Local Group Galaxies Divakara Mayya INAOE Advanced Lectures on Galaxies (2008 INAOE): Chapter 1 and 3a

Reference Ultra Deep Field Galaxies in the Universe: An Introduction Linda S. Sparke and John S. Gallagher

Binggeli Adopted from Eva K. Grebel Astronomical Institute University of Basel Astro-ph/

3 Grebel 1999

LMC: Multi-wavelength view

LMC and SMC: Milky Way’s satellites

4 The Local Group Grebel 1999 dSphs dEs dSph/dIrrs dIrrs

2 Why the Local Group? Ultra Deep Field Proximity  Resolution (individual stars) ‏  Depth (faintest absolute luminosities) ‏  Measurements of:  Lowest stellar masses  Oldest stellar ages  Metallicities, element abundances  Detailed stellar and gas kinematics  Highest level of detail and accuracy Variety (of galaxy types) ‏  Range of masses, ages, metallicities  Range of morphological types  Range of environments Tests of galaxy evolution theories Understanding distant, unresolved galaxies

9 Buonanno et al. 1998

13 Age structure in a synthetic color- magnitude diagram Gallart et al Shown: Constant star formation rate from 15 Gyr to the present, no photom. errors. Global star formation histories

14 Smecker-Hane, Gallagher, Cole, Stetson, 2002, ApJ, 566, Star CMDs from WFPC2: LMC Star Formation Histories DiskBar

CMDs: Galactic bulge vs LMC disk

Fornax dwarf spheroidal galaxy

Carina dwarf spheroidal galaxy: M/L=74

10 Feltzing et al. 1998; Wyse et al Luminosity function of Ursa Minor: Indistinguishable from Galactic globulars

5 Morphological Segregation Grebel 2000 Gas-poor, low-mass dwarfs Gas-rich, higher-mass dwarfs

6 1. The Earliest Epoch of Star Formation Cold dark matter models predict: Low-mass systems: first sites of star formation (z ~ 30) ‏ Larger systems form through hierarchical merging of smaller systems Re-ionization may squelch star formation in low-mass substructures Galaxies less massive than 10 9 M  lose star- forming material during re-ionization Kravtsov & Klypin (CfCP & NCSA) ‏

7 Consequences:  Low-mass galaxies must form stars prior to re- ionization; must contain ancient populations  Sharp drop / cessation of star formation activity after re-ionization, may resume only much later  High-mass galaxies’ oldest populations must be as old as low-mass galaxies’ populations or younger Testable predictions! Redshifts of not (yet?) accessible Dwarf galaxies at those redshifts would be extremely difficult targets anyway  Exploit fossil record in nearby Universe instead  Local Group ideal target since oldest populations resolved and accessible with HST 1. The Earliest Epoch of Star Formation

10 1. The Earliest Epoch of Star Formation Old populations ubiquitous but fractions vary Evidence for a common epoch of star formation  Globular clusters with main-sequence photometry (Galactic halo & bulge,Sgr, LMC,For) ‏  Field populations with main-sequence photometry (Sgr,LMC,Dra,UMi,Scl,Car,For,LeoII) ‏  Inferred from globular clusters (e.g., BHBs, spectra): M31, WLM, NGC 6822) ‏  Inferred from BHBs in field populations: Leo I, Phe, And I, II, III, V, VI, VII, Cet, Tuc Possible evidence for delayed formation?  Inferred from GC MS: SMC’s NGC 121 (2-3 Gyr). (However, lack of ancient globulars does not imply absence of ancient field population.) ‏ Results (largely based on HST):

11 1. The Earliest Epoch of Star Formation Limitations: Deep data for direct (MSTO) age measurements lack in dwarfs beyond ~ 300 kpc. True fraction of old stars still poorly known (incomplete area coverage & unknown tidal loss) ‏ No data on Population III stars and their ages Confirmed: Ancient Population II in Milky Way, LMC, and dwarf spheroidal galaxies ~ coeval (± 1 Gyr) ‏  Consistent with building block scenario All galaxies studied in sufficient detail so far contain ancient populations In contrast to CDM predictions: No cessation of star formation activity in low-mass galaxies during re-ionization Considerable enrichment: Episodes of several Gyr Grebel & Gallagher 2004

