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From YouTube: SJAA Imaging 4 19 22 Nikola Nikolov, Astroimaging and photometry in near infrared spectrum with a ba
Description
Astroimaging and photometry in near-infrared spectrum with a backyard telescope rig
Nikola Nikolov
Most astrophotography rigs use filters within the visible light spectrum to create beautiful and colorful images of deep-sky objects. However, there is a different set of filters used by scientific telescopes for photometric measurements, knowns as SDSS u, g, r, I, z filters. They have been initially used by Sloan Digital Sky Survey and today they are also available for small backyard telescopes thanks to Astrodon and Las Cumbres Global Telescope Network. If you have a telescope with a CCD camera and SDSS filters, you can do scientific astronomy and photometric measurements from the backyard.
In this talk, I will show interesting results with SDSS near-infrared filters, which cut off most of the visible light and leave only photons with wavelengths greater than 800nm. Near-infrared astroimaging reveals interesting details of galaxy structures which are usually obscured in LRGB stacks, extremely distant galactic clusters, and sometimes hidden objects in our Milky Way.
A
B
But
one
of
the
problems
that
we
all
face
as
a
photo
for
the
images
is
that
we
live
in
very
light.
Polluted
areas
right
and
living
in
such
light-rooted
areas
causes
a
lot
of
limitations
of
what
we
can
take
image
of
right
and
if
you
have
been
actually
following,
the
sikh
meetings
in
the
astro
imaging
group
in
aja
probably
learn
how
what
are
the
techniques
that
we
are
mostly
popular
for
imaging
from
city
skies
and
light
polluted
areas.
B
Of
course,
if
you
live
in
very
very
light
potential,
you
can
actually
image
of
the
sun
right
with
the
sword.
Telescope,
the
moon,
which
is
very
bright,
some
few
bright
planets
and
the
recent
technology
in
astrophotography
automotive
story
allows
us
to
actually
allow
us
to
image
a
mission
nebula
with
nato
bank
filters
and
that's
pretty
much
it
right
if
you
live
in
this
lightbulb.
Various
and
one
of
the
questions
that
I
have
been
kind
of
curious
is
what
else
can
be
done.
B
What
else
can
we
can
be
seen
in
from
these
latitude
areas
if
you
have
certain
equipment
to
do
to
do
that?
So
this
is
an
example
of
what
the
left
solution
scan
looks
like
in
the
emission
spectrum.
Basically,
so
this
is
actually
a
real
data
set
a
real
spectrum
measured
in
vienna,
austria
in
2018,
and
it
actually
represents
the
relative
irradiance
intensity
of
the
light
in
the
sky
versus
the
wavelength.
B
And
what
you
can
see
is
that
you
see
this
kind
of
bell
shaped
spectrum
which
is
centered
around.
They
are
between
550
nanometer
up
to
620
nanometer.
I
think
so
that
shows
you
that
actually
light
pollution
is
very
spread
in
different
wavelengths,
but
it's
mostly
within
the
area
of
yellow
wavelength,
basically
green
or
yellowish
light,
and
this
is
actually
used
by
both
professional
astronomers
and
astrophotographers
to
actually
use
specific
filters
and
cut
off
that
part
of
the
spectrum.
C
B
That
we
want
to
see-
and
these
two
areas
are
even
higher-
with
lower
wavelength,
which
means
we're
going
to
uv
or
a
shorter
wavelength,
or
we
can
go
into
high
overhang
means
we
go
to
red
or
infrared
spectrum,
and
the
dots
are
actually
the
data
and
the
simulation
is
is
in
the
year.
The
blue
area
means
that
simulation
and
experiment.
They
fit
pretty
much
well
and
on
top
of
it,
if
you
live
in,
if
we
when
we
live
in
light
pooled
areas,
the
situation
is
getting
even
worse.
B
B
What
is
the
radiance
from
the
from
the
from
the
boom
for
the
reflection
and
what
you
see
that
is
actually
the
spectrum
is
very
steep
and
quickly
going
down
into
shorter
wavelength
means
that
for
blue
light
and
more
like
near
uv
ultraviolet,
the
intensity
is
going
down
pretty
quickly
and
then
the
density
is
actually
decreasing.
