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First Light with the Echelon-‐Cross-‐Echelle Spectrograph on SOFIA
Future Flights and Observing Availability • EXES final three commissioning flights will occur between 17-‐24 February 2015, followed by one
Cycle 2 science flight and two Cycle 3 science flights. Twelve Cycle 3 science flights are scheduled for August/September 2015.
• Cycle 4 proposals will be due in Summer 2015. • Proposals for Directors DiscrePonary Time (e.g. comets, Jovian storms) are accepted at any Pme. hTps://www.sofia.usra.edu/Science/proposals/DDT/instrucPons.html • EXES exposure Pme calculator with sensiPviPes and realisPc depicPon of spectral modes hTp://irastro.physics.ucdavis.edu/exes/etc/ • Proposers are encouraged to contact EXES team for advice and assistance.
MaThew Richter mjrichter@physics.ucdavis.edu or CurPs DeWiT curPsdewiT@gmail.com
CurPs DeWiT1,2, MaThew J. Richter1, KrisPn Kulas3,2, Mark E. McKelvey2, Michael E. Case1,, William Vacca4, Melanie Clarke4, Thérèse Encrenaz5, Thomas Greathouse6, Graham Harper7, Robert McMurray2
1 UC Davis Department of Physics, 2 NASA Ames Research Center, 3 Santa Clara University 4 University Space Research Association (USRA), 5 Observatoire Paris-Site de Meudon, 6 Southwest Research Institute (SwRI), 7 Trinity College Dublin
H2 emission maps of Jupiter’s stratosphere
Aluminum R10 echelon graPng for EXES (40” x 4”)
What is EXES? • Mid-‐IR High-‐ResoluPon spectrograph for SOFIA • 1024 x 1024 Si:As detector • 4.5 -‐ 28.3 μm range • 0.5-‐4% spectral coverage per sekng, depending on choice of cross-‐disperser and spaPal slit length • Three spectral modes: high (R=100,000) medium (R=15000) and low (R=3000) • Observing modes: nodding & mapping
References
DeWiT et al., "Preflight performance of the Echelon-‐Cross-‐Echelle spectrograph for SOFIA," Ground-‐based and Airborne InstrumentaPon for Astronomy IV, Ian S. McLean, Suzanne K. Ramsay, & Hideki Takami Editors, Proc. SPIE 8446, 84461A (2012) Richter et al., "Status of the Echelon-‐cross-‐Echelle Spectrograph for SOFIA," Ground-‐based and Airborne InstrumentaPon for Astronomy III, Ian S. McLean, Suzanne K. Ramsay, & Hideki Takami, Editors, Proc. SPIE 7735, 77356Q (2010)
• R=55,000 maps of Jupiter at H2 S(0) 28.3 μm and H2 S(1) 17.0 μm, achieved by stepping slit posiPon across planet disk.
• H2 Para/Ortho state raPo when paired with CH4 temperature gives a measure of mixing into the stratosphere.
Commissioning in April 2014 EXES successfully executed its first commissioning flights on April 7 and 9th, 2014. We targeted 11 sources in high-‐resoluPon mode and 15 different wavelength sekngs. Targets included Mars, Jupiter, telluric calibrators, AFGL 2591 and a number of IR standard K and M giants. Commissioning will be completed in February 2015, tesPng and characterizing the medium-‐ and low-‐resoluPon modes as well as honing our overhead management and improving spectral focus and throughput.
23” slit length and 0.7% wavelength coverage
4” slit length and 2.5% wavelength coverage
Unresolved Jovian C2H2 lines at 13.7 μm,
R=75,000 with 1.9” slit. 4/9/14
H2O and HDO abundance maps on Mars at 7.2 μm • H2O and HDO lines acquired simultaneously for D/H map over one hemisphere; previous studies found a global Mars D/H value 5 x higher than Earth, but it is expected to vary regionally.
• R=85,000 on unresolved CO2 lines with 1.44” slit.
7.2 μm conPnuum map of Mars. Image is 21” x 24.5” composed from two scans with slit length of 14”. FWHMPSF = 3.4”
EXES spectrum of total Mars disk (blue). Models of telluric transmission and MarPan molecular absorpPon are offset and color-‐coded by species.
Preliminary SensiPviPes at 17.0 and 28.2 μm 17.0 μm, per pixel : 0.1 for 1 σ : 1 sec NEFD 17.0 μm, per : 0.03 for 1 σ : 1 sec NEFD resoluPon element
28.2 μm, per pixel : 0.5 for 1 σ : 1 sec NEFD 28.2 μm, per : 0.2 for 1 σ : 1 sec NEFD resoluPon element
ergss cm2cm−1SR
ergss cm2cm−1SR
ergss cm2cm−1SR
ergss cm2cm−1SR
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