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From YouTube: SJAA Speaker Series: You can almost touch the stars
Description
Topic: You can almost touch the stars
Speaker: Tom Field
Description: Even if you wanted to touch a star, they’re all impossibly distant. Despite these great distances, astronomers have learned an enormous amount about stars. How? The most common method to study the stars is called spectroscopy, which is the science of analyzing the colorful rainbow spectrum produced by a prism-like device.
Until recently, spectroscopy was too expensive and too complicated for all but a handful of amateurs. Today, though, new tools make spectroscopy accessible to almost all of us. You no longer need a PhD, dark skies, long exposures, enormous aperture … or a big budget! With your current telescope and FITS camera (or a simple web cam or even a DSLR without a telescope) you can now easily study the stars yourself. Wouldn’t you like to detect the atmosphere on Neptune or the red shift of a quasar right from your own backyard?!
This talk, with lots of interesting examples, will show you what it’s all about and help you understand how spectroscopy is used in research. Even if you are an armchair astronomer, understanding this field will enhance your understanding of the things your read and the night sky. We’ll do a live Q&A after Tom’s 45-minute presentation.
A
A
Okay,
hello,
everyone.
So
today
we
are
here
at
another
talk
of
ours
from
sja.
We
are
an
astronomy
club
here
in
san
jose
california,
for
those
who
are
joining
us
from
places
afar
and,
like
our
speaker,
actually
is
in
seattle
right
now.
So
this
is
a
covered,
adapt
adaptation
of
our
speaker
program
and
I'm
very
happy
that
it
has
allowed
us
to
reach
out
to
people
outside
san
jose
or
outside
bay
area.
California,
and
actually
also
have
speakers
join
us
from
other
parts
of
the
world
and
the
country
at
a
minimum.
A
So
to
give
you
a
brief
background
on
the
club
we
have
been
around,
for,
I
actually
don't
know
the
exact
number
of
years,
but
like
it's
it's
close
to
25
years
or
plus,
more
than
that
and
it's
we
are
very
active
club.
We
have
like
about
350
to
400
members,
and
all
of
us
are
just
basically
really
enthusiastic
about
astronomy
and
like
what
we
like
to
learn
on
our
own.
All
of
us
are
also
very
learning
on
our
own
kind
of
like
amateur
astronomers.
A
Is
the
typical
term
used
where
we
just
study
astronomy
on
our
own
just
play
with
the
telescopes
and
like
do
the
stargazing
whenever
the
time
allows
us
to
do
so?
So
today
we
have
one
of
our
programs
that
we
we
do,
which
is
speaker
program,
and
today
we
have
somebody
join
us
from
seattle.
Like
I
mentioned,
his
name
is
tom
field.
A
B
Thank
you,
sukada,
and
thank
you
also
for
doing
all
the
background
work
to
get
this
arranged.
I
think
some
people
sometimes
don't
realize
how
much
work
it
is
to
get
all
the
schedules
right
and
urls,
and
all
that.
So
thank
you
for
that
and
thanks
to
the
club
for
inviting
me,
I
appreciate
the
opportunity
to
speak
to
you,
I'm
going
to
talk
for
45
or
50
minutes
and
again
because
we're
doing
this
on
youtube.
It's
not
quite
bi-directional.
B
You
know
we're
still
in
our
local,
very
localized
region.
Of
course
images.
We
can
see
the
universe
in
two
dimensions
and
with
eclipses
we
can
see
a
little
bit
of
you
know
3d
or
depth
z-axis,
and
then,
if
you
wait
a
while
the
time
dimension
reveals,
you
can
see
some
of
the
stars,
there's
one
in
the
upper
right
hand
corner
for
a
moment
for
a
moment
or
for
a
second,
you
can
see
changing
of
these
standard
candles.
These
are
lyrae
stars.
B
If
we
spread
the
colors
out,
we
get
an
as
if
fifth
dimension
notice
the
air
quotes.
This
is
the
spectrum
of
the
sun
as
it
turns
out,
and
all
those
dark
lines
actually
have
meaning
it's
beautiful.
Aesthetically
too.
I
love
to
look
at
the
colors
and
go.
Where
does
this
blue
turn
to
green?
You
know,
or
where
does
this
you
know
green
or
you
know
all
those
transitions
very
smooth?
B
These
barcodes
help
us
understand
a
lot
about
the
stars.
They
say
70
or
80
of
the
research.
That's
done
in
astronomy
is
done
using
spectroscopy
in
my
next
life.
I'm
going
to
choose
a
field
where
there
are
fewer
syllables
in
the
specialty
that
I'm
involved
in
spectroscopy
can
be
a
mouthful,
but
these
barcodes
can
show
us
a
lot
of
different
things.
I
won't
read
the
bullets
here
because
I'm
going
to
give
you
some
examples
of
these
as
we
go
through
tonight.
B
So
let's
just
get
started
by
talking
a
little
bit
about
the
science
just
to
get
everybody
to
the
same
level.
Forgive
me
if
you're
familiar
with
this
I'll,
try
and
move
quickly
through
this.
The
good
news
is,
you,
don't
have
to
know
a
lot
of
science.
You
don't!
Thank
goodness.
You
don't
have
to
have
a
phd
to
do
spectroscopy.
B
I
don't
have
an
undergraduate
degree
in
science
and
in
fact
I
had
a
quote
that
I
put
up
on
a
talk
I
gave
earlier
today.
I
haven't
decided
whether
to
incorporate
it
into
my
general
talks,
and
that
is
the
quote
went
something
like.
If,
if
you
were
going
to
wait
till
you
had
a
phd
in
astrophysics
to
do
astronomy,
dot,
dot
dot,
you
wouldn't
be
an
amateur
astronomer
today.
B
B
We
can
also
bounce
it
off
of
a
dvd,
a
finely
lined
surface
like
a
dvd
or
even
pass
it
through
a
ruled
piece
of
glass
called
a
diffraction
grating
bunsen.
He
was
the
first
person
to
actually
systematically
study
spectra.
He
burnt
samples
in
a
flame
and
he
put
the
light
through
a
prism
and
he
looked
at
the
results
he
burnt.
He
was
a
pyromaniac.
He
burned
everything
he
could
find,
and
the
great
thing
is
that
he
kept
notes
really
clearly,
so
he
created
a
catalog
that
has
served
us.
B
Its
grand
great
great
great
great
grandchild
has
served
us
today
as
we'll
see
in
a
few
minutes
over
on
the
right
here.
This
guy
kirkoff
was
a
contemporary,
a
colleague
of
his.
We
won't
spend
a
lot
of
time
with
him,
but
the
one
thing
I
wanted
to
point
out
related
to
what
he
thought
about,
and
that
was
that
some
spectra
have
like
a
rainbow.
In
the
background
with
gaps,
you
can
see
those
gaps
there
and
other
spectra
have
a
more
or
less
black
that
background
and
lines.
B
Now
the
nice
thing
about
this
is
regardless
of
which
it
is
the
lines
or
the
gaps
are
in
the
same
position
now,
which
one
you
get
depends
on
things
we
won't
talk
about.
The
kirchhoff
talked
about
the
temperature
of
the
gas
that
the
light
is
going
through
things
like
that,
but
because
we'll
see
examples
of
these
two,
I
just
wanted
to
point
this
out.
As
we
get
started.
B
B
So,
in
fact,
hydrogen
is,
of
course,
is
so
common
in
the
universe,
and
we
use
it
so
often
that
it's
nice
to
have
this
term
of
for
all
of
the
lines
in
hydrogen
called
the
hydrogen
bomber
lines
and
we've
even
named
the
lines
with
greek
letters
like
we
made.
We
named
the
stars
in
constellations
by
intensity
by
other
greek
letters
so,
for
example,
hydrogen
beta
here
that's
sort
of
a
that's
like
robin
egg,
blue,
for
example,
and
there's
the
gamma
and
the
alpha
and
the
red
here's
a
periodic
table.
B
I
created
a
few
years
ago.