But
slowly
when
we
go
to
bigger
wavelengths
than
into
red
and
infrared
spectrum,
but.
C
B
The
centroid
is
actually
located
near
the
yellow,
yellow,
color,
yellowish
color
or
greenish
color.
This
is
also
good
news,
because
we
can
one
can
be
designed
filters
which
cut
off
this
part
of
the
spectrum,
and
we
can
image
object
in
deep
sky
which
are
outside
this
yellow
area
of
the
spectrum,
and
this
is
the
case
with
the
emission
nebula.
B
B
But
to
get
this
image,
he
uses
three
filters
right:
the
aero
band
filters
which
are
oxygen,
three,
which
is
around
500
nanometer,
then
hydrogen,
alpha
or
h,
alpha,
which
is
six
hundred
and
six
seven
sixty
nanometer
right
and
silicon
silver,
two,
which
is
the
second
filter.
So
both
these
two
filters
are
red
and
this
one
also
increases
green.
B
But
by
using
stacking
softwares
like
fixed
inside,
you
can
create
artificial
colors
of
each
filter
in
rgb
and
we
can
actually
stack
them
together.
You
can
see
you
can
actually
get
a
cultural
picture
like
this
of
the
nebula
right,
but
this
is
just
one
kind
of
objects
that
we
can
actually
take
image
of
right.
So
this
is
specifically
for
a
mission
nebula
and
not
all
the
time
we
around
the
year.
B
So
they're
not
so,
if
you
use
narrowband
futures,
you
can
see
the
galaxy,
but
you
can't
get
pretty
images,
and
this
is
the
case
where,
basically,
if
you
want
to
take
pictures
of
faint
objects
like
galaxies
or
dusty
clouds
in
the
sky,
deep
sky,
basically
you
need
a
different
technique.
Different
set
of
filters
called
lrgb
right.
B
These
are
four
filters
we
also
which
actually,
when
you
stack
the
images
together,
you
get
a
call
for
image,
but
you
cannot
use
this
technique
from
city
sky
from
white
bullet
area.
So,
basically,
if
you
want
to
use
lrgb
filters,
you
have
to
take
your
car
drive
two
hours
from
here
and
you
can
collect
this
data
and
make
pictures
like
this.
So
this
is
actually
image
of
a
reflection
nebula
from
australia.
I
I
actually
collected
the
data,
but
the
location
in
australia
is
very
remote
and
very
far
away
from
cities.
B
So
these
are
the
two
major
techniques
that
are
currently
used
for
us
imaging
photography,
and
so,
if
you
look
at
where
these
filters
actually
are
located,
so
all
the
filters
that
we
use
for
streamaging
they're
into
the
visible,
visible
wavelengths
of
the
spectrum,
basically
visible
light
right.
These
are
that's
why
we
can
actually
make
these
colorful
pictures
because
they
are
close
to
what
our
eyes
can
see
as
a
natural
colors.
B
So,
however,
there
are
other
kind
of
filters
which
are
called
photometric
filters
and
they're
used,
mostly
in
scientific
photography
and
also
used
into
photometry
in
general,
for
different
reasons,
mostly
for
scientific
reason,
but
also
for
calibration
of
telescopes
right
occupational
optics
or
we
want
to
sometimes
measure
the
sensitivity
of
the
camera
or
some
parametric
parameters
of
the
cameras
that
we
use.
So
we
use
this
automatic
filters
to
do
measurements,
so
these
filters
are
not
for
getting
colorful
pictures,
but
for
data,
basically
collecting
numbers,
and
we
use
these
numbers
for
different
different
things.
B
Which
seems
to
be
accessible
from
city
sky,
so
in
specific
conditions-
and
I
haven't
explored
the
near
uv
yet,
but
it's
also
interesting
and
for
me
in
the
future.
I
can
try
that
as
well,
so
for
the
metric
filters
that
they're
using
the
scientific,
astronomy,
they're,
actually
public
published
online,
and
this
is
the
naming
convention.
B
That's
why
it's
yellow
right
red,
which
is
very
close
to
h,
alpha
right
this,
this
kind
of
region,
and
then
we
have
a
lot
a
bunch
of
filters
in
infrared,
starting
with
I
z
and
all
these
set
of
filters,
and
you
can
see
that
the
wavelength
is
actually
between
86
nanometer
up
to
3
microns
right.
