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Radial-velocity observations of pulsating stars with a new Poznań Spectroscopic Telescope

This article discusses the radial velocity observations of pulsating stars using the new Poznań Spectroscopic Telescope at the Astronomical Observatory of Adam Mickiewicz University in Poznań, Poland. The telescope's capabilities, including its optical system, fibers, and guiding cameras, are described. The echelle spectrograph used for spectral analysis is also discussed, along with its spectral range and resolution. The article concludes with statistics on the observations and future perspectives for upgrades and calibration improvements.

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Radial-velocity observations of pulsating stars with a new Poznań Spectroscopic Telescope

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  1. Poznań Astronomical Observatory Adam Mickiewicz University Poznań, Poland Radial-velocity observations of pulsating stars with a new Poznań Spectroscopic Telescope 23 June 2008

  2. Our team • R. Baranowski, P. Bartczak, W. Borczyk, • W. Dimitrov, M. Fagas, K. Kamiński, T. Kwiatkowski, • R. Ratajczak, A. Rożek, A. Schwarzenberg-Czerny

  3. The „dome”

  4. The telescope Mirors diameter – 0.4 m Focal length – 1.8 m Optical system – Newtonian Diameter of the fibers – 50 m Accesible altitudes h>24° Mean. slewing rate 90°/min Guiding cameras ST7

  5. The echellé spectrograph Baudrand and Bohm (1992)

  6. CCD camera: Andor DZ 436 5-stage peltier cooling Temp. –95°C 2048 x 2048 pix pixel size 13.5 x 13.5μm dark current <1el/h readout noise 2.1 el/pix Echellé spectrograph Spectral range: 4480 Å – 9250 Å Resolution: R=35000 (~8 km/s)

  7. Acquisition box

  8. Echellé spectrum – 64 orders 4480 Å – 9250 Å blue range: 1pix = 0.04 Å order length = 80 Å every order adds 40 Å middle: 1pix = 0.05 Å ~2.5 km/s order length = 100 Åevery order adds 80 Å red range: 1pix = 0.08 Å order length = 160 Å every order adds 125 Å

  9. ThAr calibration spectrum 1400 lines

  10. Flatfield and fringe effect

  11. Flatfield and fringe effect

  12. Telluric lines removal

  13. Flux calibration

  14. Line profiles Sp=B1 V=1m exp=250s Hβ 4861 Å

  15. Limiting magnitude - BD+39 3012C 11m.2 Sp=F5 exp=30min

  16. 28 And δ Sct Sp=A7III V=5m.2 exp=600s analysed by T. Kwiatkowski, W. Borczyk & A. Rożek

  17. γ Peg β Cep Sp=B2IV V=2m.8 exp=600s or 300s period=3.4h υ1=6.59 c/d analysed by W. Borczyk

  18. V440 Per δ Cep Sp=F7Ib V=6m.3 exp=600s • σpoz=136 m/s • --2 harmonics • --1 harmonic analysed by A.Schwarzenberg-Czerny and M. Fagas

  19. Polaris analysed by M. Fagas and K. Kamiński

  20. Statistics • 13 august 2007 - 30 may 2008 • 83 nights • 637 hours • 1080 science spectra • Colaborators • Warsaw CAMK • Vienna Institute of Astronomy • Wrocław Astronomical Institute • Toruń Centre for Astronomy

  21. Future perspectives • Upgrade of the telescope: • 2 x 0.5m mirrors • simultaneous exposure of two fibers • better automatisation and remote control • Upgrade of the calibration, some ideas: • experiment - mixing the ThAr and stellar light • Vrad accuracy increase with a iodine cell • spectral resolution increase with the EDI interferometer • Radial velocity measurements: • broadening function • TODCOR • spectral disentangling

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