Transit of Venus Observations From National Solar Observatory

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