000262435 001__ 262435
000262435 005__ 20190122102802.0
000262435 022__ $$a0035-8711
000262435 022__ $$a1365-2966
000262435 02470 $$a000449614800092$$2isi
000262435 0247_ $$a10.1093/mnras/sty1986$$2doi
000262435 037__ $$aARTICLE
000262435 245__ $$aPristine dwarf galaxy survey - I. A detailed photometric and spectroscopic study of the very metal-poor Draco II satellite
000262435 260__ $$c2018$$aOxford$$bOXFORD UNIV PRESS
000262435 269__ $$a2018-10-01
000262435 336__ $$aJournal Articles
000262435 520__ $$aWe present a detailed study of the faint Milky Way satellite Draco II (Dra II) from deep CFHT/MegaCam broad-band g and i photometry and narrow-band metallicity-sensitive CaliK observations, along with follow-up Keck II/DEIMOS multi-object spectroscopy. Forward modelling of the deep photometry allows us to refine the structural and photometric properties of Dra II: the distribution of stars in colour-magnitude space implies Dra II is old (13.5 +/- 0.5 Gyr), very metal-poor, very faint (L-v = 180(-72)(+124) L-circle dot), and at a distance d = 21.5 +/- 0.4 kpc. The narrow-band, metallicity-sensitive Cal-IK Pristine photometry confirms this very low metallicity ([Fe/H] = -2.7 +/- 0.1 dex). Even though our study benefits from a doubling of the spectroscopic sample size compared to previous investigations, the velocity dispersion of the system is still only marginally resolved (sigma(vr) < 5.9 km s(-1) at the 95 per cent confidence level) and confirms that Dra II is a dynamically cold stellar system with a large recessional velocity (< v(r)> = -342.5(-1.2)(+1.1)km s(-)1). We further show that the spectroscopically confirmed members of Dra II have a mean proper motion of (mu(alpha)*, mu(delta)) = (1.26 +/- 0.27, 0.94 +/- 0.28) mas/yr in the Gaia DR2 data, which translates to an orbit with a pericentre and an apocentre of 21.3(-1.0)(+0.7) and 153.8(-34.7)(+56.7) kpc, respectively. Taken altogether, these properties favour the scenario of Dra II being a potentially disrupting dwarf galaxy. The low-significance extra-tidal features we map around the satellite tentatively support this scenario.
000262435 650__ $$aAstronomy & Astrophysics
000262435 650__ $$aAstronomy & Astrophysics
000262435 6531_ $$agalaxies: dwarf
000262435 6531_ $$agalaxies: individual: draco ii
000262435 6531_ $$alocal group
000262435 6531_ $$ana-o anticorrelation
000262435 6531_ $$amilky-way satellite
000262435 6531_ $$aglobular-cluster
000262435 6531_ $$ahorizontal branches
000262435 6531_ $$astellar-systems
000262435 6531_ $$aomega-centauri
000262435 6531_ $$alocal group
000262435 6531_ $$aursa-major
000262435 6531_ $$afaint
000262435 6531_ $$adiscovery
000262435 700__ $$aLongeard, Nicolas
000262435 700__ $$aMartin, Nicolas$$0247039
000262435 700__ $$aStarkenburg, Else
000262435 700__ $$aIbata, Rodrigo A.
000262435 700__ $$aCollins, Michelle L. M.
000262435 700__ $$aGeha, Marla
000262435 700__ $$aLaevens, Benjamin P. M.
000262435 700__ $$aRich, R. Michael
000262435 700__ $$aAguado, David S.
000262435 700__ $$aArentsen, Anke
000262435 700__ $$aCarlberg, Raymond G.
000262435 700__ $$aCote, Patrick
000262435 700__ $$aHill, Vanessa
000262435 700__ $$aJablonka, Pascale$$0245069
000262435 700__ $$aGonzalez Hernandez, Jonay I.
000262435 700__ $$aNavarro, Julio F.
000262435 700__ $$aSanchez-Janssen, Ruben
000262435 700__ $$aTolstoy, Eline
000262435 700__ $$aVenn, Kim A.
000262435 700__ $$aYouakim, Kris
000262435 773__ $$k2$$j480$$q2609-2627$$tMonthly Notices Of The Royal Astronomical Society
000262435 8560_ $$fyves.revaz@epfl.ch
000262435 909C0 $$zPasquier, Simon$$0252365$$yApproved$$pLASTRO$$xU10933$$myves.revaz@epfl.ch
000262435 909CO $$particle$$ooai:infoscience.epfl.ch:262435$$pSB
000262435 961__ $$afantin.reichler@epfl.ch
000262435 973__ $$aEPFL$$sPUBLISHED$$rREVIEWED
000262435 980__ $$aARTICLE
000262435 980__ $$aWoS
000262435 981__ $$aoverwrite
000262435 999C0 $$xU11963$$pPV-LAB$$zMarselli, Béatrice$$mhassan.laaroussi@epfl.ch$$mchristophe.ballif@epfl.ch$$0252194