<p>So GN z-11 is the latest &quot;furthest away&quot; galaxy. It has a claimed redshift measurement of <span class="math-container">$z=11.1$</span>, meaning that we are seeing the light it emitted about 400 Myr after the big bang (dependent on an assumed set of cosmological parameters).</p>
<p>To get the redshift measurement, the discoverers used grism (relatively low resolution) spectroscopy in the near infrared. What they were looking for is the rest-frame<a href="https://en.wikipedia.org/wiki/Lyman-break_galaxy" rel="nofollow noreferrer">Lyman continuum break</a> and resonant absorption/scattering of UV rest-frame photons, which would be redshifted into this wavelength range.</p>
<p>The Lyman continuum break is caused by the absorption of nearly all ultraviolet photons with wavelengths smaller than 92 nm.
These high energy photons are capable of photoionising the neutral hydrogen present in and around the galaxy and in the intergalactic medium at a range of lower redshifts. At wavelengths between this and the Lyman alpha line at 121 nm, the flux is still heavily suppressed by resonant scattering by clouds of neutral hydrogen along the line of site to the galaxy, when their redshift means the UV photon has a wavelength of 121 nm in their rest frame.</p>
<p>This neutral hydrogen is present in abundance at redshifts greater than 6, as it had not yet been <em>re-ionised</em> by quasars and starlight. The consequence is that almost no light is expected to reach us from rest-frame wavelengths shortwards of 121 nm, but a galaxy's light <em>can</em> reach us from rest-frame wavelengths that are longer than this. When one <em>observes</em> the spectrum, we see flux at long wavelengths which suddenly cuts off at shorter wavelengths. The wavelength of the break is <span class="math-container">$\lambda = 121 \times (1+z)$</span> nm, where <span class="math-container">$z$</span> is the redshift.</p>
<p>It is this Lyman (alpha) continuum break that has been identified at an observed wavelength of 1470 nm. This leads to the redshift estimate of <span class="math-container">$z= (1470/121)-1 = 11.1$</span>.</p>
<p>The details are presented in <a href="http://arxiv.org/abs/1603.00461" rel="nofollow noreferrer">Oesch et al. (2016)</a>. The break is the only thing visible in the spectrum. The authors are confident that this is what it is because their previous broadband photometry had given them an estimated redshift of <span class="math-container">$&gt;10$</span> (which is why they observed this candidate in the first place).</p>

CC BY-SA 4.0
2022-08-08T14:18:29.003Z
You know this, of course, but have perhaps accidentally mixed up LyC and Lyα: Lyman α photons do not _photoionize_ HI, but are _scattered_ out of the line of sight. Observationally though, the effect is the same: a break.
pela
CC BY-SA 4.0
2022-08-08T15:00:59.750Z
@pela, yes, sloppy. Hopefully corrected.
ProfRob
CC BY-SA 4.0
2016-03-06T23:06:32.257Z
2022-08-08T15:00:43.897Z
2022-08-08T15:00:43.897Z
ProfRob
<p>The news media recently reported that galaxy GN-z11, formed just 400 million years after the big bang, is much further away than originally thought at perhaps 13.2 billion light years.  They say, </p>

<blockquote>
  <p>The key to the discovery was precisely measuring the shift of the
  galaxy's light into longer, redder wavelengths, which correspond to
  how far the photons had traveled before reaching Hubble's eye.
  (Reuters).</p>
</blockquote>

<p>So, suppose I'm standing next to, but safely away from, some train tracks.  As the train approaches, sounding its whistle constantly, the pitch will appear to increase until it reaches me, upon which I will briefly hear the whistle's 'rest pitch' (the pitch of the whistle as if I were aboard the train), then it would decrease as the train moves away.  Thus, the lower the pitch, the further away the train is.  I hope that's right.  So, if we know the rest frequency of galaxy GN-z11, its measured frequency indicates how far away it is from earth. Trouble is, how do we know what the rest frequency of light coming from this distant galaxy is?   </p>

CC BY-SA 3.0
2016-03-06T17:09:51.367Z
This might help explain it to you (http://astro.wku.edu/astr106/Hubble_intro.html), but basically they can measure rest wavelengths in a lab because they are looking for particular emission or absorption lines in elements such as Hydrogen. These are fundamental properties of all elements, no matter where they are in the universe, so by pinpointing them on the spectrum, they can calculate by how much they are red-shifted.
Dean
CC BY-SA 3.0
2016-03-06T19:16:42.297Z
Thank you so much for the reference Dean.  I appreciate it!
Michael Lee
<galaxy><distances><doppler-effect>
How do we know galaxy GN-z11 is as far away as it is?
Michael Lee
# How do we know galaxy GN-z11 is as far away as it is?

