<p><strong>TLDR;</strong></p>
<p>Its a diagram showing all the physics and modeling choices that go into different models (the colored boxes in the middle) to compute an SED.</p>
<p><strong>Longer answer:</strong></p>
<p>First a SED is a <a href="https://en.wikipedia.org/wiki/Spectral_energy_distribution" rel="noreferrer">spectral energy distribution</a>, i.e how the amount of light varies as a function of wavelength. These kind of plots help understand to understand the underlying physics of an object.</p>
<p>This is affected by many things, firstly things that emit light (stars and AGN (Active galactic nuclei), and then by the things that get in the way of the light (gas and dust).</p>
<p>So to build a model of a SED first you need to know when stars form (star formation histories), what their masses are (initial mass functions), how many metals they have and whether that changes over time (metallicity). Then you need to know what those stars would look like (Stellar templates). Then you can sprinkle in some models of active galactic nucli (AGN templates).</p>
<p>Now we have the sources of light, we have to worry what dust is going to do the light (dust attenuation and dust emission), and throw in any other physics you missed (other and emission lines) before we see the final distribution.</p>
<p>But for each bit of physics there can be one or more choices to be made, some models will only cover some region of parameter space so they may need to be combined. For instance the initial mass function box has 4 sub-boxes with map to papers which describe well known initial mass functions. So you need to pick one. Other physics choices you may need to pick one or more sub-box depending on what physics you want to include.</p>
<p>So now we know the background physics of what we need, we need to combine the models into one overall model (the colored lines going to the colored boxes). So what this is showing is what physics is included in each model and in turns into a bit of a mess as each model can include multiple bits of physics (either physics is being combined or different pieces of physics are given as an option to use).</p>

