The Orbit and Origin of the Ultra-faint Dwarf Galaxy Segue 1

Abstract

We present the first proper motion measurement for an ultra-faint dwarf spheroidal galaxy, Segue 1, using SDSS and LBC data as the first and second epochs separated by a baseline of $\sim 10$ years. We obtain a motion of ${\mu }_{\alpha }\cos (\delta )=-0.37\pm 0.57$ mas yr${}^{-1}$ and ${\mu }_{\delta }=-3.39\pm 0.58$ mas yr${}^{-1}$. Combining this with the known line-of-sight velocity, this corresponds to a Galactocentric V${}_{\mathrm{rad}}=84\pm 9$ and V${}_{\tan }=164_{-55}^{+66}$ km s${}^{-1}$. Applying Milky Way halo masses between 0.8 to 1.6$\times 10^{12}$ M${}_{\odot }$ results in an apocenter at 33.9${}_{-7.4}^{+21.7}$ kpc and pericenter at 15.4${}_{-9.0}^{+10.1}$ kpc from the Galactic center, indicating Segue~1 is rather tightly bound to the Milky Way. Since neither the orbital pole of Segue 1 nor its distance to the Milky Way is similar to the more massive classical dwarfs, it is very unlikely that Segue 1 was once a satellite of a massive known galaxy. Using cosmological zoom-in simulations of Milky Way-mass galaxies, we identify subhalos on similar orbits as Segue~1, which imply the following orbital properties: a median first infall 8.1${}_{-4.3}^{+3.6}$ Gyrs ago, a median of 4 pericentric passages since then and a pericenter of 22.8${}_{-4.8}^{+4.7}$ kpc. This is slightly larger than the pericenter derived directly from Segue 1 and Milky Way parameters, because galaxies with a small pericenter are more likely to be destroyed. Of the surviving subhalo analogs only 27\% were previously a satellite of a more massive dwarf galaxy (that is now destroyed), thus Segue 1 is more likely to have been accreted on its own.

arXiv comment16 pages, 7 figures, accepted by ApJ

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