The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

Silber, Joseph H.; Fagrelius, Parker; Fanning, Kevin; Schubnell, M.; Aguilar, Jessica Nicole; Ahlen, S. P.; Ameel, Jon; Ballester, O.; Baltay, C.; Bebek, C.; Beard, Dominic Benton; Besuner, Robert; Cardiel-Sas, Laia; Casas, R.; Castander, F. J.; Claybaugh, Todd; Dobson, C. A.; Duan, Yutong; Dunlop, P.S.M.; Edelstein, Jerry; Emmet, W.; Elliott, Ann; Evatt, Matthew; Gershkovich, Irena; Guy, J.; Harris, Stu; Heetderks, H.; Heetderks, Ian; Honscheid, K.; Illa, J. M.; Jelinsky, Patrick; Jelinsky, Sharon R.; Jiménez, Jorge; Karcher, A.; Kent, Stephen M.; Kirkby, D.; Kneib, Jean-Paul; Lambert, A.; Lampton, M.; Leitner, D.; Levi, Michael; McCauley, Jeremy; Meisner, Aaron M.; Miller, Timothy N.; Miquel, R.; Mundet, J.; Poppett, Claire; Rabinowitz, D.; Reil, K.; Riaño, David; Schlegel, David J.; Serrano, S.; Shourt, William V.; Sprayberry, David; Tarlè, G.; Tie, Suk Sien; Weaverdyck, Curtis; Zhang, Kai; Azzaro, M.; Bailey, S.; Becerril, S.; Blackwell, Tami; Bouri, Mohamed; Buckley-Geer, E.; Castro, Jose Peñate; Derwent, Mark; Dey, Arjun; Dhungana, G.; Doel, P.; Eisenstein, Daniel J.; Fahim, Nasib; García-Bellido, J.; Gaztañaga, E.; Gontcho, Satya Gontcho A; Gutiérrez, G.; Hörler, Philipp; Kehoe, R.; Kisner, T. S.; Kremin, Anthony; Kronig, Luzius; Landriau, Martin; Guillou, L. Le; Martini, Paul; Moustakas, John; Palanque-Delabrouille, N.; Peng, Xiyan; Percival, Will J.; Prada, Francisco; Prieto, C. Allende; Rivera, Guillermo González de; Sánchez, E.; Sánchez, J.; Sharples, R. M.; Soares-Santos, M.; Schlafly, Edward F.; Weaver, B. A.; Zhou, Zhimin; Zhu, Y. Y.; Zou, Hu

doi:10.3847/1538-3881/ac9ab1

Cited by 67 publications

(50 citation statements)

References 45 publications

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“…Moreover, on each tile, DESI allocates 50 fiber positioners to flux standards and 40-65 fibers to blank sky locations, per spectrograph petal, which leaves at most 4500 fibers available for science targets. This will be reduced further by nonoperational fiber positioners, the number of which will vary over the course of the survey and is ∼15% as of 2021 December (Silber et al 2023).…”

Section: Target Density and Fiber Assignmentmentioning

confidence: 99%

“…DESI deploys 5000 fibers over a 3°.2 diameter field of view at the prime focus of the Mayall 4 m telescope at Kitt Peak National Observatory (DESI Collaboration et al 2016b;T. Miller et al 2022, in preparation;Silber et al 2023). The fibers feed 10 identical three-arm spectrographs, each spanning 3600-9824 Å at an FWHM resolution of about 1.8 Å.…”

Section: Introductionmentioning

confidence: 99%

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Overview of the DESI Milky Way Survey

Cooper

Koposov

Prieto

et al. 2023

ApJ

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We describe the Milky Way Survey (MWS) that will be undertaken with the Dark Energy Spectroscopic Instrument (DESI) on the Mayall 4 m telescope at the Kitt Peak National Observatory. Over the next 5 yr DESI MWS will observe approximately seven million stars at Galactic latitudes ∣b∣ > 20°, with an inclusive target selection scheme focused on the thick disk and stellar halo. MWS will also include several high-completeness samples of rare stellar types, including white dwarfs, low-mass stars within 100 pc of the Sun, and horizontal branch stars. We summarize the potential of DESI to advance understanding of the Galactic structure and stellar evolution. We introduce the final definitions of the main MWS target classes and estimate the number of stars in each class that will be observed. We describe our pipelines for deriving radial velocities, atmospheric parameters, and chemical abundances. We use ≃500,000 spectra of unique stellar targets from the DESI Survey Validation program (SV) to demonstrate that our pipelines can measure radial velocities to ≃1 km s−1 and [Fe/H] accurate to ≃0.2 dex for typical stars in our main sample. We find the stellar parameter distributions from ≈100 deg2 of SV observations with ≳90% completeness on our main sample are in good agreement with expectations from mock catalogs and previous surveys.