12 Grebel & Gallagher 2004 Star formation activity in low-mass galaxies (~10 7 M  ) ‏ Cosmology: flat,  m = 0.27, H 0 = 71 km/s/Mpc

16 Correlation between SFH and distance

17 Star formation history - distance correlation Faint (M V > -14) Milky Way companions: Increasingly higher intermediate-age population fractions with increasing distance from the MW  Environmental influence of Milky Way? Star-forming material might have been removed earlier on from closer companions via  ram-pressure stripping  SN-driven winds from Milky Way  high UV flux from proto-Milky Way  tidal stripping (van den Bergh 1994) ‏ If environment is primarily responsible for gas- poor dSphs, then existence of isolated Cetus & Tucana is difficult to understand. Caveat: Argument considers only present-day distances; orbits still poorly known / unknown.

18

19 If the apparent trend of low-mass galaxy properties with distance from the primary generally holds, we should also find it for M31’s low-mass companions…

20 No obvious distance correlation for M31 dSphs More luminous dwarf Harbeck, Gallagher, & Grebel 2004

21 3. Harrassment and Accretion Can we find evidence for this in the surroundings of massive galaxies in the Local Group? in the massive galaxies of the Local Group themselves?  Structural properties of nearby galaxies  Stellar content and population properties of nearby galaxies (including abundance patterns) ‏  Streams around and within massive galaxies Dwarf galaxies might be considered the few survivors of a once more numerous dark matter “building block” galaxy population.

22 Hierarchical structure formation: Numerous mergers leave imprint on halo (and disk) ‏ Thus expected:  Overdensities  Lots of streams  Identification photometrically / kinematically 2MASS + Johnston streams

3. Dwarf galaxy accretion: Sagittarius’ tidal stream within the Milky Way 23 2MASS: Detection of Sgr’s tidal stream across the entire sky (area coverage advantage of shallow of all-sky survey). Recent detection of second dSph in state of advanced accretion: Monoceros (SDSS, Newberg et al ); “CMa dSph”. Majewski et al. 2003

25 Ibata et al. 2001, Ferguson et al Zucker et al ongoing HST follow-up

26 Brown et al Extremely deep HST imaging of M31’s halo Old populations present, but intermediate -age, metal-rich populations dominate.

32 Essential science: The Local Group as a test case for galaxy evolution theories What we know now: All nearby galaxies contain ancient populations; fractions vary; ~ coeval Population II. No two galaxies alike in star formation histories, population fractions, mean metallicities and abundance spreads. But: global correlations (e.g., mass-metallicity) ‏ Environmental impact and CDM building blocks: Morphology-density Distance - HI content Accretion events Coeval ancient SF But: Tucana, Cetus Uncertain distance - SFH Number and [  / Fe] Extended SF in low-mass galaxies (vs. reionization) ‏

Galaxies (Class III): Types Giant galaxies Dwarf galaxies Galaxies with a prominent nucleus E Sp IrrI, IrrII Peculiar LSB dE dSph dIrr HII, BCD, Haro … Starburst, post-starburst AGN

Ellipticals, lenticulars, spirals and irregulars fit into the classical Tunic-fork diagram What about the rest?

Irregular II or Amorphous galaxies

Ring galaxies (Romano et al 2008)

Ellipticals: 4 Flavors Giant cDs, centers of clusters/groups, masses 10^13-10^14 Msolar Normal Es: Masses from 10^8 (not many, M32 holds down the low mass range of most correlations…) to 10^13 Msolar Spheroidals: dSphs in the local group, lower surface brightness dwarfs (10^7-10^9) in clusters Dwarf Ellipticals