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 . . . Victoria Meadows, Eddie . Schwieterman. , . Giada. . Arney. , Drake Deming. ,. . Amit. . Misra. , Benjamin . Charnay. , Ty Robinson, . Antigona. Segura, Shawn. . JWST Community Lecture. Jay Anderson, STScI. Nov 29, 2016. Astrometric Calibration. What is Distortion?. Any “non-conformal” mapping . . (shift, scale, rotation). Linear terms (“skew”). Non-linear terms. 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) . Kristin Benke. ISMS. . 2017. Ultrafast tabletop XUV spectroscopy. 2. 3p. 6. 3d. n. . 3p. 5. 3d. n 1.  . High harmonic generation (HHG). Gas-filled cell. . NIR laser. Popmintchev. , T., . et. al. Proc. Natl. Acad. Sci.. 2. UV Spectroscopy. Introduction. UV radiation and Electronic Excitations. The difference in energy between molecular bonding, non-bonding and anti-bonding orbitals ranges from 125-650 kJ/mole. This energy corresponds to EM radiation in the ultraviolet (UV) region, 100-350 nm, and visible (VIS) regions 350-700 nm of the spectrum. 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. Ottillia Ni. Mentor: Dr. . Kristan. Corwin. August . 5, 2016. Motivation. Expand gas. -filled hollow fiber references . to 1.6 microns wavelengths.. Absorption spectroscopy and sub-Doppler spectroscopy in methane-filled hollow fibers. 1 IR-Spectroscopy IR region The part of electromagnetic radiation between the visible and microwave regions 0.8  m to 50  m ( 12,500 cm -1 - 200 cm -1 ) is called IR region Most interested region in Infrared Spectroscopy is between 2.5 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 . 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. .