J/A+A/688/A224ivo://CDS.VizieR/J/A+A/688/A224doi:10.26093/cds/vizier.36880224CDSSanchez N.Nespoli E.Gonzalez M.Climent J.B.2024-11-29T20:04:54Z2024-08-26T07:34:40ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frearly-type-starsyoung-stellar-objectsinfrared-photometryStar formation is a complex process involving several physical mechanisms that interact with each other at different spatial scales. One way to shed some light on the star formation process is to analyse the relationship between the spatial distributions of gas and newly formed stars. In order to obtain robust results, it is necessary for this comparison to be made using quantitative and consistent descriptors applied to the same star-forming region. We used fractal analysis to characterise and compare in a self-consistent way the structure of the cloud and the distribution of young stellar objects (YSO) in the Dragonfish star-forming complex. Different emission maps of the Dragonfish nebula were retrieved from the NASA/IPAC Infrared Science and the Planck Legacy archives. Moreover, we used photometric information from the AllWISE catalogue to select a total of 1082 YSOs in the region. We derived the physical properties for some of these from their spectral energy distributions (SEDs). For the cloud images and YSOs, the three-dimensional fractal dimension (Df) was calculated using previously developed and calibrated algorithms. The fractal dimension of the Dragonfish Nebula (Df=2.6-2.7) agrees very well with values previously obtained for the Orion, Ophiuchus, and Perseus clouds. On the other hand, YSOs exhibit on average a significantly smaller value (Df=1.9-2.0) that indicates a much more clumpy structure than the material from which they formed. This is a clear and direct evidence that the clustering degree of the newly born stars is significantly higher than that of the parent cloud from which they formed, but the physical mechanism behind this behaviour is still not clear. Additionally, younger Class I and Class II sources have smaller values (Df=1.7+/-0.1) than more evolved Transition Disk objects (Df=2.2+/-0.1), evidencing a certain evolutionary effect where an initially clumpy structure tends to gradually disappear over time. The structure of the Dragonfish complex is similar to that of other molecular clouds in the Galaxy. However, we found clear and direct evidence that the clustering degree of the newly born stars is significantly higher than that of the parent cloud from which they formed. The physical mechanism behind this behaviour is still not clear.2024A&A...688A.224Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/688/A224CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/328 : AllWISE Data Release (Cutri+ 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/688/A224https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/688/A224http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/688/A224https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/688/A224https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/688/A224http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/688/A224GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/688/A224/table2 (List of YSOs and their properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/688/A224/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/688/A224/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/688/A224/table2?GETtext/xml+votable180.050000true179.6673155-63.26401060.0055555555555555565/2811 2814 6/6109 6111 11239 11243 11250-11251 112607.952274030004205e-20 1.7798557115773645e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/688/A224?format=asciiInfrareddefaultJ/A+A/688/A224/table2List of YSOs and their propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllWISEID from AllWISEmeta.id;meta.maincharGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latdoubleRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.maine_Kmag? Mean error on Kmagmagstat.error;phot.magfloatnullableClassObject class (1)meta.code.classcharREFReferences for previously identified YSOs (2)meta.refcharClusterSubstructure IDmeta.id.parentcharModelfitBest model used for SED fittingmeta.id;stat.fitcharTeff? Effective temperature from SED fittingKphys.temperature.effectivefloatnullableAv? Visual extinction from SED fittingmagphys.absorptionfloatnullablelogg? Surface gravity from SED fittinglog(cm.s**-2)phys.gravityfloatnullablePlx? Gaia parallaxmaspos.parallaxfloatnullablee_Plx? Error on Plxmasstat.error;pos.parallaxfloatnullableW1mag? W1 band magnitudemagphot.mag;em.IR.3-4umfloatnullablee_W1mag? Mean error on W1magmagstat.error;phot.magfloatnullableW2mag? W2 band magnitudemagphot.mag;em.IR.4-8umfloatnullablee_W2mag? Mean error on W2magmagstat.error;phot.magfloatnullableW3mag? W3 band magnitudemagphot.flux.density;em.IR.8-15umfloatnullablee_W3mag? Mean error on W3magmagstat.error;phot.magfloatnullableW4mag? W4 band magnitudemagphot.flux.density;em.IR.15-30umfloatnullablee_W4mag? Mean error on W4magmagstat.error;phot.magfloatnullableJmag? J band magnitudemagphot.mag;em.IR.Jfloatnullablee_Jmag? Mean error on Jmagmagstat.error;phot.magfloatnullableHmag? H band magnitudemagphot.mag;em.IR.Hfloatnullablee_Hmag? Mean error on Hmagmagstat.error;phot.magfloatnullableKmag? K band magnitudemagphot.mag;em.IR.Kfloatnullable