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Project NAROO

Project creating a center for measurement and analysis of astronomical photographic plates, emphasizing astrometry, celestial mechanics, and evolving systems.

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Project NAROO

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  1. Project NAROO A New Astrometric Reduction of Old Observations Project of creating a centre for sub-micrometric measurements of astronomical photographic plates and of image analysis J.E. Arlot – CIAS Oct. 14-18, 2015

  2. The project • Making a new reduction of old observations: « observing in the past » • Analyzing old data especially photographic plates • Creating a center for digitizing and analyzing old data but not for saving only old photographic plates • Emphazing the scientific goals: astrometry, celestial mechanics, dynamical systems and evoluting systems with time

  3. The status of old data • More interest for old data in the framework of solar system evolution studies • Several different projects • Archiving • Saving • Photometry • Spectrometry • Work at IMCCE in solar system dynamics and astrometry • Maintaining data bases • Reducing astrometric observational data • Progress of reference star catalogues (UCAC, URAT) • Progress of technology: sub-micrometric scanners • Arrival of the GAIA reference star catalogue

  4. The progresses of astrometry

  5. The star proper motions provided by Gaia will allow to reduce old data with today accuracy

  6. Observational techniques of solar system objects

  7. The present star catalogues

  8. Scientific goals • Observing evoluting events with time (dynamics, photometry) • Extracting new informations from old data • Getting one order of magnitude in accuracy • New scanning machines • New reduction softwares • New reference star catalogues • UCAC2, UCAC4, GAIA, …

  9. Scientific goals Astrometry: • Dissipation of energy because of tides in the planetary satellites system: constraints on the formation of the systems and on the internal structure • Solar system ephemerides extrapolation • Pre-discoveries of NEO and TNO Spectrometry • Pre-discoveries of extra-solar planets in old spectra Photometry • Evolution of the photometry of variable stars (Be stars)

  10. Observing in the past • the number of available plates makes necessary the coordination of this task • selecting plates from scientific purpose • Objects • Period of time • scanning the plates with adapted scanners and optimal criteria (pixel size, accuracy of positioning,…) • reducing them starting with UCAC2 waiting for GAIA • keeping images and distortion parameters for later re-reduction

  11. What are old data? • Photographic plates made from the end of the XIXth century • CCD observations made in the 1980’s • Space astrometric data made in the XXth century • All observations made and reduced before the Gaia catalogue

  12. Old observations1) Photographic plates • Since 1890 • Large or small fields • « Carte du ciel », astrographs, large refractors, Schmidt telescopes

  13. The « Carte du ciel » 33cm astrograph of Bordeaux Observatoryf = 3,43m; scale = 60’’/mm

  14. Greenwich astrographs Refractor 13 inches (1890) f=3m43 Refractor 26 inches (1896) f= 5m44

  15. Long focus astrographs The USNO 61-inch refractor f= 10m; scale = 20 ’’/mm The 38cm refractor of Bordeaux Obs.f = 6,82m; scale = 30’’/mm

  16. Looking for positions of comets one century ago

  17. Jupiter system From « Carte du ciel » instruments with mask with filter

  18. Galilean Satellites of Jupiter (refractor f=10m)  extraction of not « visible » stars

  19. Saturnian system USNO photographic plate taken in the 1970’s; f=10m

  20. Satellites of Mars f=10m

  21. Plates with Mars, Phobos et Deimos Phobos  Deimos

  22. Pre-discoveries of asteroids (NEO, TNO, …)

  23. The criteria of digitization • -Choosing the criteria for digitization • Size of a pixel, photometric dynamic • From negative to positive • Reciprocity curve • Accuracy of positioning (depending on the scanner?)

  24. Photographic plate errors · mapping defects of the optics, · larger scale systematics due to centering errors of the optical system, • effects from the mechanical and darkroom processes, non homogeneous developing, rinsing and drying of the plates. All this can and will produce systematic and random errors of any correlation length (i.e. the emulsion shifts are correlated over mm or cm range). • Reference stars will be used to reduce these errors

  25. Digitizing plates Digitizing a photographic plate may be made: ·      ‘on the fly’ (using a digital detector moving with constant speed in one direction) ·      ‘on the step’ (using a digital detector at rest). The digital detector could be: - a CCD (Charge Coupled Device) - a CMOS (Complementary Metal Oxide Semiconductor) It may have: ·      only one pixel (zero dimensional), ·      a row of pixels (one dimensional) or ·      an array of pixels (two dimensional).

