Overview of the DESI Milky Way Survey

Cooper, Andrew P.; Koposov, Sergey E.; Allende Prieto, Carlos; Manser, Christopher J.; Kizhuprakkat, Namitha; Myers, Adam D.; Dey, Arjun; Gänsicke, Boris T.; Li, Ting S.; Rockosi, Constance; Valluri, Monica; Najita, Joan; Deason, Alis; Raichoor, Anand; Wang, M. -Y.; Ting, Y. -S.; Kim, Bokyoung; Carrillo, Andreia; Wang, Wenting; Beraldo e Silva, Leandro; Han, Jiwon Jesse; Ding, Jiani; Sánchez-Conde, Miguel; Aguilar, Jessica N.; Ahlen, Steven; Bailey, Stephen; Belokurov, Vasily; Brooks, David; Cunha, Katia; Dawson, Kyle; de la Macorra, Axel; Doel, Peter; Eisenstein, Daniel J.; Fagrelius, Parker; Fanning, Kevin; Font-Ribera, Andreu; Forero-Romero, Jaime E.; Gaztañaga, Enrique; Gontcho a Gontcho, Satya; Guy, Julien; Honscheid, Klaus; Kehoe, Robert; Kisner, Theodore; Kremin, Anthony; Landriau, Martin; Levi, Michael E.; Martini, Paul; Meisner, Aaron M.; Miquel, Ramon; Moustakas, John; Nie, Jundan J. D.; Palanque-Delabrouille, Nathalie; Percival, Will J.; Poppett, Claire; Prada, Francisco; Rehemtulla, Nabeel; Schlafly, Edward; Schlegel, David; Schubnell, Michael; Sharples, Ray M.; Tarlé, Gregory; Wechsler, Risa H.; Weinberg, David H.; Zhou, Zhimin; Zou, Hu
Bibliographical reference

The Astrophysical Journal

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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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spectrum of mercury lamp
Chemical Abundances in Stars
Stellar spectroscopy allows us to determine the properties and chemical compositions of stars. From this information for stars of different ages in the Milky Way, it is possible to reconstruct the chemical evolution of the Galaxy, as well as the origin of the elements heavier than boron, created mainly in stellar interiors. It is also possible to
Allende Prieto