(Asked by: username_0 on 2016-03-06)

The news media recently reported that galaxy GN-z11, formed just 400 million years after the big bang, is much further away than originally thought at perhaps 13.2 billion light years. They say,

> The key to the discovery was precisely measuring the shift of the
> galaxy's light into longer, redder wavelengths, which correspond to
> how far the photons had traveled before reaching Hubble's eye.
> (Reuters).

So, suppose I'm standing next to, but safely away from, some train tracks. As the train approaches, sounding its whistle constantly, the pitch will appear to increase until it reaches me, upon which I will briefly hear the whistle's 'rest pitch' (the pitch of the whistle as if I were aboard the train), then it would decrease as the train moves away. Thus, the lower the pitch, the further away the train is. I hope that's right. So, if we know the rest frequency of galaxy GN-z11, its measured frequency indicates how far away it is from earth. Trouble is, how do we know what the rest frequency of light coming from this distant galaxy is?

**Tags:** galaxy, distances, doppler-effect
> **Comments:**
> **username_1**: This might help explain it to you (http://astro.wku.edu/astr106/Hubble_intro.html), but basically they can measure rest wavelengths in a lab because they are looking for particular emission or absorption lines in elements such as Hydrogen. These are fundamental properties of all elements, no matter where they are in the universe, so by pinpointing them on the spectrum, they can calculate by how much they are red-shifted.  
> **username_0**: Thank you so much for the reference Dean.  I appreciate it!  

---

## 1 answers

### Answer by username_2 on 2016-03-06. Score: 8 | Accepted answer

So GN z-11 is the latest "furthest away" galaxy. It has a claimed redshift measurement of $z=11.1$, meaning that we are seeing the light it emitted about 400 Myr after the big bang (dependent on an assumed set of cosmological parameters).

To get the redshift measurement, the discoverers used grism (relatively low resolution) spectroscopy in the near infrared. What they were looking for is the rest-frame[Lyman continuum break](https://en.wikipedia.org/wiki/Lyman-break_galaxy) and resonant absorption/scattering of UV rest-frame photons, which would be redshifted into this wavelength range.

The Lyman continuum break is caused by the absorption of nearly all ultraviolet photons with wavelengths smaller than 92 nm.
These high energy photons are capable of photoionising the neutral hydrogen present in and around the galaxy and in the intergalactic medium at a range of lower redshifts. At wavelengths between this and the Lyman alpha line at 121 nm, the flux is still heavily suppressed by resonant scattering by clouds of neutral hydrogen along the line of site to the galaxy, when their redshift means the UV photon has a wavelength of 121 nm in their rest frame.

This neutral hydrogen is present in abundance at redshifts greater than 6, as it had not yet been *re-ionised* by quasars and starlight. The consequence is that almost no light is expected to reach us from rest-frame wavelengths shortwards of 121 nm, but a galaxy's light *can* reach us from rest-frame wavelengths that are longer than this. When one *observes* the spectrum, we see flux at long wavelengths which suddenly cuts off at shorter wavelengths. The wavelength of the break is $\lambda = 121 \times (1+z)$ nm, where $z$ is the redshift.

It is this Lyman (alpha) continuum break that has been identified at an observed wavelength of 1470 nm. This leads to the redshift estimate of $z= (1470/121)-1 = 11.1$.

The details are presented in [Oesch et al. (2016)](http://arxiv.org/abs/1603.00461). The break is the only thing visible in the spectrum. The authors are confident that this is what it is because their previous broadband photometry had given them an estimated redshift of $>10$ (which is why they observed this candidate in the first place).

> **Comments:**
> **username_3**: You know this, of course, but have perhaps accidentally mixed up LyC and Lyα: Lyman α photons do not _photoionize_ HI, but are _scattered_ out of the line of sight. Observationally though, the effect is the same: a break.  
> **username_2**: @pela, yes, sloppy. Hopefully corrected.  

---

