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Description
The Tycho Tracker
Daniel Parrott
Tycho is a new software program to improve upon the detection and measurement of astronomical objects including asteroids, comets, variable stars, and exoplanets. One of its unique features is that of synthetic tracking, which permits one to detect very faint asteroids by exploring a wide range of motion vectors with GPU acceleration. In 2021, over 60 new Near Earth Objects (NEOs) were discovered by amateur astronomers using the Tycho software.
A
B
Thank
you.
So
let
me
go
ahead
and
start
off.
I
will
share
my
screen
here,
so
this
is
what
I've
been
titled
asteroid,
hunting
and
photometry
with
tycho.
So
tycho
is
the
kind
of
the
software
that
I've
been
working
on
these
past
couple
of
years,
and
so
I'm
going
to
start
off
with
is
basically
the
detection
of
asteroids.
So
before
you
can
do
anything
interesting,
you
have
to
first
be
able
to
detect
the
the
object
of
interest.
B
So
I'll
talk
into
some
detail
about
how
you
would
go
about
the
detection
process
and
then
I
will
follow
that
up
with
once
you've
detected
it
then
what
kind
of
measurements
can
you
perform?
So
this
would
involve
primarily
two
different
subjects.
Here
we
can
consider
astrometry,
which
is
concerned
with
the
precise
positioning
location
of
the
object
so
where
it
is
at
a
given
point
in
time
and
then
photometry,
which
is
concerned
with
how
bright
the
object
is
over
time.
B
So
you
can
consider
a
light
curve
of
an
asteroid
and
from
that
you
could
deduce
its
rotation
period
and
glean
other
characteristics
of
the
object.
So
we
first
want
to
be
able
to
detect
the
object,
and
then
we
can
do
measurements,
and
this
also
leads
into
other
fields
as
well
with
photometry.
You
could
do
measurements
with
variable
stars
exoplanets
and
a
more
recent
one
I
could
talk
a
little
bit
about.
Is
the
james
webb
space
telescope?
So
I
I
have
some
data
on
that.
That's
kind
of
interesting
to
look
at.
B
B
So
this
is
commonly
used
by
the
professional
surveys.
They
have
these
large
one
meter
class
instruments
typically,
and
this
involves
taking
three
or
four
images.
Typically
spaced
20
minutes
apart,
so
you'll
you'll
take
a
an
image,
a
snapshot
of
some
fill
the
view
of
the
sky
and
then
20
minutes
later
you'll,
follow
it
up
with
another
image
and
so
forth
until
you
have
three
or
four
of
those
exposures
now.
This
is
great.
You
get
a
lot
of
skype
coverage.
B
So
a
lot
of
you
are
familiar,
I'm
sure,
with
the
principle
of
stacking,
so
that's
kind
of
what
we're
able
to
do
now
with
with
a
technique
that
is
called
synthetic
tracking.
Others
might
call
it
also
digital
tracking,
but
the
common
term
here
that
I'm
going
to
be
using
is
synthetic
tracking
and
so,
with
this
technique,
you're
actually
able
to
detect
objects
about
10
times
fainter
than
would
be
possible
with
the
conventional
technique.
B
B
That's
become
more
popular,
especially
with
the
the
advancements
in
modern
hardware
and
I'll
go
into
a
little
bit
discussion
on
that
in
just
a
moment,
but
it's
also
useful
not
just
for
discovery
but
also
recovery,
and
what
I
mean
by
recovery
is
that
whenever
you
have
just
initially
discovered
or
detected
an
object,
you
have
very
high
uncertainty
in
its
motion.
Typically,
so
you've
just
got
a
few
measurements,
a
few
observations
from
one
night
and
you
want
to
try
to
follow
it
up
the
next
night.
B
Well,
sometimes
you
can-
and
sometimes
you
can't
just
depending
upon
the
the
the
uncertainty
of
those
measurements
and
so
catalina
survey,
just
as
one
example
they've
been
using
the
tyco
software
in
2021,
they
used
it
to
recover
15
of
their
near-earth
objects.
That
would
otherwise
have
been
lost,
and
so
synthetic
tracking
is
proving
useful
for
both
of
those
use
cases.
B
These
are
all
what
I
call
trial
stacks
of
the
same
object.
So
what
I
mean
by
that
is
an
object,
can
have
a
speed
and
it
can
also
have
a
position
angle,
so
it
this
defines
its
mo
its
motion
and
what
you're
trying
to
do
here
is
create
a
a
trial,
stack
you're,
trying
to
stack
those
images
according
to
its
motion,
and
so
just
just
a
way
to
visualize.
