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1 al lines, and the selected parameters of the spectrograph.
2 y detector coupled to a Mattauch-Herzog mass spectrograph.
3 axies were studied with the Planetary Nebula Spectrograph.
4 lving power of high-resolution astrophysical spectrographs.
5 usly by the ultraviolet and infrared imaging spectrographs.
6 esolvable using typical astronomical grating spectrographs.
11 either requires a complicated setup with two spectrographs and detectors or two measurements must be
12 pulsed tunable dye laser, a high-resolution spectrograph, and an intensified charged-couple device.
13 beams is imaged onto the slit of an imaging spectrograph as two spatially separated signals, i.e., t
14 ocal Group, with the Space Telescope Imaging Spectrograph at a resolution at least a factor of 10 hig
15 spectrum as revealed by the Hamilton echelle Spectrograph at Lick Observatory (resolution approximate
16 ry nebulae secured with the Hamilton Echelle spectrograph at Lick Observatory combined with previousl
18 is analyzed with a high resolution, compact spectrograph consisting of an echelle grating and a high
19 995, the Hubble Space Telescope Faint Object Spectrograph detected ultraviolet fluorescent emissions
21 004, just before the Space Telescope Imaging Spectrograph failed, we find that the Lyalpha and Halpha
22 nd fitted to a Mattauch-Herzog geometry mass spectrograph for the simultaneous acquisition of multipl
23 infrared (PA-IR) technique, which utilizes a spectrograph for wavelength dispersion and a mid-infrare
24 servations with the Interface Region Imaging Spectrograph (IRIS) at the solar limb reveal a plethora
25 vations with NASA's Interface Region Imaging Spectrograph (IRIS) reveal a chromosphere and TR that ar
26 servations with the Interface Region Imaging Spectrograph (IRIS) reveal rapid variability (~20 to 60
27 observations by the Interface Region Imaging Spectrograph (IRIS) reveal that it is difficult to deter
28 en motion capture (mocap) technology and the spectrograph is flawed because only vocal articulators a
30 , has been coupled to a Mattauch-Herzog mass spectrograph (MHMS) with an inductively coupled plasma i
32 spectrum obtained with the Hamilton Echelle spectrograph on the 3-m Shane Telescope, implies a densi
33 d with the University College London Echelle Spectrograph on the 3.9-m Anglo-Australian Telescope, re
34 e nightside of Venus with HIRES, the echelle spectrograph on the W. M. Keck I 10-meter telescope.
35 kirts of 42 galaxies with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope, we dete
36 man Alpha Mapping Project (LAMP) ultraviolet spectrograph onboard the Lunar Reconnaissance Orbiter (L
37 cattering signals is dispersed by an imaging spectrograph onto a CCD detector, giving 16 independent
38 servations from the Interface Region Imaging Spectrograph reveal the prevalence of intermittent small
39 moon Europa taken by Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST)
41 resnel spectrometer that contains a complete spectrograph system, including the detection hardware an
42 coupled plasma Mattauch-Herzog geometry mass spectrograph, thereby offering simultaneous acquisition
43 But it has proved difficult for existing spectrographs to characterize them using their ultraviol
44 e such Doppler shift resolution via improved spectrograph wavelength calibration, with recent encoura
45 ppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spati
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