<p>This is a term known at the limiting magnitude. This term refers simply to the faintest apparent magnitude your instrument can detect. Wikipedia has an article describing <a href="https://en.wikipedia.org/wiki/Limiting_magnitude" rel="nofollow">limiting magnitude</a>.  I pulled the info from there.</p>

<p>The wiki article begins off explaining the basic way of finding limiting magnitude. </p>

<p>$$5 \cdot \log_{10}\left(\frac{D_1}{D_0}\right) $$</p>

<p>Now, if we simply plug in some values, 254 mm telescope and assuming the eye is 6 mm, we get an answer of 8.13.  This can be rounded to nearest base and we can say that it increases the magnitude by 8.  </p>

<p>The article goes into more description about the contrast of the given medium. With Earth, we have the atmosphere, lights, and pollution to worry about. The more you are able to reduce these effects, the better. That's why for telescopes at observatories, we place them in high places, usually away from populated areas to help reduce these worrisome effects. This helps increase the contrast between the object you are looking at and its medium (in astronomy the night sky).</p>

<p>In the article it explains this with the formula below:</p>

<p>$$m \cdot v = m_{nakedeye} - 2 + 2.5 \cdot \log_{10}(D \cdot P \cdot t)$$</p>

<ul>
<li>$D$ = objective or main mirror diameter in mm</li>
<li>$P$ = power or magnification</li>
<li>$t$ = transmission factor, usually 0.85–0.9</li>
</ul>

<p>Simply putting in our values from above and estimating a 10" telescope has a 250x magnification with a transmission factor of 0.85, we get how the wiki article states that the answer of a 10" telescope easily getting a magnitude 15 is possible.</p>

<p>Now for observational laboratories and something like the Hubble telescope, they use additional factors, including image processing mechanisms that help reduce noise in the image and integration time of the object you are viewing.  This means using a sensor that can capture the image at low light levels AND while it moves.</p>

<p>If you really want to know more, <a href="http://www.stsci.edu/hst/acs/documents/handbooks/cycle19/c01_intro.html" rel="nofollow">go here</a>. This link actually explains in very technical detail the technology behind the imaging discovery efficiency.  Basically, it helps boost the limiting magnitude to detect extremely faint objects.</p>

CC BY-SA 3.0
2016-08-24T05:29:47.820Z
There doesn't seem to be a citation for the " $log_{10} (D \ P \ t)$" equation in that Wikipedia article - is there an alternate source for this equation? The linear dependence of the argument on magnification needs some better explanation - why not quadratic to reflect intensity/solid angle, and to what limit (it can't go on for arbitrarily large magnification, considering effects of atmospheric seeing and diffraction will make the unresolved star-blob" grow  and dim with increasing magnification). Is this equation actually explained somewhere deep inside the HST proposal link? Where?
uhoh
CC BY-SA 3.0
2016-08-24T13:27:06.463Z
Skyglow and light pollution fit in there somehow too for earth-based telescopes. Zodiacal light causes trouble for even space-based scopes.
Wayfaring Stranger
CC BY-SA 3.0
2016-08-24T15:30:34.147Z
http://articles.adsabs.harvard.edu//full/1990PASP..102..212S/0000212.000.html

I'd like to submit this here. It's an old study that sort of explains limiting magnitude found in the journal, Astronomical Society of the Pacific. And a follow up:

http://web.telia.com/~u41105032/visual/Schaefer.htm

It's not a direct reference, but for further reading seems to be informative.
El Bromista
CC BY-SA 3.0
2016-08-23T16:11:07.263Z
2016-08-23T19:21:12.403Z
2016-08-23T19:21:12.403Z
El Bromista
<p><a href="http://hubblesite.org/hubble_discoveries/10th/vault/allabout.shtml" rel="nofollow">This</a> website claims:</p>

<blockquote>
  <p>The space telescope can detect objects as faint as 31st magnitude...</p>
</blockquote>

<p>It's referring to Hubble, but does not cite any source or math. How do you calculate the faintest (apparent) magnitude that a space telescope can detect?</p>

<telescope><light><optics>
What is the faintest magnitude a telescope can see?
DrZ214
# What is the faintest magnitude a telescope can see?

(Asked by: username_0 on 2016-08-23)

[This](http://hubblesite.org/hubble_discoveries/10th/vault/allabout.shtml) website claims:

> The space telescope can detect objects as faint as 31st magnitude...

It's referring to Hubble, but does not cite any source or math. How do you calculate the faintest (apparent) magnitude that a space telescope can detect?

**Tags:** telescope, light, optics

---

## 1 answers

### Answer by username_1 on 2016-08-23. Score: 6

This is a term known at the limiting magnitude. This term refers simply to the faintest apparent magnitude your instrument can detect. Wikipedia has an article describing [limiting magnitude](https://en.wikipedia.org/wiki/Limiting_magnitude). I pulled the info from there.

The wiki article begins off explaining the basic way of finding limiting magnitude.

$$5 \cdot \log\_{10}\left(\frac{D\_1}{D\_0}\right) $$

Now, if we simply plug in some values, 254 mm telescope and assuming the eye is 6 mm, we get an answer of 8.13. This can be rounded to nearest base and we can say that it increases the magnitude by 8.

The article goes into more description about the contrast of the given medium. With Earth, we have the atmosphere, lights, and pollution to worry about. The more you are able to reduce these effects, the better. That's why for telescopes at observatories, we place them in high places, usually away from populated areas to help reduce these worrisome effects. This helps increase the contrast between the object you are looking at and its medium (in astronomy the night sky).

In the article it explains this with the formula below:

$$m \cdot v = m\_{nakedeye} - 2 + 2.5 \cdot \log\_{10}(D \cdot P \cdot t)$$

* $D$ = objective or main mirror diameter in mm
* $P$ = power or magnification
* $t$ = transmission factor, usually 0.85–0.9

Simply putting in our values from above and estimating a 10" telescope has a 250x magnification with a transmission factor of 0.85, we get how the wiki article states that the answer of a 10" telescope easily getting a magnitude 15 is possible.

Now for observational laboratories and something like the Hubble telescope, they use additional factors, including image processing mechanisms that help reduce noise in the image and integration time of the object you are viewing. This means using a sensor that can capture the image at low light levels AND while it moves.

If you really want to know more, [go here](http://www.stsci.edu/hst/acs/documents/handbooks/cycle19/c01_intro.html). This link actually explains in very technical detail the technology behind the imaging discovery efficiency. Basically, it helps boost the limiting magnitude to detect extremely faint objects.

> **Comments:**
> **username_2**: There doesn't seem to be a citation for the " $log_{10} (D \ P \ t)$" equation in that Wikipedia article - is there an alternate source for this equation? The linear dependence of the argument on magnification needs some better explanation - why not quadratic to reflect intensity/solid angle, and to what limit (it can't go on for arbitrarily large magnification, considering effects of atmospheric seeing and diffraction will make the unresolved star-blob" grow  and dim with increasing magnification). Is this equation actually explained somewhere deep inside the HST proposal link? Where?  
> **username_3**: Skyglow and light pollution fit in there somehow too for earth-based telescopes. Zodiacal light causes trouble for even space-based scopes.  
> **username_1**: http://articles.adsabs.harvard.edu//full/1990PASP..102..212S/0000212.000.html  I'd like to submit this here. It's an old study that sort of explains limiting magnitude found in the journal, Astronomical Society of the Pacific. And a follow up:  http://web.telia.com/~u41105032/visual/Schaefer.htm  It's not a direct reference, but for further reading seems to be informative.  

---

