There are numerous exoplanet-related catalogs available online, each with its own criteria on which objects to include in their list of planets. As such, users may notice different numbers associated with each information source.
The NASA Exoplanet Archive has adopted a policy of including and classifying all objects as planetary that meet the following criteria:
An example of an object that has not been included is the companion to SCR 1845. This object was detected via imaging and has an estimated mass larger than the 30 Jupiter mass criteria stated above.
For HD 45364 b and c from Mayor et al 2004, the time of periastron passage is computed from the period, base date, longitude of periastron omega (ω) and mean longitude of the date lambda (λ) as follows:
tperi= base date - P* (λ-ω)/360 = basedate - P*λ/360 - P*ω/360
where P is period and M = λ-ω is the mean anomaly and the error is propagated from errors in the period and angles as follows:
σt,peri2 = σP2 * ((λ-ω)/360)2 + (σω2+σλ2) *(P/360)2
These criteria may change in the future as our understanding of exoplanets improves. If you find an error or have an update on the parameter values on our site, please submit a Helpdesk ticket. We will confirm and update our values accordingly.
For papers that report multiple values for an exoplanet or host star parameter, a single value is chosen as the default, and the user can access the paper for the additional values. For papers that report a range of values for an exoplanet or host star parameter, as opposed to a single value and uncertainties, we adopt the mean of the range as the single value and the range/2 as the uncertainty. For example, Liu et al. (2011) reports a mass for CFBDSIR J1458+1013 b of 6-15 Jupiter masses. We adopt a value of 10.5+/-4.5 Jupiter masses.
Occasionally, we will remove an object from the archive when its status changes. A list of these objects is given on the Targets Removed from the Archive page.
Occasionally, planet parameters in the archive are different from those in the published literature. These discrepancies are identified by the comments from the scientific community, and are confirmed by the authors. We track these errors in the table below, which is updated periodically.
There is also a page listing the targets removed or disregarded from the archive.
|Host Name||Planet Letter||Parameter||Literature Value||Exoplanet Archive Value||Literature Reference||Notes|
|Kepler-10||c||Orbital Period||42.29485 days||45.29485 days||Fressin et al. 2011 ||Typo in published period in Table 2, confirmed with author|
|CoRoT-20||b||Distance to System||1.23+/-120 kpc||1.23+/-0.12 kpc||Deleuil et al. 2012||Typo in Table 3|
Orbit Semi-Major Axis
|119 AU||115 AU||Kalas et al 2008||119 AU is quoted in the abstract, but 115 AU appears repeatedly throughout the paper|
|GJ 3470||b||RV Semi-Amplitude||0.00901+/-0.00075 m/s||9.01+/-0.75 m/s||Bonfils et al. 2012||Unit in Table 2 should be km/s|
|HD 203030||b||Planet Letter||B||b||Metchev & Hillenbrand 2006||The Exoplanet Archive adopts lower-case letters for planetary mass companions|
|b||RV semi-amplitude||0.0912+/-0.002 m/s||91.2+/-2 m/s||Brown et al. 2012||Unit in Table 7 should be km/s|
|Kepler-46||d||Planet Letter||c||d||Rowe et al. 2014||Typo, Kepler-46 c already exists in literature|
|HD 60532||b, c||Stellar Surface Gravity||-3.83||3.83||Desort et al. 2014||Typo in Table 1|
|Kepler-289||c, d||Planet Letter||PH3 d
|Schmitt et al. 2014||Kepler-289 c already exists in literature|
|BD+49 828||log (Stellar Age) [yr]||9.37+/-18||9.37+/-0.18||Niedzielski et al. 2015||Typo; missing decimal place in uncertainty. Note that Exoplanet Archive provides age in Gyr.|
Last update: 25 February 2015