SDSS-IV and eboss Science. Hyunmi Song (KIAS)
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1 SDSS-IV and eboss Science Hyunmi Song (KIAS) 3rd Korea-Japan Workshop on Dark Energy April 4, 2016 at KASI
2 Sloan Digital Sky Survey 2.5m telescopes at Apache Point Observatory (US) and Las Campanas Observatory (Chile, included for SDSS-IV)
3 SDSS SDSS facility s key advantage is its wide-field spectrographs that observe many objects simultaneously.
4 SDSS a SDSS plug plate and fibers 640 holes
5 SDSS SDSS-I/II Legacy, Supernova, SEGUE-1 SDSS-III APOGEE, BOSS, MARVELS, SEGUE-2 SDSS-IV APOGEE-2, eboss, MaNGA
6 SDSS Three SDSS projects (I-III) created an extraordinary legacy of mapping structure across a vast range of scales, from asteroids in our own Solar System to quasars over 10 million light-years away. SDSS-IV will expand this legacy by studying the detailed assembly history of the Milky Way (APOGEE-2) and thousands of other nearby galaxies (MaNGA), and extending precision measurements of expansion to the cosmic epochs when dark energy first became important (eboss).
7 APOGEE project description
8 MaNGA project description
9 eboss project description
10 eboss xtended
11 BOSS
12 Baryonic Oscillation Spectroscopic Survey
13 Baryonic Acoustic Oscillation matter photon
14 Baryonic Acoustic Oscillation matter photon
15 Baryonic Acoustic Oscillation matter photon
16 Baryonic Acoustic Oscillation matter photon
17 Baryonic Acoustic Oscillation matter photon
18 Baryonic Acoustic Oscillation matter photon
19 Baryonic Acoustic Oscillation matter photon
20 Baryonic Acoustic Oscillation matter photon
21 BAO standard ruler ~150Mpc
22 BAO Tracers SDSS Luminous Red Galaxies (LRGs) BOSS galaxies (extension of SDSS LRG) BOSS Lya quasars (suggested as a new tracer in SDSS-III BOSS)
23 BOSS in a nutshell sqdeg (1/4 of entire sky) low-z galaxies (LOWZ, z median =0.32) mid-z galaxies (CMASS, z median =0.57) quasars at 2.1<z<3.5
24 BOSS/eBOSS Spectrograph, compared to SDSS-I/II more objects (640 -> 1000 holes per plate) improved spectrographs (smaller fibers 3 ->2, new improved detectors, higher throughput, and a wider wavelength range)
25 eboss Compared to BOSS additional imaging resources of infrared imaging data from WISE (previously entirely based on SDSS photometry)
26 eboss Compared to BOSS higher redshift first measurement across the critical epoch, the predicted onset time for dark energy
27 eboss Compared to BOSS new tracer star-forming galaxies /Emission Line Galaxies (ELGs)
28 ELG Emission lines in blue galaxies with significant star formation facilitate spectroscopic confirmation at high redshifts with an optical spectrograph. Because ELGs are numerous and have emission line fluxes correlated with the observed u or g-band magnitudes, they can be selected at a much higher density than LRG sample.
29 ELG spectra Comparat et al. 2015
30 eboss 1.4 million targets in 4 different classes (target #) elliptical galaxies (LRGs, at 0.6<z<0.8) star-forming galaxies ( at 0.6<z<1, over a 1500 sqdeg) mid-z quasars ( at 1<z<2.2) high-z quasars ( at 2.2<z<3.5)
31 eboss Geometrical constraint (BAO) Growth of structure Cristiano Sabiu s talk on Friday Seokcheon Lee s talk on Wednesday Redshift Space Distortion (RSD) - how galaxies are moving in response to gravity
32 ddddd Dawson et al. 2015
33 Dawson et al. 2015
34 eboss forecast BOSS constrains the distance to a precision of 2.1% at z=0.32 (LOWZ) 1.7% at z=0.57 (CMASS) 2.1% 2.1<z<3.5 (Lya) eboss aims at 1%, 2%, and 2% BAO distance measurements on the LRG, quasar, and ELG samples.
35 Dawson et al. 2015
36 eboss Sub-programs TDSS (Time Domain Spectroscopic Survey) SPIDERS (SPectroscopic IDentification of Rosita Sources)
37 Other than BAO Alcock-Paczynski test Xiao-Dong Li s talk on Friday Large-scale structures Ho Seong Hwang s talk on Friday Galaxy evolution and environment cf. Benjamin L Huillier talk
38 Public Data Release DR13 (the first data release of SDSS-IV) will be in July Few hundred Terabytes of data New datacubes from MaNGA + new photometry and SEQUELS spectra from eboss/tdss/spiders + new reductions of all APOGEE data from SDSS-III + legacy data
39 Access to data slide from Adam Bolton s SDSS-IV collaboration meeting
40 slide from Jean-Paul Kneib s SDSS-IV collaboration meeting
41
42 eboss While photometric selection for BOSS galaxy sample was based entirely on imaging from SDSS (cf. UKIRT Infrared Deep Sky Survey/UKIDSS and the Galaxy Evolution Explorer/GALEX were used for Lya forest quasar selection), additional imaging resources for eboss are considered highly-uniform, infrared imaging data from WISE satellite (3.4 and 4.6 micro-m)
43 eboss ELG target selection still under investigation SDSS griz + South Galactic Cap U-band Sky Survey (SCUSS) U-band available over the entire SGC area deeper grz imaging from the Dark Energy Camera (DECam) deeper imaging data allows more precise identification of strong emission-line galaxies
44 eboss Over six years, eboss will provide the first percent-level distance measurements with BAO and RSD in the redshift range 0.6<z<2, where cosmic expansion transitioned from deceleration to acceleration. Using LRG, quasar, ELG, and Lya absorption as tracers of the underlying density field, eboss will probe the largest volume to date of any cosmological redshift survey.
45 eboss In total, the final eboss spectroscopy will consist of: LRG targets (0.6<z<1.0) at a density of 50/sqdeg and desired purity exceeding 80%, ELG targets at a somewhat higher redshift over 300 dedicated plates with a desired purity exceeding 74%, clustering quasar targets (QSO_CORE) to directly trace largescale structure (0.9<z<2.2) at a density of 90/ sqdeg and desired purity exceeding 50%, reobservations of faint BOSS Lya quasar (z>2.1) at a density of 8/sqdeg, and new Lya quasar candidates identified by variability at an average density of 18/ sqdeg.
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