Kavli Affiliate: Risa H. Wechsler
| First 5 Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang
| Summary:
We present the third Data Release (DR3) of the Satellites Around Galactic
Analogs (SAGA) Survey, a spectroscopic survey characterizing satellite galaxies
around Milky Way (MW)-mass galaxies. The SAGA Survey DR3 includes 378
satellites identified across 101 MW-mass systems in the distance range 25-40.75
Mpc, and an accompanying redshift catalog of background galaxies (including
about 46,000 taken by SAGA) in the SAGA footprint of 84.7 sq. deg. The number
of confirmed satellites per system ranges from zero to 13, in the stellar mass
range 10^6 to 10^10 solar masses. Based on a detailed completeness model, this
sample accounts for 94% of the true satellite population down to a stellar mass
of 10^7.5 solar masses. We find that the mass of the most massive satellite in
SAGA systems is the strongest predictor of satellite abundance; one-third of
the SAGA systems contain LMC-mass satellites, and they tend to have more
satellites than the MW. The SAGA satellite radial distribution is less
concentrated than the MW, and the SAGA quenched fraction below 10^8.5 solar
masses is lower than the MW, but in both cases, the MW is within 1 sigma of
SAGA system-to-system scatter. SAGA satellites do not exhibit a clear
corotating signal as has been suggested in the MW/M31 satellite systems.
Although the MW differs in many respects from the typical SAGA system, these
differences can be reconciled if the MW is an older, slightly less massive host
with a recently accreted LMC/SMC system.
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