
in
at
least
two
patches
of
>
10
sq
deg
–  ~40
visits
:
Cadence
TBD
J,
H,
K
(5σ
point
source)
R+I+Z
(10σ
extended
source)
Depth
Each
Visit
(AB
mag)
Final
Depth
(AB
mag)
24
26
24.5
26.5
Above:
Euclid
deep
survey
parameters:
imaging
Parameters
of
a
Euclid
SN
survey
(ii)
Spectroscopy
•  Deep
survey
–  spectroscopic
z
for
brighter
host
galaxies
–  some
spectroscopic
SN
types.
Photo
typing
needs
to
be
invesHgated
•  Details
TBD
Depth
Each
Visit
(AB
mag)
Final
Depth
(AB
mag)
Slitless
spectroscopy
(conHnuum)
H~19.5
H~21.5
DMD
spectroscopy
(conHnuum)
H~22
H~24
Above:
Euclid
deep
survey
parameters:
spectroscopy
PotenHal
for
valuable
SN
survey:
Deep
(esp
NIR),
wide
area,
stable
Expected
Euclid
SN
counts
in
J
band
Counts
for
a
5
year
survey
assuming
10
sq
deg
monitored
at
any
Hme.
Produces
1000‐2000
SNeIa
to
z<0.7
Plus
a
further
1000‐2000
to
z<1
(detecHons
only)
Comparable
number
of
CC
SNe
N(z)
for
SNe
detected
1
mag
fainter
than
peak,
esHmated
by
A.
Goobar
based
on
assumpHons
in
Goobar
et
al
arXiv:0810.4932
(SN
Ia
rates
from
Dahlen
et
al
2004).
“DetecHon‐only”
curve
is
an
esHmate
(IH)
of
total
number
of
detectable
SNeIa
(no
lightcurves)
IdenHfied
systemaHcs
in
SNLS3
(preliminary)
Systematic
•  Brightness‐colour
relaHon
is
complex
•  Different
RV
cf
our
Galaxy?
•  SN
show
intrinsic
colour‐L
relaHon
(β)
•  Possible
z
variaHon
of
β
•  Euclid
NIR
photometry
will
disentangle
these
effects
% <w>
Extra
error
Statistical only
4.3
…
SNLS zero points
4.5
1.3
SNLS filters
4.4
0.6
External zero points
4.7
1.9
External filters
4.5
0.8
SN colour relation
5.0
2.5
BD+17 colours
5.1
2.6
BD+17 SED
4.4
0.4
Peculiar velocities
4.4
0.5
Malmquist bias
4.4
0.7
Nicmos non-linearity
4.4
0.7
Non-Ia contamination
4.4
0.7
All systematics
6.8
5.0
Conley
et
al.
in
prep
Euclid’s
role
in
SN
cosmology
•  Large
sample
–  1000
‐
2000
SNeIa
z<0.7
•  Deep,
stable
IR
photometry
–  Control
of
dust
exHncHon
–  Smaller
scaRer
in
Hubble
diagram
at
longer
rest‐frame
wavelengths
•  Benefit
of
coordinated
ground‐based
opHcal
campaign
–  measure
standard
rest‐frame
B‐band
and
I‐band
distances
to
the
same
supernovae
SN
Ia
mix
vs
redshin
RelaHve
mix
of
young+old
evolves
strongly
with
redshin
Euclid
rate
measurement
accurate
to
~
5%
in
Δz=0.1
bins
Less
affected
by
dust
(Sullivan
et
al
2006)
SNe
with
Euclid
:
Summary
•  Euclid
deep
surveys
can
provide
(“for
free”)
•  SNIa
cosmology
–  much‐improved
exHncHon
correcHons
–  Rest‐frame
I‐band
Hubble
diagram
with
thousands
of
objects
to
z
~
0.7
–  Benefit
of
coordinated
ground‐based
opHcal
campaign
measure
standard
rest‐frame
B‐band
and
I‐band
distances
to
the
same
supernovae
•  Accurate
SN
rates
–  Including
exHncted
SNe
–  Use
to
constrain
progenitor
models,
models
of
feedback
processes,
SFH,
beRer
understanding
of
SNeIa
for
cosmology