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Section: Target Density and Fiber Assignmentmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Overview of the DESI Milky Way Survey

Cooper

Koposov

Prieto

et al. 2023

ApJ

Self Cite

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“…The focal plane of DESI contains 5000 fibers arranged in 10 wedge-shaped petals. Each fiber is controlled by a robotic fiber positioner, which can rotate on two arms and be positioned within a circular patrol region of radius 1 48 (DESI Collaboration et al 2016aCollaboration et al , 2022Schubnell et al 2016;Silber et al 2023). The patrol regions of adjacent positioners slightly overlap; however, there are gaps in the regions between the petals.…”

Section: Fiber Assignment Strategymentioning

confidence: 99%

The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation

Hahn

Wilson

Ruiz-Macias

et al. 2023

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Over the next 5 yr, the Dark Energy Spectroscopic Instrument (DESI) will use 10 spectrographs with 5000 fibers on the 4 m Mayall Telescope at Kitt Peak National Observatory to conduct the first Stage IV dark energy galaxy survey. At z < 0.6, the DESI Bright Galaxy Survey (BGS) will produce the most detailed map of the universe during the dark-energy-dominated epoch with redshifts of >10 million galaxies spanning 14,000 deg2. In this work, we present and validate the final BGS target selection and survey design. From the Legacy Surveys, BGS will target an r < 19.5 mag limited sample (BGS Bright), a fainter 19.5 < r < 20.175 color-selected sample (BGS Faint), and a smaller low-z quasar sample. BGS will observe these targets using exposure times scaled to achieve homogeneous completeness and cover the footprint three times. We use observations from the Survey Validation programs conducted prior to the main survey along with simulations to show that BGS can complete its strategy and make optimal use of “bright” time. BGS targets have stellar contamination <1%, and their densities do not depend strongly on imaging properties. BGS Bright will achieve >80% fiber assignment efficiency. Finally, BGS Bright and BGS Faint will achieve >95% redshift success over any observing condition. BGS meets the requirements for an extensive range of scientific applications. BGS will yield the most precise baryon acoustic oscillation and redshift-space distortion measurements at z < 0.4. It presents opportunities for new methods that require highly complete and dense samples (e.g., N-point statistics, multitracers). BGS further provides a powerful tool to study galaxy populations and the relations between galaxies and dark matter.

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“…The DESI-M2 data were observed on nights in 2021 from May 14th through July 9th on 304 dark time and 342 bright time 'tiles'. Each tile represents a specific sky location pointing of the telescope and specific target selection for each of the 5000 robotic positioners populating the DESI focal plane (Silber et al 2022) determined by the DESI fiberassign software (Raichoor et al in prep). The The DESI-M2 tiles are primarily first pass tiles that do not overlap each other.…”

Section: Desi Early Data: General Aspectsmentioning

confidence: 99%

Data from Identification of Developmental Endothelial Locus-1 on Circulating Extracellular Vesicles as a Novel Biomarker for Early Breast Cancer Detection

Moon¹,

Lee²,

Cho³

et al. 2023

Preprint

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<div>AbstractPurpose: Currently, there are no molecular biomarkers for the early detection of breast cancer. This study focused on identifying surface proteins found on circulating extracellular vesicles (EVs) for detecting early-stage breast cancer.Experimental Design: Circulating EVs, isolated from the plasma of 10 patients with breast cancer (stages I and II) and 5 healthy controls, were analyzed using LC-MS/MS. Developmental endothelial locus-1 protein (Del-1) was selected as a candidate biomarker. Two different ELISAs were used to measure Del-1 in plasma samples from healthy controls (n = 81), patients with breast cancer (n = 269), breast cancer patients after surgical resection (n = 50), patients with benign breast tumors (n = 64), and patients with noncancerous diseases (n = 98) in two cohorts.Results: Plasma Del-1 levels were significantly higher (P < 0.0001) in patients with breast cancer than in all controls and returned to almost normal after tumor removal. The diagnostic accuracy of Del-1 was AUC, 0.961 [95% confidence interval (CI), 0.924–0.983], sensitivity of 94.70%, and specificity of 86.36% in test cohort and 0.968 (0.933–0.988), 92.31%, and 86.62% in validation cohort for early-stage breast cancer by one type of ELISA. Furthermore, Del-1 maintained diagnostic accuracy for patients with early-stage breast cancer using the other type of ELISA [0.946 (0.905–0.972), 90.90%, and 77.14% in the test cohort; 0.943 (0.900–0.971), 89.23%, and 80.99% in the validation cohort].Conclusions: Del-1 on circulating EVs is a promising marker to improve identification of patients with early-stage breast cancer and distinguish breast cancer from benign breast tumors and noncancerous diseases. Clin Cancer Res; 22(7); 1757–66. ©2015 AACR.</div>

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The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

Cited by 67 publications

References 45 publications

Overview of the DESI Milky Way Survey

Overview of the DESI Milky Way Survey

The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation

Data from Identification of Developmental Endothelial Locus-1 on Circulating Extracellular Vesicles as a Novel Biomarker for Early Breast Cancer Detection

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