The Structural Properties of Milky Way Dwarf Galaxies. Ricardo Muñoz (Universidad de Chile) Collaborators:

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1 The Structural Properties of Milky Way Dwarf Galaxies Ricardo Muñoz (Universidad de Chile) Milky Way inner 100 kpc Collaborators: Marla Geha (Yale) Patrick Côté (HIA/DAO) Peter Stetson (HIA/DAO) Josh Simon (Carnegie) George Djorgovski (Caltech) Felipe Santana (U. de Chile) Dwarf Galaxies (post-2005) Dwarf Galaxies (pre-2005)

2 2004: Eleven known Milky Way satellite galaxies. Visual searches provide no evidence for a larger population... (Simon & Blitz 2002, Willman et al. 2002, Whiting et al. 2002)

3 2005-present: SDSS has revolutionized the field Belokurov et al. (2006)

4 2005-present: SDSS has revolutionized the field Belokurov et al. (2006) tidal stream

5 2005-present: SDSS has revolutionized the field Belokurov et al. (2006) globular clusters tidal stream

6 2005-present: SDSS has revolutionized the field Belokurov et al. (2006) globular clusters new dwarf tidal stream

7 The New Milky Way Dwarf Galaxy Landscape Sloan Digital Sky Survey (SDSS) coverage Belokurov et al. (2006) The Satellite Numbers: Classical dsphs = 11 Ultra-Faint dwarfs = To SDSS depth, full sky = x17 80 To LSST depth, full sky > 400 MW dwarfs Name Year Discovered LMC B.C SMC B.C Sculptor 1937 Fornax 1938 Leo II 1950 Leo I 1950 Ursa Minor 1954 Draco 1954 Carina 1977 Sextans 1990 Sagittarius 1994 Ursa Major I 2005 Willman I 2005 Ursa Major II 2006 Bootes I 2006 Canes Venatici I 2006 Canes Venatici II 2006 Coma Berencies 2006 Segue I 2006 Leo IV 2006 Hercules 2006 Leo T 2007 Bootes II 2007 Leo V 2008 Segue II 2009 Pisces I 2009 Bootes III 2009 Pisces II 2010

8 How faint are the Milky way dwarfs? Fornax Sculptor Carina Sextans from

9 How faint are the Milky way dwarfs?

10 How faint are the Milky way dwarfs?

11 How faint are the Milky way dwarfs?

12 Photometric Properties of Milky Way dwarf galaxies Globular Clusters Classical Dwarf dsphs Luminosity Size Martin et al. (2008)

13 Photometric Properties of Milky Way dwarf galaxies Globular Clusters Classical Dwarf dsphs Luminosity UFDs Size Martin et al. (2008)

14 Why do we call them galaxies?: kinematics UFDs M/L dsph UFDs seem to be the most dark matter dominated systems in the Universe! GCs MW Mass Wolf et al. (2010)

15 New luminosity regime poses a serious challenge to do a proper photometric characterization.

16 New luminosity regime poses a serious challenge to do a proper photometric characterization. SDSS photometry Belokurov et al. (2007)

17 A New Deep Survey (CFHT/Magellan)

18 Comparison between SDSS y Megacam Coma Berenices, Belokurov et al. (2007) Muñoz, Geha & Willman (2010) SDSS photometry Megacam photometry

19 Photometric Properties of Milky Way dwarf galaxies Mr rhalf (pc) Muñoz et al. (2014)

20 Photometric Properties of Milky Way dwarf galaxies Mr rhalf (pc) Muñoz et al. (2014)

21 Photometric Properties of Milky Way dwarf galaxies Mr rhalf (pc) Muñoz et al. (2014)

22 Photometric Properties of Milky Way dwarf galaxies Mr Line of constant surface brightness rhalf (pc)

23 Photometric Properties of Milky Way dwarf galaxies Muñoz et al. (2014)

24 Photometric Properties of Milky Way dwarf galaxies Surface brightness floor probably a selection bias Muñoz et al. (2014)

25 Photometric Properties of Milky Way dwarf galaxies Surface brightness floor probably real. Muñoz et al. (2014)

26 Photometric Properties of Milky Way dwarf galaxies Muñoz et al. (2014)

27 Photometric Properties of Milky Way dwarf galaxies Galaxies are intrinsically elongated Muñoz et al. (2014)

28 Photometric Properties of Milky Way dwarf galaxies Galaxies are intrinsically elongated Globular Clusters seem intrinsically round Muñoz et al. (2014)

29 Photometric Properties of Milky Way dwarf galaxies Muñoz et al. (2014)

30 Photometric Properties of Milky Way dwarf galaxies Muñoz et al. (2014)

31 Photometric Properties of Milky Way dwarf galaxies Muñoz et al. (2014)

32 Metallicity-Luminosity Relationship [Fe/H] Metallicity-Luminosity relationship also suggests that UFDs are indeed galaxies. Luminosity (Lsun)

33 Metallicity-Luminosity Relationship Metallicity-Luminosity relationship also suggests that UFDs are indeed galaxies.

34 Metallicity-Luminosity Relationship UFDs? Metallicity-Luminosity relationship also suggests that UFDs are indeed galaxies.

35 Metallicity-Luminosity Relationship or tidally disrupting? Metallicity-Luminosity relationship also suggests that UFDs are indeed galaxies.

36 The Future

37 The Future Bullock et al. (2009) Diemand et al. (2008)

38 final thoughts Milky Way dwarfs are good probes of dark matter and galaxy formation: Good targets for indirect dark matter detection experiments (Fermi, ACTs). Phase space density constraints. Good for studying galaxy formation thresholds. However, the UFDs represent a new regime in luminosity that greatly impacts our ability to study them High quality, deep photometry is required to determine reliable structural parameters and to investigate their morphologies. CFHT/Magellan survey is nearly finished. It represents the deepest and most comprehensive database for outer halo structure. STAY TUNED. The Future is bright, only 1% of virial volume of Milky Way has been exhaustively searched (and only northern sky)

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