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<ri:Resource created="2026-03-17T08:13:46Z" status="active" updated="2026-04-02T06:28:33Z" 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>Precise determination of disk lifetimes</title><shortName>J/A+A/707/A216</shortName><identifier>ivo://CDS.VizieR/J/A+A/707/A216</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Polnitzky F.A.</name></creator><creator><name>Ratzenbock S.</name></creator><creator><name>Grossschedl J.</name></creator><creator><name>Alves J.</name></creator><date role="Updated">2026-04-02T06:28:33Z</date><date role="Created">2026-03-17T08:13:46Z</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>young-stellar-objects</subject><subject>stellar-ages</subject><subject>visible-astronomy</subject><subject>infrared-photometry</subject><description>Determining how long circumstellar disks last is key to understanding the timescale of planet formation. Typically, this is done by measuring the fraction of young stars with infrared-excess, a sign of circumstellar material, in stellar clusters of different ages. However, comparing data from different star-forming regions at different distances introduces uncertainties and biases because of the different sample completeness and environment. This study addresses these challenges by analyzing 33 clusters, aged 3 to 21 million years (PARSEC isochrones), within the Scorpius-Centaurus OB association, sampling the stellar IMF from the hydrogen burning limit to about 8M_{sun{_. By using Gaia, 2MASS, and WISE data, we identified stars with infrared-excess through color-color diagrams and spectral energy distributions, ensuring a consistent selection of disk-bearing sources. Our results indicate a disk lifetime of 5.8+/-0.3Myr, about a factor of two longer than most previous estimates, suggesting that planet formation may have more time than previously thought. We also find that an exponential decay model best describes disk dispersal. These findings emphasize the importance of studying disk evolution in a single star-forming region to reduce uncertainties and refine our understanding of planet formation timelines.</description><source format="bibcode">2026A&amp;A...707A.216P</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/707/A216</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/I/355">I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/678/A71">J/A+A/678/A71 : Cluster ages in Sco-Cen (Ratzenboeck+, 2023)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/163/25">J/AJ/163/25 : Circumstellar disk populations in the Sco-Cen complex</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/707/A216</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/707/A216</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/707/A216</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL 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Galactic latitude from Gaia (b)</description><unit>deg</unit><ucd>pos.galactic.lat</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>ruwe</name><description>? The RUWE parameter from Gaia (ruwe)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>W1mag</name><description>? W1 magnitude from AllWISE (W1mag)</description><unit>mag</unit><ucd>phot.mag;em.IR.3-4um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W1mag</name><description>? Uncertainty in the W1 magnitude from AllWISE (e_W1mag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W2mag</name><description>? W2 magnitude from AllWISE (W2mag)</description><unit>mag</unit><ucd>phot.mag;em.IR.4-8um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W2mag</name><description>? Uncertainty in the W2 magnitude from AllWISE (e_W2mag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W3mag</name><description>? W3 magnitude from AllWISE (W3mag)</description><unit>mag</unit><ucd>phot.flux.density;em.IR.8-15um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W3mag</name><description>? Uncertainty in the W3 magnitude from AllWISE (e_W3mag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W4mag</name><description>? W4 magnitude from AllWISE (W4mag)</description><unit>mag</unit><ucd>phot.flux.density;em.IR.15-30um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W4mag</name><description>? Uncertainty in the W4 magnitude from AllWISE (e_W4mag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Jmag</name><description>? Magnitude in the J band from 2MASS (Jmag)</description><unit>mag</unit><ucd>phot.mag;em.IR.J</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Jmag</name><description>? Uncertainty in the magnitude in the J band from 2MASS (e_Jmag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Hmag</name><description>? Magnitude in the H band from 2MASS (Hmag)</description><unit>mag</unit><ucd>phot.mag;em.IR.H</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Hmag</name><description>? Uncertainty in the magnitude in the H band from 2MASS (e_Hmag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Kmag</name><description>? Magnitude in the KS band from 2MASS (Kmag)</description><unit>mag</unit><ucd>phot.mag;em.IR.K</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Kmag</name><description>? Uncertainty in the magnitude in the KS band from 2MASS (e_Kmag)</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>snr1</name><description>? Signal-to-noise ratio in the W1 band from AllWISE (snr1)</description><ucd>stat.snr</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>chi2W1</name><description>? Reduced