B
That
is
at
the
very
center
here
you
have
what
would
be
considered
the
ideal
trial
stack,
and
so
then,
away
from
that,
you
have
other
stacks
that
had
not
quite
the
correct
motion.
The
speed
might
have
been
too
fast
or
too
slow,
or
its
position
angle
was
off.
So
what
you're
able
to
do
again
with
modern
hardware
is
basically
in
a
brute
force
fashion.
You
can
explore
these
thousands
of
different
motion
vectors
and
then
extract
the
object
that
had
this
correct
motion
here.
B
So
again,
these
these
advancements
that
have
taken
place
I'll
talk
about
three
of
them
here,
so
we
one
we've
had
certainly
a
lot
of
improvements
with
graphics
processing
hardware,
so
gpu
hardware
has
come
a
long
way.
Then
we've
also
had
the
advent
of
full-frame
cmos
cameras,
and
this
is
important
because
with
this
technique,
when
you're
taking
these
short
exposures,
you
want
to
have
low
readout
noise,
and
so
these
cmos
cameras
are
well
known.
B
So
I'll
just
point
out
one
example
here
this
is
one
discovery,
2020
bu6
that
had
a
size
of
860
meters,
and
this
is
one
of
the
largest
near
objects
found
by
an
amateur
in
recent
years,
and
so
here's
a
diagram
showing
what
its
orbit
looks
like.
So
you
can
see
here.
I
went
past
the
orbit
of
mars,
but
it
is
considered
a
near
object
here,
and
so
this
is
what
it
looks
like
on
raw
image
data.
B
B
So
it's
again
on
a
single
exposure.
You
can't
really
do
much
with
that,
but
here
we
have
a
stack
of
21
exposures
and
you
can
start
to
see.
This
object
presents
itself
with
the
stack
of
21
exposures
and
what
I'm
going
to
do
here
is
just
show
as
they
zoom
out.
You
can
kind
of
get
an
appreciation
for
this
field
of
view,
so
here's
1x
zoom
and
then
I
zoom
out
more
and
then
a
one
quarter,
zoom
and
then
so.
This
is
really
brings
into
focus.
B
B
B
A
I
ask
so
so
you
take
a
patch
of
sky,
you
know,
like
it
looked
like
around
a
degree
or
two
you
know
in
with,
and
you
take
a
shot
and
say.
Is
there
an
asteroid
in
my
field
of
view
it
sounds
like
and,
and
you
know,
shoot
it
for
20
minutes
or
half
an
hour.
What
are
the
odds
that
there's
something
in
there.
B
The
odds
are
pretty
good,
especially
if
you
are
imaging
at
the
ecliptic
and
and
so
yeah
I
actually
using
just
a
127
millimeter
refractor
I
was
able
to.
This
was
just
kind
of
one
of
those
see
what
would
happen
kind
of
things,
but
I
image
at
the
ecliptic
and
even
with
the
smaller
instrument
I
was
able
to
detect
over
200
asteroids
in
the
field
of
view,
so.
B
B
B
So
that's
what
this
is
here
and
this
is
basically
a
list
of
whatever
images
you
want
to
work
with,
so
I'm
going
to
go
ahead
and
add
some
images
to
my
image
manager,
and
this
will
be
again
I'm
starting
off
with
the
the
data
set
for
taiko
user
guide,
and
so
I
I've
selected
my
images
and
I
brought
them
into
taiko.
It
tells
me
I
have
60
images
here.
B
Each
one
is
two
minutes
or
120
seconds
in
duration
and
the
total
exposure
time
is
two
hours
so
six
sixty
of
them.
You
get
the
idea,
so
I
I've
also
already
plate
solved
these
images,
so
we
have
a
plate
solution
and
just
if
I
want
to,
I
can
go
ahead
and
do
view
images
so
from
the
main
menu
here
you
can
go
to
action,
view
images,
and
this
brings
up
what
I
call
the
image
viewer.
So
what
we're
looking
at
here?
B
These
are
just
the
basically
the
the
raw
images
here
and
they've
been
calibrated,
but
basically
you
know
you
can
zoom
in
you
can
pan
do
whatever
you
want
to.
So
this
is
just
getting
started
now
we
might
want
to
know.
Okay,
you
know
a
question
earlier:
would
we
have
any
asteroids
in
this
field
of
view?
So
one
way
I
can
answer
that
question
is,
I
can
go
to
file
load,
known
objects
and
that's
going
to
bring
up
this
known,
object,
module
and
so
what
this
does
for
us
is
it.
B
B
So
I've
clicked
on
38826,
that's
the
number
of
the
asteroid,
and
I
can
zoom
in
now
I'll
notice
that
I
need
to
update
my
observatory.
