1 / 17

Transit of Venus Observations From National Solar Observatory

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.

jody
Download Presentation

Transit of Venus Observations From National Solar Observatory

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Transit of Venus Observations From National Solar Observatory

  2. 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

  3. Transit Conditions – Sacramento Peak

  4. Interferometric BIdimensional Spectrometer (IBIS) Dual Fabry-Perot Imaging Spectrometer P.I. - Fabio Cavallini (INAF/Arcetri) Facility Instrument at the NSO/Dunn Solar Telescope since 2005 Publication List: http://tinyurl.com/ibis-pubs Instrument 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

  5. Interferometric BIdimensional Spectrometer (IBIS) • Spectral Range: 5400 - 8600 Å • FWHM: 20-45 mÅ • FOV: 98 x 98 arcsec • Pixel Size: 0.098 arcsec2/pixel • Exposure Times: 20-50 msec • Strehl Ratio: ~0.95 • Frame Rate: 8 – 12 frames/sec • Data Rate: ≥ 100 GB/hour (two CCD’s) • Application of post-facto image correction techniques: • Destretching • Speckle Reconstruction • Multi-Object Multi-Frame Blind Deconvolution Spectral resolution ~200,000 – 260,000 • Available Filters • 543.4 – Fe I [g=0] • 617.3 – Fe I (SDO/HMI) • 630.1/630.2 – Fe I • 676.8 – Ni I (MDI ; GONG) • 709.0 – Fe I [g=0] • 722.4 – Fe II [g=0] • 587.6 – He I D3 • 589.0 – Na D2 • 589.6 – Na D1 • 656.3 – Ha • 854.2 – Ca II

  6. Mercury Transit – 06 November 2006 Hα Imaging at Ingress IBIS/DST

  7. Mercury Transit – 06 November 2006 – IBIS/DST Imaging Spectroscopy of planetary transit Na D2 589.0 nm : Scan range = 1.5 Å : Δλ = 0.009 Å 0.083 arcsec/pixel

  8. Mercury Transit – 06 November 2006 IBIS/DST Observations of Mercury Exosphere in Na D2 Equivalent Width Gaussian Amplitude Gaussian Shift Gaussian Width

  9. IBIS Field of View Mercury d=10” 98 x 98 arcsec

  10. IBIS Field of View Venus D=60” 98 x 98 arcsec

  11. Spectral Line Selection for IBIS • Upper wavelength limit of 8700 Å • Need strongest line to improve SNR • Need to minimize contamination from other solar or terrestrial spectral lines • Pascal Hedelt simulated Venus CO2 absorption spectrum from 780 – 4500 nm • Compared simulated spectrum (corrected from vacuum to air wavelengths!) to solar atlas

  12. Spectra at 870 nm – Noisy Continuum! Solar + terrestrial atlas spectrum Simulated Cytherian CO2 spectrum

  13. Solar, Terrestrial, Cytherian Spectra – 780 nm Solar + terrestrial atlas spectrum Simulated Cytherian CO2 spectrum

  14. Solar, Terrestrial, Cytherian Spectra IBIS Prefilter Profile Solar + terrestrial atlas spectrum Simulated Cytherian CO2 spectrum

  15. Imaging of Aureole Rapid Oscillations of the Solar Atmosphere (ROSA) http://star.pst.qub.ac.uk/rosa/ Six Andor 1000 x 1000 pixel CCD’s, 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 processes Possible addition of 2k x 2k, 50 fps detector For higher cadence and resolution

  16. Facility Infrared Imaging Spectrograph(FIRS) Full Stokes Spectropolarimetry Slit scanning Slit length Spectral coverage: ~60 Å (λ/250) Observe same spectral interval as Hedelt et al. 2011?

  17. McMath-Pierce TelescopeNSO Array Camera (NAC) Full Stokes Spectropolarimetry 1024x 1024, helium cooled, InSb array Spectral Range: 1.6 –2.5 μm, 4.67 μm Spectral Resolution: ~50,000 – 70,000 Spectral coverage: ~60 Å Spectral interval(s) to observe? 1.6 and/or 2.2 μm bands

More Related