Transit of Venus Observations From National Solar Observatory

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Transit of Venus Observations From National Solar Observatory. National Solar Observatory Facilities. Dunn Solar Telescope Sunspot, New Mexico, USA D = 76cm, λ =380-1700 nm. McMath-Pierce Telescope Kitt Peak, Arizona, USA D = 160 cm, λ =1000-5000 nm. Transit Conditions – Sacramento Peak. - PowerPoint PPT Presentation

Transcript of Transit of Venus Observations From National Solar Observatory

  • Transit of Venus ObservationsFrom National Solar Observatory

  • National Solar Observatory FacilitiesDunn Solar TelescopeSunspot, New Mexico, USAD = 76cm, =380-1700 nmMcMath-Pierce TelescopeKitt Peak, Arizona, USAD = 160 cm, =1000-5000 nm

  • Transit Conditions Sacramento Peak

  • Interferometric BIdimensional Spectrometer (IBIS)Dual Fabry-Perot Imaging SpectrometerP.I. - Fabio Cavallini (INAF/Arcetri)Facility Instrument at the NSO/Dunn Solar Telescope since 2005Publication List: http://tinyurl.com/ibis-pubsInstrument Design: Cavallini, F., 2006, Solar Phys., 236, 415.Spectral Profile: Reardon, K., Cavallini, F., 2008, A & A, 481, 897.MTF: Righini, A., Cavallini, F., Reardon, K., 2010, A & A, 515, 85.References

  • Spectral Range: 5400 - 8600 FWHM:20-45 mFOV:98 x 98 arcsecPixel Size: 0.098 arcsec2/pixelExposure Times:20-50 msecStrehl Ratio: ~0.95Frame Rate: 8 12 frames/secData Rate: 100 GB/hour (two CCDs)

    Application of post-facto image correction techniques: Destretching Speckle Reconstruction Multi-Object Multi-Frame Blind DeconvolutionAvailable FiltersInterferometric BIdimensional Spectrometer (IBIS)Spectral resolution ~200,000 260,000

  • Mercury Transit 06 November 2006H Imaging at IngressIBIS/DST

  • Mercury Transit 06 November 2006 IBIS/DSTImaging Spectroscopy of planetary transitNa D2 589.0 nm : Scan range = 1.5 : = 0.009 0.083 arcsec/pixel

  • EquivalentWidthGaussianWidthGaussianAmplitudeGaussianShiftMercury Transit 06 November 2006IBIS/DST Observations of Mercury Exosphere in Na D2

  • IBIS Field of View98 x 98 arcsecMercuryd=10

  • 98 x 98 arcsecVenusD=60IBIS Field of View

  • Upper wavelength limit of 8700 Need strongest line to improve SNRNeed to minimize contamination from other solar or terrestrial spectral linesPascal Hedelt simulated Venus CO2 absorption spectrum from 780 4500 nmCompared simulated spectrum (corrected from vacuum to air wavelengths!) to solar atlas

    Spectral Line Selection for IBIS

  • Solar + terrestrial atlas spectrumSimulated Cytherian CO2 spectrumSpectra at 870 nm Noisy Continuum!

  • Solar, Terrestrial, Cytherian Spectra 780 nmSolar + terrestrial atlas spectrumSimulated Cytherian CO2 spectrum

  • Solar + terrestrial atlas spectrumSimulated Cytherian CO2 spectrumIBIS Prefilter ProfileSolar, Terrestrial, Cytherian Spectra

  • Imaging of AureoleRapid Oscillations of the Solar Atmosphere (ROSA)http://star.pst.qub.ac.uk/rosa/

    Six Andor 1000 x 1000 pixel CCDs, 30 frames/sec sustained+ image reconstruction techniques

    Will use ROSA to take multiwavelength observations (380 500 nm) at high cadence during ingress

    Look for wavelength dependence of aureole due to scattering processesPossible addition of 2k x 2k, 50 fps detectorFor higher cadence and resolution

  • Facility Infrared Imaging Spectrograph(FIRS)Spectral coverage: ~60 (/250)Slit lengthSlit scanningFull Stokes SpectropolarimetryObserve same spectral interval as Hedelt et al. 2011?

  • McMath-Pierce TelescopeNSO Array Camera (NAC) 1024 x 1024, helium cooled, InSb array

    Spectral Range: 1.6 2.5 m, 4.67 mSpectral Resolution: ~50,000 70,000Spectral coverage: ~60

    Full Stokes SpectropolarimetrySpectral interval(s) to observe?1.6 and/or 2.2 m bands

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