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Oct 16, 2023 •229 likes •419 views

Measuring the spin of the directly imaged sub-stellar companion GQ Lupi b Henriette Schwarz Ignas Snellen, Matteo Brogi, Remco de Kok, Jayne Birkby, Christian Ginski Connection between formation and spin [Snellen et al. 2014] 1 / 17

  1. Measuring the spin of the directly imaged sub-stellar companion GQ Lupi b Henriette Schwarz Ignas Snellen, Matteo Brogi, Remco de Kok, Jayne Birkby, Christian Ginski

  2. Connection between formation and spin [Snellen et al. 2014] 1 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  3. β Pic b: first spin measurement 2 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  4. New CRIRES observations HIP 78530 b GSC 6214-210 GQ Lupi b K planet 14.1 14.9 13.3 K star 6.9 9.1 7.1 Angular 4.5" 2.2" 0.7" separation Age estimate 5 Myr 11 Myr 1 Myr Planetary mass 23 Mjup 17 Mjup 21.5 Mjup estimate 3 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  5. GQ Lupi b: a directly imaged sub-stellar companion 4 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  6. Cross-correlating with model spectra Hot Jupiters Young massive giants ● Transmission spectra or ● Directly imaged planets thermal emission ● Fast orbital motion ● Slow orbital motion ● Changing Doppler-shift of ● Constant radial velocity planetary lines shift relative to host ● No spatial separation from ● Spatial separation from host host 5 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  7. Data analysis: a spectrum for each slit position Slit position Wavelength 6 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  8. CO detection, companion position 7 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  9. CO detection, companion position 8 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  10. CO & H 2 O detection 9 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  11. The measured companion parameters vsin(i) = 6.0 ± 0.8 km/s rv = 2.1 ± 0.4 km/s 10 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  12. GQ Lupi b's CO signal is very narrow GQ Lupi b Mass 21.5 Mjup Radius 3.5 Rjup Age 0-5 Myr Teff 2650 K Beta Pic b Mass 7 Mjup Radius 1.65 Rjup Age 8-20 Myr Teff 1600 K 11 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  13. The stellar spectrum has molecular lines 12 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  14. Removing stellar CO lines affects shape of planetary CO lines 13 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  15. Constraining the orbital parameters LSMC constraints from astrometry on orbital elements of GQ Lupi b [Ginski et al. 2014] eccentricity eccentricity 14 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  16. Constraining the orbital parameters rv = 2.1 ± 0.4 km/s eccentricity eccentricity 15 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  17. Constraining the orbital parameters rv = 2.1 ± 0.4 km/s eccentricity eccentricity 16 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

  18. Summary ● Spin measurements of exoplanets may hold clues to the formation process ● Combining high dispersion spectroscopy and adaptive optics it is possible to measure the spin of directly imaged planets ● Molecular lines in colder stars present a challenge ● GQ Lupi b has a vsin(i) of 6.0 ± 0.8 km/s ● Rotates slowly, possibly because it is young and bloated 17 / 17 Henriette Schwarz, schwarz@strw.leidenuniv.nl

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