So
I
took
these
images
with
an
observatory
located
in
australia.
So
q62
is
sighting
spring
observatory,
so
I'm
just
going
to
make
that
my
active
observatory.
The
reason
that's
important
for
this
example
is
that
if
you
want
to
have
the
precise
positioning,
the
top
eccentric
coordinates
to
be
precise,
then
it
has
to
know
sort
of
the
lat
lawn,
the
basically
the
location
where
you
took
those
images.
B
So
I've
updated
that
I'll.
Just
refresh
this
here,
real,
quick
and
now
you'll
notice
that
whenever
I
click
on
38826,
it
is
now
centered
correctly
in
the
crosshairs.
So
this
is
the
asteroid
here
again,
that's
on
a
single
exposure.
If
I
want
to,
I
could
just
do
a
quick
animation.
I
could
go
back
to
the
image
manager
and
do
an
animation,
and
you
can
kind
of
see
that
animation,
as
the
asteroid
has
movement
here
across
these
60
images.
So
this
is
kind
of
just
a
fun
little
experiment,
again
you're
just
working
with
known
objects.
B
B
So
here
we
are.
This
is
that
that
object
here
and
you'll
notice
that
the
stars,
the
image,
are
our
trails
at
this
point,
so
it's
almost
like
you
had
taken
your
mount
and
you
had
specified
the
the
motion
of
the
object,
but
you've
done
it
after
the
fact,
so
that's
kind
of
a
nice
thing
to
be
able
to
do
but
again,
at
this
point,
we've
only
been
working
with
known
objects.
Now
we
want
to
ask
we
want
to
answer
the
question.
B
What
if
I
want
to
discover
a
new
object?
How
would
that
look
like
what?
What
would
that
look
like,
so
what
I
can
do
there
is.
I
can
go
to
action.
Synthetic
tracker
okay,
so
I
mentioned
earlier.
Synthetic
tracking
is
kind
of
this
nice
little
technique
for
detection,
especially
as
an
amateur
astronomer.
So
let's
go
to
synthetic
tracker
and
it
will
prompt
us
for
a
sensitivity
threshold.
So
how
sensitive
do
you
want
the
search
to
be
and
99
of
the
time?
B
I
just
recommend
using
the
balanced
preset
option
here,
so
click,
ok
and
here's
where
we
can
specify
what
kind
of
limits
we
want
on
the
search.
So
if
I
want
to
do
a
blind
search,
if
I
want
to
mostly
just
do
search
for
all
possible
motions,
I
could
uncheck
those
limits
and
just
do
that
and
it
would.
It
would
come
back
with
121
000
motion
vectors
for
this
particular
data
set.
B
Now,
if
I
want
to
again,
I
I
could
say
well,
maybe
I
just
want
to
look
for
main
belt
objects,
main
belt,
asteroids
and
then
main
build
asteroids
would
typically
have
a
speed
between
around
0.2
and
0.7.
So
let's
just
take
a
look
and
see
just
just
for
the
perfect
purpose
of
a
very
quick
demonstration
here.
What
that
would
look
like
so
so.
This
is
2029
motion,
vectors
and
again
what
that
really
looks
like
again,
if
you're
familiar
with
stacking
you've
got
your
60
images
and
you're
going
to
stack
them
in
some
way.
B
You
can
do
a
median
combine.
You
can
do
an
average
combine
ultimately
you're
going
to
be.
You
know
again
working
with
60
images
here
we're
going
to
do
that
2029
times,
so
we're
going
to
stack
60
images
over
2000
times,
so
I'm
going
to
click.
Ok-
and
let's
just
give
it
a
moment
here
to
do
that,
and
also
while
it's
doing
that
stacking
operation,
it's
also
exploring
those
trial
stacks
to
see
if
there
are
any
detected
objects,
so
it's
already
finished
and
so
that
that's
the
power
of
gpu
acceleration.
B
Again
I
have
this-
I'm
not
going
to
go
into
in
super
detail
here,
but
you
can
configure
your
graphics
device
and
set
it
up
to
do
that,
but
here's
the
results,
so
we've
come
back
now
with
the
our
track
navigator.
These
are
all
the
detected
objects
in
that
field
of
view,
and
so
what
I
can
go
ahead
and
start
off
with
is,
I
can
say:
well,
let's,
let's
compute
the
confidence
and
these
detections.
So
it's
gonna
tell
us
how
confident
it
is
that
these
are
actually
real
objects.
D
B
B
If
I
want
to,
I
could
also
double
click
on
an
object
and
that's
going
to
bring
up
a
verify
track
module,
and
so
what
this
looks
like
here
is
it's
going
to
do
an
animation
of
the
the
frames,
and
so
it
tells
us
if
we
want
to.
