J/A+A/711/A292ivo://CDS.VizieR/J/A+A/711/A292CDSLatour J.Christiaens V.Absil O.Bonse M.Savonet R.Juillard S.,Hammond I.Casassus S.Cieza L.Cugno G.Desgrange C.Lacour S.,Mawet D.Montesinos M.Perez S.Pinte C.Reggiani M.Stolker T.,van der Marel N.Zurlo A.2026-07-23T07:34:09Z2026-07-23T08:33:49ZCDS support team

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

cds-question@unistra.frvariable-starspolarimetryinfrared-astronomyThe HD 135344B (SAO 206462) disk exhibits strong signposts of planet formation both in scattered light and sub-mm continuum images. ALMA images in the sub-mm revealed a gap-crossing dust filament whose position coincides with a twist detected in the scattered-light spiral structure. Analysis of the spiral dynamics in polarized light also hints at a spiral-driving protoplanet in the sub-mm gap. We aim to study the overall dynamics of the three spirals in the disk, as well as the motion of the twist over a 10-year baseline, at different IR wavelengths. We also seek to assess the authenticity of a candidate protoplanet recently claimed in the disk. We use high-fidelity post-processing algorithms such as iterative principal component analysis to minimize the biases induced by angular differential imaging on extended sources and conduct a thorough analysis of archival VLT/NACO, VLT/SPHERE, and VLT/ERIS datasets in order to obtain the spiral traces and measure their orbital motion in multiple wavelength bands in scattered light. We also reprocess archival JWST/NIRCam datasets with these algorithms. We measure an average spiral orbital motion of 0.81+/-0.05deg/year, in agreement with the literature value of about 0.85 deg/year at all wavelengths. With simple modeling of the twist morphology, we confirm that it is indeed co-moving with the spiral in which it is embedded. While the position angle of the twist coincides with the dust filament, it is located at a smaller angular separation from the star, which we attribute to the fact that the spiral trace moves away from the central star with increasing wavelength. We find that a previously claimed protoplanet candidate in the disk can be adequately explained as a post-processing artifact. Our confirmation that the motion of the scattered light twist is consistent with the orbital velocity of a planet at 69+-4 au over a 10-year baseline suggests that the spirals, the gap and the dust filament in the sub-mm continuum, as well as the twist in scattered light, could indeed all be attributed to the same hypothetical protoplanet deeply embedded within the spiral. A perplexing trend for a wavelength-dependence of the angular distance of the spiral traces to the central star still remains to be explained.2026A&A...711A.292Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/711/A292CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/711/A292https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/711/A292http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/711/A292https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/711/A292https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/711/A292http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/711/A292GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/711/A292/list (List of fits image)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/711/A292/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/711/A292/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/711/A292/list?GETtext/xml+votable180.050000true228.9518333-37.15444440.0055555555555555566/44049https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/711/A292?format=asciiInfrareddefaultJ/A+A/711/A292/listList of fits imagerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Simbad right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Simbad declination (J2000)pos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.dateObservation datestime.epoch;obsnullablesizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar