J/A+A/712/L13ivo://CDS.VizieR/J/A+A/712/L13CDSSwastik C.Bestha M.Sonith L.S.Facchini S.Sivarani T.Banyal R.K.,Wahhaj Z.Choudhary A.Gopinathan M.Saraf P.Mallik A.Navaneeth M.P.,Biswas S.Khushbu K.2026-08-05T13:46:35Z2026-08-04T09:10:50ZCDS support team

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

cds-question@unistra.frpre-main-sequence-starsvisible-astronomyspectroscopyWISPIT 2 is a young pre-main-sequence star hosting a multi-ringed transition disk and two directly imaged accreting protoplanets, the closest known analogue to PDS 70, yet its central star has no published optical spectrum. Population-synthesis models predict that stellar accretion can be strongly suppressed once two or more giant planets have formed, so characterising the atmospheric and accretion properties of such hosts is essential. We present the first optical spectrum of WISPIT 2 and use it to derive the host atmospheric parameters, test its youth spectroscopically, and constrain its stellar accretion state relative to PDS 70 and to the embedded planets. We analysed low-resolution HFOSC spectra (R about 1200 for Grism 7 and R about 2200 for Grism 8) from the 2-m Himalayan Chandra Telescope with iSpec, validating the pipeline at HFOSC resolution against Gaia FGK Benchmark Stars and K-type pre-main-sequence templates from the public Manara et al. library. The Halpha residual filling was measured relative to synthetic photospheric profiles and compared with the chromospheric-noise level of Manara et al. (2013A&A...551A.107M, Cat. J/A+A/551/A107). Halpha remains in net absorption but is partially filled in by emission. The weak residual filling, at 1.5-2.0 sigma, lies about 1dex below the chromospheric-noise level, consistent with chromospheric emission and no detectable accretion. We place a 95 percent upper limit of dM_acc_/dt<3.6x10^-11^M_{sun}_/yr, below even the lowest epoch of PDS 70 monitoring and implying a host-to-planet ratio (dM_star/dt)/(dM_2b_/dt)<18. We also measure Teff= 4551+/-150K and a first, low-resolution, model-dependent global metallicity [M/H]=-0.17+/- 0.16; the surface gravity and Li I equivalent width support the pre-main-sequence nature of the host. Both known double-protoplanet hosts, PDS 70 and WISPIT 2, therefore appear to show strongly suppressed or undetectable stellar accretion. Larger spectroscopic samples are needed to test whether this is common in multi-protoplanet transition disks.2026A&A...712L..13Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/712/L13CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/712/L13https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/712/L13http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/712/L13https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/712/L13https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/712/L13http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/712/L13GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/712/L13/listList of fits spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.dateObservation datestime.epoch;obsnullableWminFirst released wavelength0.1nmem.wlfloatWmaxLast released wavelength0.1nmem.wlfloatdWWavelength resolution0.1nmspect.resolutiondoublesizeSize of FITS fileKibytephys.size;meta.fitsintspShow the spectrummeta.ref.urlcharFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar