Evolution stellar populations in galaxies
is one of the key ingredients of our
understanding of galaxy evolution in
general.
If we look at colors of galaxies nearby we
can immediately see that there is a
bimodel distribution.
There is a fairly narrow red, peak, which
is due to the elliptical galaxies and
bulges.
And there is a fairly broad blue
distribution, that corresponds to the
discs of spirals.
In more modern renderings, you can plot
colors as a function of intrinsic
luminosity.
And you still see those same two blobs.
But they're a little tilted.
In the case of elliptical galaxies that
ridge line.
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The more luminous the.
The ellipticals retain more of their,
chemical evolution products.
Their more metal rich metals absorb more
like in the ultraviolet galaxy look
redder.
So this is largely mass metallicity
sequence.
For spirals there isn't a very simple
relation like that.
Their colors are combination of mixture of
stellar ages.
Star formation rates as well as extinction
by dust.
So we can produce predicted theoretical
spectra of evolving galaxies in the
following fashion.
We have to make an assumption of what the
star formation history is.
This is a purely pre-parametering the
model, but we can make reasonable guesses.
We need to know what is the initial mass
function, the distribution of stars by
mass when they're formed, because stars of
different masses can be involved in very
different[UNKNOWN].
Then for each stellar mass and, and, and
age we need a spectrum.
So we need libraries of stellar spectra
that can be associated with all components
of the stellar population at any given
age.
This is actually not an easy thing to do,
because we can observe a lot near us.
But for example, we have no spectra of
very metal poor very massive stars,
because those have burnt out long time
ago.
And, again from theory, tested by
observations of star clusters and so on,
we need stellar population evolution
tracks.
How does distribution of stars and color
magnitudes space the HR Diagram changes
the function of time for a given amount
of.
Chemical enrichment and so on.
You take a quantity of gas and turn it all
into stars instantaneously.
A delta function star formation rate
distributed according to your initial mass
function.
And then follow it's evolution in time.
This is what's known as a simple stellar
population.
There is no such thing in reality,
although globular clusters come close.
And then it can represent net total star
formation history of a galaxy is a
collection of these, and follow the map.
One popular way of expressing star
formation histories is a exponentially
declining rate.
Which is probalby not a bad overall
assumption Average or many galaxies.
In this case, for early type galaxies
there is a lot of star formation early on.
The exponential very steep.
For this galaxy very shallow.
For irregular galaxies may be essentially
flat or even rising.
Stellar evolution is one of the best
understood Segments of astrophysics.
We really do know how stars work and
evolve.
And that's been confirmed again and again
through many decades of observations.
There are certainly details that still
need to be ironed out.
But at the level that we care about here,
we really do understand that.
An important thing to remember is that
more massive stars They are much faster,
they are more luminous, they are also
hotter, so they are[UNKNOWN] more
important but not for long.
Thus, spectrum of an evolving galaxy will
change more rapidly in the blue parts of
the spectrum, thanks to the short life
times of these massive stars.
And will be changing relatively slowly in
the red parts of the spectrum where the
most of the light may be coming from well
of all slowly evolving population of red
giants.
There are many stellar populations indices
methods out there.
And they sometimes disagree on some
details.
But by and large the agreement's pretty
good.
One popular set is called Giselle.
Which is a library of The galaxy evolution
spectra by[UNKNOWN] and[UNKNOWN].
We know how stars evolve.
We even have spectra of lots of different
kinds of stars.
And we have some idea of the initial mass
function.
At least we measure it locally in the
milky way.
And then we have to make assumptions what
it's saying in all galaxies at all times.
We can test some of those assumptions.
But then we have to assume star formation
rate which again is a completely free
parameter in this exercise.
This is what stellar evolution tracks look
like.
They're computed from stellar evolution
models.
And a star evolves it moves in the color
magnitude space.
How and where depends very much or almost
entirely on its mass with minor dependence
on its metallicity.
So we get these stellar evolutionary
tracks from theory, our understanding of
stellar structure and evolution it's
pretty solid.
Then, we need to have their spectra.
And for kinds of stars that we can observe
near us, that's an easy thing to acquire.
For kinds of stars that are no longer with
us, say, very young, metal poor, very high
mass stars.
This will require some theoretical
modeling, and stripulation.
We make an assumption about initial mass
function, and again we understand that in
the local Milky Way condition, but it
would be very different in the early
universe where, say, stars were made out
of, Of hydrogen and helium, and hardly
anything else.
In fact, we believe that was the case,
that the initial mass function of
primordial stars was very different.
And then again, we have to assume star
formation history.
In reality, we assume some types of star
formation histories.
Compute the consequences, compared it to
iterations and iterate until we have a
model that seems to fit observations and
that's telling us what the likely star
formation history of these galaxies was.
So stars evolve, the blue ones keep
disappearing faster.
Galaxies will be changing their colors and
here in color, color space you can follow
the, theoretical behavior of evolving
stellar populations.
You can also see where the galaxies are,
and indeed they form something of a.
Sequence that corresponds to the younger,
hotter stars on late Hubble types, older,
redder stars for the early Hubble types.
Here is a comparison of predictions of
three different types of stellar
population and synthesis models by
different groups.
And it shows predicted colors and mass to
light ratios for model galaxies.
By and large they agree very well.
The minor disagreements usually are very
young ages and there is some debate
actually what is the correct thing to
assume but.
Qualitatively at least, we understand very
well how things are working.
And so this is what evolving spectra of
stellar populations look like.
This is for a simple stellar population.
Remember this is a scoop of stars made all
at once, and let go.
Note, these are logarithmic plots of log
flux versus log wavelength.
So.
They really hide the strong contrast.
And if you stare at curves which are
labeled by their age, those near the top
tends to be youngest because younger stars
are more luminous.
You find out that in the ultraviolet, blue
part of the spectrum, the flux will
plummet very quickly.
Whereas it would be changing in the red
part of the spectrum, but much slower
which is exactly what we expect.
Here is a comparison of predicted model
spectral of different ages assuming
different libraries of stellar population
evolution tracs and spectra.
And again you see that.
Different models seem to be in an
excellent mutual agreement.
Which is giving us some confidence that we
actually do understand how this works.
Another kind of models that they are now
more popular are so called,
semi-analytical, or hybrid models, where
one can use telepopulation synthesis
models.
Associate them with galaxies that they're
being assembled through hierarchical
structure formation.
Either from a numerical simulation, or
from some statistical description thereof.
And make predictions of how will they ch,
colors change and so on.
There are unfortunately way too many two
level parameters in these models.
And so they have some modest success, but
they illustrate of all different things
that have to be taken into account, and a
lot of assumptions that have to be made.
Next time we will turn to the actual
observations of galaxy evolution.