This
is
3
almost
3.5,
microns
wavelength
and
then
it
goes
even
further
with
the
mid
infrared
where
the
wavelength
is
actually
up
to
21
microns.
C
B
B
C
B
There
is
a
metric
scale
and
based
on
that,
astronomers
can
tell
whether
the
star
is
more
bluish
or
more
greenish
or
more
yellowish,
but
for
different
different
wavelengths.
There
are
different
details
from
the
stars
and
galaxies
that
are
interesting
in
these
different
regions
and
that's
why
people
use
these
filters
to
see
these
details.
These
are
not
narrow
band
filters,
they're
actually
wide
bent,
but
in
much
bigger
with
away
from
the
visible
spectrum
right
and
they're
also
available
for
purchase.
B
B
B
So
if
you
go
to
astrodome
webpage,
this
is
how
the
transmission
spectrum
looks
like
it's
a
bit
blurred
of
the
graph,
but
you
see
the
all
the
filters
with
different
colors
and
what
are
the
wavelengths
there
of
they
cover?
As
I
mentioned,
these
are
white
white
band
filters,
so
they
cover
much
larger
portion
of
the
spectrum
than
the
narrow
band
and
today,
we'll
focus
mostly
on
I
and
z
z
filters,
and
I
can
show
you
how
the
deep
sky
looks
like
with
these
filters
and
what
are
the
surprises.
B
A
B
D
Yeah,
I
have
a
question
back
on
the
spectrum
of
light
pollution.
It
showed
that
the
light
pollution
was
strongest
in
the
yellow
green
area.
That's
exactly
where
the
human
eye
is
most
sensitive.
Also,
is
there
some
feedback?
Is
this
data
feedback
with
respect
to
human
perception,
or
is
that
just
a
happy
coincidence,
as
it
were.
B
It's
not
it's
not
coincidence.
Actually,
this
is
the
reason
why
light
pollution
is
bad
for
us
because
it
actually
interrupts
our
sleep
sleep
hours,
especially
when
the
weather
is
cloudy
and
the
reflection
of
the
white
portion
hits
those
the
clouds
and
the
faces
backward,
and
it
interrupts
our
natural
need
of
sleep.
B
B
B
So
if
you
look
at
this,
the
light
potion
spectrum,
so
we
are
when
I
use
I
filter.
We
are
beyond
700
nanometers,
so
we
are
always
in
the
in
the
very
right
end
of
the
light
fusion
spectrum.
So
it's
yeah
close
to
zero,
but
we
still
see
this
deal
from
moonlight
right
because
moonlight
if
it's
full
moonlight
is
the
radius
is
still
not
zero
right.
C
B
I
need
to
check
that,
let's
see,
I
think
this
could
be
yeah.
This
is.
I
can
check
whether
this
is
95
percent,
or
I
mean
min
and
max
around
the
mean.
I
want
the
mean-
and
I
can
tell
you
what
exactly
is
this
yeah?
So
this
is
probably
the
maximum
intensity
of
the
light
that
you
get
from
the
moon
because
it
could
be,
it
could
vary
from.
B
B
Yeah
yeah,
so
that's
true
yeah,
but
I
haven't.
I
haven't,
actually
tried
with
really
far
away
near
infrared
filters,
yet
I'm
still
into
the
8
kilometer
range,
which
is
at
least
not
impacted
so
much
by
the
white
viper
for
now,
but
all
these
filters
below
they
could
be
impacted,
but
I
haven't
tried
it.
B
B
The
famous
database
so
on
the
left
is
the
image
of
horsehead
nebula
with
visible
wavelength,
and
this
is
the
image
that
we
like
to
see
with
the
nebula
and
the
dusty
regions
around
and
all
the
star
under
cores
right
and
on
the
right
is
the
same
part
of
the
sky,
the
same
object,
but
with
two
microns
wavelength.
Okay.
B
This
is
the
famous
two
mass
measure
telescope,
which
actually
created
data
in
the
past,
and
what
you
can
see
is
that
when
you
go
to
two
microns
wavelength,
essentially
the
nebula
is
gold
right.