We
sell
most
of
them
to
to
schools,
chemistry,
physics,
astronomy
departments
and
some
amateurs
get
them
too
they're
real
nerds.
So
I've
got
one
and
in
fact
I
can
brag
and
neil
neil
degrasse
tyson
told
me
he
has
one
hanging
on
the
wall
of
his
office.
So
we're
happy
about
that.
Also,
there's
one
on
the
sofia:
boeing,
747
airborne
telescope.
B
B
So
these
days
we
don't
have
to
actually
burn
things.
We
have
a
gas
tubes
and,
let's
see
if
I
can
show
you
one
here-
here's
a
gas
tube
over
here.
I
can
turn
it
on.
You
can
see
the
brightness
there
it's
you
know
it's
just
a
tube
with
some
sort
of
rarefied
gas
in
it.
In
this
case,
maybe
you
can
see
the
lettering
there.
It's
helium
so,
and
this
is
actually
a
a
device
that
we
use
in
our
in
classrooms.
B
This
is
a
little
spectrometer
that
works
with
our
software,
that
physics
and
chemistry
and,
as
I
mentioned
astronomy
teachers
use
to
teach
those
topics.
We
have
a
lot
of
those
around
the
world
in
a
lot
of
different
schools,
the
closest
one
to
you.
I
can't
remember
the
name
of
it
I'll
think
of
it,
while
we're
talking
tonight
so
so
far,
everybody
I've
mentioned
have
been
old
white
men.
B
What
about
some
people?
Who
aren't
old
white
men?
We
saw
a
great
example
of
non-old
white
men,
a
man
giving
a
speech
earlier
today.
Some
of
you
may
have,
but
let's
look
at
annie,
jump
cannon
and
her
women
called
the
computers
they
were
prohibited
because
of
their
gender
about
100
years
ago
from
accessing
the
telescopes
at
harvard.
B
B
She
was
a
big
proponent
of
the
hubble
space
telescope,
which
is
in
the
background
there.
Thankfully
she
had
a
hand
in
making
it
happen.
Elisa
quintana
studies
exoplanets
and
has
discovered
some
in
the
goldilocks
zone
around
some
red
giants
where
there
might
be
water
and
and
thus
perhaps
life,
of
the
sort
we're
familiar
with
and
finally,
jedediah
isler
is
she's
a
dartmouth
and
she
studies
a
gravitational
lensing
around
black
hole.
So
this
is
a
new
slide
for
my
presentation
that
I
made
this
summer.
B
B
So
what
I
want
to
talk
about
tonight
is
this
grading
here,
it's
a
star,
analyzer
grading,
it
costs
about
200,
and
that's
all
you
need
to
add
to
your
current
kit
to
do
this.
So
if,
if
people
are
thinking
or
or
telling
you,
oh
man
you're
going
to
have
to
spend
thousands
of
dollars-
and
you
know
really
carefully
calibrate
all
these
things
that
you've
never
used
before
a
couple
hundred
bucks
get.
B
You
started
really
simply
so
here's
some
examples
of
how
we
might
mount
a
star,
analyzer
grading
in
the
upper
left
there
you
can
see
in
my
video
here.
Here's
a
dslr
with
this
is
just
a
little
adapter
that
that
we
we
offer
it
screws
into
the
lens
cap
threads
like
that,
and
then
you
can
put
the
grading
in
now
it's.
Of
course
this
is
relatively
low
resolution
and
very
small
aperture,
but
you
can
actually
do
dslr
spectroscopy
with
the
grading
here
before
the
lens.
B
It's
called
an
objective
grading
and
some
people,
even
though
they
have
much
more
sophisticated
gear,
also
use
this
to
capture
interesting
spectra.
I'll
show
you,
for
example,
one
of
a
comment
in
a
few
minutes.
Here's
a
just
an
example
of
a
fitz
camera.
It
could
be
cool
uncooled
on
the
lower
right
there
again,
that's
like
a
one
of
these
zwo
cameras
where
again,
fortunately,
the
grating
often
just
screws
directly
into
the
nose
piece.
I
need
one
more
hand
here
in
order
to
accomplish
that,
I
will
talk
about
mounting
it.
A
little
bit
also
could
be.
B
Color
can
be
mono,
as
I
mentioned,
or
you
can
put
it
in
a
filter
wheel.
So
there's
lots
of
ways
to
use
these
gratings
now.
The
other
thing
to
mention
about
dslrs
is
that
you
can
piggyback
on
your
current
equipment,
so
you're
not
messing
around
with
whatever
imaging
equipment
you
have
set
up
on
at
the
prime
focus.
Okay,
so
enough
history
theory
equipment.
What
can
we
actually
do?
B
We
get
that
rainbow
spectrum
and
the
starlight
also
some
of
it
goes
straight
through
and
we
can
capture
that
on
our
sensor.
Let's
look
at
our
first
example:
it's
really
an
amazing
one,
so
these
are
all
different
spectra
captured
at
a
different
time
by
torsten
hanson
and
look.
He
used
just
an
8-inch
newtonian
with
an
imaging
source,
video
camera
so
and
these
stars
are
in
temperature
order.
B
B
B
So
this
is
how
astronomers
actually
tell
the
different
temperatures
of
stars,
and
if
we
look
down
here
at
this
region,
I
mean
that's
not
like
a
line.
That's
like
a
forest
of
lines
right
well
on
these
cooler
type
m
stars,
they're
cool
enough
that
in
the
outer
atmosphere
in
the
outer
shell,
some
more
complex
molecules
than
just
hydrogen
or
helium
this.
These
are
actually
titanium
oxide
can
survive
without
getting
incinerated.
B
Now
truth
be
told,
I
don't
know
anything
else
more
about
titanium
oxide
than
what
I've
just
told
you
the
great
thing
about
being
the
adults
we
are
and
spectroscopy
is
you
don't
have
to
dig
down
deep,
deep,
deep
and
study
for
the
final
exam?
You
learn
as
much
as
you
want
and
there's
lots
of
different
places
to
learn
things.
B
So
here's
the
deal
the
way
these
lines
get
made.
You
may
remember
some
of
this
from
school
is
in
the
bohr
model
of
the
atom.
We
have
these
orbits
that
the
electrons
are
in
and
sometimes
they
jump
either
up
or
down
between
orbits
and
this.
This
is
what
in
the
roman
egg
blue.
So
that's
the
hydrogen
beta
and
that's
the
jump
from
orbit
four
to
orbit
two,
it's
again
when
it's
jumping
up
so
there's
this
jumping
up
and
down,
and
you
get
either
emission
lines
or
absorption
lines
depending
on
the
jumping.
B
We
need
not
get
into
that
detail
so
on
these
hotter
stars,
a
lot
of
the
electrons
they
get
pumped
up,
but
they
go
because
the
stars
are
more
energetic
because
they're
hot
right,
past
level,
four
and
out,
perhaps
so-
we
don't
have
as
many
electrons
sitting
at
four
to
drop
down
between
two
and
four
and
the
same
thing
down
here.
These
stars.
B
B
Spectroscopy
is
really
a
lot
more
immune
to
urban
light
pollution,
because,
unlike
the
the
video
imaging
that
you
do-
and
I
know
you
all-
some
of
you
go
out
to
morgan
hill
and
and
other
dark
sky
relatively
dark
sky
sites,
because
you
are
imagers,
you
know
how
problematic
urban
light
pollution
is
everybody
pretty
much
knows,
but
with
imaging
we're
really
interested
in
the
aesthetic
quality
and
the
balance
and
we're.
You
know
we
do
a
lot
of
tweaking
and
we
need
all
the
photons
we
can
get
with
the
least
the
best
signal
noise.
B
Let's
say
so,
but
with
spectroscopy
because
we're
doing
science
we
don't
want
to
mess
with
the
photons
after
they've
hit
our
sensor.
We
don't
want
to
be
tweaking
or
enhancing
in
any
way
and,
as
I
said,
because
we're
just
looking
for
peaks
and
valleys
rather
than
the
overall
aesthetic
balance
and
contrast
and
so
forth.
