Satellite Accretion and Disruption in the Caterpillar Simulations

Satellite Accretion and Disruption in the Caterpillar Simulations

W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
THE
C AT E R P I L L A R
PROJECT
BRENDAN GRIFFEN
MIT
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
C U R R E N T S TAT E - O F - T H E - A R T:
M I L K Y W AY S I Z E D S Y S T E M S
particle mass [M☉]
103
GHALO
Via Lactea II
104
Aquarius
Sawala et al.
105
1
BRENDAN GRIFFEN
6
ELVIS
12
48
Springel et al. (2006)
# of halos in suite
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
M A S S O F T H E M I L K Y W AY ?
We need more
halos…
this will enable a
statistical approach to
better understand the
assembly of the Milky
Way…
Wang et al. (2015)
BRENDAN GRIFFEN
but we also need
resolution.
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
C U R R E N T S TAT E - O F - T H E - A R T:
M I L K Y W AY S I Z E D S Y S T E M S
particle mass [M☉]
103
GHALO
Via Lactea II
104
Aquarius
Sawala et al.
105
1
BRENDAN GRIFFEN
6
ELVIS
70
12
48
Springel et al. (2006)
# of halos in suite
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
T H E C AT E R P I L L A R P R O J E C T
www.caterpillarproject.org
Anna Frebel
Brian O’Shea
Facundo Gómez
Greg Dooley
Alex Ji
Mark Vogelsberger
mass of halos
0.7 - 3 x 1012 M⦿
number of halos
70
cosmology
Planck13: σ8 = 0.83, Ωm = 0.31, ΩΛ = 0.68, ns = 0.96, h = 0.67
mass resolution
~ 104 M⦿
spatial resolution
~75 pc
temporal resolution
codes
10 Myrs/snapshot to z = 6, then ~50 Myrs/snapshot
MUSIC,Gadget-3/4,ROCKSTAR+,SUBFIND
data product
4-6TB/halo ~ 350 TB total
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
QUESTIONS
What is the origin and evolution of the Milky Way satellites?
Can we characterise the phase-space distribution of stars in
the solar neighbourhood?
Can we trace back these remnants to reconstruct the
assembly history of the Milky Way?
How do the bulk stream properties vary with host assembly?
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
A C C R E T I O N H I S T O RY
Aquarius
BRENDAN GRIFFEN
Caterpillar
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
A C C R E T I O N H I S T O RY
Aquarius
BRENDAN GRIFFEN
Caterpillar
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
F I R S T 2 4 C AT E R P I L L A R H A L O S
Springel et al. (2006)
Griffen et al. in prep.
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
STREAMS IN AQUARIUS
Cooper et al. (2010)
Gomez et al. (2013)
Springel et al. (2008)
Weisz et al. (2015)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
PRELIMINARY
RESULTS
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
0 - 10 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
10 - 30 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
30 - 50 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
50 - 80 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
80 - 120 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
120 - 150 KPC
Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
TA G G I N G A N D T H E S O L A R N E I G H B O U R H O O D
• tag 1% most bound at infall
• assign stellar masses using redshift dependent Moster et al. (2010)
abundance matching
• rotate halo to its principal axis (since halos are triaxial)
• place sphere along the direction of the major axis at 8 kpc
• select tagged particles within 2.5 kpc (set by Gaia)
• all methods above are being improved upon (e.g. proper SAM etc.)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
Enorm
S O M E H AV E V E R Y F E W S T R E A M S
Lz (103 kpc km/s) Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
Enorm
S O M E H AV E M A N Y S T R E A M S
Lz (103 kpc km/s) Springel et al. (2006)
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
[MIT | MKI]
NUMBER OF SIGNIFICANT PROGENITORS
Defined as the number of significant stellar mass contributors within 2.5kpc
of the solar neighbourhood. Count the number of halos that contribute to
90% of the stellar mass in that volume.
# Caterpillar halos
8
6
4
2
0
1
2
3
4
5
6
9
number of significant progenitors
BRENDAN GRIFFEN
RINGBERG CASTLE
W W W. C A T E R P I L L A R P R O J E C T. O R G
www.caterpillarproject.org
S
New High Resolution Simulation Suite Of Milky Way Sized Halos
70 halos, available at end of 2015
6
reliably resolve: M ~10 M⦿ progenitors
contamination free zones: 1 - 2 Mpc from host
[MIT | MKI]
U
M
M
A
R
Y
Status: On-going
24 completed, paper out very soon!
3
10 M⦿ high-z sims. running, hydro 2016
Converged mass functions, assembly histories & halo profiles.
Take Home Stream Science From Preliminary Results
Stream progenitors in Milky Way sized galaxies have widely different internal phase-space
configurations. The number of significant stellar mass progenitors across our sample is mostly
less than 5.
Moving Forward
We aim to statistically probe the formation history of Milky Way sized galaxies. Understanding
stream formation and evolution across varied assembly histories is crucial in interpreting
upcoming Gaia data! (& vice-versa!)
BRENDAN GRIFFEN
RINGBERG CASTLE