CC BY-SA 4.0
2021-08-16T09:22:31.410Z
2021-08-16T11:06:45.197Z
2021-08-16T11:06:45.197Z
Rob
<h1>SED fitting</h1>
<p>SED fitting is the practice of inferring physical properties of a stellar population (a galaxy, a cluster...) from measures of the <a href="https://en.wikipedia.org/wiki/Spectral_energy_distribution" rel="noreferrer">Spectral Energy Distribution</a>.</p>
<p>The spectrum of a stellar population is extremely information rich. It can be used to infer age, redshift, metallicity, present and past star formation rate, total stellar, dust and gas mass, as well as the relative proportion of the different kind of stars.</p>
<p>In order to infer these parameters, one needs a software that is able, given the parameters, to generate (synthesize) a template spectrum. The template spectrum is then compared to the measured spectrum. The software is also able to search the parameters space in order to find the set of parameters that provide a spectrum that is the most similar to the measured one. Some softwares search for the parameters that minimize the <span class="math-container">$\chi^2$</span> of the data, others provide a full Bayesian analysis of the parameter space.</p>
<p>The center of the diagram contains the name of different popular SED fitting softwares. A longer and more comprehensive list can be found at <a href="http://www.sedfitting.org/Fitting.html" rel="noreferrer">http://www.sedfitting.org/Fitting.html</a>.</p>
<h1>How to synthesize a SED</h1>
<p>A synthetic SED must take into account many aspects that can influence the spectrum of a stellar population. Different studies give different prescriptions about the treatment of these phenomena. The outer ring of the picture presents some of the most popular prescriptions and link them with the SED fitters that use them. In this sense, the figure is a quick reference to see what each software is taking into account. One expert that works in the field will know at a glance the pros and cons of every prescription, and will be able to select the SED fitter according to their present needs.</p>
<h2>Stellar templates</h2>
<p>As a first approximation, the SED of a stellar population is the sum of the spectra of the single stars. It then goes without saying that a SED fitting software will need a stellar spectra library. Synthesizing the spectrum of a single star is a very complicated task. Authors of SED fitters don't usually roll their own stellar spectra generators, but use other public software. These codes provide a library of precomputed stellar spectra, for different ages and metallicity.</p>
<h2>Initial mass function</h2>
<p>Not all stars are created equal. When stars form, some are more massive and others are lighter. Different masses will lead to extremely different lives and spectra. When <span class="math-container">$100 M_\odot$</span> of gas convert into newborn stars, the SED fitter needs to decide how this mass is distributed among the stars. For example, we know that the majority of stars have <span class="math-container">$M \le 1M_\odot$</span> and very few stars have <span class="math-container">$M&gt;10M_\odot$</span>. The initial mass function (IMF) is the distribution of masses among a newborn stellar population.</p>
<p>In the figure there are some of the most popular IMFs, reported with the name of the first author of the paper that proposed them. They usually consist of power laws, or broken power laws.</p>
<h2>Star formation History</h2>
<p>Were all the stars born in a single burst, like in a globular cluster? Or did they form more slowly? In repeated bursts? Is the star formation still going on now? These questions are answered by the star formation history function, that gives the star formation rate (solar masses per year) as a function of time since the birth of the first stars until now. Young stars have a very different spectrum than old ones, therefore when generating a SED it is important to keep track of the different ages of the stars in the stellar population.</p>
<h2>Dust attenuation and emission</h2>
<p>The presence of dust can significantly alter the shape of a SED. Dust particles absorb visible and UV light, and emit the energy back in the infrared. Different models have been proposed to take care of the effect of dust on a SED.</p>
<h2>AGN templates</h2>
<p>If the galaxy contains an Active Galactic Nucleus, it is fundamental to include it in the synthetic SED. The flux of the AGN can single-handedly exceed the flux of the <em>whole galaxy</em>. Again, different AGN templates can be used.</p>
<h2>Metallicity</h2>
<p>The metallicity of a star greatly influences its spectrum. The metallicity of a star is usually taken to be equal to the metallicity of the gas from which the star formed. In the early universe the metallicity of the gas was low, but stars produce metals and release them to the interstellar medium, therefore the second generation of stars will tend to have a greater metallicity, and so on. A SED fitter may choose to ignore this fact, and keep the metallicity constant (for example if it is specialized on single burst populations), or may try to model the varying metallicity in a more complicated way.</p>
<h2>Emission Lines</h2>
<p>A SED fitter may choose to take into account a detailed treatment of emission lines from H2 regions, planetary nebulae, supernovae, interstellar, circumstellar, and intergalatic medium etc...</p>
<h2>Other</h2>
<p>Some SED fitters are extend their focus on some extreme part of the EM spectrum (most of them typically only treat IR-visible-UV) like radio or X-ray.</p>

CC BY-SA 4.0
2021-08-16T10:16:18.533Z
2021-08-16T11:14:51.840Z
2021-08-16T11:14:51.840Z
Prallax
<p>Twitter user BenneHolwerda (@BenneHolwerda) recently tweeted <a href="https://twitter.com/BenneHolwerda/status/1425120666777489408" rel="nofollow noreferrer">August 10 Astronomy Plot of the Week</a>:</p>
<blockquote>
<p>And I think <a href="https://twitter.com/SabineBellstedt" rel="nofollow noreferrer">@SabineBellstedt</a> and <a href="https://twitter.com/_jessthorne" rel="nofollow noreferrer">@_jessthorne</a> summary graph deserves a spot for sure.</p>
<blockquote>
<p>If you work on <a href="https://twitter.com/hashtag/SED?src=hashtag_click" rel="nofollow noreferrer">#SED</a> fitting you definitely must have this figure. Thanks to
<a href="https://twitter.com/_jessthorne" rel="nofollow noreferrer">@_jessthorne</a> who took the time to make it!. I've been writing a paper introduction and let me tell you it's extremely useful to develop comparisons between the different fitters</p>
</blockquote>
</blockquote>
<p><strong>Question:</strong> What does this tweeted Astronomy Plot of the Week mean?  What does it represent?</p>
<p>It seems that &quot;it's extremely useful to develop comparisons between the different fitters&quot; offers a clue, but I think only someone with substantial knowledge in stellar astrophysics can appreciate all that's going on here at first glance. I don't know where to even begin!</p>
<p><a href="https://i.sstatic.net/WaP8y.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/WaP8y.jpg" alt="enter image description here" /></a></p>
<p><a href="https://twitter.com/Jurgenvilla/status/1369239084204503041" rel="nofollow noreferrer">Source</a></p>

