<p>As you've correctly mentioned observation biases play a huge role in current understanding of planetary populations. Let's have a look at a slightly outdated plot (age 2 months) that shows us the semimajor-axis vs mass distribution of currently known planets including KOI's (unconfirmed planets).</p>

<p><a href="https://i.sstatic.net/2avQl.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/2avQl.png" alt="Current planetary population"></a></p>

<p>Here we see two things:</p>

<ul>
<li>Hot Jupiters seem to make up a significant part of the confirmed planets (confirmed = RV + Transit)</li>
<li>The farther out we go, the less likely it is to have a measured planetary radius (black dots)</li>
</ul>

<p>Now knowing how our methods and instrumentation work, we can try and debias this data.<br>
Transit measurments pose the easiest ones to do this: as for transits the detection probability is a simple geometric function of planetary alignment, radius and stellar radius one can overplot the found planets with this probability. So this is usually of not very massive interest to the planetary community.<br>
<strong>edit</strong><br>
The probability usually is given as $\sim r_{stellar}/2 a$, with $r_{stellar}$ being the stellar radius and $a$ the planet's semi-major axis. A simple derivation is <a href="http://kepler.nasa.gov/Science/about/characteristicsOfTransits/" rel="nofollow noreferrer">here</a>. Discussion how everything gets more complicated when combining with RV measurments <a href="http://astrobites.org/2013/05/23/transit-probabilities-not-as-simple-as-they-seem/" rel="nofollow noreferrer">here</a>.<br>
<strong>/edit</strong></p>

<p>Any instrument one uses however, will have their own quirks and biases and starspots or eclipsing binaries can lead to false positives. <a href="http://adsabs.harvard.edu/abs/2013PNAS..11019273P" rel="nofollow noreferrer">Petigura+ 2013, fig. 1</a> try to asses those effects for Kepler transits and come up with the following detection probability map.</p>

<p><a href="https://i.sstatic.net/fXkJW.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/fXkJW.png" alt="Rough correction for transit incompleteness"></a></p>

<p>The corrected population then would be found by dividing $\rm\frac{found population}{completeness}$. Mathematical issues like dividing by zero are easily interpreted as issues stemming from the incomplete data. As where the detectability is zero, we can't know if there are 0 or 1 or 20 planets hidden in a bin.
When projected on one axis or the other those corrected data-plots then result in corrected Radius- or Period occurence rates.<br>
I won't show those for the transit method, as I want to encourage to check the original reference.  </p>

<p>I show one of those plots for the radial velocity method however. From <a href="http://adsabs.harvard.edu/abs/2011arXiv1109.2497M" rel="nofollow noreferrer">Mayor+ 2011, fig. 12</a> that analyse their HARPS-spectrograph data from the preceeding decade:</p>

<p><a href="https://i.sstatic.net/L0ph7.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/L0ph7.png" alt="enter image description here"></a></p>

<p><strong>In black</strong>: Found planets, <strong>red</strong>: debiased radial-velocity population
Note: A Jupiter-mass is roughly 320 Earth-masses, so in this plot the Hot Jupiters are on the far right. This now closes the thematic circle to my initial note about Hot Jupiters: While in black Jupiter-like planets seem very common, in the debiased version this is not the case anymore. Mayor et al. estimate the Hot Jupiters to make up only 0.5% of the total planetary population with this method.</p>

<p>Note also that although the debiased number of terrestrial planets increases significantly, their error bars explode in size. This stems simply from doing statistics with low numbers. Also for reasons of simplicity and clarity the error bars on the first two plots are not shown.</p>

<hr>

<p><strong>Concluding</strong>:<br>
It is important to debias the data we have about exoplanets by method.<br>
When doing this, we get rough ideas about how the true planetary populations look like.  </p>

<p>Recent results and non-stop public announcments about "hundreds of newly found planets" can lead to a certain, totally understandable euphoria that we now know everything about planets.<br>
This is however very far from true. The Number distribution in full mass-radius-semimajor axis space is still very, very thinly spread. So in the end we do low-number statistics when debiasing, which is scientifically simply unsatisfying.<br>
Or said differently: There is still a lot of exciting work to be done!</p>

