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An ACS High-latitude Survey
The stellar perspective......

Neill Reid, STScI
1. 2. 3. Starcounts 101 Galactic halo ­ science issues Observational strategies


Starcounts 101
· N(d) (d) . V(d) ~ (d) .d^2 . d where d is the distance along the line of sight Density laws disk - double exponential

·

H~2500 pc (radial) 92% h~300 pc (vertical) thick disk - double exponential H~3500 pc 8% h~700 pc halo - radial power-law, n ~ 3 to 3.5 0.1%

·

Preferred distance for each population ~ 2h


Starcounts 101
· N(d) (d) . V(d) ~ (d) .d^2 . d where d is the distance along the line of sight Density laws disk - double exponential

·

H~2500 pc (radial) 92% h~300 pc (vertical) thick disk - double exponential H~3500 pc 8% h~700 pc halo - radial power-law, n ~ 3 to 3.5 0.1%

·

Preferred distance for each population ~ 2h


m-M disk TD halo 9 12 16

Fainter apparent magnitude = Fainter absolute magnitude


Bimodal distribution (J, (J-F)) Kron (1978) - NGP blue stars ­ halo red stars - disk


Bimodal distribution (J, (J-F)) Kron (1978) - NGP blue stars ­ halo red stars - disk


Analysing starcounts
1. 2. 3. Galactic structure analyses are based on photometric parallax (colour, mag.) > ([M/H], luminosity) > distance The disk is well-sampled at bright magnitude (V<19) The halo is well sampled at faint magnitudes (V>20) Stars outnumber galaxies V < 20 Galaxies outnumber stars V > 21 high spatial resolution is essential at faint magnitudes


Analysing starcounts
1. 2. 3. Galactic structure analyses are based on photometric parallax (colour, mag.) > ([M/H], luminosity) > distance The disk is well-sampled at bright magnitude (V<19) The halo is well sampled at faint magnitudes (V>20) Stars outnumber galaxies V < 20 Galaxies outnumber stars V > 21 high spatial resolution is essential at faint magnitudes


Analysing starcounts
1. 2. 3. Galactic structure analyses are based on photometric parallax (colour, mag.) > ([M/H], luminosity) > distance The disk is well-sampled at bright magnitude (V<19) The halo is well sampled at faint magnitudes (V>20) Stars outnumber galaxies V < 20 Galaxies outnumber stars V > 21 high spatial resolution is essential at faint magnitudes

HST is favoured for studies of the Galactic Halo


Stellar Number Densities
Baseline ­ Keck LRIS observations of PSR1640 field (l=41, b=38) 42 sq. arcmin VRI (Reid et al, 1996) ~4 ACS WFC fields R N(stars) N(galaxies) 21.5 30 99 22.5 33 208 23.5 44 435 24.5 75 911 ~50% Halo, ~50% Disk (all components)


Stellar Number Densities
Baseline ­ Keck LRIS observations of PSR1640 field (l=41, b=38) 42 sq. arcmin VRI (Reid et al, 1996) ~4 ACS WFC fields R N(stars) N(galaxies) 21.5 30 99 22.5 33 208 23.5 44 435 24.5 75 911 ~50% Halo, ~50% Disk (all components)


Science Issues
Halo structure : average density distribution sub-structure/tidal tails chemical abundance distribution stellar luminosity/mass function lensing/MACHOs intrinsic variability rare objects

Miscellania

:


H1: The Halo Density Law
Two principal parameters : power-law exponent, n axial ratio, c/a

Ground-based starcounts ­ overall (V, (B-V)) RR Lyraes globular clusters generally favour n ~ 3 to 3.5, c/a ~ 0.8 to 1 Halo structure may be complex ­ flattened inner halo ( bulge?) - near-spherical outer halo Tri-axial? Truncation ­ where does the halo end?


H2: Sub-structure
Originally detected kinematically ­ Majewski, Munn & Hawley (1994) - signature of merger fragments - tidal disruption evident in Sagittarius dwarf, globulars At least a subset of the halo is not kinematically well-mixed Surveys ­ Majewski, Johnston et al Morrison, Mateo et al (Spaghetti group) Are there perceptible spatial variations in the general halo starcounts? How lumpy is the halo?


H3: Chemical Abundance
The halo abundance distribution is known locally - high-resolution spectroscopy of proper motion stars Limited information in the far halo ­ globular clusters - metal-poor giants (selection?) <[M/H]> as f ( R ) probes formation mechanisms - relative importance of monolithic collapse and fragment accretion


H4: The Luminosity Function
(mag) + M/L relation gives (M) (M) is well measured for local stars ­ solar abundance Disk - globular clusters (dynamical effects?) What of the field halo? Complications: distances from photometric parallaxes - CMD varies a f([M/H]) non-linearities can bias (M) - very few VLM dwarfs


H4: The Luminosity Function
(mag) + M/L relation gives (M) (M) is well measured for local stars ­ solar abundance Disk - globular clusters (dynamical effects?) What of the field halo? Complications: distances from photometric parallaxes - CMD varies a f([M/H]) non-linearities can bias (M) - very few VLM dwarfs


Miscellania
1. Lensing/Machos ­ low density of background sources individual events are likely to be rare possible detection of high motion objects - but faint, distant, difficult to confirm Variability ­ interacting binaries - flare stars Rare objects ­ carbon dwarfs - ultracool M, L and T dwarfs Limited search volume ­ e.g. ~100 cubic parsecs for T dwarfs (2MASS ~ 14,000 cubic parsecs)

2. 3.


Strategies: Halo Structure
1. Multiple lines of sight over a range of (l, b) [H1, H2, H3, H4] - (l=90; b=30, 60) gives c/a - (l=90, 180; b=30/60) measures triaxiality - 2+ fields at similar (l, b) for substructure [H1, H2, H4] Multicolour data are crucial ­ VRI(z) - add g (or ramp filters at Mgb?) for [M/H] [H3] How deep? V ~ 26, R ~ 25, I ~ 25 S/N ~ 20 - ~4000 secs VRI, ~6000 secs with z : 2 orbits/pointing How wide? 4 LRIS fields (~0.05 sq. deg.) ­ 16 ACS WFC/field 100-300 stars / mag R=21 to 25 Supplementary groundbased BVRI(z) V > 14, ~1 sq. deg. - disk starcounts in the same fields

2. 3. 4. 5.


Strategies: Miscellania
1. Require multiple epochs - t > 2 years for astrometry [M1, M2]

2.

- many visits for variability statistics Multicolour ­ at least 2 passbands [M1, M2] - gVRIz (+ Ramp filters?) for rare object detection

Desire for solid angle coverage competes against necessity for nultiple visits


Tentative Conclusions
A medium-deep, moderate solid-angle survey can provide interesting constraints on halo structural parameters Desiderata: a) well-sampled in (l, b) b) contiguous fields not required, but at least 10-16 ACS WFC fields within ~10 deg. c) 2 passbands essential, 3 more than useful Baseline survey: 4 fields, 16 WFC pointings/field 2 orbits/pointing = 128 orbits