The M31 Dwarf Galaxy Population

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1 The M31 Dwarf Galaxy Population Marla Geha (Yale) Google Sky IRAS map Raja Guhathakurta (UCSC) Jason Kalirai (STScI) Steve Majewski (UVa) Roeland van der Marel (STScI) Racheal Beaton (UVa) Kirsten Howley (LLNL) Nhung Ho (Yale) Erik Tollerud (UCI/Yale)

2 The M31 Dwarf Galaxy Population Marla Geha (Yale) 150 kpc Raja Guhathakurta (UCSC) Jason Kalirai (STScI) Steve Majewski (UVa) Roeland van der Marel (STScI) Racheal Beaton (UVa) Kirsten Howley (LLNL) Nhung Ho (Yale) Erik Tollerud (UCI/Yale) Google Sky IRAS map

3 The M31 Dwarf Galaxy Population 150 kpc 31 M31 satellites And XXIX And XXVIII Bell et al. (2011) Slater et al. (2011) PAndAS Survey: Richardson et al. (2011)

4 Local Group Dwarf Satellites Milky Way: 26 dwarf satellites M31: 31 (20) dwarf satellites v_mw (km/s) v_m31 (km/s) Dist_MW (kpc) Dist_M31 (kpc) McConnachie (2012)

5 Local Group Dwarf Satellites M31 dsph MW dsph MW GC Faintest M31 satellite MV = -6.1 PAndAS limit To this mag limit, M31 has 2.5x more satellites than MW SDSS limit

6 Quenched M31 Dwarf Satellites McConnachie (2012) Most MW/M31 satellites are quenched galaxies (no ongoing SF, little to no HI). MHI / LV Distance (kpc)

7 Environment and Quenched Dwarf Galaxies MG et al (2012): Quenched fractions as a function of distance to a massive host galaxy 0 out of 2950 quenched SDSS dwarf galaxies > 1.5 Mpc Below LMC stellar mass, *all* quenched galaxies found within ~4 rvir of a massive host.

Keck/DEIMOS Observations of M31 Satellites Majority of work on M31 satellite kinematics and metallicities enabled by Keck/DEIMOS spectrograph: Chapman et al. 2005, Geha et al. 2006, Majewski et al.

8 Keck/DEIMOS Observations of M31 Satellites Majority of work on M31 satellite kinematics and metallicities enabled by Keck/DEIMOS spectrograph: Chapman et al. 2005, Geha et al. 2006, Majewski et al. 2007, Kalirai et al. 2009, Letarte et al. 2009, Geha et al. 2010, Kalirai et al. 2010, Collins et al. 2010, Howley et al. 2012, Ho et al. 2012, Tollerud et al 2012 RGB stars selected from photometry. Typically Ca II triplet region, v ~2-3 km/s. Radial velocities for ~hundred of RGB stars in one hour in good conditions. spatial -> wavelength ->

9 A Quick Tour of M31 s Satellites LMC NGC 205 SMC Sgr For Leo I Scl

10 NGC 205 Tidal radius (5 = 1 kpc ) Geha et al. (2006) Simien & Prugniel (2000) velocity (km/s) radius (arcmin) Inner rotation = 15 km s -1 Velocity turn-over at tidal radius (730 stars) NGC 205 on first passage? (Howley et al. 2008)

11 A Quick Tour of M31 s Satellites LMC M32 NGC 205 SMC Sgr For Leo I Scl

2001; Verolme et al. 2002; Tremaine et al. 2002; van der Marel et al.

12 M32: Compact Elliptical with a Black Hole M32 has a central black hole MBH = (2.4± 1.0) 10 6 M : Goodman & Lee 1989; Bender, Kormendy & Dehnen 1996; van der Marel et al. 1998b; Joseph et al. 2001; Verolme et al. 2002; Tremaine et al. 2002; van der Marel et al. 1997; van den Bosch & de Zeeuw 2010 Based on kinematics within r_eff = 30 = 0.1 kpc Choi, Guhathakurta & Johnston (2002): Distorted M32 isophotes around 150, consistent with tidal interactions.

13 M32: Compact Elliptical with a Black Hole Howley et al. (2012) velocity (km/s) BH + M/L = 1.2 sigma (km/s) radius (arcmin) M32 kinematics appear well-behave out to large radius

14 A Quick Tour of M31 s Satellites LMC M32 NGC 205 SMC NGC 147 NGC 185 Sgr For Leo I Scl

15 NGC 147 and NGC 185: Normal des NGC 147 NGC 185 Keck/ DEIMOS spectroscopy HST WPFC2 HST ACS HST WFC3

16 NGC 147 and NGC 185: Normal des NGC 147 NGC 185 Vrot = 17 ± 2 km/s Vrot = 15 ± 5 km/s 8 r eff Geha et al (2010)

17 NGC 147 and NGC 185: Normal des NGC 147 Intermediate + old stars <age> ~ 7.5 Gyr HST/ACS: Geha et al. (2012) NGC 185 Intermediate + old stars <age> ~ 10 Gyr

18 A Quick Tour of M31 s Satellites LMC M32 NGC 205 SMC NGC 147 NGC 185 Leo I Scl For And II Sgr

19 Ho, MG, et al. (2012) And II v rad (km/s) (J2000) ( o ) Non member Member (J2000) ( o ) Radius (kpc) Prolate or triaxial rotation: dynamically stable?

20 And II M32 More M31 satellites with rotation as compared to MW

21 A Quick Tour of M31 s Satellites LMC M32 NGC 205 SMC NGC 147 NGC 185 Leo I Scl And V For And II Sgr And XII

22 And XII: M V = -6.2 sigma =?? (2 member stars) CMD Velocity Velocity vs. radius Tollerud et al. (2012) See also poster by M. Collins!

23 M31 vs. MW Satellite Systems from M. Collins sigma (km/s) MW M31

24 M31 vs. MW Satellite Systems McConnachie (2012) Dynamical Mass (<rh) MV MV MV

25 The M31 Dwarf Galaxy Population The Milky Way satellite system provides strong constrain on cosmological models (number of satellites, central densities, ages/metallicities) M31 satellites now have competitive observational dataset -- M31 satellite system is similar to MW: -- Basic scaling relations -- Evidence for on-going tidal interactions/merging -- M31 satellite system is different to MW: -- Basic scaling relations -- Number of satellites -- Detailed properties

Substructure in the Stellar Halo of the Andromeda Spiral Galaxy

Substructure in the Stellar Halo of the Andromeda Spiral Galaxy Raja Guhathakurta University of California Observatories (Lick, Keck, TMT) University of California at Santa Cruz M31 s extended stellar