CC BY-SA 3.0
2015-11-09T09:11:50.647Z
Can exoplanets discovered by microlensing be assumed to be unbiased? [19 found](https://en.wikipedia.org/wiki/List_of_exoplanets_detected_by_microlensing) increased by 8 last year soon becomes a useful sample size.
LocalFluff
CC BY-SA 3.0
2015-11-09T17:01:21.593Z
As I don't really know much about microlensing, I can only cite the PP6-companion: "Because
the images [of the lensed planet] generally appear close to the Einstein ring,
microlensing is most sensitive to planets with projected separations
equal to the physical size of the Einstein ring in the
lens plane". Now the primary Einstein ring is mainly a function of the mass of the lensing star. Lensing stars will follow the regular stellar mass distribution, in that most of them are M-dwarves. According to the quote this means that a certain physical star-planet separation will be preferably detecte
AtmosphericPrisonEscape
CC BY-SA 3.0
2015-11-09T17:01:59.500Z
Source for the quote (and also an interesting review):
http://www.mpia.de/homes/ppvi/chapter/fischer.pdf
AtmosphericPrisonEscape
CC BY-SA 3.0
2015-11-09T17:09:45.370Z
@LocalFluff: Also for a "useful sample size" you have to state which random variables you are talking about. As the variables probed by lensing are at least Mass and physical distance, I think way more data than $\mathcal{O}(10-100)$ planets is needed.
AtmosphericPrisonEscape
CC BY-SA 3.0
2015-11-08T23:53:43.760Z
2015-11-09T14:58:16.877Z
2015-11-09T14:58:16.877Z
AtmosphericPrisonEscape
<p>I am interested in current estimate of distribution of planets of various radii in various distances from their parent star. There is many sources, where one can find database of presently known exoplanets, for example <a href="http://exoplanets.org/" rel="nofollow">exoplanets.org</a>, <a href="http://www.openexoplanetcatalogue.com/" rel="nofollow">www.openexoplanetcatalogue.com</a> and others. However, the known exoplanets are, of course, subject to conditional probability of detection by various methods. One cannot take the database as representative distribution, because, for example, hot Jupiters or big planets in general would be greatly overestimated.</p>

<p>What are the best resources to obtain current unbiased estimates of exoplanet radii and distances?</p>

CC BY-SA 3.0
2015-11-08T10:57:33.867Z
The best estimates probably come from models of planetary system formation. But the models are still being refined, to explain the range of systems that we observe.
James K
<exoplanet><star-systems>
Estimates of exoplanets distribution consistent with current data
Irigi
# Estimates of exoplanets distribution consistent with current data

(Asked by: username_0 on 2015-11-08)

I am interested in current estimate of distribution of planets of various radii in various distances from their parent star. There is many sources, where one can find database of presently known exoplanets, for example [exoplanets.org](http://exoplanets.org/), [www.openexoplanetcatalogue.com](http://www.openexoplanetcatalogue.com/) and others. However, the known exoplanets are, of course, subject to conditional probability of detection by various methods. One cannot take the database as representative distribution, because, for example, hot Jupiters or big planets in general would be greatly overestimated.

What are the best resources to obtain current unbiased estimates of exoplanet radii and distances?

**Tags:** exoplanet, star-systems
> **Comments:**
> **username_1**: The best estimates probably come from models of planetary system formation. But the models are still being refined, to explain the range of systems that we observe.  

---

## 1 answers

### Answer by username_2 on 2015-11-08. Score: 7 | Accepted answer

As you've correctly mentioned observation biases play a huge role in current understanding of planetary populations. Let's have a look at a slightly outdated plot (age 2 months) that shows us the semimajor-axis vs mass distribution of currently known planets including KOI's (unconfirmed planets).

