TargetedSupernovaSearchwith CoherentWaveBurst - PowerPoint PPT Presentation

Targeted
Supernova
Search
with
 Coherent
Wave
Burst
 M.
Zanolin
(ERAU),
L.
Corpuz
(ERAU),
and
the
 cWB
Team 
 LSC Burst Face to Face – Krakow, Poland 2010

Why
can
we
benefit
from
a
new
 approach
to
Supernova
searches?
 The light curves below can be used to back track from the first recorded signal to the probable time of the explosion Kaufman et al. 2010 As we can see from this table, the uncertainty in the explosion time ranges from ±6 sec to ± 4 days. For the list of optically detected SN within ~20Mpc during S6, the uncertainty may be even longer.

Op8cally
Discovered
SN
Within
20Mpc
During
S6
 SN
Name
 SN
Type
 Host
Galaxy
 Distance
 2010u
 ?
 NGC
4214
 ~2.7‐3.5
 2010k
 IIp
 12
02
46.67
+02
24
05
 ?
 2010gi
 IIb
 IC
4660
 ~16.4
 2010br
 Ib/c
IIb
 NGC
4051
 ~10.9
 2009mk
 II
 ESO
293‐34
 ~18.3
 2009md
 II
 NGC
3389
 ~15.9
 2009ls
 II
 NGC
3423
 ~10.9
 2009kr
 IIn
 NGC
1832
 ~14.2
 2009js
 II
 NGC
0918
 ~17
 2009ip
 II
 NGC
7259
 ~20
 2009ib
 IIp
 NGC
1559
 ~12.6
 2009hq
 IIp
 NGC
4152
 ~13.1
 These were taken from a complete list compiled by CBAT http://www.cfa.harvard.edu/iau/lists/Supernovae.html

Search
Configura8on
 The
standard
configura8on
of
cWB
will
be
modified
by
introducing
a
sky
mask,
 • during
produc8on,
to
both
the
foreground
and
the
background
runs.
The
smallest
 sky
mask
we
can
implement
is
0.5°x0.5°
(one
pixel).
We
are
also

exploring
larger
 sky
masks
to
keep
into
account
the
angular
resolu8on.
 - The
frequency
band
we
will
use
will
be
from
100‐2000Hz.
 - The
characteris8c
GW
frequency
evolves
from
~100
Hz
just
a_er
bounce
to
 ~300‐400
Hz,
with
higher
frequencies
corresponding
to
higher
mass
 progenitors…
‐
hap://stellarcollapse.org/gwcatalog/murphyetal2009
 [PNS Core Pulsation] C. Ott - http://tapir.pbworks.com/f/Ott_CCSN_GW_predictions.pdf

Search
Configura8on
Con8nued
 • We
will
use
larger
windows,
on
the
order
of
weeks,
to
include
the
 error
in
extrapola8ng
the
exact
8me
of
the
first
EM
SN
emission
 • haps://svn.ligo.caltech.edu/svn/snsearch/papers/surf_report2010/
 • PNS
Pulsa8on
models
suggest
we
search
within
±1day
of
the
first
EM
 signature
–
Luc
Dessart
 - http://tapir.pbworks.com/f/Dessart.pdf • In
collabora8on
with
the
CalTech
effort,
we
will
perform
simula8on
 studies
with
the
following
waveforms:
 1. Analy8c
Bar
Modes
 2. Convec8on/SASI
 3. PNS
g‐modes
 4. More?
 • Data
quality
will
be
handled
the
same
way
as
the
all‐sky
cWB
search
 on
S6
 • We
are
working
on
procedures
to
combine
double
and
triple
 coincidence
data
both
for
 detecKon 
and
 upper
limit
 purposes.



Expecta8ons
and
Time
Scales
 • We
expect
to
improve
the
sensi8vity
of
the
all‐sky
all‐ 8me
search
by
a
factor
of
2
 S.
Klimenko
 http://tapir.pbworks.com/f/caltechSN.pdf 
 • • We
might
not
be
able
to
conclusively
determine
the
 supernova
mechanism
from
the
waveform.
 See
C.
Oa’s
discussion
at:
 • http://stellarcollapse.org/talks/Ott_APS_April_2008.pdf • We
aim
to
do
the
analysis
and
produce
a
paper
in
 about
a
year