B
We
can
do
a
lot
more
in
the
city,
which
means
that
a
lot
of
people
do
this
in
the
city
and
then
when
they
go
out
to
the
country
they
or
the
dark
sky
sites,
they
do
a
little
bit
more
deep,
imaging
or
if
they
get
really
hooked
on
spectroscopy,
they
just
do
more
spectroscopy
out
there
with
dark
skies.
So
you
see
that
crosshairs
there.
B
But
you
know
if,
if
I
had
time
on-
let's
say
the
hubble
space
telescope
and
I
was
capturing
spectra-
and
I
wrote
a
paper
that
said
yeah-
we
captured
the
spectrum
and
and
we
we
got
a
little
dimming
in
the
robin
egg-
blue,
that's
not
that's,
not
publishable
is
it
so
we
have
to
become
quantitative
and
to
do
that,
we
graph
the
intensity
of
this
region.
It's
really
pretty
straightforward.
B
This
axis
here
is
intensity
and
you
can
see
the
star,
for
example,
is
very
bright
and
narrow.
So
this
is
a
very
high
peak
and
it's
not
very
wide,
whereas
this
thing
is
very
wide.
It's
sort
of
dim
in
this
area
and
then
it
gets
brighter
brighter
brighter
and
then
dimmer
dimmer
dimmer.
So
this
starts
at
dim
and
gets
brighter
brighter
brighter
and
dimmer
dimmer
dimmer.
But
look
at
this
see
that
dip.
B
That's
where
the
science
is
now,
even
though
we
can't
quite
see
it
visually
and
there's
another
dip
there,
maybe
that's
down
there
and
that
dip
might
be
that
in
order
to
do
science
now
we
can
measure
the
full
width
half
maximum
of
that
dip.
We
can
look
at
the
area,
that's
enclosed
by
that
dip
or
look
at
how
it
relates
to
other
stars
or
this
star
on
other
nights
or
other
pieces
of
equipment.
B
Well,
my
story
is
in
I've
been
an
amateur
since
what
about
1990,
but
in
about
2009
I
wanted
to
do
some
science,
and
so
I
got
a
grading
when
out
in
my
backyard,
I've
got
a
sct
an
eight
inch.
Just
like
you
said
you
have
zooka
don.
In
fact,
I
went
out
in
the
yard.
You
know
it's
right
outside
the
window
there.
B
If
I
can
get
my
pointer
finger
in
the
view-
and
it
was
a
saturday
night-
I'm
three
miles
from
pike
place
market,
I'm
in
more
or
less
in
downtown,
and
I
came
in
at
midnight
and
I
actually
I
found
it
the
other
day
I
was
cleaning
my
office.
I
was
just
using
this
logitech
webcam.
You
can
still
see
the
residue
of
the
duct
tape,
as
I
duct
taped
it
to
the
nose
piece
or
a
barrel
on
an
eyepiece,
and
I
mean
it
was
a
mess
I
came
in
at
midnight.
B
I
I
had
some
video
of
vega.
I
had
a
sore
neck.
My
knees
on
my
blue
jeans
were
were
well
it's
vega
in
august.
What
do
you
expect
and
sunday
morning-
and
this
literally,
is
that
image
sunday
morning?
I
wanted
to
create
this
graph
and
I
failed.
I
downloaded
the
freeware
that
was
out
there.
I
had
trouble
installing
it
there
was.
B
It
was
like
dll
hell,
I
you
know
it
was
crashing
half
of
it
was
in
french
and
there
was
no
manual
it
just
wasn't
up
to
the
usability
level
that
we're
all
accustomed
to
these
days,
and
so
I
quit.
I
gave
up
I'm
a
little
embarrassed
to
admit
that
who
likes
to
embarra
to
admit
they've
quit.
I
told
my
wife,
I
said:
look
I'm
supposed
to
be
having
fun.
This
is
a
hobby.
This
isn't
a
job.
B
I
had
fun
in
my
job
too,
but
but
I
couldn't
just
quit
as
easily
as
I
could
quit
this.
So
I
put
the
grating
in
the
drawer.
Well,
a
few
weeks
went
by
and
it
kept
bugging
me
because
I
really
wanted
to
do
this,
and
so
I
figured
okay
saturday
at
the
end
of
the
work
week,
I'm
gonna.
I
wish
it
was
always
the
end
of
the
work
week,
but
work.
These
days
is
often
seven
days
a
week.
B
So
I
figured
I'd
just
write
a
piece
of
software
to
generate
this
curve
and
I
did
sunday
morning
I
was
done
and
now
I
don't
know
10
or
15
000
hours
later
the
software
is
almost
done.
My
wife
keeps
saying,
would
you
finish
the
software,
so
we
can
start
having
dinner
together
on
time?
It's
done,
but
you
know
the
thing
is
that
I
didn't
intend
to
create
a
product.
I
you
know
I
had
my
other
job
and
everything,
but
people
really
got
excited
about
what
I'd
done.
B
One
of
the
obstacles
to
starting
something
new
like
spectroscopy
is
oh,
no,
another
piece
of
software
to
learn
another
learning
curve.
So
I
want
to
relieve
you
of
that
misconception
now.
I
know
it's
after
dinner
here
I
talk
to
a
lot
of
clubs
back
east
and
I'll,
be
it'd,
be
four
o'clock
here
and
seven
o'clock
there,
and
it's
always
after
dinner
for
them,
but
for
all
of
us
here
on
the
west
coast.
Now
it's
nice
to
talk
to
a
club
on
the
west
coast.
For
me
I
know
it's
after
dinner,
I'll
lose
you.
B
If
this
turns
into
a
software
demonstration.
I
know
I
will
so
I
don't
want
to
spend
much
time
with
this,
but
I
do
want
to
show
you
a
screen
or
two,
because
I
think
it's
important
for
you
to
see
how
easy
it
is
to
do
so.
Here's
an
image
it
happens
to
be
in
color,
of
course,
color
cameras
aren't
quite
as
sensitive
and
they
have
some
other
scientific
shortcomings.
Color
is
great,
though,
for
outreach
and
also
for
people.
B
Newcomers
to
sort
of
understand,
what's
going
on,
there's
the
star:
there's
the
spectrum,
there's
a
gap,
there's
maybe
some
gaps
there.
All
we
do
is
bracket
in
our
spectrum
like
that,
and
we
have
that
intensity
curve
over
here.
That
peak
is
the
star,
and
this
thing
here
is
that
and
see
that
gap
right
there.
It's
that
dip,
that's
oxygen
in
the
atmosphere
so
and
that
dip
there
in
the
robin
egg
blue.
What
do
you
suppose
that
is
that's
our
hydrogen
beta
line?
B
So
how
do
we
identify
all
these
dips?
Well,
remember
I
mentioned
that
bunsen
created
a
catalog
and
the
grand
grand
grand
grand
grand
catalog
descendant
is
one
that
still
serves
us
all
today
and
it's
built
into
the
software
here
I
can
come
down
and
say
just
two
or
three
more
clicks
and
we're
done
with
the
software,
but
I
can
come
down
here
and
say:
show
me
where
the
bomber
series
would
be
if
there
are
dips,
where
all
these
lines
are,
we
can
be
pretty
sure
somewhere
between
us
and
the
star.
There's
some
hydrogen.
B
That's
absorbing
some
light
because
of
those
electrons
jumping
and
look:
we've
got
a
dip
there.
One
matches
there
there
isn't
that
amazing.
So
now,
with
a
backyard
telescope,
this
is
literally
a
frame
from
that
first
video.
I
shot
backyard
telescope
in
the
city,
we're
detecting
scientific
data
from
a
distant
star
I'll
show
you
some
distant
objects
that
are
billions
of
light
years
away
in
a
few
minutes,
so
this
is
actually
a
frame
from
the
video.
I
first
shot
that
night.
It's
I'm
going
to
play
it
back
here
at
two
frames
per
second
now.
B
The
image
here
is
jumping
around
because
my
seeing
so
so
is
the
graph.
