2021AJ....161..148W

Query : 2021AJ....161..148W

2021AJ....161..148W - Astron. J., 161, 148-148 (2021/March-0)

Constraining the nature of the PDS 70 protoplanets with VLTI/GRAVITY.

WANG J.J., VIGAN A., LACOUR S., NOWAK M., STOLKER T., DE ROSA R.J., GINZBURG S., GAO P., ABUTER R., AMORIM A., ASENSIO-TORRES R., BAUBOCK M., BENISTY M., BERGER J.P., BEUST H., BEUZIT J.-L., BLUNT S., BOCCALETTI A., BOHN A., BONNEFOY M., BONNET H., BRANDNER W., CANTALLOUBE F., CASELLI P., CHARNAY B., CHAUVIN G., CHOQUET E., CHRISTIAENS V., CLENET Y., COUDE DU FORESTO V., CRIDLAND A., DE ZEEUW P.T., DEMBET R., DEXTER J., DRESCHER A., DUVERT G., ECKART A., EISENHAUER F., FACCHINI S., GAO F., GARCIA P., GARCIA LOPEZ R., GARDNER T., GENDRON E., GENZEL R., GILLESSEN S., GIRARD J., HAUBOIS X., HEISSEL G., HENNING T., HINKLEY S., HIPPLER S., HORROBIN M., HOULLE M., HUBERT Z., JIMENEZ-ROSALES A., JOCOU L., KAMMERER J., KEPPLER M., KERVELLA P., MEYER M., KREIDBERG L., LAGRANGE A.-M., LAPEYRERE V., LE BOUQUIN J.-B., LENA P., LUTZ D., MAIRE A.-L., MENARD F., MERAND A., MOLLIERE P., MONNIER J.D., MOUILLET D., MULLER A., NASEDKIN E., OTT T., OTTEN G.P.P.L., PALADINI C., PAUMARD T., PERRAUT K., PERRIN G., PFUHL O., PUEYO L., RAMEAU J., RODET L., RODRIGUEZ-COIRA G., ROUSSET G., SCHEITHAUER S., SHANGGUAN J., SHIMIZU T., STADLER J., STRAUB O., STRAUBMEIER C., STURM E., TACCONI L.J., VAN DISHOECK E.F., VINCENT F., VON FELLENBERG S.D., WARD-DUONG K., WIDMANN F., WIEPRECHT E., WIEZORREK E., WOILLEZ J. (The GRAVITY Collaboration)

Abstract (from CDS):

We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 µas precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of 0.17 ± 0.06, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 MJup, while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1-5 µm spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-astronomical-unit spatial resolution, placing an upper limit of 0.3 au on the size of a bright disk around PDS 70 b.

Abstract Copyright: © 2021. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Exoplanet formation - Exoplanet atmospheres - Orbit determination - Long baseline interferometry

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (2000)
RA 		ICRS (2000)
DEC 		Proper motions Parallaxes Redshift Rad. vel. cz Mag U Mag B Mag V Mag R Mag I Sp type Morph. type Angular size #ref
1983 - 2024
1 CD-40 8434 TTauri* 14 08 10.1545500744 -41 23 52.573291080 -29.697 -24.041 8.8975 0.000010 3.13 3.13   13.42 12.18 11.71 10.506 K7IVe ~ ~ ~ ~ 367
2 CD-40 8434b Planet 14 08 10.1545500744 -41 23 52.573291080 -29.697 -24.041 8.8975 ~ ~ ~           ~ ~ ~ ~ ~ 207
3 CD-40 8434c Planet 14 08 10.1545500744 -41 23 52.573291080 -29.697 -24.041 8.8975 ~ ~ ~           ~ ~ ~ ~ ~ 157
4 HD 124058 Star 14 12 15.6382324872 -41 15 00.447605856 17.745 -5.403 2.3509 0.000066 19.90 19.90   11.133 10.297     K0III ~ ~ ~ ~ 8
5 HD 218396e Planet 23 07 28.7157209544 +21 08 03.310767492 108.284 -50.040 24.462 ~ ~ ~           ~ ~ ~ ~ ~ 211
6 HD 218396d Planet 23 07 28.7157209544 +21 08 03.310767492 108.284 -50.040 24.462 ~ ~ ~           ~ ~ ~ ~ ~ 241
7 HD 218396 EllipVar 23 07 28.7157209544 +21 08 03.310767492 108.284 -50.040 24.4620 -0.000035 -10.41 -10.41   6.21 5.953     F0+VkA5mA5 ~ ~ ~ ~ 1135

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