We
can
follow
the
object
or
we
could
just
let
it
the
object,
move
and
and
not
follow
it.
So
we
have
that
way
to
animate
the
frames
again.
You
can
choose,
however,
many
sub
stacks.
B
A
B
A
lot
of
main
belt
asteroids
have
the
same
motion:
okay,
thanks,
yeah
yeah,
so
I'm
not
sure
which,
let's
see
if
I
double
click
on
this
one,
so
it
happens
to
be
the
next
result
here.
So
it
has
a
speed
of
0.58
arc
seconds
per
minute.
The
other
one
had
0.69,
so
there
one's
just
a
little
bit
faster
than
the
other,
but
most
importantly,
they
both
have
a
similar
direction,
so
243
degrees
versus
264
degrees,
so
that
the
motion
is
quite
similar
to
this
particular
data
set.
B
So
if
I
want
to,
I
can
go
ahead
and
create
you
know
measurements
of
each
of
these
objects,
but
I'll
just
show
an
example
here.
So
this
is
what
that
would
look
like.
So
I
can,
I
can
click,
add
observations
and
what
that's
going
to
do.
I
can
input
the
so
the
designation
of
the
object,
so
it
has
a
permanent
id,
provisional
id
and
so
forth.
There's
a
lot
more
detail
on
what
these
mean.
B
If
you
get
interested
in
pursuing
this
further
but
suffice
to
say,
permanent
id
is
its
number
and
then
a
provisional
id
whenever
an
object
is
newly
discovered
it
has
a
provisional
id.
So
that's
typically
the
year
followed
by
some
alphanumeric
collection.
So
I
click
okay
here
and
now
we've
got
three
measurements
of
that
object.
B
So
if
I
click
on
the
first
measurement
here,
I
can
zoom
in
a
bit
and
you
can
see
that's
the
first
sub
stack
of
the
object
and
I
can
click
on
another
measurement
here
and
then
and
then
finally,
the
last
one.
So
you
can,
you
can
see
what
we've
done
here
is:
we've
generated
measurements
of
that
detected
object,
and
so,
if
I
wanted
to,
I
could
generate
a
report.
We
can
do
it.
There's
two
different
types
of
reports.
B
The
the
original
format
was
npc,
1992
came
out
in
1992
and
then
the
more
recent
one
is
called
ades,
it's
an
acronym,
but
this
one
is
still
popular.
So
again,
I
I
could
spend
a
lot
of
the
discussion
just
talking
about
all
these
little
nuances
here,
but
suffice
to
say
what
I'm
getting
at.
Is
you
you
basically
image
the
object,
you're
able
to
detect
it
and
then
you're
able
to
generate
measurements
of
it
and
so
that
that's
what
I'm
showing
here
and.
B
Right
yeah,
so,
if
you
wanted
to,
you
could
do
60
measurements,
but
the
minor
planet
center
prefers
that
you
only
send
three
observations
per
night,
typically
three
or
four
per
night,
and
the
way
that
works
here
is
that
you
want
to.
Certainly
when
you're
you're
focused
on
these
fainter
objects,
you
want
to
generate
your
measurement
on
a
sub
stack
of
the
object.
So
let's
just
take
a
look
at
that
in
more
detail.
So
here's
this
object.
B
B
This
one
is
barely
detectable,
even
with
sub
stacks.
So
what
we've
done
here
is
we
again.
This
is
an
animation
of
three
sub
stacks
and
it's
it's
very
faint.
If
we
were
to
look
at
that
with
our
single
images
here,
you
can
see
that
it
just
kind
of
gets
lost
in
the
noise
on
these
single
exposures,
and
so
you
wouldn't
really
want
to
generate
measurements
of
it
on
all
all
60
images.
Here
there
would
be
too
much
noise
and
the
measurements
wouldn't
be
very
good.
B
Okay,
okay,
so
what
we've
done
here
again
is,
I
you
know,
we've
taken.
This
is
just
one
example.
This
is
using
this
the
synthetic
tracker
and
it
came
back
with
these
results.
So
it's
it's
pretty
cool
that
again,
this
is
just
using
you
know:
amateur
astronomer
equipment.
You
can
do
these
kind
of
measurements,
you
can
you
can
do
this
kind
of
detection
as
well,
and
that's
that's
in
my
mind.
That's
that's
pretty
fascinating,
especially
that
you
could
actually
make
a
potential
discovery
with
this.
B
B
So
this
is
an
observatory
again
from
the
itelescope.net
network.
