PPT-JWST Spectroscopy

of transiting planets Drake Deming University of Maryland at College Park K2 Science Conference November 5 2015 In the early days of transiting planets we were interested in what JWST could . R. epeatability. WFC3 – spatial . s. can mode analysis – . work in progress. Mark Swain, Pieter . Deroo. , . Kiri. . Wagstaff. IPAC . JWST workshop . 3/11/14. Jet Propulsion Laboratory, California Institute of Technology. . . Victoria Meadows, Eddie . Schwieterman. , . Giada. . Arney. , Drake Deming. ,. . Amit. . Misra. , Benjamin . Charnay. , Ty Robinson, . Antigona. Segura, Shawn. . Goddard Space Flight Center, Greenbelt MD. Joint Base Andrews, MD. Johnson Space . Center,. Houston TX. Northrop-Grumman, Los Angeles CA. Panama Canal. ESA Kourou, French Guiana. L2. JWST. Road to. The stars. Mandell. NASA GSFC. Collaborators. :. Korey. Haynes. Evan . Sinukoff. Drake . Deming. Adam Burrows. Nikku. . Madhusudhan. Mark . Clampin. Don . Lindler. Natasha . Batalha. Heather Knutson. (others as well) . 12. th. International User Meeting on Cavity Enhanced Spectroscopy, 13 June, 2017. 1A12. Charles R. Markus. , Jefferson E. McCollum, Thomas S. Dieter, Philip A. . Kocheril. , and Benjamin J. McCall. Fall . 2017. First Order Spectra. For a spectrum to be 1. st. order, the . D. n. between the chemical shifts of any given pair of nuclei must be much larger than the value of the coupling constant . NIRCam. Grism Mode for Transit Observations. C. Beichman, Dimitra . Touli. ,. Gautam . Vasisht. , Roger Smith. Tom Greene. 4 March 2014. JWST grism simulator. 1. Caltech Detector Testbed. Caltech testbed (Roger Smith) projects simulated spectra and other images onto HgCdTe array to assess precision photometry for transits, weak lensing, etc. for Explorer concepts, JWST, WFIRST, EUCLID. Piet Van Duppen. ISOLDE CERN, Switzerland. IKS-. K.U.Leuven. , Belgium. K.U. Leuven. University of Western Scotland, U.K. - . K.U.Leuven. , Belgium - SCK-CEN-Mol, Belgium - . U.Gent. , Belgium - . Commenius. JWST:Coronagraphy. 2. High Contrast Imaging allows observing. Extended emission. surrounding stars. Debris disks. AGN. . hosts. Faint companions. High contrast imaging combines the suppression of light from the host (“optical cancellation”) with post-processing by subtracting the scaled point-spread function (PSF) from the science image. Space . Telescope. John . Mather . JWST . Senior Project Scientist . AAAC Oct 13 2011. JWST . Science Updates. 4 (. original) . major themes: first light, galaxy assembly, star & planet formation, evolution of planetary systems. 40 Balmer jump and slopes 4000 age Very young population x0000- emission lines UV slopes Old star populations in high-z objects eg Egami et al 2005 Eyles et al 2005 Richard et al 2011 Zeng e 2. Nuclear Magnetic Resonance Spectroscopy. After hydrogen, the most useful atom providing information is carbon-13.. The . overall intensity of a . 13. C signal is about 6400 . times . less than the intensity of an . Marie-Laure Mauborgne. SLB. CSG17 – July 17. th. 2023. 1. Founded by a physicist and an engineer in 1926 to conduct the first geophysical measurements of rock formations . What is SLB?. (former Schlumberger). contained in this document is subject to export controls under the International Traffic in Arms Regulations (Title 22, CFR . Presented by Basil Jeffers. JWST Project Lead EEE Parts Engineer. JWST Worldwide Team/Partners. .