You
can
see
a
little
bit
of
the
silhouette
of
the
nebula,
but
most
of
it
is
gone.
And
what
is
the
surprise
is
that
in
this
region,
where
the
the
dark
that
that
dusty
region
is
kind
of,
looks
like
nothing,
is
there
all
of
a
sudden?
B
So
why
astronomers
need
to
remove
neighborhoods
from
the
images
right.
This
is
a
image
of
normal
galaxy
cluster,
which
is
actually
I
made
it,
especially
if
took
these
images.
For
today's
talk,
so
I
posted
the
image.
The
final
result
on
last
rubin
and
this
this
image
is
actually
a
stack
of
data
from
my
telescope.
B
I
use
actually
a
rasa
system
specifically
because
they
wanted
to
capture
the
the
the
the
star
field
of
normal
galaxy
cluster,
because
the
galaxy
crystal
is
actually
hidden
inside
the
milky
way
lactic
plane,
and
this
is
the
result.
After
one
hour
of
data,
you
see
countless
number
of
stars
and
you
cannot
really
recognize.
Where
is
the
galaxy
cluster?
But
it's
here
right.
B
So
I
know
by
because
I
I
played
solve
the
result,
and
I
know
where
the
galaxy
cluster
is
so
these
dots
that
look
like
stars
are
actually
galaxies
and
there
are
more
galaxies
on
the
image
but
they're
basically
obscured
from
from
the
start
field,
and
this
area
of
the
sky
is
also
known
as
the
great
attractor,
because
there
is
a
strong
gravitational
field
which
pulls
all
galaxies
in
the
re
and
this
classic
cluster
in
one
direction.
There's
no
known
root
cause.
Yet
why?
What
causes
the
great
attractor?
B
So
I
use
also
I
telescope,
because
it's
not
accessible
from
here
and
now
I
see
much
less
number
of
stars
and
things
which
are
more
likely
like
a
galaxy
right.
This
is
really
a
galaxy
right.
Another
galaxy
here,
a
lot
of
galaxy
here
more
here
right.
You
start
seeing
details
of
this
galaxy
cluster
in
much
better
way
than
this
way
right.
B
So
so,
when
we
switch
to
new
infrared,
you
can
check.
Is
she
remove
big
portion
of
the
star
field
and
the
dust
and
actually
see
through
it?
And
we
can
see
these
distant
galaxies
there
right
and
we
can
do
this
also
in
northern
hemisphere.
Actually,
I
have
an
example,
but
I
have
to
switch
the
screens
just.
B
B
B
You
know,
sinus
constellation
is
mostly
known
with
the
nebula
and
the
ngc
7000,
and
all
these
nice
areas
for
h
alpha
and
the
different
nebula
there.
But
there
is
a
galaxy
cluster
there
and
this
galaxy
cluster
is
actually
hidden
behind
the
star
field,
and
I
was
actually
surprised
that
if
I
take
my,
I
filter
i2
filter
just
from
the
retailer
and
put
on
my
61
millimeter
winning
optics,
I
was
able
to
see
the
galaxies
within
in
between
the
stars
right.
B
I
see
this
is
a
galaxy
I
played
solve
it
and
I
compare
with
y
field
infrared
survey,
which
is
online
and
I
see
the
same
same
galaxy
in
the
same
occasion
right
and
the
reason
why
I
can
this.
The
telescope
can't
see
this
galaxy
in
the
same
reason
that
was
showing
with
the
normal
cluster,
because
when
we
image
with
near
infrared,
it
actually
cuts
off
a
lot
of
the
stars
and
still
leaves
the
galaxies
of
the
image.
B
So
I
actually
investigate.
Why
is
that?
And
whether
it's
true
for
all
galaxies,
it
turns
out
that
when
we
image
with
infrared
filters,
we
can
see
a
lot
of
galaxies
on
the
image,
but
particularly
galaxies,
which
have
active
core
means
that
these
galaxies
actually
have
x-ray
or
black
hole
in
the
in
the
center
of
the
galaxy
which
actually
meets
strong
radiation
and
then
actually,
when
you
image
with
eye
filters
or
near
infrared
filters,
you
can
see
them
because
they
are
very
bright.