So
I'll
give
them
a
moment
here
to
finish
loading
up
these
images,
and
here
we
are
so
I've
got.
This
is
what
that
looks
like
here.
So
again,
I
could
animate
the
frames
and
if
I
zoom
in
a
bit
you
you
might
be
able
to
see
the
moving
object.
B
It's
pretty
bright
in
this
case,
so
we've
got
our
asteroid
here
and
it's
just
moving
along
the
field
of
view
and
what
we
would
like
to
do
is
we
would
like
to
take
measurements
of
it.
In
this
case.
One
measurement
per
image,
so
here
this
kind
of
is
actually
the
opposite.
Where
I
I
mentioned,
you
only
want
three
or
four
measurements
per
night.
B
So
a
couple
ways
to
do
this:
this
is
a
known
object.
So,
if
I
wanted
to,
I
could
go
to
file
load,
known
object,
and
so,
let's
just
give
it
a
moment
here
to
finish
that,
and
so
here
it
is
it's
the
first
result.
This
is
asteroid,
1884
skip
and
it
basically
it
shows
us
the
trajectory
of
that
object.
And
so
again,
if
I
were
to
do
the
animation,
you
can
see
how
it
it
moves
across
that
line
there,
but
basically
again
what
we
want
to
do
is
try
to
create
that
light
curve.
B
So
what
this
means
is
we're
going
to
be
invoking
the
photometry
module
and
a
lot
again
lots
of
ways
to
do
this,
but
I
like
to
start
off
with
just
finding
comparison
stars.
So
I'm
going
to
into
a
bit
of
detail
here
for
those
of
you
who
might
not
be
familiar
with
photometry.
I
realize
that
this
is
a
bit
of
detail
to
take
in,
but
I
promise
I'll
make
it
a
little
bit
quick
here
so
find
compstars
these.
B
B
So
it's
actually
going
to
measure
all
these
comp
stars
across
the
the
field
of
view
here
and
across
the
image
sequence,
and
so
we
we
can
look
at
the
graph
here
and
we
can
see
what
that
looks
like
this.
One
doesn't
look
so
good,
so
I'll
just
go
ahead
and
remove
that
one,
but
these
other
ones
we
can
probably
work
with
now.
B
If
I
want
to,
I
can
also
verify
my
starcat
log
settings,
so
I'm
using
the
atlas
catalog-
and
this
is
a
very
good
catalog
to
use
for
photometry
purposes,
and
so
I'm
just
going
to
go
ahead
and
click.
Ok
here
and
again,
this
is
just
a
starting
point,
but
I
can
go
ahead
and
if
I
want
to
create
my
light
curve,
let
me
go
ahead
and
go
to
the
first
position
of
the
object
here
so
again
known
objects.
B
I
can
double
click
on
it
and
I
can
say,
create
marker
one,
so
I'm
indicating
the
first
position
of
the
object
and
then
I
can
scroll
down
a
ways
and
then
go
to
create
marker
two.
So
what
I'm
really
doing
is
I'm
defining
the
motion
of
this
object
and
now,
I
can
say,
create
photometry
from
markers,
so
let's
go
ahead
and
give
it
a
moment
to
see
what
it
comes
back
with
here.
B
So
we've
now
generated
240
measurements,
one
for
each
image
and
the
data
set
and
I'm
just
going
to
go
ahead
and
plot
all
sets
here,
and
so
this
is
kind
of
what
that
looks
like.
So
it's
basically
generated
a
light
curve
and
again
I
can
go
ahead
and
give
this
a
title.
The
correct
title
here
would
be
skip
1884.
B
B
So
I
click
find
period,
and
now
it's
come
back
with
the
2.89
two
hours
as
its
first
analysis
here,
so
that
that's
actually
a
very
good
result.
If
I
go
to
the
tools
menu
and
go
to
lightcurve
database,
I
can
actually
consult
a
database
of
known
objects
here.
So
if
I
click
on
search
and
1884
skip
is
one
of
these
results,
it
says
2.8887
would
be
a
rotation
period,
and
so
this
is
actually
pretty
good
because
keep
in
mind
again.
B
B
B
So
this
is
your
typical
interface
here
you
can
work
with
the
raw
data.
You
can
also
apply
object,
data.
What
that
means
here
is
that,
if
you
search
for
the
object,
it's
going
to
give
you
additional
information
information
on
it,
so
the
phase
angle
and
so
forth.
What
that
allows
you
to
do
is
you
can
also
compensate
for
light
term
light
time.
Correction.
B
You
can
apply
h,
minus
g
correction,
and
so
this
this
becomes
more
important.