  26. Needs for the project • Digitizing in secure files • High astrometric accuracy (sub-micrometric) • The best choice for the digitizing criteria (resolution, precision, speed, photometric dynamic) • New softwares for analyzing the images and for the reduction

  27. The material • A sub-micrometric digitizing scanner • astrometry vs photometry • high accuracy vs fastness • softwares for extracting information • Collaborations • Other laboratories • Observations outside the solar system • Non astronomical plates

  28. The other projects for digitization • MAMA - observatoire de Paris (1000 nm) • Starscan – U.S. Naval Observatory (500 nm) _____________________________________________________ • Harvard University scanning « Historic Sky Project » (1000 nm) • Pulkovo Fantasy digitizer (1000 nm) • DAMIAN-Royal Observatory of Belgium (70 nm) • Our project NAROO: a sub-micrometric scanner (70 nm) Our project

  29. Preliminary works (1) • Convention with the Royal Observatory of Belgium for using the DAMIAN scanner for test plates « USNO 1967-1998 » • Test of star catalogues (UCAC2, USNO-A2) • Evaluation of errors all along the digitizing process: • Positioning of the plate: 2 nm • Static repeatability • Dynamical repeatability • Distorsion of the optics • Recording on CCD • Converting into fits file • Final precision: 70 nm

  30. Preliminary works (2) • Optimizingdigitizingcriteria • Size of the pixel • Photometricdynamics • Recordingintosecure files • New reduction methods • Extracting the sources • Increase of precisionreferred to the former manualmeasurements • Starting the reductionswith catalogues such as UCAC2,4 or similar (precision 50 mas) • Preparing the reductions with the future catalogues and Gaia (precision < 1 mas)

  31. The selection of old data to bere-reduced Example: using the database of natural satellites to select the old data to bere-reduced • Satellites of Mars: 3000 observations from 1877 to 1988 (14 per year per satellite) Need to digitize plates from 1990’s in order to avoid gap • Galilean satellites of Jupiter: 12000 observations from 1891 to 2001 (27 observations per year per satellite) Need to digitizeold plates from 1890’s in order to improveold data and all un-reduced observations Need to reduced data in intersatellitesinto RA and DEC • Main satellites of Saturn 50641 observations from 1874 to 2003 (49 observations per year per satellite) Need to digitize plates from 1920’s to avoid gaps Need to reduced data in intersatellitesinto RA and DEC

  32. Choosing a digitizing machine (1) - Airbearing XY-table, with cooled CMOS camera. - Power LED illumination in transmission mode. - Grayscale images. - Sizes up to : 350 mm x 350 mm sheets or plates; - Resolution: 7µm x 7µm pixels , (3620 dpi). - Geometric final accuracy: 0.07µm. - Scan speed: 24cm x 24cm image in less than 10 min. - Data stream: 10 MB/s. • Production: 24 x 7, maintenance < 5%.

  33. Choosing a digitizing machine (2) - Automatic conversion of analogue images into digital images. - Post processing and data extraction in near real time. - Distributed software and hardware architecture. - Climatised clean room and archive room (20°  0.1° C, 50%  1% RH)

  34. The machine successfully tested in Belgium Bench marks with USNO plates

  35. Preliminary works • Identification of interesting targets • Icy Satellites • Irregular Satellites • Pre-décoveries of NEO and TNO • Inventory of accessible plates • Large number of available plates (until 200 000 plates) • Plates with a field from a few minutes of degree to several degrees • Plates from 1890 withmetadata • Plates in good shape

  36. Inventory Pulkovo observatory

  37. Inventory objects (Pulkovo obs.) • Saturn and its satellites –800 plates (1972 -2007). • Jupiter and Galilean satellites –500 plates (1976 –2005). • Mars –763 plates (1960 -1988). • Uranus and its satellites –250 plates (1910-2004). • Neptune –237 plates (1899 -1955). • Pluto –272 plates (1930 –1994) • 18 selected asteroids –2655 plates (1949-2004)