B
However,
with
the
galaxy
is
not
active
with
not
active
nucleus
or
core,
it's
actually
faint
on
the
image.
It's
not
the
same
result.
So
there
is
a
trade-off,
so
you
can
actually
use
an
infrared
filter
to
see
galaxies
in
the
in
the
field,
but
these
galaxies
are
mostly
active
with
active
core
and
wheelchair.
We
don't
have
actually
active
core
to
be
fainter,
so
not
all
galaxies
are
responding.
The
same
way
for
the
eye
filter.
A
B
B
B
B
So
I
telescope
network
is
useful
for
photometric
measurements
because
many
of
the
telescopes
they
have
streaming
filters
like
narrowband
and
lrgb,
but
also
these
telescopes
are
equipped
with
photometric
filters
and
that's
one
of
the
differences
with
telescope
live
telescope
life.
I
use
the
risk
of
life,
but
they
use
mostly
lrgb
and
narrowband,
but
they
don't
have
these
automatic
filters.
B
Well,
I
telescope
has
telescope
bricks
which,
for
with
photometric
filters
and
for
scientific
purpose
and
t5
telescope
from
from
its
complete,
is
actually
one
of
the
cheapest
rigs
for
scientific
astronomy
and
many
astronomers
actually
use
it
this
week
for
measurements,
and
you
can
actually
have
it
the
telescope
for
24
dollars
one
hour
right.
Sometimes
it's
free
when
the
moon
is
actually
bright.
B
My
telescope
gives
you
for
free.
So
last
time
I
didn't.
They
didn't
even
charge
me
for
one
hour
imaging
because
it's
a
full
moon
rate.
So
what
is
one
this
thing
about
this
star,
big
c
monk,
zeros
right?
If
you
go
to
zimbab,
it
will
tell
you
that
this
is
a
symbiotic
star
so,
and
it
has
very
strange
symbols
in
front.
B
So
this
is
a
variable
star
when
you
see
v
star.
That
means
this
star
is
variable,
and
it
tells
you
also
what
type
of
style
it
is
and
what
is
the
physics
behind,
and
when
I
go
to
the
literature,
we
see
that
what
is
symbiotic
star
stellar
system
definition
for
it
so
symbiotic.
Star
system
is
actually
a
binary
system
of
cold
red
giant
star
and
a
hot
white
dwarf.
B
However,
these
stars
are
stereo.
Systems
are
very
complex
because
their
variability
is
non-linear.
They
basically
don't
have
periodicity
very
nice
periodicity
of
normal
variable
stars.
They
have
actually
unpredictable
flashes
and
their
behavior
is
still
under
investigation
and
still
to
understand
what
causes
this
complexity
and
burst
of
energy.
B
B
B
B
B
I
can
click
here
and
see
all
the
reference
telescope
that
you
can
actually
compare
results
with.
You
can
have
deep
sky
survey
with
color
red
blue
two
micron,
two
mass
telescope
white
field
went
a
field
infrared
a
bunch
of
telescopes
around.
You
can
actually
quickly
see
the
same
part
of
the
sky
with
different
wavelengths,
and
if
I
click
red
I
mean
color,
you
see
a
lot
of
stars
here.
Our
target
star
is
in
the
center
and
not
much
around
happening.
You
see
a
bunch
of
stars
but
again
looks
like
normal
sky
right
now.
B
B
B
B
All
right
and
what
it
says
for
this
star
is
that
so
these
are
pulsating
stars
characterized
by
very
red
colors,
with
posseting
period
about
longer
than
100
days,
and
these
are
giants
again
and
they
expel
their
outer
layers
and
they
actually
become
eventually
planetary,
nebula
and
white
dwarf
right.
So
this
explains
why
we
see
this
this
flash.
Basically,
if
feel
like
it's
here,
so
when
I
go
to
game
to
just
color,
it's
they're
not
they're,
like
they
disappear
right.
B
They
don't
they're
not
there,
but
if
I
go
to
two
micron
wow,
so
that
means
that
in
two
micron
wavelength
they
look
bigger
and
that
corresponds
to
what
this
explains
it
does.
This
is
a
red
giants
and
they're
pulsating
right
and
eventually
this
will
actually
be
a
planetary
enabler
in
the
future.