CC BY-SA 4.0
2021-08-16T01:05:48.070Z
How am I driving? [How to write and format tweet-based questions in Astronomy SE?](https://astronomy.meta.stackexchange.com/q/788/7982)
uhoh
<observational-astronomy><stellar-evolution><stellar-astrophysics><stellar-dynamics><modeling>
What does this tweeted Astronomy Plot of the Week mean? What does it represent?
uhoh
# What does this tweeted Astronomy Plot of the Week mean? What does it represent?

(Asked by: username_0 on 2021-08-16)

Twitter user BenneHolwerda (@BenneHolwerda) recently tweeted [August 10 Astronomy Plot of the Week](https://twitter.com/BenneHolwerda/status/1425120666777489408):

> And I think [@SabineBellstedt](https://twitter.com/SabineBellstedt) and [@\_jessthorne](https://twitter.com/_jessthorne) summary graph deserves a spot for sure.
>
> > If you work on [#SED](https://twitter.com/hashtag/SED?src=hashtag_click) fitting you definitely must have this figure. Thanks to
> > [@\_jessthorne](https://twitter.com/_jessthorne) who took the time to make it!. I've been writing a paper introduction and let me tell you it's extremely useful to develop comparisons between the different fitters

**Question:** What does this tweeted Astronomy Plot of the Week mean? What does it represent?

It seems that "it's extremely useful to develop comparisons between the different fitters" offers a clue, but I think only someone with substantial knowledge in stellar astrophysics can appreciate all that's going on here at first glance. I don't know where to even begin!

[![enter image description here](https://i.sstatic.net/WaP8y.jpg)](https://i.sstatic.net/WaP8y.jpg)

[Source](https://twitter.com/Jurgenvilla/status/1369239084204503041)

**Tags:** observational-astronomy, stellar-evolution, stellar-astrophysics, stellar-dynamics, modeling

> **Comments:**
> **username_0**: How am I driving? [How to write and format tweet-based questions in Astronomy SE?](https://astronomy.meta.stackexchange.com/q/788/7982)  

---

## 2 answers

### Answer by username_2 on 2021-08-16. Score: 6 | Accepted answer

# SED fitting

SED fitting is the practice of inferring physical properties of a stellar population (a galaxy, a cluster...) from measures of the [Spectral Energy Distribution](https://en.wikipedia.org/wiki/Spectral_energy_distribution).

The spectrum of a stellar population is extremely information rich. It can be used to infer age, redshift, metallicity, present and past star formation rate, total stellar, dust and gas mass, as well as the relative proportion of the different kind of stars.

In order to infer these parameters, one needs a software that is able, given the parameters, to generate (synthesize) a template spectrum. The template spectrum is then compared to the measured spectrum. The software is also able to search the parameters space in order to find the set of parameters that provide a spectrum that is the most similar to the measured one. Some softwares search for the parameters that minimize the $\chi^2$ of the data, others provide a full Bayesian analysis of the parameter space.

The center of the diagram contains the name of different popular SED fitting softwares. A longer and more comprehensive list can be found at <http://www.sedfitting.org/Fitting.html>.

# How to synthesize a SED

A synthetic SED must take into account many aspects that can influence the spectrum of a stellar population. Different studies give different prescriptions about the treatment of these phenomena. The outer ring of the picture presents some of the most popular prescriptions and link them with the SED fitters that use them. In this sense, the figure is a quick reference to see what each software is taking into account. One expert that works in the field will know at a glance the pros and cons of every prescription, and will be able to select the SED fitter according to their present needs.