Whenever
you
have
several
nights
of
data
because
with
multiple
nights
of
data
you
start
to
have
these
offsets
and
it's
good
to
be
able
to
have
those
corrections
applied,
but
again,
we'll
still
have
a
very
similar
result,
as
we
did
before
so.
B
B
So
it's
it's
going
to
vary
in
brightness
by
this.
You
know
a
quarter
magnitude,
let's
say
so.
What
you
would
want
to
make
sure
of
is
that
your
again,
this
is
just
like
any
kind
of
measurement.
It's
going
to
have
some
error
bars
in
it,
so
you
want
to
try
to
make
sure
that
your
error
bars
are
going
to
be
significantly
lower
than
that
amplitude.
B
So
if,
if
you're
going
through
a
lot
more
sky-
or
you
know-
you
have
more
air
mass
than
as
long
as
you
still
have
good
signal
to
noise
ratio
on
that
object,
such
that
you
have
the
the
error
bars
are
lower
than
that
amplitude.
That
then
you
should
be
okay,
thanks,
yeah,
okay,
okay,
any
other
questions.
B
Okay,
moving
right
along
I'm
going
to
go
ahead
and
close
out
this
data
set
and
then,
let's
take
a
look
at
the
james
webb
space
telescope,
so
this
is
kind
of
a
fun
one.
It's
just
a
you
know
once
in
a
lifetime
opportunity
that
have
imaged
it
as
it
was
in
route
to
l2
point,
and
so
here
I've
got
179
images
and
this
spans
a
total
elapsed
time
of
4.2
hours
anyway.
B
So
I'll
give
it
a
moment
to
do
that,
and
if
I
want
to,
I
can
zoom
out
a
bit.
I
can
animate
the
frames
now
you
may
or
may
not
see
it,
but
here
it
is
it's
kind
of
trucking
along
through
this
field
of
view.
You
can.
You
can
see
that
moving
object
here
now.
Another
way
to
do
this
is.
I
could
also
attach
epimerous
information
to
this
data
set,
and
this
is
actually
somewhat
of
a
new
feature
so
with
this
interface
to
jpl
horizons,
I've
just
recently
added
it.
B
B
So,
for
example,
if
I
do
a
major
body
lookup,
this
is
actually
going
to
bring
up
a
list
of
results
here
and
they've
got
482
what
what
they
consider
to
be
major
bodies
as
opposed
to
small
bodies,
so
a
small
body
would
be
an
asteroid
or
a
comet,
but
a
major
body
to
use
their
terminology
would
be
a
planet.
It
would
be
a
spacecraft.
B
B
So
what
we're
basically
saying
is
that
we
would
like
to
generate
ephemeris
information
for
this
particular
target
and
we'd
like
to
do
so
and
attach
it
to
this
data
set
of
images.
So
what
that
means
is
I'm
going
to
request
the
all
of
this
information
of
that
object
pertaining
to
when
these
images
were
taken,
so
I'm
going
to
choose
ephemeris
attached
to
data
set,
and
so
it's
going
out
to
the
jpl
horizons
portal
and
we've
just
now.
It's
it's
already
returned
with
the
result
here.
B
So
all
of
these
columns
have
been
populated
for
each
image.
One
of
these
is
is
the
object
in
the
field
of
view,
so
that's
kind
of
a
basic
question.
You
know
you'd
like
to
know:
did
you
actually
capture
the
object
in
the
field
of
view
so
either
yes
or
no,
and
it
also
tells
you
the
speed
of
the
object,
the
position
angle
of
the
object,
the
altitude
of
the
object
above
the
horizon,
azimuth
and
so
forth.
B
So
you
get
all
this
useful
information
and
what
you
can
do
is
once
you've
applied
that
ephemeris
information.
Now
I
can
actually
just
click
on
an
image
in
the
image
of
your
manager
and
you'll
notice
that
it
tracks
it
in
the
image
viewer.
So
I
can
actually
just
go
ahead
and
scroll
through
here
and
you
can
kind
of
get
an
idea.
What
that
looks
like
so
we're
able
to
track
the
james
webb
space
telescope
across
our
179
images,
and
you
you
can
probably
see
already
it
does
have
quite
a
changing
brightness.
B
Another
way
I
can
do
this
is
in
false
color
mode,
so
I
can
toggle
that
and
you
can
notice
that
again
it
gets
darker
and
then
it
gets
brighter.
So
it
certainly
has
a
change
in
brightness
over
time.
Another
way
to
do
this
is,
I
can
also
select
all
of
the
images
here
and
do
a
max
combine,
and
now
you
can
kind
of
see
that
better.
So
it
started
here.
This
was
the
first
image,
and
so
it
was
a
little
bit
faint
and
then
it
progressed
to
be
eventually
got
brighter.