Okay,
now
we're
all
familiar
with
stacking,
how
we
can
average
out
noise.
This
is
fun
to
watch
I'll
watch
this.
This
will
be
the
last
thing.
I
show
you
here.
There's
our
hydrogen
alpha
line
there.
We
can
see
the
little
label
but
notice
that
dip
is
sort
of
coming
and
going
and
moving
around
because
of
our
noise.
Let's
turn
on
simple
stacking
in
the
software
watch.
B
How,
in
a
matter
of
a
few
seconds,
maybe
10
or
15
frames
that
dip
becomes
very
stable.
The
video
is
still
playing,
but
now
we've
averaged
out
all
that
noise.
So
that's
really
all
I
wanted
to
show
you
here.
The
only
the
only
other
thing
I'd
ask
you
is
to
remember:
let's
get
the
right
key
here
in
your
mind's
eye.
B
If
you
would
remember
that
view,
this
happens
to
be
vega,
it's
a
type
a
star,
but
we've
got
these
lines
showing
the
bomber
series,
because
I
want
to
show
you
some
discoveries
that
were
made
with
this
data
as
we
go
forward
tonight.
So
let
me
get
the
right
screen
up
here
there
we
go,
get
rid
of
that
thing
there.
So
here's
a
cool
thing
in
fact,
now
that
I
left
that
screen,
I
meant
to
mention
to
you
just
one
more
thing
here:
I
won't
click
anything.
B
This
is
a
fantastic
screen
for
when
you're
doing
outreach,
because
the
color
and
the
movement,
and
even
better,
yet
it
can
act
as
a
platform
for
you
to
transition
into
a
scientific
discussion.
You
don't
have
to
know
a
lot,
but
to
talk
with
people
a
little
bit
about
how
we
understand
the
stars
can
go
a
long
way
now.
The
other
thing
you
can
do
is
you
can
go
and
look
how
sometimes
those
dips
are
really
deep.
B
B
Hey,
let's
look
at
the
sun
or
or
something
it's
another
thing
to
say:
we've
got
some
science
to
do
here
and
you
can
act
as
a
mentor
to
high
school
students
and
it's
incredibly
rewarding.
So
let
me
stop
that
playback
and
now
head
back
to
the
software.
This
is
an
example
of
some
outreach
that
you
could
do.
This
is
of
a
gas
tube.
B
It's
my
software.
This
is
actually
in
marseille,
france.
This
might
not
be
something
you
could
do
in
a
dark
sky
site
with
all
that
light,
but
they
transitioned
into
looking
at
stars
after
this
introduction.
So
here's
a
dslr
image
with
the
grading
on
the
nosepiece
and
you
can
see
some
stars
in
their
associated
spectra.
There's
a
gap
there.
Here's
a
star
here
with
these
lumps
right.
Well,
those
again
those
are
emission
lines.
They
were
so
bright,
they
saturated
our
pixels.
We've
got
some
blooming,
but
let's
look
at
a.
B
In
fact,
let's
look
at
a
wolfry
a
star
here
now
I
have
a
confession
to
make
to
the
group
when
janet
simpson,
I
couldn't
remember
her
name.
I've
probably
said
it
400
times
when
janet
simpson
sent
me
this.
Some
years
ago,
I
couldn't
remember
what
a
wolfry
a
star
was
now,
maybe
you're
in
the
same
shoes,
which
is
pretty
much.
B
What
I
found-
and
the
reason
I
bring
this
up,
is
what
I
found
is-
and
you
may
have
found
this
if
you're
an
imager
and
by
the
way,
if
you're,
not
an
imager.
I
should
have
said
this
earlier
before
you
tuned
out,
if
you're
not
an
imager
even
following
along
tonight,
I
think
that
you'll
learn
a
lot
about
how
imaging
and
how
spectra
get
captured
and
that
will
serve
you
while
you're
reading
magazines
or
you
know
things
online.
B
So
this
isn't
just
a
talk
for
images
who
might
want
to
do
this
kind
of
thing.
So
wikipedia
is
our
friend
right.
Wolf
really
stars
are
late
stage
stars
headed
perhaps
to
becoming
a
supernova
they're
massive
they're
25
times
as
large
as
the
sun.
A
very
hot,
intense
stellar
winds
dissipating
the
outer
shell
and
here's.
What
that
emission
spectra
right,
these
peaks
look
like
carbon
carbon
carbon.
B
Why
would
we
be
seeing
carbon
well?
Remember.
Stars
burn
through
the
elements
one
by
one,
hydrogen
helium
on
up
and
part
of
that
process,
as
the
star
has
matured
has
involved
carbon
and
we're
seeing
that
glowing
carbon
or
you
could
almost
call
it
soot.
It's
not
really
soot,
but
this
is
the
kind
of
thing
and
look
at
the
numbers
at
the
bottom.
There
30
seconds
with
a
dslr
who
would
have
thought.
B
So
this
is
an
emission
object
and
the
reason
by
the
way
we
can
see
these
peaks
with
such
simple
gear
is
because
that
intense
stellar
wind
has
widened
those
peaks
from
what
they
would
normally
be.
Let's
look
at
another
emission
object.
Our
beloved
ring
nebula,
there's
what
it
looks
like
you
can
see,
there's
just
two
colors
or
two
elements
emitting
here
we
have
hydrogen
alpha
and
we
have
an
ionized
oxygen.
That's
what
that
roman
numeral
three
means,
if
you're
not
familiar
with
that.
B
It
just
means
some
of
the
electrons
have
been
pulled
out
so
but
most
extended
objects
other
than
this
one
are
pretty
boring
without
a
slit.
If
it's
just
this,
and
so
in
fact,
let
me
show
you
an
extended
object
with
a
slit
spectrometer.
First
of
all,
here
are
the
slit
devices
that
typically
amateurs
use.
You
can
see
they're
like
an
order
of
magnitude,
more
expensive
and
and
probably
equally
that
much
harder
to
use,
because
now
you're
acquiring
your
target
and
guiding
on
it
having
to
track
it
on
like
a
20
micron
slip.
B
Starts
with
this
to
understand
the
field
and
to
get
that
foundation
of
skills
as
well
as
knowledge,
but
here's
a
slit,
spectrometer
image
of
orion
nebula
here
are
these
emission
peaks
and
there's
our
our
red
hydrogen
alpha
and
there's
that
ionized
oxygen
with
that
roman
numeral.
Three.
Of
course
this
is
the
beginning
of
stars,
rather
than
the
end
of
stars
like
that
wolf-free
a-star.
B
So
now
real
quickly
since
we're
not
in
zoom,
I
can't
query
you
live,
and
I
know
it's
it's
the
topic
of
religious
wars
as
to
whether
to
use
zoom
or
not.
I
prefer
zoom,
although
the
club
has
good
reason
to
use
youtube
for
present
presentations
like
this,
because
that
way
we
can
break
out
and
have
discussions,
but
so
my
story
instead
of
queering
you
on
on
yours
and.
B
That
different
than
this
I
wanted
to
do
astronomy.
I
found
a
club
I
was
living
in
denver.
I
went
out
one
night
in
the
city
first
quarter,
star
party,
I
walked
out
on
the
observing
field,
I'd
never
seen
telescopes
before,
but
I've
seen
pictures
in
magazines
and
I
look
out
on
the
observing
field.
You
know
it's
sort
of
cool
when
you
can
remember
when
you
didn't
know
something.
When
I
looked
at
that
observing
field,
the
honest
truth
truth
here
I
thought
I
looked
and
went.
B
What
are
all
you
know,
those
cannons
that
they
shoot
people
out
of
in
the
in
the
circus.
That's
what
I
thought
I
would
I'm
going.
What
what
is
this?
What
I
thought
I
was
gonna
see:
telescopes.
Of
course
they
were
dobbs,
but
I
didn't
know
any
better.
I
queued
up
at
a
dob.
Somebody
was
running
it
much
like
some
of
you
and
I
have
done
they
were
pointing
at
m42.
