<p>You're confusing error and uncertainty.</p>

<p>In school labs or other situations where the true value of a quantity is known, the difference between a measured value and that true value is sometimes referred to as the "error" in the measurement. A lower error is taken as an indication that the results are successful. </p>

<p>When making observations, the true value of a quantity is seldom known. Indeed, that's usually the purpose of making observations: not as a pedagogical tool but as a way to determine something about the world. In this case, we're concerned with the <em>uncertainty</em> in the measurement - that is, essentially how confident we are in the value we determine. More quantitatively, we might give something like a <span class="math-container">$3\sigma$</span> uncertainty that explains how likely it is that the true value falls within 3 standard deviations of the measurement. That's a way of showing how robust the results are.</p>

<p>It's also helpful for comparing sets of measurements - if one group says that (and I'm making up numbers here) that their measurements have determined the Hubble constant to be <span class="math-container">$H_0=67.0\pm1.2\text{ km}\text{ s}^{-1}\text{ Mpc}^{-1}$</span> and another group says that <em>their</em> methods have found it to instead be <span class="math-container">$H_0=74.00\pm0.75\text{ km}\text{ s}^{-1}\text{ Mpc}^{-1}$</span>, then we can see from the uncertainties that the two results are in fairly strong tension with one another.</p>

<p>If you're determining something like redshift, you presumably have some raw data measuring other quantities. Perhaps you've identified H<span class="math-container">$\alpha$</span> emission from a source and found it to be at <span class="math-container">$\lambda=8540\pm30$</span> angstroms, while the rest wavelength is <span class="math-container">$\lambda_0=6562.8$</span> angstroms. Then you can use standard <a href="https://en.wikipedia.org/wiki/Propagation_of_uncertainty" rel="nofollow noreferrer">uncertainty propagation methods</a> to determine the uncertainty in the redshift of the source. In this case, the redshift is
<span class="math-container">$$z=\frac{\lambda}{\lambda_0}-1$$</span>
The uncertainty in <span class="math-container">$z$</span> is then
<span class="math-container">$$\sigma_z=\sqrt{\left(\frac{\partial z}{\partial\lambda}\right)^2\sigma_{\lambda}^2+\left(\frac{\partial z}{\partial\lambda_0}\right)^2\sigma_{\lambda_0}^2}$$</span>
where I've included <span class="math-container">$\sigma_{\lambda_0}$</span>, though realistically it should be much smaller than <span class="math-container">$\sigma_{\lambda}$</span>. Keep in mind also that <span class="math-container">$\sigma_{\lambda}$</span> has itself presumably been determined through error propagation from the raw data collected.</p>

<p>(Side note: As pela pointed out, this assumes that the redshift is entirely due to the motion of the object you're looking at, and that's not always the case. I originally picked Lyman <span class="math-container">$\alpha$</span> has my line, which turns out to not be particularly useful. Additionally, the toy redshift ended up being quite low and therefore even more sensitive to other not-recessional contributions, like stellar winds. H<span class="math-container">$\alpha$</span> is, I think, a better example, especially with this higher redshift.)</p>

CC BY-SA 4.0
2020-04-23T10:42:35.727Z
+1, but small note: If possible, avoid using Lyman α to get the redshift, as it will usually be offset from the systemic, and asymmetric so not easily fitted with a Gaussian. Note also that emission lines and absorption line may not necessarily probe the same physics. For instance, O III emission will usually probe the star-forming regions (~systemic), whereas Mg II absorption may probe outflowing winds and hence be blueshifted from the systemic.
pela
CC BY-SA 4.0
2020-04-23T13:37:27.953Z
@pela Thanks, I didn't know about those issues with Lyman $\alpha$. I've changed it to the Balmer series and made a note on systemic/non-systemic contributions.
HDE 226868
CC BY-SA 4.0
2020-04-23T14:02:51.480Z
It's not at all uncommon to use Lyα, especially at high redshift, because it's often the only line visible, but complex radiative transfer effect tends to shift the line somewhat, usually redward, because of outflows (as opposed to absorption lines in such winds, which are shifted blueward). The shift is small, but you're not going to have 4-digit precision in z with Lyα, so Hα is a safer choice :)
pela
CC BY-SA 4.0
2020-04-22T16:15:48.450Z
2020-04-23T13:36:40.593Z
2020-04-23T13:36:40.593Z
HDE 226868
<p>I am struggling to calculate the redshift error of a galaxy. I was able to determine the redshifts of the absorption and emission lines from the galaxy's spectrum and then took the average of the redshift of the lines to determine the (overall) redshift of the galaxy. I know "error" is associated with the true and measured values but I don't know the true value of the redshift of the galaxy. Is there an explicit formula or something that I can use to calculate the redshift error of the galaxy without reference to the true redshift of the galaxy? All I know are the emitted and observed wavelengths of the emission and absorption lines of the galaxy spectrum.</p>

CC BY-SA 4.0
2020-04-22T15:22:54.743Z
But the errors in your measurements don't depend on the true value. I'm not sure this is an astronomy question so much as a misconception about measurement uncertainties.
ProfRob
CC BY-SA 4.0
2020-04-22T15:39:17.303Z
From my understanding, measurement error is the amount of inaccuracy so it is associated with the true and measured values.
RUNN
CC BY-SA 4.0
2020-04-22T15:46:17.543Z
Well no, it isn't. The error here refers to your measurement precision. That is what an "error bar" is.
ProfRob
CC BY-SA 4.0
2020-04-22T15:55:14.010Z
Oh, thanks for your help.
RUNN
<galaxy><distances><redshift>
How do we determine a redshift error?
RUNN
# How do we determine a redshift error?