B
Pretty
bright
here
got
a
little
bit
fainter.
Now
I've
got
really
bright
so
now
what
we'd
like
to
do
is
actually
analyze
this
with
some
numbers
we'd
actually
like
to
measure
it
have
some
meaningful
measurements
taken
of
this
object.
So
what
I'm
going
to
do
like
I
did
before
is
I'm
going
to
invoke
the
photometry
module.
B
B
B
Probably
want
to
get
rid
of
this
one,
and-
and
maybe
this
one
too,
so
I'm
just
going
to
start
with
that.
This
is
the
first
stab
at
it.
But
again
the
other
nice
useful
feature
here,
because
I
have
attached
ephemera's
information
before
I
had
this
feature.
I
I
tried
to
do
a
photometry
set
with
this
object,
so
I
would
try
to
say
well
here
here
it
is.
B
So
if
I,
if
I
do
my
it's,
it's
almost
a
straight
line,
but
it
kind
of
deviates
a
little
bit
from
that.
So
this
little
bit
of
deviation
here
is
just
barely
enough
that
you
wouldn't
get
super
good
results
with
with
this
approach.
So
that's
why
now,
if
I
want
to
I'm
going
to
do,
photometry
set
I'm
going
to
create
photometry
using
ephemeris
information
now
the
other
way
I
did
it
before.
B
B
So
again,
that's
the
raw
plot
and
if
I
wanted
to
I
could
I
could
click
on
a
data
point
here:
okay,
so
that
that
moves
to
that
particular
image
and
you
can
see
how
it's
that
kind
of
that
intensity
there.
And
if
I
go
to
one
where
it's
a
bit
fainter,
you
then
you'll
notice.
It
is
indeed
a
fainter
object
there
presentation,
so
this
is
in
fact
the
light
curve
in
in
university
of
hertfordshire.
B
A
So
I
assume
the
the
reason
for
the
odd
light
curve
is
just
light
reflecting
off
different
surfaces
of
the
telescope.
Is
you
know
like
it's
really
close
and
and
and
the
same
thing
by
the
way
for
the
curve
versus
straight
line?
It's
so
close
to
us
that
we're
really
seeing
details
of
its
you
know
curved
orbit
as
as
opposed
to
you
know
something
so
far
away.
B
B
C
B
C
You
know
like
with
the
asteroid
the
the
center
of
mass
is
going
to
be
basically
around
wherever
the
primary
mirrors
are
and
the
equipment
is.
It
has
this
big
boom
out
here
with
a
with
a
big
sun
sail,
and
it's
sticking
out
there
that's
very
low
mass
in
comparison
this
this
will
be
rotating
around
with
you.
Would
you
be
able
to
remove
be
able
to
detect
side
to
side
oscillation,
rather
than
the
straight
line
that
the
center
of
mass
would
tend
to
make
in
the
sky?
E
B
D
C
D
Imaged
them,
I
think
it
was.
I
should
look
at
my
astra
bin
for
the
names
one
of
them
was
florence,
and
I
don't
remember
the
second
one,
but
most
of
all
the
as
and
the
way
I
work
with
asteroids
is
by
somebody
mentioned
at
the
beginning,
by
removing
them
from
by
checking
the
pixel
inside
removes
them
correctly.
F
F
Know
I'm
trying
to
remember:
it's
been
a
while.
I
may
have
used
apcc,
which
is
the
you
know,
kind
of
new
fancy
control
program
for
the
astrophysics
mounts
and
it
has
horizons
interface.
Also,
okay,
and
so
you
can.
You
can
program
it
to
try
to
try
to
track,
but
it's
been
long
enough
now
that
I
don't
remember
if
I
ever
got
that
going,
I
think
I
did,
though.
B
A
B
This
this
is
a
way
to
generate
some
ephemeris
information,
so
you
could
do
this
again
from
jpl
horizons,
and
so,
if
I
want
to,
I
could
pull
up
asteroid
skip
and
attach
it
to
the
session
planner,
and
here
we
go
it
now
populates
with
this
list
and
we
we
can
know
the
coordinates
of
that
object
at
these
given
dates
and
times.
So
it's
it's
a
it's
a
helper
tool,
it's
kind
of
nice
to
have
it
this
capability
and
again
you
could
use
that
not
just
for
asteroids
or
comets.
B
Now
you
might
be
wondering
what
is
find
orb
find
orb
is
a
really
useful
tool,
and
what
I
I
like
about
it
is
that
you
can
use
find
orb
on
really
newly
discovered
objects.
