KSPEC-a near-infrared cross-dispersed spectrograph

Hodapp, Klaus W.; Hora, J. L.; Irwin, Everett M.; Young, Tony T.

doi:10.1086/133347

Cited by 23 publications

(20 citation statements)

References 1 publication

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“…The spectrum of this well-studied young, low-excitation PN was previously shown to be dominated by lines of H I and He I in the near-IR, with a hot dust continuum (Willner et al 1979;Zhang & Kwok 1992;Hodapp et al 1994). Hora et al (1993) and Paper I showed broad-and narrowband near-IR images of the PN, showing the elliptical, double-lobed structure in the IR.…”

Section: Ic 418mentioning

confidence: 83%

Investigating the Near‐Infrared Properties of Planetary Nebulae. II. Medium‐Resolution Spectra

Hora

Latter

Deutsch

1999

ASTROPHYS J SUPPL S

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107

125

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We present medium-resolution (R ∼ 700) near-infrared (λ = 1 − 2.5 µm) spectra of a sample of planetary nebulae (PNe). A narrow slit was used which sampled discrete locations within the nebulae; observations were obtained at one or more positions in the 41 objects included in the survey. The PN spectra fall into one of four general categories: H I emission line-dominated PNe, H I and H 2 emission line PNe, H 2 emission line-dominated PNe, and continuum-dominated PNe. These categories correlate with morphological type, with the elliptical PNe falling into the first group, and the bipolar PNe primarily in the H 2 and continuum emission groups. The categories also correlate with C/O ratio, with the O-rich objects generally falling into the first group and the C-rich objects in the other groups. Other spectral features were observed in all categories, such as continuum emission from the central star, C 2 , CN, and CO emission, and warm dust continuum emission towards the long wavelength end of the spectra.Molecular hydrogen was detected for the first time in four PNe. An excitation analysis was performed using the H 2 line ratios for all of the PN spectra in the survey where a sufficient number of lines were observed. From the near-infrared spectrum, we determined an ortho-to-para ratio, the rotational and vibrational excitation temperatures, and the dominant excitation mechanism of the H 2 for many objects surveyed. One unexpected result from this analysis is that the H 2 is excited by absorption of ultraviolet photons in most of the PNe surveyed, although for several PNe in our survey collisional excitation in moderate velocity shocks plays an important role. The correlation between bipolar morphology and H 2 emission has been strengthened with the new detections of H 2 in this survey. We discuss the role of winds and photons to the excitation of H 2 in PNe, and consider some implications to the utility of H 2 as a nebular diagnostic and to our understanding of PNe structure and evolution.

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Section: Ic 418mentioning

confidence: 83%

Investigating the Near‐Infrared Properties of Planetary Nebulae. II. Medium‐Resolution Spectra

Hora

Latter

Deutsch

1999

ASTROPHYS J SUPPL S

Self Cite

107

125

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“…First, we used currently proven technologies to minimize the need for and cost of research and development. For example, at the time of NIRIMÏs design phase, the NICMOS3 arrays, developed by Rockwell International Science Center, had been proven in other astronomical cameras (e.g., Hodapp, Rayner, & Irwin 1992 ;Hodapp et al 1994 ; Thompson et al 1994 ;Nadeau et al 1994). Second, we kept the engineering of the design to a minimum.…”

Section: Introductionmentioning

confidence: 99%

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

Meixner

Owl

Leach

1999

PUBL ASTRON SOC PAC

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ABSTRACT. We present the design and performance characteristics of the Near-Infrared Imager (NIRIM), which is a near-infrared camera operating in the 0.76[2.5 km wavelength range. NIRIM is an example of a cost-e †ective way to expand two telescopesÏ capabilities to infrared wavelengths. NIRIM has been used for photometry and wide-Ðeld imaging on our 1 m telescope at the Mount Laguna (8@ .5 ] 8@ .5) Observatory since 1995 August. In the future, NIRIM will also be used for high angular resolution imaging with the University of Illinois Seeing Improvement System (UnISIS), which is a laser guided adaptive optics system at the focus of the Mount Wilson 2.5 m telescope. coude

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“…1). Originally a near-infrared cross-dispersed grating spectrometer, 9 KSPEC was repurposed for ultra-low noise detector characterization for the JWST Packaging and Manufacturing Technology program, where the background was shown to be at the level of a few photons/pixel/hour for 5 µm cutoff material.…”

Section: Saphiramentioning

confidence: 99%

Observatory deployment and characterization of SAPHIRA HgCdTe APD arrays

et al. 2014

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We report the performance of Selex ES' SAPHIRA APD arrays from both laboratory characterization and telescope deployment. The arrays are produced using the MOVPE production method, allowing for solid state engineering and thus produce superior performance to similar liquid phase epitaxy efforts. With an avalanche gain slightly over 50 and read noise of ∼9e − , the detectors are easily capable of single-frame sub-electron read noise, and the 32 output readout and flexible windowing allow an excellent readout speed. Gain-corrected dark current/glow is found to be 10-20 e − /s at low bias, and drops below basline at high avalanche gains. The detectors were also tested on-sky at both IRTF on Maunakea and the 1.5-m telescope at Palomar Observatory, demonstrating that the SAPHIRA is an ideal device for both tip-tilt NGS guiding and infrared lucky imaging, in the latter providing diffraction-limited resolution for the 3-meter IRTF without the benefit of adaptive optics correction.

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KSPEC-a near-infrared cross-dispersed spectrograph

Cited by 23 publications

References 1 publication

Investigating the Near‐Infrared Properties of Planetary Nebulae. II. Medium‐Resolution Spectra

Investigating the Near‐Infrared Properties of Planetary Nebulae. II. Medium‐Resolution Spectra

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

Observatory deployment and characterization of SAPHIRA HgCdTe APD arrays

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