Will we start seeing galaxies disappear due to Universe expansion? Does the fact that universe is currently expanding at an accelerating rate means that far far away objects (FAO) might start disappearing with time, set aside the "red shift"? 

I'm saying this because from what I understand until now:


we receive photons from FAO that were emitted long long ago
now due to space expansion, some of those objects are now moving away at speed greater than the speed of light, but at the time the photons we receive today were emitted, these FAO where not moving away faster than light


So there must be a point in time at which these far away objects disappear from view. How is this concept called?, or is it only a mistake I'm doing in my thinking? 

Here's a simple drawing to illustrate:


at t=-11 billion years(By), photons are emitted in a slow expanding universe, and today we can view the object as it was
at t=-2 By, the object moves faster than speed of light, so photon emitted at that time will never reach us, even if we wait the 9 by + "expansion correction" needed...




I couldn't be convinced by the answer I found here, saying nothing disappears out of horizon. I don't see how it complies with that answer were event horizon approaches us.
It is a common misconception that galaxies receding faster than light cannot be observed. There are two versions of this misconception:

Galaxies that are now receding faster than light cannot be seen.
If we observe a galaxy today, it may recede faster than light now, but when it emitted the light we see now, it did not.

Both are incorrect.
Intuitive explanation
This is most easily seen in a spacetime diagram. But before showing that, a somewhat intuitive way of understanding this apparent paradox is to consider the journey of the photon from the reference frame of the emitting galaxy: In this frame, the photon leaves the emitter with a velocity $v=c$ (as it should), but since its velocity is always $v$ locally, then in the frame of the emitter, its velocity increases without bounds. This is not a proof, but may help to show that &quot;light may travel faster the the speed of light&quot;.
Spacetime diagram
Now to the spacetime diagram. My favorite version is from the classic paper by Davis &amp; Lineweaver (2004), but I actually like better this version from Pulsar's excellent (!) post:

Real example of a galaxy that has always been, and always will be, receding with superluminal velocity
Such a diagram shows age (or, equivalently, size) of the Universe, as a function of the corresponding comoving distance$^1$ of events. A lot of things are going on in this diagram, and I'll refer to Pulsar's answer for an interesting discussion of all this. For our purposes, consider the only thing the I have added to the figure: the world line — i.e. the &quot;path&quot; taken through spacetime of some object — of the galaxy GN-z11, seen as a vertical dashed line at a comoving distance $d_C \simeq 32.2\,\mathrm{Gly}$. It is vertical, because it doesn't move in comoving coordinates. We observe it at a redshift of $z=11.09$, which means that the light we see (moving at 45º toward our worldline which is at $d_C=0$) was emitted when the Universe was roughly 400 Myr old. At that time, GN-z11 was receding at a velocity $v\simeq4c$!
Hubble sphere and event horizon
The innermost green bubble (labeled &quot;$v_\mathrm{rec}=c$&quot;) is the Hubble sphere, defined such that at any point in time, everything outside recedes faster than $c$. Meanwhile, the red line shows the event horizon, which defines the boundary between everything that can eventually be observed (light red region), and everything that cannot. A subset of this is out past lightcone (orange region) which is stuff that we have already observed (or at least have had the chance to).
Everything lying in between the Hubble sphere and the event horizon consists of events that we have been, or will eventually be, able to see, but which recede faster than the speed of light when it emits the light we see.
As you can see the region becomes narrower with time$^2$, meaning that the accelerated expansion of the Universe makes it harder and harder for photons emitted far away to reach us. We will never be able to see galaxies that today are farther away than roughly 17 Gly. But galaxies that are nearer will be seen (if we look), and a subset of these — namely the ones with $14\,\mathrm{Gly} \lesssim d_C \lesssim 17\,\mathrm{Gly}$ — are currently receding faster than the speed of light.
The size of the observable Universe always increases
The observable Universe is defined as the region within which light has had the time to reach us. The &quot;edge&quot; of this is called the particle horizon, and as seen from the blue line, it always increases its distance from us (in comoving coordinates, and thus even more so in physical coordinates). In comoving coodinates, it reach a maximum size of roughly 63 Gly. That means that more and more galaxies will enter our observable Universe, but as time goes they will do so at an ever-decreasing pace, asymptotically reaching a finite value (of 5 trillion galaxies, more or less). Once inside the particle horizon, a galaxy will never leave. It will, however, keep increasing its distance from us in physical coordinates, as well as its speed, and thus redshift without bounds and fade to black.

$^1$Comoving coordinates are defined so that they &quot;expand with the expansion of the Universe&quot;. That means that in these coordinates, galaxies lie approximately still wrt. each other. To get the physical coordinates — i.e. what you would measure if you froze the Universe and laid out measuring rods — multiply the comoving coordinates by the scale factor $a$ seen on the right $y$ axis. Since today $a\equiv1$, comoving and physical coordinates coincide today.
$^2$The fact that the diagram is in comoving coordinates makes it a bit hard to see, but this is still the case in physical coordinates.