## Stellar templates

As a first approximation, the SED of a stellar population is the sum of the spectra of the single stars. It then goes without saying that a SED fitting software will need a stellar spectra library. Synthesizing the spectrum of a single star is a very complicated task. Authors of SED fitters don't usually roll their own stellar spectra generators, but use other public software. These codes provide a library of precomputed stellar spectra, for different ages and metallicity.

## Initial mass function

Not all stars are created equal. When stars form, some are more massive and others are lighter. Different masses will lead to extremely different lives and spectra. When $100 M\_\odot$ of gas convert into newborn stars, the SED fitter needs to decide how this mass is distributed among the stars. For example, we know that the majority of stars have $M \le 1M\_\odot$ and very few stars have $M>10M\_\odot$. The initial mass function (IMF) is the distribution of masses among a newborn stellar population.

In the figure there are some of the most popular IMFs, reported with the name of the first author of the paper that proposed them. They usually consist of power laws, or broken power laws.

## Star formation History

Were all the stars born in a single burst, like in a globular cluster? Or did they form more slowly? In repeated bursts? Is the star formation still going on now? These questions are answered by the star formation history function, that gives the star formation rate (solar masses per year) as a function of time since the birth of the first stars until now. Young stars have a very different spectrum than old ones, therefore when generating a SED it is important to keep track of the different ages of the stars in the stellar population.

## Dust attenuation and emission

The presence of dust can significantly alter the shape of a SED. Dust particles absorb visible and UV light, and emit the energy back in the infrared. Different models have been proposed to take care of the effect of dust on a SED.

## AGN templates

If the galaxy contains an Active Galactic Nucleus, it is fundamental to include it in the synthetic SED. The flux of the AGN can single-handedly exceed the flux of the *whole galaxy*. Again, different AGN templates can be used.

## Metallicity

The metallicity of a star greatly influences its spectrum. The metallicity of a star is usually taken to be equal to the metallicity of the gas from which the star formed. In the early universe the metallicity of the gas was low, but stars produce metals and release them to the interstellar medium, therefore the second generation of stars will tend to have a greater metallicity, and so on. A SED fitter may choose to ignore this fact, and keep the metallicity constant (for example if it is specialized on single burst populations), or may try to model the varying metallicity in a more complicated way.

## Emission Lines

A SED fitter may choose to take into account a detailed treatment of emission lines from H2 regions, planetary nebulae, supernovae, interstellar, circumstellar, and intergalatic medium etc...

## Other

Some SED fitters are extend their focus on some extreme part of the EM spectrum (most of them typically only treat IR-visible-UV) like radio or X-ray.


---

### Answer by username_1 on 2021-08-16. Score: 12

**TLDR;**

Its a diagram showing all the physics and modeling choices that go into different models (the colored boxes in the middle) to compute an SED.

**Longer answer:**

First a SED is a [spectral energy distribution](https://en.wikipedia.org/wiki/Spectral_energy_distribution), i.e how the amount of light varies as a function of wavelength. These kind of plots help understand to understand the underlying physics of an object.

This is affected by many things, firstly things that emit light (stars and AGN (Active galactic nuclei), and then by the things that get in the way of the light (gas and dust).

So to build a model of a SED first you need to know when stars form (star formation histories), what their masses are (initial mass functions), how many metals they have and whether that changes over time (metallicity). Then you need to know what those stars would look like (Stellar templates). Then you can sprinkle in some models of active galactic nucli (AGN templates).

Now we have the sources of light, we have to worry what dust is going to do the light (dust attenuation and dust emission), and throw in any other physics you missed (other and emission lines) before we see the final distribution.

But for each bit of physics there can be one or more choices to be made, some models will only cover some region of parameter space so they may need to be combined. For instance the initial mass function box has 4 sub-boxes with map to papers which describe well known initial mass functions. So you need to pick one. Other physics choices you may need to pick one or more sub-box depending on what physics you want to include.

So now we know the background physics of what we need, we need to combine the models into one overall model (the colored lines going to the colored boxes). So what this is showing is what physics is included in each model and in turns into a bit of a mess as each model can include multiple bits of physics (either physics is being combined or different pieces of physics are given as an option to use).


---