I
was
all
excited
and
you
know
I
got
up
to
the
front
of
the
line.
I
looked
through
the
telescope
and
I
was
really
let
down.
B
I
was
really
disappointed.
It
was
a
smudge.
That's
the
most
common
word.
I
hear
when
I
ask
club
meetings
to
describe
their
first
experience
with
m42.
It's
a
smudge.
It
was
mono,
it
was
nothing
so.
Fortunately
I
kept
with
it,
as
did
all
of
you
or
you
wouldn't
be
here
today.
So
why
do
I
still
go
back
as
well
as
you
go
back
to
look
at
m42?
What's
changed?
B
B
I
think
the
reason
we
go
back
is
because
now,
when
we
go
back,
we
understand
what
it
is
we're
looking
at.
We
know
it's
the
stellar
nursery,
the
birthplace
of
stars
and
when
the
reason
I
mention
this
is
because
when
we
bring
that
understanding
to
our
visual
observing
it
gets
that
much
more
interesting.
It's
a
much
deeper
experience
and
that's
something
that
spectroscopy
has
done
for
me.
B
So
here's
an
example
of
uranus
and
neptune.
You
can
see
in
the
spectra
themselves
these
these
big
gaps
and,
of
course
there
it
is
on
the
intensity
graph,
and
there
is
that
band.
What
did
we
learn
earlier
about
type
m
stars
when
we
saw
a
band
that
meant
that
it
was
relatively
cool
and
some
more
complex
molecules
could
exist?
B
Well,
these,
of
course
aren't
stars,
but
they
are
cool
and
what
we're
seeing
here
is
a
complex
molecule
with
again
same
guy
torsten
hanson,
using
that
eight
inch
newtonian
and
a
well
camera
like
this.
It's
the
imaging
source,
but
in
this
case
most
of
us
would
use
perhaps
a
zwo
camera
or
a
malin
cam.
B
So
with
quarter
second
exposures,
you
know
running
at
four
frames,
a
second
or
even
slower,
we're
able
to
capture
the
the
the
methane
on
these
planets
the
atmosphere
and,
of
course,
one
of
the
ways
that
we
are
searching
and
we'll
eventually,
if
we
do
detect
et
some
sort
of
extraterrestrial
life
will
be
by
observing
the
atmosphere
of
these
exoplanets.
Much
like
we
observed
something
in
venus
not
long
ago.
We're
not
sure
what
it
showed
us
at
this
point,
but
it's
cool
that
we
can
do
that
ourselves.
B
B
It
looks
great
okay,
good
thanks
yeah,
so
there's
a
spectrum
of
a
comet,
it's
pretty
in
itself
and
there
you
can
see
the
intensity
peaks
of
the
swan
bands.
Those
are
carbon
now
this
is,
you
know,
pretty
cool,
it's
an
extended
object,
but
it's
compact
enough
that
we
can
still
use
a
slitless
inexpensive
grading
like
this,
so
this
was
captured
by
vikrant
agnihotri
he's
a
nuclear
power
plant
engineer
in
rajasthan
in
northwest
india
and
in
19
2013,
I'm
dating
myself
in
2013.
B
He
was
a
newcomer
and
now
today
he's
a
real
expert
and
I
learn
from
him
what
teacher
doesn't
want
to
learn
from
their
student?
Really,
it's
just
wonderful
to
talk
with
him
and
again.
I
spend
a
lot
of
time:
mentoring
and
teaching
amateurs
and
and
even
high
school
students,
because
it's
just
fun
it's
something
that
I
enjoy
doing
very
nourishing
for
me.
So
here's
another
more
timely
example.
We
can
see
the
peak
here
in
the
yellow
for
the
sodium
in
neo
wise
and
this
is
you
see
that
word
objective?
Grading?
I'm
not
sure.
B
Now
any
anybody
who
uses
a
c-clamp,
that's
my
kind
of
amateur.
I
break
just
about
everything.
You
know,
in
fact,
that's
another
reason
I
like
the
grading,
is
because
it's
tough
to
break
there's
now
that
I've
lost
it.
Oh
here
it
is
so,
but
this
was
a
spectrum
and
a
setup
put
together
by
a
guy
named
robin
lead
beater
who
designed
the
star
analyzer,
actually
see.
My
problem
is
since
I
break
everything.
B
In
fact,
you
know
my
favorite
command
in
windows
is
control,
z
or
edit
undo,
but
I'd
probably
have
cranked
that
c
clamp
down
too
tight
and
and
collapsed
the
camera
housing
and
destroyed
the
camera.
So
he
didn't,
thank
goodness.
He
attached
a
star
analyzer
to
the
video
camera
in
a
perseid
meteor
shower
and
here's
a
secret
excuse
me
a
single
frame
that
he
captured.
B
B
Excuse
me,
so
this
is
rather
specialized
right.
There
aren't
meteors
every
night
to
look
at
and
you've
got
to
capture
them
right
and
you
know
there's
lots
of
challenges,
but
some
people
love
doing
this
thing.
Whatever
floats
your
boat,
why
not
so
we're
not
going
to
spend
much
time
talking
about
the
flash
spectrum
but
again
one
advantage
of
low
resolution.
B
Spectroscopy
like
this
is
you
can
get
the
whole
spectrum
in
one
view,
and
we've
heard
a
lot
about
the
sun
recently
we
will
be
again
in
the
next
several
years,
just
to
point
out
here
that
it
was
in
1868.
We
observed
during
the
total
eclipse
of
the
sun
that
this
yellow
line.
We
didn't
know
what
it
was:
bunsen
hadn't
cataloged
anything
with
that
yellow
line,
so
they
just
figured
okay.
We
don't
know
what
it
is.
It's
on
the
sun
greek
for
sun
is
helios.
Let's
give
it
the
name
helium.
B
Now
you
fast
forward
20
or
30
or
40
years,
a
couple
of
researchers
discovered
spectroscopically.
Some
saw
a
gas
here
on
earth
that
they
had
created
that
had
the
same
yellow
line.
They
had
discovered
helium
here
on
the
earth
after
we
had
already
identified
a
physical
property
of
it
on
the
sun.
It's
amazing
story
and
told
rather
quickly
sorry
for
the
speed.
Do
you
feel
like
you're
drinking
from
a
fire
hose?
I
apologize
so
novi
with
a
dslr.
B
You
can
see
some
have
iron
absorption
lines,
others
don't
if
that's
something
that
that
you're
interested
in
doing
a
quick
reminder
about
doppler
shift
again,
it's
the
change
in
pitch
or
wavelength
of
sound,
that's
moving
towards
or
away
from
us.
A
common
example
is
when
a
train
goes
through
the
station.
It
goes
air
right
so
higher
coming
towards
you
lower
going
away.
B
Well,
the
same
thing
happens
to
light.
So
if
we
were
expecting
to
see
this
triplet,
I
love
the
term.
It's
almost
self-defining
right
there
and
instead
we
saw
it
shoved
over
to
the
right.
What
would
that
mean?
Well,
that
would
mean
that
it
was
moving
away
from
us
right
as
the
car
moves
away
from
us.
The
sound
is
stretched
a
little
longer
lower.
B
That
would
be
redshift,
but
on
the
other
hand,
if
it
was
over
here
instead
of
where
we
expected
it
we'd
know
that
the
object
was
moving
towards
us
or
blue
shift.
Let's
look
at
a
really
cool
example,
so
supernovas
there's
a
lot
of
different
exploding
stars
again,
some
of
you
probably
more
than
a
handful,
know
more
about
this
topic
than
I
do,
but
there's
different
types
of
supernovae,
one
particular
type,
is
called
a
type
1a
and
it's
a
basically
it's
a
binary
system.
B
B
You
know
it's
a
binary
system,
it's
two
stars
so
without
getting
into
the
details
enough
enough
of
our
wordplay
a
type
1a
supernova
is
when
a
really
hot
star
dumps
gas
onto
a
white
dwarf,
and
when
you
put
gas
onto
a
hot
surface,
what
happens
it
explodes
so
here's
a
supernova
in
m101
there.
