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  • Other Sources  (5)
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  • 1
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    Lambda Equals 2.4 - 5 Micron Spectroscopy with the JWST NIRCam Instrument (2017)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The James Webb Space Telescope near-infrared camera (JWST NIRCam) has two 2'2 x 2'2 fields of view that can be observed with either imaging or spectroscopic modes. Either of two R ~1500 grisms with orthogonal dispersion directions can be used for slitless spectroscopy over lambda = 2.4 - 5.0 microns in each module, and shorter wavelength observations of the same fields can be obtained simultaneously. We describe the design drivers and parameters of the grisms and present the latest predicted spectroscopic sensitivities, saturation limits, resolving powers, and wavelength coverage values. Simultaneous short wavelength (0.6 -- 2.3 microns) imaging observations of the 2.4 -- 5.0 microns spectroscopic field can be performed in one of several different filter bands, either in-focus or defocused via weak lenses internal to NIRCam. The grisms are available for single-object time series spectroscopy and wide-field multi-object slitless spectroscopy modes in the first cycle of JWST observations. We present and discuss operational considerations including subarray sizes and data volume limits. Potential scientific uses of the grisms are illustrated with simulated observations of deep extragalactic fields, dark clouds, and transiting exoplanets. Information needed to plan observations using these spectroscopic modes are also provided.
    Keywords: Astronomy
    Type: Paper 17010P , ARC-E-DAA-TN43262 , Journal of Astronomical Telescopes, Instruments, and Systems (ISSN 2329-4124) (e-ISSN 2329-4221); 3; 3; 035001
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  • 2
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    Lambda = 2.4 to 5 Micron Spectroscopy with the James Webb Space Telescope NIRCam Instrument (2017)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The James Webb Space Telescope near-infrared camera (JWST NIRCam) has two 2'2 x 2'2 fields of view that can be observed with either imaging or spectroscopic modes. Either of two R approx.1500 grisms with orthogonal dispersion directions can be used for slitless spectroscopy over lambda = 2.4 - 5.0 microns in each module, and shorter wavelength observations of the same fields can be obtained simultaneously. We describe the design drivers and parameters of the grisms and present the latest predicted spectroscopic sensitivities, saturation limits, resolving powers, and wavelength coverage values. Simultaneous short wavelength (0.6 - 2.3 microns) imaging observations of the 2.4 - 5.0 microns spectroscopic field can be performed in one of several different filter bands, either in-focus or defocused via weak lenses internal to NIRCam. The grisms are available for single-object time series spectroscopy and wide-field multi-object slitless spectroscopy modes in the first cycle of JWST observations. We present and discuss operational considerations including subarray sizes and data volume limits. Potential scientific uses of the grisms are illustrated with simulated observations of deep extragalactic fields, dark clouds, and transiting exoplanets. Information needed to plan observations using these spectroscopic modes are also provided.
    Keywords: Astronomy
    Type: ARC-E-DAA-TN43297 , Journal of Astronomical Telescopes, Instruments, and Systems (ISSN 2329-4124) (e-ISSN 2329-4221); o 3; 3; 035001
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  • 3
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    Lambda = 2.4 - 5 Micron Spectroscopy With the James Webb Space Telescope NIRCam Instrument (2017)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The James Webb Space Telescope near-infrared camera (JWST NIRCam) has two 2.2' x 2.2' fields of view that can be observed with either imaging or spectroscopic modes. Either of two R 1500 grisms with orthogonal dispersion directions can be used for slitless spectroscopy over 2.4 - 5.0 microns wavelength in each module, and shorter wavelength observations of the same fields can be obtained simultaneously. We describe the design drivers and parameters of the grisms and present the latest predicted spectroscopic sensitivities, saturation limits, resolving powers, and wavelength coverage values. Simultaneous short wavelength (0.6 -- 2.3 microns) imaging observations of the 2.4 -- 5.0 microns spectroscopic field can be performed in one of several different filter bands, either in-focus or defocused via weak lenses internal to NIRCam. The grisms are available for single-object time series spectroscopy and wide-field multi-object slitless spectroscopy modes in the first cycle of JWST observations. Potential scientific uses of the grisms are illustrated with simulated observations of deep extragalactic fields, dark clouds, and transiting exoplanets. Information needed to plan observations using these spectroscopic modes are also provided.
    Keywords: Instrumentation and Photography
    Type: ARC-E-DAA-TN44370 , Journal of Astronomical Telescopes, Instruments, and Systems (ISSN 2329-4124) (e-ISSN 2329-4221); 3; 3; 035001
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  • 4
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    The Gray Needle: Large Grains in the HD 15115 Debris Disk from LBT*/PISCES/K s and LBTIi+/LMIRcam/L(prime) Adaptive Optics Imaging (2012)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: We present diffraction-limited K s band and L(prime) adaptive optics images of the edge-on debris disk around the nearby F2 star HD 15115, obtained with a single 8.4 m primary mirror at the Large Binocular Telescope. At the Ks band, the disk is detected at signal-to-noise per resolution element (SNRE) approx. 3-8 from approx. 1 to 2".5 (45-113 AU) on the western side and from approx. 1". 2 to 2".1 (63-90 AU) on the east. At L the disk is detected at SNRE approx. 2.5 from approx. 1 to 1".45 (45-90 AU) on both sides, implying more symmetric disk structure at 3.8 micrometers. At both wavelengths the disk has a bow-like shape and is offset from the star to the north by a few AU. A surface brightness asymmetry exists between the two sides of the disk at the Ks band, but not at L(prime). The surface brightness at the K s band declines inside 1"(approx. 45 AU), which may be indicative of a gap in the disk near 1".The K s L(prime) disk color, after removal of the stellar color, is mostly gray for both sides of the disk. This suggests that scattered light is coming from large dust grains, with 3-10 micrometers sized grains on the east side and 1-10 micrometers dust grains on the west. This may suggest that the west side is composed of smaller dust grains than the east side, which would support the interpretation that the disk is being dynamically affected by interactions with the local interstellar medium.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN9545 , Astrophysical Journal (ISSN 0004-637X) (e-ISSN 1538-4357); 752; 1; 57
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  • 5
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    Disentangling the Origin and Heating Mechanism of Supernova Dust: Late-Time Spitzer Spectroscopy of the Type IIn SN 2005ip (2010)
    In:  CASI
    Details
    Publication Date: 2019-07-12
    Description: This paper presents late-time near-infrared and Spitzer mid-infrared photometric and spectroscopic observations of warm dust in the Type IIn SN 2005ip in NGC 2906. The spectra show evidence for two dust components with different temperatures. Spanning the peak of the thermal emission, these observations provide strong constraints on the dust mass, temperature, and luminosity, which serve as critical diagnostics for disentangling the origin and heating mechanism of each component. The results suggest the warmer dust has a mass of approx. 5 x 10(exp -4) Solar Mass and originates from newly formed dust in the ejecta, continuously heated by the circumstellar interaction. By contrast, the cooler component likely originates from a circumstellar shock echo that forms from the heating of a large, pre-existing dust shell approx. 0.01 - 0.05 Solar Mass by the late-time circumstellar interaction. The progenitor wind velocity derived from the blue edge of the He I 1.083 micro P Cygni profile indicates a progenitor eruption likely formed this dust shell approx.100 years prior to the supernova explosion, which is consistent with a Luminous Blue Variable (LBV) progenitor star. Subject
    Keywords: Astronomy
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