[![Current planetary population](https://i.sstatic.net/2avQl.png)](https://i.sstatic.net/2avQl.png)

Here we see two things:

* Hot Jupiters seem to make up a significant part of the confirmed planets (confirmed = RV + Transit)
* The farther out we go, the less likely it is to have a measured planetary radius (black dots)

Now knowing how our methods and instrumentation work, we can try and debias this data.  
Transit measurments pose the easiest ones to do this: as for transits the detection probability is a simple geometric function of planetary alignment, radius and stellar radius one can overplot the found planets with this probability. So this is usually of not very massive interest to the planetary community.  
**edit**  
The probability usually is given as $\sim r\_{stellar}/2 a$, with $r\_{stellar}$ being the stellar radius and $a$ the planet's semi-major axis. A simple derivation is [here](http://kepler.nasa.gov/Science/about/characteristicsOfTransits/). Discussion how everything gets more complicated when combining with RV measurments [here](http://astrobites.org/2013/05/23/transit-probabilities-not-as-simple-as-they-seem/).  
**/edit**

Any instrument one uses however, will have their own quirks and biases and starspots or eclipsing binaries can lead to false positives. [Petigura+ 2013, fig. 1](http://adsabs.harvard.edu/abs/2013PNAS..11019273P) try to asses those effects for Kepler transits and come up with the following detection probability map.

[![Rough correction for transit incompleteness](https://i.sstatic.net/fXkJW.png)](https://i.sstatic.net/fXkJW.png)

The corrected population then would be found by dividing $\rm\frac{found population}{completeness}$. Mathematical issues like dividing by zero are easily interpreted as issues stemming from the incomplete data. As where the detectability is zero, we can't know if there are 0 or 1 or 20 planets hidden in a bin.
When projected on one axis or the other those corrected data-plots then result in corrected Radius- or Period occurence rates.  
I won't show those for the transit method, as I want to encourage to check the original reference.

I show one of those plots for the radial velocity method however. From [Mayor+ 2011, fig. 12](http://adsabs.harvard.edu/abs/2011arXiv1109.2497M) that analyse their HARPS-spectrograph data from the preceeding decade:

[![enter image description here](https://i.sstatic.net/L0ph7.png)](https://i.sstatic.net/L0ph7.png)

**In black**: Found planets, **red**: debiased radial-velocity population
Note: A Jupiter-mass is roughly 320 Earth-masses, so in this plot the Hot Jupiters are on the far right. This now closes the thematic circle to my initial note about Hot Jupiters: While in black Jupiter-like planets seem very common, in the debiased version this is not the case anymore. Mayor et al. estimate the Hot Jupiters to make up only 0.5% of the total planetary population with this method.

Note also that although the debiased number of terrestrial planets increases significantly, their error bars explode in size. This stems simply from doing statistics with low numbers. Also for reasons of simplicity and clarity the error bars on the first two plots are not shown.

---

**Concluding**:  
It is important to debias the data we have about exoplanets by method.  
When doing this, we get rough ideas about how the true planetary populations look like.

Recent results and non-stop public announcments about "hundreds of newly found planets" can lead to a certain, totally understandable euphoria that we now know everything about planets.  
This is however very far from true. The Number distribution in full mass-radius-semimajor axis space is still very, very thinly spread. So in the end we do low-number statistics when debiasing, which is scientifically simply unsatisfying.  
Or said differently: There is still a lot of exciting work to be done!

> **Comments:**
> **username_3**: Can exoplanets discovered by microlensing be assumed to be unbiased? [19 found](https://en.wikipedia.org/wiki/List_of_exoplanets_detected_by_microlensing) increased by 8 last year soon becomes a useful sample size.  
> **username_2**: As I don't really know much about microlensing, I can only cite the PP6-companion: "Because the images [of the lensed planet] generally appear close to the Einstein ring, microlensing is most sensitive to planets with projected separations equal to the physical size of the Einstein ring in the lens plane". Now the primary Einstein ring is mainly a function of the mass of the lensing star. Lensing stars will follow the regular stellar mass distribution, in that most of them are M-dwarves. According to the quote this means that a certain physical star-planet separation will be preferably detecte  
> **username_2**: Source for the quote (and also an interesting review): http://www.mpia.de/homes/ppvi/chapter/fischer.pdf  
> **username_2**: @LocalFluff: Also for a "useful sample size" you have to state which random variables you are talking about. As the variables probed by lensing are at least Mass and physical distance, I think way more data than $\mathcal{O}(10-100)$ planets is needed.  

---

