The DEIMOS spectrograph for the Keck II Telescope: integration and testing

By S. Faber, A. Phillips, R. Kibrick, B. Alcott, S. Allen, J. Burrous, T. Cantrall, D. Clarke, A. Coil, D. Cowley and 17 more. SPIE Astronomical Telescopes + Instrumentation, 2003

671 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d1fc4be8be766730b2fa300296c8429e72c6cf35

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj (2009, methodology): “Optical and Near-Infrared Spectroscopy We acquired optical spectra using ISIS on the WHT, La Palma, and DEIMOS (Faber et al. 2003) on the 10 m Keck 2 telescope, Hawaii.”
The All-Wavelength Extended Groth Strip International Survey (AEGIS) Data Sets (2006, methodology): “All spectra were taken with the DEIMOS spectrograph (Faber et al. 2003) at the Keck II telescope.”
Berkeley Supernova Ia Program – I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae (2012, methodology): “…Spectrometer (LRIS; Oke et al. 1995, both before and after the addition of the blue arm), 3.0 per cent were obtained using the DEep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003), and 1.8 per cent were obtained using the Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002).”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, methodology): “Redshifts were measured spectroscopically using the DEIMOS spectrograph (Faber et al. 2003) on the Keck 2 telescope.”
THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016 GHz (2013, methodology): “Further imaging was conducted with the Deep Imaging Multi-Object Spectrograph (DEIMOS, Faber et al. 2003) on 2013 June 9 in the R band and also reduced using standard techniques.”
THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, methodology): “In order to maintain the homogeneity of the spectroscopic data by using only Keck/DEIMOS (Faber et al. 2003) spectroscopy, we ob- served only galaxies visible from Mauna Kea.”
TWO BRIGHT SUBMILLIMETER GALAXIES IN A z = 4.05 PROTOCLUSTER IN GOODS-NORTH, AND ACCURATE RADIO-INFRARED PHOTOMETRIC REDSHIFTS (2008, methodology): “The counterpart of GN20 was observed with the Deep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) on the Keck II telescope several times between 2004 and 2007, though only the final observations on UT 2007 April 14−15 were in good conditions.”
Quasars Probing Quasars. I. Optically Thick Absorbers near Luminous Quasars (2006, methodology): “Finally, we observed the quasar pair SDSS J1427 0121 with the DEep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) on the Keck II telescope on UT 2005 May 5.”
The Team Keck Treasury Redshift Survey of the GOODS-North Field (2004, methodology): “Its efficient new DEIMOS spectrograph (Faber et al. 2003) on the Keck II telescope was designed specifically for acquiring multislit spectroscopy of over 100 faint galaxies at once, and with its 16′ field of view is ide- ally suited to survey the 10′ × 16′ GOODS-North (hereafter GOODS-N) field.”
A Large Sample of Spectroscopic Redshifts in the ACS-GOODS Region of the Hubble Deep Field North (2004, methodology): “The recent implementation of the Deep Extragalactic Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) on the Keck II 10 m telescope has greatly increased the speed with which such observations may be carried out.”
The AIMSS Project I: bridging the star cluster, galaxy divide (2014, methodology): “The majority of our Northern hemisphere candidates were spectroscopically confirmed using the DEIMOS and ESI instruments on the Keck telescope (Sheinis et al. 2002; Faber et al. 2003).”
Science Objectives and Early Results of the DEEP2 Redshift Survey (2002, background): “for galaxies with 0.74 < Z < 1.44. At the planned spectral resolution, the velocity resolution will be 56 km/s. Such high resolution is unconventional for faint objects but has several beneﬁts: (1) as shown above, most of the spectrum will be free of terrestrial OH night-sky interference; (2) ”
SN 2006tf: Precursor Eruptions and the Optically Thick Regime of Extremely Luminous Type IIn Supernovae (2008, methodology): “…we obtained visual-wavelength spectra of SN 2006tf on five separate dates at the Keck Observatory using the low resolution imaging spectrometer (LRIS; Oke et al. 1995) and the Deep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003), with the observations summarized in Table 2.”
THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, methodology): “DEEP2 + DEEP3 Redshift Survey Spectroscopic redshifts were measured in the DEEP2 redshift survey using the DEIMOS spectrograph (Faber et al. 2003) on the Keck II telescope (Davis et al. 2003; Newman et al. 2012).”
THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, methodology): “The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048.”
Closing in on a Short-Hard Burst Progenitor: Constraints from Early-Time Optical Imaging and Spectroscopy of a Possible Host Galaxy of GRB 050509b (2005, methodology): “The analysis pipeline used to reduce the DEIMOS data was developed at U.C. Berkeley with support from NSF grant AST-0071048.”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. II. PROPERTIES OF WISE-SELECTED ACTIVE GALACTIC NUCLEI IN THE NDWFS BOÖTES FIELD (2012, methodology): “We observed three Keck slitmasks in the Boötes field with the DEep Imaging Multi- Object Spectrograph (DEIMOS; Faber et al. 2003) on UT 2011 April 1-3.”