  38. Small plates, Greenwich 1897-1898 Small plates, Franklin Adams Greenwich Astrographic 'D' 26 inch Small plates Small plates, Radcliffe 36 inch B dome focus test plates, Saturn fields 24 inch Maclean Wide angle plates, B, Y and V, various fields 24 inch Radcliffe, KA, South Africa, B & V plates Cape 40 inch astrometric camera, V plates, various fields I and III Cordoba plates Cape plates Special South African Kapetyn Area Plates Cape Astrographic plates Cape Maclean twin 24 and 18 inch, BV and a few P Radcliffe notebooks / proper m. / Hartmann cards Cape Overlap CPC2 Greenwich 13 inch Astrographic plates Herstmonceux 13 inch Astrographic plates Greenwich 13 inch Astrograph notebooks Oxford Astrographic plates Moon 16cm plates Inventory: Greenwich observatory Curtis Schmidt / Cerro Tololo Stonyhurst Discs, 8.5 inch, 4 boxes Small glass Kottamia Spectra 8, Radcliffe Spectra 2 and 65 AAO Schmidt plates Observation cards 16cm Eros Series plates 16cm INT Astrograph INT Small Plates 30 inch in 26 inch dome 30 inch in 26 inch dome, Spectra Spectra 36 inch I and III Prism slit spectrographs Slitless 36 inch spectrograph Various Reseaux scale etc, No3 sq yellow filter and copies Miscellaneous, Ottawa Rotation spectra, spot and eclipse spectra 16cm, 30 inch Greenwich 16cm, 26 inch Greenwich Observers books 16cm, 26 inch - 4 unnumbered Greenwich notebooks Thompson Equatorial & Astrographic Equatorial logbooks 16cm, 26 inch Herstmonceux

  39. The first results • Scan test with DAMIAN (scanner at the Royal Observatory of Belgium)) • 506 plates of the Galilean satellites made from 1967 until 1998 at the USNO (Washington DC) • 425 plates of the Martian satellites made from1967 to 1997 at the USNO • 526 plates of the satellites of Saturn made from 1974 to 1998 • Use of UCAC2 and UCAC4 • Comparison with former reductions • Results • on the X,Y (Galileans)  precision of 30 mas instead of 100 mas • on the a and d (Galileans)  positions of Jupiter, precision 60 mas where reduction was not possible

  40. Testing the quality of the planet Jupiter ephemeridesusing USNO platesMeanresidual in a and in d and dispersion (in mas) (1967-1998) 2200 observations from 1967 to 1998 Results using the UCAC2 catalogue

  41. The Martian system: residuals and dispersion INPOP10 for Mars and IMCCE for the satellites DE423 for Mars and JPL MAR097 for the satellites 777 observations made from 1967 to 1997 Results using the UCAC2 catalogue

  42. Results on Martian USNO plates: relative RA/IMCCE Martian satellites ephem.

  43. Results on Martian USNO plates: RA/INPOP10

  44. The first results for the Saturnian satellites in RA and DEC Residuals in RA and DEC are calculated using INPOP10 for Saturn and the JPL SAT351 ephemeris for the satellites Results using the UCAC2 catalogue

  45. 2) CCD observations • CCD observations made in the 1980’s are « old » observations • The astrometric reduction was difficult due to small fields important progress with a new reduction

  46. CCD observations are old observations… CCD observations of Dione, Tethys and the Lagrange L4 librators Helene and Telesto with the Flagstaff 61-inch telescope

  47. CCD observations The large satellites: the Eight main satellites of Saturn Not enough stars due to the short exposure because of the brightness of the satellites

  48. CCD observations of the Uranian satellites  CCD observation (small field) •  For the Uranian system, the unknown precession is reachable through the observation of the satellites (very time dependant)

  49. The irregularouter satellites of the giantplanets  • Outer satellites of Jupiter: two families • Scanner les plaques de Schmidt?

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