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Processing Status

Processing Status. June 2009. Mary Williams Padova Meeting, 11/06/09. Talk Outline. Archive status Data flow New Status Reports Zero-points FP3 Stellar parameters: temperatures. Mary Williams Padova Meeting, 11/06/09. Archive status. As of 9th June 2009 285,503 spectra

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Processing Status

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  1. Processing Status June 2009 Mary Williams Padova Meeting, 11/06/09

  2. Talk Outline • Archive status • Data flow • New Status Reports • Zero-points • FP3 • Stellar parameters: temperatures Mary Williams Padova Meeting, 11/06/09

  3. Archive status • As of 9th June 2009 • 285,503 spectra • Last date in internal and reduced archives: 20090328 • Last date in raw archive: 20090328 Mary Williams Padova Meeting, 11/06/09

  4. Sky Coverage First year data Mary Williams Padova Meeting, 11/06/09 25,689 RVs, ~4,500 deg2

  5. Sky Coverage Second year data Mary Williams Padova Meeting, 11/06/09 26,906 RVs, ~5,000 deg2

  6. Sky Coverage Third year data Mary Williams Padova Meeting, 11/06/09 37,292 RVs, ~8,800 deg2

  7. Sky Coverage Fourth year data Mary Williams Padova Meeting, 11/06/09 87,261 RVs, ~17,200 deg2

  8. Sky Coverage Fifth year data Mary Williams Padova Meeting, 11/06/09 41,002 RVs, ~11,000 deg2

  9. Sky Coverage Sixth year data Mary Williams Padova Meeting, 11/06/09 59,945 RVs, ~11,000 deg2

  10. Sky Coverage Full database Mary Williams Padova Meeting, 11/06/09 218,100 RVs, ~32,000 deg2

  11. Current data flow Problem fields Reduction problem fields SSO AAO (Warren) Padova Reduction (Alessandro) 3-4 days Fortnightly Fortnightly AIP archive Eyeballing of spectra (Rachel, Tomaz, Gal, Paola) AIP Archive Mary Williams Padova Meeting, 11/06/09 Complete to Dec 2007 Weekly AIP Processed Data Archive Irregular AIP Pipeline (Mary) 1/2 week Internal release (at AIP) Last release complete to March 2009

  12. New status reports Mary Williams Padova Meeting, 11/06/09

  13. New status reports Mary Williams Padova Meeting, 11/06/09

  14. New status reports Mary Williams Padova Meeting, 11/06/09

  15. New status reports Mary Williams Padova Meeting, 11/06/09

  16. New status reports Mary Williams Padova Meeting, 11/06/09

  17. Zero-points • What are they? • Temperature fluctuations cause shift in wavelength between science frames and arc frames • Mostly of the order of a 1-5 km/s • We correct with zero-point RVcorrection • ZeroPointQualityFLAG denotes quality of zero-point correction - mostly!! Mary Williams Padova Meeting, 11/06/09

  18. Zero-points • How do we calculate the correction? Un-sky subtracted spectra from single fibre Sky template  Mary Williams Padova Meeting, 11/06/09 SkyRV, eSkyRV, R for single fibre THEN….

  19. Zero-points • THEN we do a polynomial fit across the field SkyRV and eSkyRV Exclusive sky fibre Weight by R value (weight=5xR) Mary Williams Padova Meeting, 11/06/09 Threshold of R=5 The fit gives RVcorrection

  20. Zero-points • ZeroPointQualityFLAG gives the quality of the fit • 1st character: FIELD fit quality • Dispersion between SkyRV - RVcorrection • 2nd character: Sub-group fit quality • Dispersion between SkyRV - Rvcorrection for regions 1-50, 51-100, 101-150 • *: If interval between usable sky velocities > 15 Mary Williams Padova Meeting, 11/06/09

  21. Zero-points • The fit can sometimes be very bad… It can become unbound if there are insufficient fibres with R>5 Mary Williams Padova Meeting, 11/06/09 Fiorangela La Forgia

  22. Zero-points • Sometimes bad zero-points are hard to spot • X-correlation with sky has |50| km/s limit • If outside those bounds • SkyRV=0, eSkyRV=0 or large, R<0.1 • The RVs for such spectra can be wrong by as much as 100 km/s! • Affects small number of fields • These data are removed from the database Mary Williams Padova Meeting, 11/06/09