It
is
for
a
brief
time
brighter
than
all
of
the
stars
in
this
galaxy.
B
B
Well,
there's
a
spectrum
captured
with
our
star
analyzer
grading
by
david,
strange
with
a
9-inch
sct
and
less
than
15
minutes
worth
of
stacked
images
and
there's
the
profile
intensity
graph.
Now
you
can
see
a
little
dimming
here,
but
look
how
bright
it
is
in
the
graph.
Now
you
know
it's.
It's
almost
an
overused
phrase.
B
I
sometimes
wonder
whether
I
should
just
dump
it,
but
you
know
they
say
we're
standing
on
the
shoulders
of
the
giants
and
the
giants
are
really
smart
men
and
women
and
they
figured
out
that
the
different
types
of
supernova,
just
like
the
elements,
the
different
types
of
supernova,
whether
it's
this
binary
system,
or
whether
it's
a
a
single
star
collapsing
on
itself,
a
core
collapse.
When
it
runs
out
of
fuel,
they
all
have
different
fingerprint
specter.
B
Now
this
next
slide,
it's
not
going
to
be
on
the
quiz,
but
here
it
is
for
a
type
1a
supernova
notice
that
deep
dip
right
there
around
6000,
that's
silicon,
but
these
other
core
collapse
spectra
these
down.
Here
they
don't
have
a
deep
dip
in
silicon
they
have.
Other
fingerprints
like
this
type.
2
has
a
very
strong
emission
line.
That's
a
hydrogen
emission
line,
but
we
can
use
these
fingerprints
as
amateurs
to
determine
and
identify
supernova
types.
This
is
one
way
that
amateurs
can
contribute
to
the
professional
community.
B
Tim
puckett,
for
example,
a
few
years
ago,
showed
a
slide
at
a
conference.
I
was
at
with
it's
an
excel
worksheet
with
all
these
supernovae
that
had
never
really
had
confirming
data
on
them.
Now
the
problem
is
supernova
are
often
somewhat
dim,
so
it's
not
quite
as
easy
or
frequent
a
circumstance
that
you
could
do
all
the
time.
But
let
me
show
you
one
of
the
cool
things
that
david
strange
and
I
did.
First
of
all,
we
noted
the
wavelength
of
that
dip
at
61.50.
B
So
we
made
note
of
that.
Then
we
looked
up
online.
What
the
wavelength
of
silicon
would
be
if,
for
example,
bunsen
had
burnt
beach
sand.
That's
that's!
That's
good!
Bunsen
burnt
beach
sand,
that's
hard
to
say
so.
That's
the
stationary
wavelength
of
silicon
being
burnt.
Now
the
difference
between
those
is
doppler
shift.
Something's
moving.
B
I
couldn't
remember
the
doppler
shift
formula,
but
wikipedia
is
your
friend
and
you
plug
the
numbers
in
and
now
we
have
measured
the
blue
shift
of
the
shell
of
that
supernova
as
it
races
towards
us.
This
shell
is
expanding
at
22
million
miles
per
hour
and
we've
just
measured
it
on
a
backyard
telescope.
B
Now
you
may
remember
this
guy
adam
reese
when
he
won
his
nobel
prize.
It
was
for
work
that
he
and
his
team
did
just
before
the
turn
of
the
century,
studying
the
accelerating
cosmological
expansion
and
what
did
he
use
for
for
standard
candles
type,
one,
a
super
novi,
and
now
we've
measured
the
expansion
rate,
not
necessarily
the
radial
velocity,
but
the
expansion
rate,
which
would
have
given
us
the
distance,
the
expansion
rate
of
that
shell.
B
B
I
can
point
them
out,
because
this
guy
was
only
25
in
the
1960s
when
he
studied
this
and
he
was
really
frustrated
the
reason
I
know
this
is
this
wonderful
transcript
where
he
describes
this
discovery,
as
well
as
his
fears
and
the
challenges
and
it's
linked
to
on
our
site,
and
I
can
get
you
the
link
if
you
can't
find
it
just
contact
me
via
our
contact
form,
so
he
couldn't
figure
out
what
these
peaks
were.
So
he
said
in
much
of
the
science.
We
do
we
eliminate
things
as
to
being
well.
B
That's
not
that
we
see
what's
left
so
he
said
well,
let's
just
eliminate
those
from
being
the
hydrogen
bomber
lines,
so
we
brought
up
the
reference
lines
for
hydrogen
bomber,
and
this
is
that
image
from
my
software.
I
asked
you
to
keep
in
your
mind's
eye,
not
for
the
vega
part,
but
this
is
a
hydrogen
alpha,
beta
right
in
that
robin
egg,
blue
gamma
and
so
forth.
B
It's
not
hydrogen
anyway,
except
it
was
massively
shifted
to
the
right
redshifted
and
he
figured
that
out
when
he
went.
He
was
really
scared.
You
know
he
he
conferred
with
his
colleagues
before
publishing.
You
know
he
was
afraid
he
was
making
a
simple,
stupid
mistake
and
people
were
going
to
point
out
how
how
big
and
careless
he
was
to
make
that
mistake.
B
B
B
The
discovery
here
was
that
this
object
was
so
far
away
and
yet
so
bright
to
our
eyes
and
our
instruments
that
it
had
to
be
enormously
intrinsically
bright,
and
I
think
I
lost
it.
I
had
something
which
described
how
bright
it
is
intrinsically
we'll
see
if
it
comes
up
on
the
next
slide,
so
not
everything
ages
as
well
as
light.
Here's
martin
schmidt,
you
know
a
couple
years
ago
and
people
believe
me:
I've
been
justly
accused
of
throwing
rocks
in
a
glass
house.
B
B
B
So
to
look
at
the
details,
then
we
do
need
to
we
to
use
one
of
those
slit
spectrometers
and
I
wanted
to
show
you
some
examples
of
the
higher
end
work
that
we
or
professionals
can
do
so.
The
first
thing
there
is
an
amplified
or
higher
resolution
hydrogen
alpha
dip
from
vega,
very
sharp
dip.
Look
at
all
those
features.
Those
are
probably
all
things
that
could
be
identified.
B
B
There's
the
moon.
Look,
how
they're,
not
in
the
same
place
that
difference
is
again
from
doppler
shift
between
the
moon
and
blue
and
vega
in
future.
Right
so,
and
we
can
use
that
difference
to
measure
the
radial
velocity
of
vega
and
we
calculated
it
here
at
20,
kilometers
per
second
and
the
published
value
is
14.
pretty
amazing.
B
So
in
fact
this
might
be
a
good
point
just
to
take
a
brief
moment.
We've
got
one
more
example,
then,
we'll
finish
up,
my
wife
always
says
to
dress
for
success.
You
know-
and
this
is
the
hydrogen
beta
in
red
through
here
and
it's.
I
know
it's
a
mess.
I
apologize,
you
know,
the
thing
is
I
mean,
and
some
of
you
at
home
are
going
to
know
exactly
what
I'm
talking
about
here.
You
and
your
spouse
have
encountered
this.
B
Perhaps
I'm
having
trouble
finding
a
salon,
that's
open
and
has
time
for
me.
I
call
around
they're
just
not
like.
I
said
it's
a
common
problem
these
days,
I'm
hoping
that
it's
like,
I
said
it's
a
mess
now.
My
wife
does
tell
me
dress
for
success,
but
she
assures
me
this
is
not
it.
I
love
it.
It
also
keeps
me
warm
on
those
cold
nights,
so
here's
our
final
example.
B
B
So,
let's
see
what
that
looks
like
well,
here's
vega,
which
isn't
spinning
very
quickly,
but
if
the
star
this
is
just
another
explanation,
the
star
is
spinning
like
this.
The
light
coming
off
this
edge.
It's
this
edge
is
coming
towards
you,
so
it's
blue
shifted
and
this
light
is
redshifted.
So
what
we'd
expect
is
that
some
of
the
light
that
would
normally
be
here
is
going
to
be
here.