So,
for
example,
if
I
go
to
the
tools
menu
I'll,
just
give
you
an
example
here,
but
so
if
I
had
some
observations
of
an
object,
I
showed
earlier
three
eight
eight
two
six.
What
what
I
can
do
here
is,
let's
suppose,
that
we
just
had
these
recent
measurements
of
this
object.
B
So,
basically,
tycho
is
going
out
and
searching
for
find
orb
instances,
and
I
can
click.
Ok
and
again
it's
going
to
well.
Okay,
so,
as
it
turns
out,
3826
is
not
visible.
I
had
a
filter.
If
I
refresh
it,
then
you
can
see
so
this
would
be
the
result.
So
the
the
altitude
of
the
object
is
it's
below
the
horizon,
for
this
particular
object.
So
that's
the
altitude
column
there,
but
lots
of
ways
to
generate
if
you
wanted
to
have
a
session
plan.
A
So
related
to
what
we
were
talking
about
before
the
talk,
I
take
it
that
there
is
no
way
for
you
to
figure
out
not
not
ask
somebody
else
for
the
orbit,
but
to
take
a
guess
at
you
know
the
full
orbit
of
this
object.
Based
on
I
mean
you
probably
can't
do
that,
as
we
said
from
one
night's
observations
anyway,
but.
B
Yeah,
let's
go,
I
I
can
just
give
a
quick
example
here,
so
let's
go
back
to
that
data
set
taker
user
guide
and
what
I'll
do
here
is
I'll
just
pull
up
again.
This
is
this
is
an
example
of
one
night
of
data,
so
I'll
go
ahead
and
change
my
observatory
back
to
sighting
spring
australia,
real
quick,
and
so,
if
I,
if
I
pull
up,
you
know
this
view
here
and
I
can
go
back
to
my
normal
presentation
yeah.
B
What
I
can
do
is
again,
let's
run
this
hypothesis
or
this
dot
experiment
where,
let's
suppose
it's
a
newly
discovered
object,
so
I've
run
through
synthetic
tracker
and
came
back
with
some
results.
So
here's
the
track
results
here
and
again
maybe
had
high
confidence
on
on
this
object.
Okay,
so
if
I
double
click
you
can
see,
this
is
a
real
object
here,
it's
it's
very
faint,
but
nevertheless
it
is
presentable.
B
So
what
I
can
do
here
again,
these
are
my
three
measurements
I
I
can
right,
click
them
and
then
choose
view,
and
then
I
can
say
view
and
find,
or
so
this
is
going
to
bring
up,
find
orb
and
it's
going
to
compute
an
orbit
solution.
So
it's
going
to
try
to
take
those
three
measurements
and
it
has
some.
B
B
You
could
maybe
even
use
it
to
follow
it
up
the
night
after
that.
But
could
you
use
this
orbit
to
predict
where
the
object
is
going
to
be
two
months
from
now?
No
you
could
it
just
has
too
much
uncertainty.
So
you
know
a
single
night
of
observations.
That's
that's
usually
good
enough
to
get
you
where
you
can
follow
it
up
the
next
night,
especially
if
it's
a
main
belt
asteroid.
A
So
because
so
like,
if
we
wanted
to
know
the
mass
of
the
asteroid,
because
you
mentioned
that
somewhere,
where
early
in
the
talk
right,
somebody
found
an
asteroid
that
was
such
a
size
such
a
presumably,
if
it's
rock,
you
know
it's
mass,
so
so
hat.
Can
that
be
done?
I
mean
like
what
would
you
need
to
do
that.
B
B
So
if
you
so
you
you're,
considering
not
just
the
the
the
orbit
of
the
object
but
also
its
brightness,
so
and
if
you
know
its
brightness
as
well
as
its
albedo,
you,
you
can
kind
of
get
some
ideas
to
how
large
it
might
be
so
that
that's
kind
of
how
they
do
that.
There's
there's
an
online
calculator
if
you
wanted
to
play
with
it,
where
you
can
type
in
the
absolute
magnitude
of
the
object
as
well
as
I
believe
it's,
the
g,
the
slope
of
it.
B
A
G
H
H
B
B
So
here
here's
the
webpage-
and
I
I
talked
a
little
bit
earlier
about
some
data
sets
if
you
go
to
the
download
menu
here
there
are
some
data
sets
available
on
this
web
page,
so
the
one
I
was
showing
earlier
was
the
ds3.
That's
your
60
images,
it's
about
100
megabytes
in
size,
and
so,
if
you
wanted
to
download
the
tool,
you
could
also
download
some
data
sets
to
play
with
ivar
light
curve.
This
is
one
if
you're
interested
in
photometry,
then
you
could
download
these
data
sets.