So
right
now,
what
you
see
here
is,
let's
see
future
planetary,
nibblers.
B
Yeah,
these
are
four
pointer,
enables
in
the
future
yeah.
So
this
is
what
the
difference
is
when
you
switch
to
different
wavelengths.
It
actually
gives
you
hidden
details
of
this
part
of
the
sky,
which
are
not
visible
when
you
go
to
visible
wavelengths
right,
so
to
go
back
to
the
measurements
that
I
did
so,
let's.
F
B
All
right,
so
what
I
see
here
are
the
same
styles
that
are
actually
on
our
web
page
right.
These
are
the
same
guys.
These
two
finished
this
guy.
So
what
I
see
is
consistent
with
the
two
micro.
So
basically,
my
near
infrared
image
is
consistent
with
what
I
see
from
two
micron
and
here
is
actually
the
star
profile.
B
B
What
will
be
the
numerical
aperture
that
we
want
to
use
to
measure
the
energy
flux,
and
you
can
see
that
when
I
click
on
the
star
with
the
mouse,
it
gets
this
circle
right
and
it
measures
the
profile
and
it
gives
you
what
is
the
radius
of
the
object
in
pixels
and
where
is
the
background?
The
background
is
this
area,
so
we
have
three
numbers
which
are
14,
25
and
38,
and
these
numbers
are
set
in
the
software.
B
So
but,
interestingly,
what
we
see
is
that
in
I
filter
the
radius
is
actually
bigger
than
the
b
filter.
So,
and
that
is
normal,
because
this
this
star
is
actually
also
red
giant
right
with
it's
a
binary
system
of
head
gen
and
white
dwarf.
So
we
expect
that
in
high
filter
it
should
be
wider
right.
That's
why
the
radius
is
14.
B
B
It
compares
the
fluxes
of
the
two
stars
and
makes
calculations,
and
it
gives
you
the
relative
flux
of
the
target
star
versus
the
reference
star,
and
you
do
this
for
multiple
stars,
not
just
one,
but
you
have
to
take
actually
four
five
measurements,
four
different
reference
stars,
even
six
reference
stars,
collect
the
data
and
then
you
have
to
take
mean
max
and
some
statistics
to
see
how
this,
what
are
the
numbers
right?
So
I
let's
say
I
have
five
stars
reference
stars
and
versus
them.
B
B
B
The
two
these
two
boxes
and
bigger
filter
is
this
line,
so
it's
actually
counter
intuitive,
because
on
the
april
13
I
thought
probably
it
blew
looks
like
it's
a
little
bit
brighter
than
I
filter,
but
actually
it's
not
it's
actually
in
eye
filter,
it's
actually
brighter
than
blue
filter
and
because
it's
actually
the
steeper
right
and
what
we
see
that
this
change
between
13
and
82
17
is
actually
bigger
than
the
error
bar.
So
it
means
that
we're
taking
all
the
noises
and
all
the
errors
and
all
the
error
bars.
B
Of
course,
I
cannot
tell
right
now
that
this
is
a
signal,
so
I
want
to
share
first
this
with
professional
astronomers
and
the
next
couple
of
days
and
we'll
analyze
the
results
and
if
they
confirm
will
be
for
good
news.
Basically,
we'll
have
a
flash
on
the
sky
in
next
days,
but
we'll
see
how
much
will
be
how
much
brighter
we
it
may
become
right.
Some
people
may
say
it's
they
predict
will
be
as
bright
as
8
magnitude
or
maybe
7,
which
means
that
you
can
see
this
this
flash
with
the
binocular.
B
Okay,
so
this
this
kind
of
measurements
are
relatively
easy
for
those
of
you
which,
like
who
actually
want
to
learn
more.
I
can
actually
give
you
some
literature
how
to
do
this
automatic
measurements.
It's
basically,
you
could
do
it
with
astronomy
j,
which
is
manual
way,
but
it
actually
teaches
you
about
the
physics,
the
signals
that
what
kind
of
signals
do
how
to
process
the
signal
you
can
also
use
stromatic,
which
is
another
software
which
does
these
measurements
automatically,
but
asthmatic
is
basically
automated
and
is
hidden
there's.