Redshifted
and
here,
blue
shifted.
Let's
see
what
that
looks
like
there's
altair
in
blue.
B
Look,
how
broadened
I
was
going
to
say
smashed,
but
that
didn't
sound
like
the
scientific
term.
So
look
how
broadened
that
peak
is
the
giants
really
are
giants?
I
mean
imagine
just
using
such
simple
math
and
simple
equipment,
just
looking
at
the
colors
of
stars
and
being
able
to
tell
how
fast
they're
rotating.
So
how
do
you
get
started?
Well,
let's
finish
up
first,
a
grading,
as
I
mentioned
earlier,
almost
any
sort
of
camera,
some
sort
of
software.
This
is
my
software.
B
Our
spec
stands
for
real
time
spectroscopy,
because
you
can
in
real
time
you
can
look
at
a
video
and
adjust
your
focus
and
exposure
time
in
real
time.
I'm
a
rather
old
programmer.
I've
been
programming
since
literally
the
60s.
So
like
some
of
you,
I
imagine
I'm
just
this
old
guy,
but
I'm
one
of
the
people
who
remembers
punch
cards
and
using
them
and
to
me,
even
though
static
fits
imaging,
of
course,
is
much
more
sensitive,
but
static.
B
Imaging
is
sort
of
like
old
punch
card
days
right,
you
dump
the
cards
in
and
then
you
have
to
wait
for
the
result
to
come
out.
The
cool
thing
about
video
is
it's
real
time?
It's
live.
It's
like
you
know
in
a
full
real
life
I
was
gonna,
say
time
share,
but
even
that's
an
archaic
term.
Now
so
here's
the
software
which
I
mentioned
earlier,
I
tried
I'm
good
friends.
B
You
don't
want
it
to
be
too
big
or
too
small,
because
that
changes,
how
much
the
spectrum
can
spread
out
and
you
don't
want
it
too,
dim
or
too
compressed,
but
there's
a
little
calculator
on
my
site
and
you
just
enter
all
the
specs
of
your
set
up
here
or
you
email
them
to
me.
There's
a
little
form
behind
this
link
that
I'll
I'll
you
know
you
send
me
your
telescope
kit.
B
You
know
what
the
specs
are
and
so
forth,
and
I
make
a
little
screen
video
and
show
you
what
we're
looking
for
some
green
flags
over
here.
It's
pretty
easy
to
do
it's
a
little
bit
of
a
speed
bump
as
you
get
started
by
the
way.
I
use
that
term
speaking
to
a
club
in
the
uk-
and
they
pointed
out
later
that
in
the
uk
they
don't
call
them
speed
bumps.
They
call
them
sleeping
policemen.
B
I
I
love
that
idiom,
so
there's
wonderful
books
out
there
these
days
for
this
kind
of
thing,
I
want
to
talk
a
little
bit
about
the
spectral
atlas
on
my
site.
Well,
I've
highlighted
download,
but
I
meant
to
highlight
links
so
I've
been
working
on
my
show
a
little
bit
here,
so
I
haven't
proved
it
quite
as
well
as
I
needed
to
this
atlas
here.
This
hat
does
get
warm
indoors
this.
B
This
book
here
is
really
fascinating
and
just
more
than
that,
it's
great
here's,
a
page
from
it
and
you
can
see
it's
calling
out
all
the
different
things
you'd
be
seeing
how
to
identify
it.
Here's
some
oxygen,
some
helium,
but
listen,
I'm
a
knuckle
dragging
programmer.
I
don't
know
the
significance
of
any
of
these.
Who
cares
if
there's
nitrogen
there?
It
doesn't
mean
anything
to
me
so
because
I'm
not
knowledgeable
enough,
but
the
great
thing
about
this
book
is
there's
all
sorts
of
pros
aimed
at
us
amateurs
oops.
B
So
much
so
much
for
that.
Let's
see
if
I
can
get
back
to
the
show.
These
books
are
aimed
at
amateurs
like
us
who
don't
understand
or
don't
have
the
background-
it's
not
aimed
at
phds,
so
that
in
itself
is
a
great
book
one
or
two
more
slides
here.
Let's
get
my
cursor
set,
we've
got
a
great
online
forum,
there's
tons
of
people
there
who
love
to
answer.
B
B
Let
me
first
mention
that
I
gave
a
workshop
an
hour-long
workshop
to
about
a
hundred
people
in
the
avso
at
the
sas
conference
down
in
la
if
you're
familiar
with
it,
and
there
was
sample
data,
everybody
had
their
laptops
and
they
we
we
and
they
recorded
the
whole
workshop
and
it's
available
on
youtube.
So
you
could
download
the
software
free
for
30
days,
download
the
sample
data
from
the
same
page
and
then
follow
along
with
the
youtube
video.
You
could
do
that
tomorrow
morning.
B
In
fact,
it's
saturday
today,
some
of
us
have
trouble
knowing
what
day
of
the
week
it
is
these
days
so
sunday
morning.
You
could
do
that
for
a
few
hours,
even
if
you
never
planned
to
do
this
or
didn't
even
have
a
telescope,
maybe
you're
an
armchair
of
I
was
going
to
say
armchair
philosopher,
I
meant
armchair
astronomer.
B
So
excuse
me
when
you
were
done
that
you
would
have
spectroscopy
in
your
bones.
So
it's
something
you
can
do
so
also
the
site
has
a
lot
of
tutorial
videos,
they're
three
or
four
minutes
long.
It's
me
just
walking
through
the
software.
It's
not
quite
like
drinking
like
from
a
fire
hose
like
tonight,
but
there's
no
big
thick
manual
to
learn.
You
you'll
be
doing
this
literally
in
your
first
or
second
night
out
you'll
be
capturing
spectrum.
B
There
are
opportunities
for
pro-am
collaboration,
there's
a
lot
of
databases
that
amateurs
can
contribute
to
now.
The
aavso
has
one
that's
about
a
year
old.
The
baa
in
the
uk
has
one
there's
one
in
france
for
a
particular
type
of
star,
not
as
much
opportunity
as
we'd
like,
but
there's
more
coming,
especially
stella
kafka.
B
The
great
director
executive
director
of
the
avso
is
moving
the
organization
into
this
field
and
her
predecessor,
arnie
both
being
professionals,
understand
the
importance
of
of
spectroscopy
in
the
field,
so
we've
come
a
long
way
in
the
last
two
or
three
hundred
years,
as
well
as
the
last
50
or
so
minutes.
I'd
like
again
to
thank
you
for
inviting
me
tonight.
Thank
you,
hopefully
for
smiling
or
laughing
at
some
of
my
jokes
for
those
of
you
who
do
outreach
public
outreach.
B
I
really
want
to
thank
you
because
I
think
it's
the
way
we
can
pay
it
forward
and
pay
it
backward
for
the
opportunities
we've
had
and
taken
advantage
of,
I'm
here
to
answer
questions
tonight,
as
well
as
by
direct
email
or
through
the
contact
form
on
my
site
again.
Thank
you
all
very
much,
and
now
we
can
try
to
answer
some
questions
from
the
youtube
crowd.
A
No,
I
mean
no,
it
was
fascinating,
I'm
so
glad
you
had.
You
have
added
that
slide
about
contributions
from
women
astronomers
in
terms
of
in
field
of
spectroscopy,
because
that's
something
we
don't
get
to
see
much
and
and
when
you
mention
annie,
jump
cannon,
my
first
thought
went
to
and
the
human
computers,
my
first
thought
went
to
hidden
figures
and
how
I
learned
about
it
through
the
movie
for
the
first
time,
yeah
and
and
then
also
thank
you
for
the
new
mnemonic.
A
B
A
A
B
A
B
B
You
know
the
issues
of
you
know
how
to
mount
the
grading
and
the
the
standard
issues
apply,
but
for
any
imaging
it's
you
know,
exposure
levels,
tracking
focus
other
than
that.
It's
surprisingly
easy
to
do,
there's
nothing!
