1. • Wavelength
at
which
protostellar
regions
are
expected
to
peak
• Fill
in
this
essen6al
gap
in
exis6ng
SEDs
to
create
more
accurate
models
of
this
stage
in
stellar
evolu6on
A
Catalog
of
Low-­‐Mass
Star-­‐Forming
Cores
Observed
with
SHARC-­‐II
at
350
μm
Why
350
μm?
Source
Extrac6on
Procedure
NOTE:
Observa6ons
were
taken
using
SHARC-­‐II,
which
operates
at
the
Caltech
Submillimeter
Observatory.
The
observa6ons
include
many
well-­‐known
star-­‐forming
regions,
including
both
clustered
regions
and
isolated
sources,
and
were
taken
over
the
course
of
7
years,
from
May
2003
to
December
2010.
Core
Extrac6on
• Experimented
with
extrac6on
parameters
to
find
the
op6mal
combina6on
• Extracted
cores
to
find
posi6on
and
radius
Fluxes
• Calculated
the
flux
from
each
core
in
fixed
aperture
sizes
(20”,40”,
and
the
beam)
• SHARC-­‐II
beam
=
9”
• Calibrated
using
planet
point
sources
Box
vs
Lissajous
• Inves6gated
two
different
observing
modes—box
and
lissajous
• Box
scans
cover
a
larger
area
in
general
• Observed
the
same
sources
under
both
modes
and
compared
(Figure
below)
• Found
to
be
sufficiently
similar
as
to
not
be
a
source
of
error
With
and
Without
Extended
Emission
• Inves6gated
two
different
reduc6on
modes
—with
and
without
extended
emission
• Without
extended=
Much
less
noise,
no
false
sources
• With
extended=
Get
as
much
of
the
real
flux
as
possible
With
Extended
Without
Extended
NGC
1333
Serpens
Cluster
A
B335
L1551-­‐IRS5
Mo6va6on
The
goal
of
this
project
is
to
develop
a
catalog
of
protostellar
cores
in
nearby
molecular
clouds
observed
at
the
sub
millimeter
wavelength
of
350
µm.
The
images
will
be
taken
using
SHARC-­‐II
to
obtain
high
angular
resolu6on
maps—3
6mes
higher
than
those
that
currently
exist
from
the
Herschel
Space
Observatory
at
the
same
wavelength.
The
final
catalog
will
contain
82
maps
of
molecular
cloud
regions
including
basic
source
proper6es
such
as
posi6on,
flux
density,
and
radius.