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<ri:Resource created="2012-12-07T15:05:53Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Exoplanet masses derived from RVs</title><shortName>J/ApJ/733/68</shortName><identifier>ivo://CDS.VizieR/J/ApJ/733/68</identifier><altIdentifier>doi:10.26093/cds/vizier.17330068</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Brown R.A.</name></creator><date role="Updated">2022-05-05T10:40:48Z</date><date role="Created">2012-12-07T15:05:53Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>solar-system-planets</subject><subject>stellar-masses</subject><subject>multiple-stars</subject><description>Exoplanet searches using radial velocity (RV) and microlensing (ML) produce samples of "projected" mass and orbital radius, respectively. We present a new method for estimating the probability density distribution (density) of the unprojected quantity from such samples. For a sample of n data values, the method involves solving n simultaneous linear equations to determine the weights of delta functions for the raw, unsmoothed density of the unprojected quantity that cause the associated cumulative distribution function (CDF) of the projected quantity to exactly reproduce the empirical CDF of the sample at the locations of the n data values. We smooth the raw density using nonparametric kernel density estimation with a normal kernel of bandwidth {sigma}. We calibrate the dependence of {sigma} on n by Monte Carlo experiments performed on samples drawn from a theoretical density, in which the integrated square error is minimized. We scale this calibration to the ranges of real RV samples using the Normal Reference Rule. The resolution and amplitude accuracy of the estimated density improve with n. For typical RV and ML samples, we expect the fractional noise at the PDF peak to be approximately 80n^-log2^. For illustrations, we apply the new method to 67 RV values given a similar treatment by Jorissen et al. (2001A&amp;A...379..992J), and to the 308 RV values listed at exoplanets.org on 2010 October 20.</description><source format="bibcode">2011ApJ...733...68B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/733/68</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/527/A140">J/A+A/527/A140 : Mass limits on substellar companions (Reffert+, 2011)</relatedResource><relatedResource>http://exoplanets.org/ : Exoplanet orbit database web 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