J/A+A/689/A65ivo://CDS.VizieR/J/A+A/689/A65doi:10.26093/cds/vizier.36890065CDSRampinelli L.Facchini S.Leemker M.Bae J.Benisty M.Teague R.,Law C.J.Oberg K.I.Portilla-Revelo B.Cridland A.J.2024-11-29T20:06:00Z2024-09-03T09:39:33ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsspectroscopyradio-sourcesWith two directly detected protoplanets, the PDS 70 system is a unique source in which to study the complex interplay between forming planets and their natal environment. The large dust cavity carved by the two giant planets can affect the disk chemistry, and therefore the molecular emission morphology. On the other hand, chemical properties of the gas component of the disk are expected to leave an imprint on the planetary atmospheres. In this work, we reconstruct the emission morphology of a rich inventory of molecular tracers in the PDS 70 disk, and we look for possible chemical signatures of the two actively accreting protoplanets, PDS b and c. We leverage Atacama Large Millimeter/submillimeter Array (ALMA) band 6 high-angular-resolution and deep- sensitivity line emission observations, together with image and uv-plane techniques, to boost the detection of faint lines. We robustly detect ring-shaped emission from ^12^CO, ^13^CO, C^18^O, H^13^CN, HC^15^N, DCN, H_2_CO, CS, C_2_H, and H^13^CO+ lines in unprecedented detail. Most of the molecular tracers show a peak of the emission inside the millimeter dust peak. We interpret this as the direct impact of the effective irradiation of the cavity wall, as a result of the planet formation process. Moreover, we have found evidence of an O-poor gas reservoir in the outer disk, which is supported by the observations of bright C-rich molecules, the non-detection of SO, and a lower limit on the CS/SO ratio of ~1 . Eventually, we provide the first detection of the c-C_3_H_2_ transitions at 218.73GHz, and the marginal detection of an azimuthal asymmetry in the higher-energy H_2_CO (3_2,1_-2_2,0_) line, which could be due to accretion heating near PDS 70b.2024A&A...689A..65Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/689/A65CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/632/A25 : PDS70 VLT/SPHERE images (Mesa+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/689/A65https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/689/A65http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/689/A65https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/689/A65https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/689/A65http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/689/A65GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/689/A65/list (List of fits datacubes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/689/A65/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/689/A65/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/689/A65/list?GETtext/xml+votable180.050000true212.04208-41.398070.0055555555555555566/43415https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/689/A65?format=asciiRadiodefaultJ/A+A/689/A65/listList of fits datacubesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintNzNumber of slicesmeta.numberintObs.dateObservation datestime.epoch;obsnullablebFreqLower value of frequency intervalGHzem.freqfloatBFreqUpper value of frequency intervalGHzem.freqfloatdFreqFrequency resolutionHzspect.resolutiondoublesizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fits