ESI, a New Keck Observatory Echellette Spectrograph and Imager

Sheinis, Andrew; Bolte, M.; Epps, Harland W.; Kibrick, Robert I.; Miller, J. S.; Radovan, Matthew V.; Bigelow, Bruce C.; Sutin, Brian M.

doi:10.1086/341706

Cited by 374 publications

(324 citation statements)

References 18 publications

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“…Given that the throughput of ESI in echellete mode (d12%) is approximately 40% smaller than that of the prism long-slit ('' high-throughput '') mode (see Sheinis et al 2002), it is not immediately obvious why echellete spectroscopy would be able to detect the redshift of GRB 990506, whereas long-slit spectroscopy failed to detect the line. While both observing modes provide similar wavelength coverage and slit widths, however, the prism long-slit mode results in a lower dispersion with increasing wavelengths (from 1 Å pixel À1 at 4000 Å to $10 Å pixel À1 at 10000 Å ).…”

Section: Discussionmentioning

confidence: 99%

“…The observations of both GRB host galaxies were obtained in the echellete mode of the Echellete Spectro-graph Imager (ESI; Sheinis et al 2002) on the Keck II 10 m telescope atop Mauna Kea, Hawaii. The detector is a 2K Â 4K pixel Lincoln Labs CCD with low read noise (rms % 2.6 e À ) and small dark current (2.1 e À pixel À1 hr À1 ).…”

Section: Observations and Reductionsmentioning

confidence: 99%

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The Redshift Determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck

Bloom

Berger

Kulkarni

et al. 2003

The Astronomical Journal

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Using the Echellete Spectrograph Imager (ESI) on the Keck II 10 m telescope we have measured the redshifts of the host galaxies of gamma-ray bursts GRB 990506 and GRB 000418, z = 1.30658 AE 0.00004 and 1.1181 AE 0.0001, respectively. Thanks to the excellent spectral resolution of ESI ( /D = 13000), we resolved the [O ii] 3727 doublet in both cases. The measured redshift of GRB 990506 is the highest known for a darkburst GRB, though entirely consistent with the notion that dark and non-dark bursts have a common progenitor origin. The relative strengths of the [O ii], He i, [Ne iii], and H emission lines suggest that the host of GRB 000418 is a starburst galaxy, rather than a LINER or Seyfert 2. Since the host of GRB 000418 has been detected at submillimeter wavelengths, these spectroscopic observations suggest that the submillimeter emission is due to star formation (as opposed to AGN) activity. The [O ii]-derived unobscured star formation rates are 13 and 55 M yr À1 for the hosts of GRB 990506 and GRB 000418, respectively. In contrast, the star formation rate of the host of GRB 000418 derived from submillimeter observations is 20 times larger.

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Section: Discussionmentioning

confidence: 99%

Section: Observations and Reductionsmentioning

confidence: 99%

The Redshift Determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck

Bloom

Berger

Kulkarni

et al. 2003

The Astronomical Journal

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“…Eight absorbers in this work were followed up with the Echelle Imager and Spectrograph (ESI; Sheinis et al 2002) on the Keck-II telescope on March 8 & 9, 2013, using the 0.75 ′′ slit. The wavelength coverage is 3900 -11715Å and the spectral resolution is R = λ/∆λ ∼ 6000.…”

Section: Observationsmentioning

confidence: 99%

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Prochaska

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the cold neutral content (H i and C i gas) of 13 quasar 2175Å dust absorbers (2DAs) at z = 1.6 -2.5 to investigate the correlation between the presence of the UV extinction bump with other physical characteristics. These 2DAs were initially selected from the Sloan Digital Sky Surveys I -III and followed up with the Keck-II telescope and the Multiple Mirror Telescope as detailed in our Paper I. We perform a correlation analysis between metallicity, redshift, depletion level, velocity width, and explore relationships between 2DAs and other absorption line systems. The 2DAs on average have higher metallicity, higher depletion levels, and larger velocity widths than Damped Lyman-α absorbers (DLAs) or subDLAs. The correlation between [Zn/H] and [Fe/Zn] or [Zn/H] and log∆V 90 can be used as alternative stellar mass estimators based on the well-established mass-metallicity relation. The estimated stellar masses of the 2DAs in this sample are in the range of ∼ 10 9 to ∼2 × 10 11 M ⊙ with a median value of ∼2 × 10 10 M ⊙ . The relationship with other quasar absorption line systems can be described as (1) 2DAs are a subset of Mg ii and Fe ii absorbers, (2) 2DAs are preferentially metal-strong DLAs/subDLAs, (3) More importantly, all of the 2DAs show C i detections with logN(C i) > 14.0 cm −2 , (4) 2DAs can be used as molecular gas tracers. Their host galaxies are likely to be chemically enriched, evolved, massive (more massive than typical DLA/subDLA galaxies), and presumably star-forming galaxies.

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“…edu/~george/z4.qsos) were obtained with the Echellette Spectrograph and Imager (ESI, Sheinis et al 2002) mounted on the KECK II 10 m telescope. In total, 99 quasars were observed, 57 of which have already reported in the literature (see Table 1 for details).…”

Section: Observation and Data Reductionmentioning

confidence: 99%

Damped and sub-damped Lyman-α absorbers in z > 4 QSOs

Guimarães¹,

Petitjean

Carvalho

et al. 2009

A&A

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We present the results of a survey of damped (DLA, log N(H i) > 20.3) and sub-damped Lyman-α systems (19.5 < log N(H i) < 20.3) at z > 2.55 along the lines-of-sight to 77 quasars with emission redshifts in the range 4 < z em < 6.3. Intermediate resolution (R ∼ 4300) spectra were obtained with the Echellette Spectrograph and Imager (ESI) mounted on the Keck telescope. A total of 100 systems with log N(H i) > 19.5 were detected of which 40 systems are damped Lyman-α systems for an absorption length of ΔX = 378. About half of the lines of sight of this homogeneous survey have never been investigated for DLAs. We study the evolution with redshift of the cosmological density of the neutral gas and find, consistent with previous studies at similar resolution, that Ω DLA,H I decreases at z > 3.5. The overall cosmological evolution of Ω H I shows a peak around this redshift. The H i column density distribution for log N(H i) ≥ 20.3 is fitted, consistent with previous surveys, with a single power-law of index α ∼ −1.8 ± 0.25. This power-law overpredicts data at the high-end and a second, much steeper, power-law (or a gamma function) is needed. There is a flattening of the function at lower H i column densities with an index of α ∼ −1.4 for the column density range log N(H i) = 19.5−21. The fraction of H i mass in sub-DLAs is of the order of 30%. The H i column density distribution does not evolve strongly from z ∼ 2.5 to z ∼ 4.5.

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ESI, a New Keck Observatory Echellette Spectrograph and Imager

Cited by 374 publications

References 18 publications

The Redshift Determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck

The Redshift Determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Damped and sub-damped Lyman-α absorbers in z > 4 QSOs

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