  23. Zero-points • The other bad fits are hand corrected • All zero-points fits are eyeballed • Those with unbound fits are manually corrected • New flagging of affected spectra: • ZeroPointQualityFLAG=‘M’ • However, there has been an increase in problem fields… Mary Williams Padova Meeting, 11/06/09 Fiorangela La Forgia

  24. Zero-points • There were a number of causes of this increase • Shift to brighter stars, lower exposure time • Exposure times increased back again • Poor placement of sky fibres • More care taken • Deterioration of fibres meaning lower S/N • FP3 There is a backlog of correcting these fits manually • Be wary if |RVcorrection| > 10 km/s or *! • If find some high RV stars, check fellow fibres Mary Williams Padova Meeting, 11/06/09

  25. Zero-points • Correlation between RV and SkyRV • Caused by underlying stellar spectrum “tugging” on sky correlation • Not a problem for zero point calibration IF there is no mean offset in stellar RVs for one field…BUT… Mary Williams Padova Meeting, 11/06/09

  26. Zero-points • There might be such a issue • Whole fields have have • a non-zero mean RV • Causes shift in Rvcorrection • of the order of a couple • of kms-1 • Work in progress Mary Williams Padova Meeting, 11/06/09

  27. Field Plate 3 • The first 8 FP3 fields • New stiffer cabling used - potential problems! • Check stability of SkyRV Mary Williams Padova Meeting, 11/06/09 Grey : R < 5 Black: R > 5

  28. Field Plate 3 • Stability of SkyRV for R > 5 • FP3: (SkyRV)=-0.5 kms-1, (SkyRV)=1.9 kms-1 • FP1: (SkyRV)=-0.4 kms-1, (SkyRV)=2.9 kms-1 • FP2: (SkyRV)=-0.4 kms-1, (SkyRV)=2.2 kms-1 Mary Williams Padova Meeting, 11/06/09

  29. Field Plate 3 • Some of the fields include repeat observations Mary Williams Padova Meeting, 11/06/09 All but one field look good

  30. Field Plate 3 • The problem field was one of the earlier ones Mary Williams Padova Meeting, 11/06/09 So ignoring this field and |RV(FP3) - RV(previous)| < 20 kms-1

  31. Field Plate 3 • Stability of SkyRV for R > 5 • FP3: (RP3 RV-previous RV)=-0.5 kms-1 • 68.2%:=1.1 kms-1 95%:=2.3 kms-1 • ALL: (RP3 RV-previous RV)=+0.2 kms-1 • 68.2%:=1.4 kms-1 95%:=3.8 kms-1 Mary Williams Padova Meeting, 11/06/09

  32. Stellar Parameters • Comparing RAVE temperatures to others • To spot any possible systematic in RAVE temperatures • Use a variety of reference temperatures: • Photometric: V-K using Ramirez calibrations with reddening corrections and constraints • Jon’s spectroscopic temperatures: excitation balance • Soubiran and Girard temperatures: photometric, excitation balance, H • Cayrel compilation temperatures: photometric, H • Thus we have a broad range of methods to compare our temperature calculations to Mary Williams Padova Meeting, 11/06/09

  33. Stellar Parameters • There is a significant systematic for the dwarfs Mary Williams Padova Meeting, 11/06/09 GREEN - V-K photometric BLACK-Jon’s calculation CYAN- Soubiran and Girard PURPLE - Cayrel

  34. Stellar Parameters • It remains at higher S/N values Mary Williams Padova Meeting, 11/06/09 GREEN - V-K photometric BLACK-Jon’s calculation CYAN- Soubiran and Girard PURPLE - Cayrel

  35. Summary • Processing continuing as normal • New status reports to aid dissemination of data and identification of problems • Zero-points • Removal of bad fields • Manual refitting backlog: watch out! • Possible problem with star RV correlation - investigating • FP3 • Sky RVs good • Repeats good, apart from mean offset - investigating • New report out soon • Possible temperature systematic Mary Williams Padova Meeting, 11/06/09

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