000196879 001__ 196879
000196879 005__ 20180913062358.0
000196879 0247_ $$2doi$$a10.1051/0004-6361/201322452
000196879 022__ $$a0004-6361
000196879 02470 $$2ISI$$a000327847200018
000196879 037__ $$aARTICLE
000196879 245__ $$aMeasuring galaxy [OII] emission line doublet with future ground-based wide-field spectroscopic surveys (Research Note)
000196879 260__ $$aLes Ulis Cedex A$$bEDP Sciences$$c2013
000196879 269__ $$a2013
000196879 300__ $$a4
000196879 336__ $$aJournal Articles
000196879 520__ $$aThe next generation of wide-field spectroscopic redshift surveys will map the large-scale galaxy distribution in the redshift range 0.7 <= z <= 2 to measure baryonic acoustic oscillations (BAO). The primary optical signature used in this redshift range comes from the [OII] emission line doublet, which provides a unique redshift identification that can minimize confusion with other single emission lines. To derive the required spectrograph resolution for these redshift surveys, we simulate observations of the [OII] (lambda lambda 3727, 3729) doublet for various instrument resolutions, and line velocities. We foresee two strategies for the choice of the resolution for future spectrographs for BAO surveys. For bright [OII] emitter surveys ([OII] flux similar to 30 x 10(-17) erg cm(-2) s(-1) like SDSS-IV/eBOSS), a resolution of R similar to 3300 allows the separation of 90 percent of the doublets. The impact of the sky lines on the completeness in redshift is less than 6 percent. For faint [OII] emitter surveys ([OII] flux similar to 10 x 10(-17) erg cm(-2) s(-1) like DESi), the detection improves continuously with resolution, so we recommend the highest possible resolution, the limit being given by the number of pixels (4k by 4k) on the detector and the number of spectroscopic channels (2 or 3).
000196879 6531_ $$ainstrumentation: spectrographs
000196879 6531_ $$atechniques: spectroscopic
000196879 6531_ $$acosmology: observations
000196879 6531_ $$agalaxies: statistics
000196879 700__ $$aComparat, Johan$$uAix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
000196879 700__ $$0246614$$aKneib, Jean-Paul$$g222189$$uAix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
000196879 700__ $$aBacon, Roland$$uEPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland
000196879 700__ $$aMostek, Nick J.$$uUniv Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
000196879 700__ $$aNewman, Jeffrey A.$$uUniv Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA
000196879 700__ $$aSchlegel, David J.$$uUniv Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
000196879 700__ $$aYeche, Christophe
000196879 773__ $$j559$$tAstronomy & Astrophysics
000196879 909C0 $$0252365$$pLASTRO$$xU10933
000196879 909CO $$ooai:infoscience.tind.io:196879$$pSB$$particle
000196879 917Z8 $$x103317
000196879 937__ $$aEPFL-ARTICLE-196879
000196879 973__ $$aEPFL$$rREVIEWED$$sPUBLISHED
000196879 980__ $$aARTICLE