B
So
I
would
like
to
end
actually
with
the
image
that
I
we
put
on
the
talk
binary
right.
This
is
m16
106
galaxy
with
new
infrared
filter
and
the
reason
I
actually
took
these
images
within
infrared
is
because,
with
the
current
light
pollution
and
the
current
season
spring
right,
the
accessible
object
was
head
start
galaxies,
and
I
was
curious
if
I
take
a
bright
galaxy
and
put
the
near
infrared
filter
what
they
can
see
right.
What
what
the
details?
I
can
actually
see
in
the
image
so
immediately.
B
You
can
see
that
we
don't
see
a
lot
about
the
outer
layers
of
the
outer
actually
branch
of
the
galaxy.
You
can
see
it's
actually
the
center
and
but
we
see
details
in
the
structure
of
the
center
of
the
central
part
of
the
glass.
You
can
see
actually
two,
these
two
spirals,
you
see
some
interesting
objects,
and
one
thing
that
I
noticed
here
is
that
this
is
actually
not
very
visible,
but
you
see
this
small
shadow
area
which
is
actually
taking
off
the
galaxy
plane.
B
So
I
wanted
actually
to
see
whether
I
can
conceal
the
image
one
of
the
famous,
because
these
guys
has
two
jets
coming
out
of
the
core
and
francesco
will
strike
actually
to
the
reason
why
they
carried
this
mega
project
with
the
german
astronomers
is
to
see
those
two
jets
right.
So
I'm
able
to
see
a
little
bit
of
one
of
the
jets
in
infrared,
but
I
don't
see
the
next
one.
The
next
one
is
somewhere
here,
the
second
one.
B
I
only
see
barely
the
first
one
right
and
the
second
one
is
somewhere
here,
but
it's
not
visible.
So
what
we
can
conclude
from
that
little
bit.
That
kind
of
speculated
is
that,
because
this
is
near
infrared
and
when
we
image
the
sky
in
new
in
near
infrared,
we
are
actually
looking
cooler
objects
which
are
relatively
cool
to
other
objects.
That's
why
that's?
Why
we
see
this
star
a
little
bit
wider,
because
it's
actually
cooler
red
giant
right
and
that's
why
it's
with
a
greater
radius
of
the
profile.
B
So
something
similar
happened
here.
It
seems
that,
because
we
don't
see
the
second
jet
here,
we
see
an
infrared
little
bit
of
the
first
jet
or
that
area
means
that
this
this
first
jet
is
probably
a
little
bit
cooler
than
the
first
one
right.
So
we
start
seeing
these
little
bit
temperature
differences,
but.
B
This
is
just
a
rough
estimate
right.
He
has
to
take
more
images
and,
as
paul
said,
we
have
to
actually
take
care
of
this
wave
of
water
vapors
and
all
these
corrections
before
we
draw
any
conclusions
but
yeah
the
first
first
data
actually
showed
that
we
can
see
new
reference
one
of
these
jets
here
a
little
bit,
and
actually
this
is
not
with
200
hours
exposure.
I
I
use
probably
two
three
hours
right.
B
Each
expo
each
frame
is
actually
600
seconds,
just
normal
exposure
time,
which
we
typically
use
for
narrowband.
I
use
the
narrowband
strategy,
for
you
know
this
kind
of
objects.
I
use
600
seconds
exposure
for
new
infrared,
even
at
a
bright
moon
sky,
and
I
still
see
the
galaxy
here
right
on
the
image.
B
A
A
B
B
B
F
B
B
B
C
B
B
B
B
C
B
B
So
I
have
a
very
expensive
ccd
camera,
which
is
apogee
I
haven't
set
up
yet
because
I
initially
wanted
the
this
big
city
camera
to
for
normal
imaging
with
edge
alpha
note
3,
but
it's
too
heavy
for
my
rig
so
yeah.
I
cannot
balance
the
the
weight
the
telescope
with
respect
to
the
mount,
because
the
camera
is
too
big
too
heavy,
so
I
will
repurpose
it
for
scientific,
but
I
need
bigger
amount
for
that.
So
it's
a
little
bigger
mountain,
better
tracking.
In
order
to
install
this
camera,
it's
actually
full.