chi-squared value in the W1 band from AllWISE (chi2W1)</description><ucd>stat.fit.chi2</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>snr2</name><description>? Signal-to-noise ratio in the W2 band from AllWISE (snr2)</description><ucd>stat.snr</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>chi2W2</name><description>? Reduced chi-squared value in the W2 band from AllWISE (chi2W2)</description><ucd>stat.fit.chi2</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>snr3</name><description>? Signal-to-noise ratio in the W3 band from AllWISE (snr3)</description><ucd>stat.snr</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>chi2W3</name><description>? Reduced chi-squared value in the W3 band from AllWISE (chi2W3)</description><ucd>stat.fit.chi2</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>snr4</name><description>? Signal-to-noise ratio in the W4 band from AllWISE (snr4)</description><ucd>stat.snr</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>chi2W4</name><description>? Reduced chi-squared value in the W4 band from AllWISE (chi2W4)</description><ucd>stat.fit.chi2</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>W123</name><description>? Selection of disks in the W123 CCDs (W123) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>W124</name><description>? Selection of disks in the W124 CCDs (W124) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>HKW2</name><description>? Selection of disks in the HKW2 CCDs (HKW2) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>HKW3</name><description>? Selection of disks in the HKW3 CCDs (HKW3) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>DiskSED</name><description>? Selection of disks in the SED (Disk_SED) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>alphaKW3</name><description>? Slope of the SED fitting between KS to W3 (alpha_KW3)</description><ucd>meta.cryptic</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_alphaKW3</name><description>? Uncertainty in the slope of the SED fitting between KS and W3 (e_alpha_KW3)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_alphaKW4</name><description>? Uncertainty in the slope of the SED fitting between K_S and W4 (e_alpha_KW4)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_interKW4</name><description>? Uncertainty in the intercept of the SED fitting between KS to W4 (e_intercept_KW4)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>alphaW13</name><description>? Slope of the SED fitting between W1 to W3 (alpha_W13)</description><ucd>meta.cryptic</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_alphaW13</name><description>? Uncertainty in the slope of the SED fitting between W1 and W3 (e_alpha_W13)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>interW13</name><description>? Intercept of the SED fitting between W1 to W3 (intercept_W13)</description><ucd>stat.fit</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_interW13</name><description>? Uncertainty in the intercept of the SED fitting between W1 to W3 (e_intercept_W13)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>alphaW14</name><description>? Slope of the SED fitting between W1 to W4 (alpha_W14)</description><ucd>meta.cryptic</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_alphaW14</name><description>? Uncertainty in the slope of the SED fitting between W1 and W4 (e_alpha_W14)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>interW14</name><description>? Intercept of the SED fitting between W1 to W4 (intercept_W14)</description><ucd>stat.fit</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_interW14</name><description>? Uncertainty in the intercept of the SED fitting between W1 to W4 (e_intercept_W14)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>alphaKW2</name><description>? Slope of the SED fitting between KS to W2 (alpha_KW2)</description><ucd>meta.cryptic</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_alphaKW2</name><description>? Uncertainty in the slope of the SED fitting between KS and W2 (e_alpha_KW2)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>interKW2</name><description>? Intercept of the SED fitting between KS to W2 (intercept_KW2)</description><ucd>stat.fit</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_interKW2</name><description>? Uncertainty in the intercept of the SED fitting between KS to W2 (e_intercept_KW2)</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>alpha</name><description>? alpha-value used in the selection (alpha)</description><ucd>meta.cryptic</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>DiskClLuhman</name><description>? Disk type from Luhman 2022AJ....163...25L (DiskClass_Luhman)</description><ucd>src.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="21*">char</dataType></column><column><name>DiskLuhman</name><description>? Selection of disks from Luhman (2022AJ....163...25L) (Disk_Luhman) (1)</description><ucd>src.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>SigMAlabel</name><description>? Stellar cluster label to which the source belongs to (SigMA_label)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>AllWISE</name><description>? AllWISE identification number (AllWISE)</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>DiskCCD</name><description>? Selection of disks in the CCDs (Disk_CCD) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column></table></schema></tableset></ri:Resource>