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Spectroscopic Study of Open Cluster NGC 2506: Stellar Evolution Insights

This study focuses on the open cluster NGC 2506, investigating its stellar composition and evolution using advanced spectroscopic techniques with the Giraffe spectrograph at the VLT. Open clusters are intriguing due to their similar distances, ages, and chemical compositions, yet diverse masses, providing valuable data for stellar evolution theories. Our research utilizes data from various observations, aiming for a deeper understanding of the cluster's structure and dynamics. The findings contribute to ongoing discussions regarding cluster membership and physical properties, revealing much yet to explore.

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Spectroscopic Study of Open Cluster NGC 2506: Stellar Evolution Insights

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  1. NGC 2506 – a try for a spectroscopic study Ekaterina Atanasova Petr Kabath Christine Oppegaard Mª Carmen Sánchez Gil Tutor: Frédéric Royer 2nd NEON Archive Summer School 2006

  2. Open clusters – Why are they so interesting? • The members • are all at about the same distance • have approximately the same age • have about the same chemical composition • have different masses Probes for stellar evolution theories

  3. NGC 2506 Right Ascension (2000) : 08 00 01 Declination (2000) : -10 46 12 Galactic longitude : 230.564 Galactic latitude : 9.935 Distance [pc] : 3460 Reddening [mag] : 0.081 Distance modulus [mag] : 12.95 Log Age : 9.045 Metallicity : -0.37 Data from http://www.univie.ac.at/webda/ Open Cluster NGC 2506 Aladin image

  4. Spectroscopic data VLT data was obtained from the ESO Archive • 2004-01-15 Royer/Gomez • 2004-01-17 Royer/Gomez • 2004-02-14 Pallavicini et al • 2005-03-28 Grundahl et. al. • 8 scientific frames The spectra were taken using Giraffe spectrograph mounted on VLT 2 KUYEN Why Giraffe?

  5. FLAMES Instrument • Mounted on KUEYEN • Access to targets over 25' in diam. Spectrographs: • GIRAFFE R=25000 or 10000 - up to 130 targets • UVES Rmax=47000 - only 8 targets

  6. Giraffe - Spectrograph R = 7500 - 30000 Spectral region 370 – 900 nm 2K X 4K EEV CCD (15 µm pix.) Modes: • MEDUSA – 2 modes • IFU • ARGUS ARGUS: 22 times 14 1) 0.52“/microlens 2) 0.3“/microlens IFU: 20 microlenses 0.52“

  7. Possible to observe 132 objects • Resolution: each fiber equals to 1.2“ of the sky • 2 Slits - High resolution • - Low resolution • High resolution mode (HR) - 22 filters • (379 nm to 920.5 nm) • Low resolution mode (LR) - 8 filters • (385.7 nm to 881.7 nm) MEDUSA fibers (Image by ESO) MEDUSA Modes

  8. Giraffe data pipeline 3 flat fields 5 bias frames master flat field Wavelength calibration file master bias Scientific image Scientific image calibrated

  9. Calibration of a scientific frame 1 Raw bias Raw flat Master bias Master flat

  10. Calibration of a scientific frame 2 • Output = (Sci-bias)/(Master flat) • Wavelength calibration with Th-Ar Lamp Some comments • No need of dark subtraction • No flux calibration • No sky subtraction Dispersion axis Cross dispersion axis

  11. Calibrated spectra 2004-02-14

  12. Cross identification of our targets with photometric data 34 objects identified (B-V)marconi=0.032143+0.90548*(B-V)pallavicini Marconi et al., Old open clusters UBGVRI photometry of NGC 2506, MNRAS., 3 June 2006

  13. Science? 2004-02-14 Pallavicini et al. 2004-01-15 Royer/Gomez 2005-03-28 Grundahl et al. Marconi et al.

  14. Radial velocity distribution in the field =2.25206 Mean=82.8379 

  15. To be or not to be …. A member?

  16. Still a lot of work to do….but THANK YOU FOR YOUR ATTENTION:-) Jean FranÇois Petr Christine Carmen Katia

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