(Asked by: username_0 on 2020-04-22)

I am struggling to calculate the redshift error of a galaxy. I was able to determine the redshifts of the absorption and emission lines from the galaxy's spectrum and then took the average of the redshift of the lines to determine the (overall) redshift of the galaxy. I know "error" is associated with the true and measured values but I don't know the true value of the redshift of the galaxy. Is there an explicit formula or something that I can use to calculate the redshift error of the galaxy without reference to the true redshift of the galaxy? All I know are the emitted and observed wavelengths of the emission and absorption lines of the galaxy spectrum.

**Tags:** galaxy, distances, redshift
> **Comments:**
> **username_1**: But the errors in your measurements don't depend on the true value. I'm not sure this is an astronomy question so much as a misconception about measurement uncertainties.  
> **username_0**: From my understanding, measurement error is the amount of inaccuracy so it is associated with the true and measured values.  
> **username_1**: Well no, it isn't. The error here refers to your measurement precision. That is what an "error bar" is.  
> **username_0**: Oh, thanks for your help.  

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## 1 answers

### Answer by username_2 on 2020-04-22. Score: 3 | Accepted answer

You're confusing error and uncertainty.

In school labs or other situations where the true value of a quantity is known, the difference between a measured value and that true value is sometimes referred to as the "error" in the measurement. A lower error is taken as an indication that the results are successful.

When making observations, the true value of a quantity is seldom known. Indeed, that's usually the purpose of making observations: not as a pedagogical tool but as a way to determine something about the world. In this case, we're concerned with the *uncertainty* in the measurement - that is, essentially how confident we are in the value we determine. More quantitatively, we might give something like a $3\sigma$ uncertainty that explains how likely it is that the true value falls within 3 standard deviations of the measurement. That's a way of showing how robust the results are.

It's also helpful for comparing sets of measurements - if one group says that (and I'm making up numbers here) that their measurements have determined the Hubble constant to be $H\_0=67.0\pm1.2\text{ km}\text{ s}^{-1}\text{ Mpc}^{-1}$ and another group says that *their* methods have found it to instead be $H\_0=74.00\pm0.75\text{ km}\text{ s}^{-1}\text{ Mpc}^{-1}$, then we can see from the uncertainties that the two results are in fairly strong tension with one another.

If you're determining something like redshift, you presumably have some raw data measuring other quantities. Perhaps you've identified H$\alpha$ emission from a source and found it to be at $\lambda=8540\pm30$ angstroms, while the rest wavelength is $\lambda\_0=6562.8$ angstroms. Then you can use standard [uncertainty propagation methods](https://en.wikipedia.org/wiki/Propagation_of_uncertainty) to determine the uncertainty in the redshift of the source. In this case, the redshift is
$$z=\frac{\lambda}{\lambda\_0}-1$$
The uncertainty in $z$ is then
$$\sigma\_z=\sqrt{\left(\frac{\partial z}{\partial\lambda}\right)^2\sigma\_{\lambda}^2+\left(\frac{\partial z}{\partial\lambda\_0}\right)^2\sigma\_{\lambda\_0}^2}$$
where I've included $\sigma\_{\lambda\_0}$, though realistically it should be much smaller than $\sigma\_{\lambda}$. Keep in mind also that $\sigma\_{\lambda}$ has itself presumably been determined through error propagation from the raw data collected.

(Side note: As pela pointed out, this assumes that the redshift is entirely due to the motion of the object you're looking at, and that's not always the case. I originally picked Lyman $\alpha$ has my line, which turns out to not be particularly useful. Additionally, the toy redshift ended up being quite low and therefore even more sensitive to other not-recessional contributions, like stellar winds. H$\alpha$ is, I think, a better example, especially with this higher redshift.)

> **Comments:**
> **username_3**: +1, but small note: If possible, avoid using Lyman α to get the redshift, as it will usually be offset from the systemic, and asymmetric so not easily fitted with a Gaussian. Note also that emission lines and absorption line may not necessarily probe the same physics. For instance, O III emission will usually probe the star-forming regions (~systemic), whereas Mg II absorption may probe outflowing winds and hence be blueshifted from the systemic.  
> **username_2**: @pela Thanks, I didn't know about those issues with Lyman $\alpha$. I've changed it to the Balmer series and made a note on systemic/non-systemic contributions.  
> **username_3**: It's not at all uncommon to use Lyα, especially at high redshift, because it's often the only line visible, but complex radiative transfer effect tends to shift the line somewhat, usually redward, because of outflows (as opposed to absorption lines in such winds, which are shifted blueward). The shift is small, but you're not going to have 4-digit precision in z with Lyα, so Hα is a safer choice :)  

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