That's
all
that
unique
to
capturing
data
with
a
grading,
but
it's
a
good
question.
I
actually
you
know
you
and
I
before
the
meeting
were
talking
about
the
astronomy
I
can
do
up
here
in
seattle
and
it's
pretty
frustrating.
B
If
I,
if
I
had
a
my
phone
on
zoom
right
now,
I
could
show
you
in
my
living
room,
in
fact
a
quick
story
here
in
my
living
room,
I've
got
my
c8
on
the
floor
and
the
tripod.
It's
all
ready
to
go
out
on
the
deck
when
we
get
a
clear
night.
But
it's
it's
been
there
now
for
a
couple
of
weeks
and
because
we
just
don't
get
a
lot
of
clear
nights
here,
but.
B
I
think
some
of
the
people
here
in
the
meeting
they
appreciate
this.
My
wife
bless
her
heart.
We
were
going
to
have
a
safe
distance
to
cocktail
hour
with
two
friends
on
our
deck,
and
so
she
said,
you've
got
to
put
that
telescope
away
like
in
the
closet,
and
I
said
we're
just
walking
through
the
living
room.
Why
would
it
matter?
B
And
she
said
no,
you
just
you
have
to
put
it
away
and
I'm
thinking
you
know
my
nerd
friends
like
the
attendees
at
this
meeting,
they'd
see
that
there
and
that
would
be
a
badge
of
honor
for
me,
they'd
be
going
all
right.
Guy
you've
got
your
telescope
good
to
go
you're
ready,
but
the
telescope
went
in
the
closet
and
then
came
out
again
after
that
that
evening,
but
anyway,
any
questions
come
up.
B
B
A
B
A
B
I
think
what
often
happens
you
know
is
especially
the
more
technical
of
us,
the
early
adopters
who
are
really
bright
and
really
capable.
They
end
up
writing
things
or
giving
talks
that
are
too
detailed.
I
mean
I
tend
tended
you
heard
I
kept
emphasizing
you
don't
have
to
be
a
phd.
You
don't
have
to
build
stuff,
because
ken's
book
has
a
lot
of
details
which
are
sort
of
interesting,
but
you
don't
need
to
get
started,
and
so
I'm
always
worried
that
people
will
read
a
book
like
that
and
go
well.
B
B
B
B
Let's
see
I'm
still
sharing
my
screen,
so
let
me
show
you
that,
and
I've
even
rotated
this
by
1.8
degrees,
because
that
I
didn't
screw
the
grating
on
right.
You
can
see
it's
a
little
bit
at
an
angle,
so
the
software
has
a
way
to
rotate
again,
you
can
rotate
things
all
over
the
place
if
you
want
in
order
to
get
them
horizontal,
it's
not
a
good
idea
to
do
that
when
you're
getting
real
scientific,
because
it
can't
introduce
artifacts,
but
that's
a
great
question.
B
B
So
it's
pseudo
real
time
that
way,
you
can
work
with
your
imaging
software,
nebulosity
or
whatever
you're
using
and
then
when
the
image
appears
it
will
automatically
pop
in
here,
and
you
can
evaluate
it
because
you're
going
to
be
focusing
for
the
deepest
dips
here
and
exposure
levels
are
are
particularly
important.
Also.
B
Good
really
good
question.
Unfortunately,
most
of
the
planets
are
too
large
to
look
at
with
a
grating
just
like
this,
because
they're
an
extended
object
like
m57
that
we
looked
at,
but
you
can
see
the
methane,
as
I
mentioned
in
uranus
and
neptune,
and
depending
on
how
sensitive
your
system
is,
I've
got
a
visual
aid.
I'll
show
you
here
in
a
minute,
you
can
look
at
some
of
the
the
more
distant
planets.
B
B
So
you
get
some
blue
shift
and
this
edge
of
the
ring
is
moving
away
from
you
and
you
can
actually
measure
with
an
inexpensive
slit
spectrometer
the
two
thousand
dollar
version,
not
the
three
or
four
or
twenty
thousand
dollar
versions.
You
can
measure
the
rotational
speed
of
the
rings
of
saturn
or
even
of
the
planet
itself.
So
that's
the
kind
of
thing
that
you
can
do,
but
mostly
you
end
up
observing
stars
stars
are
really
the
most
common
objects.
We
look
at.
A
B
B
Yeah,
typically,
it
stars
and
actually
the
stars
that
we
want
to
look
at.
Usually
let
me
share
my
screen.
One
more
time
are
we
want
to
start
in
the
little
the
getting
started
manual
by
the
way
is
right
there.
It's
it's
really
it's
about
10,
10,
12
pages
long,
and
it
describes
this
different
stars
have
different
absorption
lines
and
it
turns
out
these
type,
a
stars
like
vega,
have
the
deepest
clearest
hydrogen
lines
and
so
those
because
of
that
perfect
temperature.
B
Those
are
the
stars
we
start
with,
but
here's
something
I
wanted
to
show
you.
That's
pretty
cool
just
to
keep
people
entertained,
because
it's
not
only
entertain
you,
and
this
is
just
very
cool.
So,
let's
turn
off
that
fill
there
for
a
second
and
then
what
I'm
going
to
do
is
open
up
a
reference
library
and
and
ask
the
software
to
show
me
what
a
type
a
stars
spectrum
would
look
like
from
a
professional.
B
B
But
the
key
is
to
always
start
on
a
type
a
star
and
that's
emphasized,
as
I
said
in
the
documentation,
because
look
at
this
I'm
going
to
go
over
to
like
a
type
f
star.
You
don't
really
see.
Actually
that's
a
bad
example.
What
about
a
g
star
there
we
go
there!
Aren't
these
really
deep
dips
for
hydrogen,
like
we
saw
in
the
type
a
star,
so
the
a
star
is
best
to
start
on,
because
the
dips
are
so
deep
that
we're
more
likely
the
absorption
lines.
B
If
I
use
the
technical
term
are
much
easier
to
see
as
we're
learning
how
to
focus
and
and
understand
our
data.
But
here's
something
that's
sort
of
cool.
I
can
go
through
all
the
stars
in
that
ob
of
fine
gkm
order
see.
I
can't
remember
that
thing
so
notice
that
all
of
the
energy
on
these
type
o
stars
most
of
the
energy,
is
outside
the
visual
light
range,
but
watch
as
I
go
through.
This
is
going
to
go
through
one
star
at
a
time
very
quickly.
B
So
this
shows
you
the
planck
curve
that
vary
because
the
star
temperatures
are
varying.
This
is
another
way
that
we
can
approximately
tell
a
star's
temperature
so
using
that
information,
here's
a
video
that
I
made
a
few
years
ago
of
alberio
a
and
b
and
we're
actually
correcting
the
curve
for
our
camera.
So
that
is
the
planck
curve
for
alberio
b
notice.
It's
a
really
hot
star,
it's
13,
000
degrees,
kelvin.
So
most
of
the
heat
most
of
the
energy
is
in
the
blue.
B
End
of
the
spectrum,
the
hotter
end
of
the
spectrum
now
I'll
play
this
video
and
in
a
moment
you'll
see
that
I
now
I'm
sampling
the
other
star
notice
that
the
shape
of
that
curve
has
changed
completely.
This
alberio
a
it's
a
double,
but
it's
a
much
cooler
star.
It's
only
4
000
degrees,
kelvin,
so
more
of
its
energy
is
over
here
in
the
red.
So
by
studying
the
shape
the
general
spectral
energy
distribution,
we
can
also
learn
something
about
a
star's
temperature.
A
B
Oh
I'd
love
to
meet
all
of
you.
This
is
a
really.
This
is
a
club
that
has
a
wonderful
reputation
and
I'm
glad
I
had
a
chance
to
meet
all
of
you
virtually
or
at
least
meet
one
of
you
but
speak
to
you,
and
I
look
forward
to
the
opportunity
to
speak
again
and
again
when
things
open
up,
I'm
here
in
seattle,
I'd
love
to
grab
coffee
anybody
who
comes
through
town
thanks
again
and.