Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility:...
Transcript of Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility:...
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Galaxy fertility: nature versus nurture
the view from the local Universe
1
Fertility = Propensity to form stars given… stellar mass
fertility =
star formation rate
stellar mass
= sSFR
I Zw 18 = fertile NGC 3379 = M105 = infertile
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Happy independence day!
2
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Do galaxy properties depend on single parameter?
3
Internal stellar velocity dispersionBernardi et al. 03; La Barbera et al. 14 (early-type galaxies)
Stellar velocity dispersion in ETGs → stellar mass (not dark matter halo)
Mamon & Łokas 05a
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
“Central” galaxy properties = f(halo mass)st
ella
r mas
s
halo mass
observationssemi-analytical
simulationhydrodynamical
simulation
Bluck+16
abundance matching: N(>Mhalo) = N(>Mstars)Marinoni & Hudson 02 …
galaxy properties = f(σv) = f(Mstars) = f(Mhalo)
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Satellite galaxies: properties = complicated!st
ella
r mas
s
halo mass
Bluck+16
(former centrals)observations
semi-analyticalsimulation
hydrodynamicalsimulation
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Another parameter for central galaxies?
6
DM
con
cent
ratio
n
log stellar mass
Wojtak & Mamon 13
Mass-orbit modeling of central galaxies traced by their satellites
redder galaxies ⇐ earlier star formation higher DM concentration ⇐ earlier halo mass assemblystar formation history (SFH) = f(halo mass AND halo assembly time)“galaxy assembly bias”
Wechsler+02
Baade 44
age matching: N(>age halo) = N(>age stars)Hearin & Watson 13
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
SDSS Legacy SurveyZehavi+11
7
Zehavi+11;see Davis & Geller 76
Galaxy 2-point correlation functionsdP = [1 + wp(rp)] d⌦
Spatial correlation vs color (age)
red galaxies more strongly clustered
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Galaxy bimodality
8
Schawinski+14(see Strateva+01)
colo
r
log stellar mass
colo
r
in color Knobel+15
log stellar masslo
g sS
FR =
SFR
/mst
ars star forming
passive
in star formation rate (SFR)sSFR = SFR/(stellar mass) = fertility
all
early-type
late-type
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Physical Processes
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
What makes galaxies fertile?
10
presence of (cold) Molecular Gas
Star formation in Giant Molecular Clouds
Bigiel+11
SFR ~ (molecular mass) / 2.4 Gyr
molecular surface density
SFR
sur
face
den
sity
Kennicutt diagram
filled=localopen=global
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Galaxy mergers
11
1.induce starbursts2.consume gas & rapidly quench SF
Di Matteo +08
time (Myr)
SFR
/ SF
R(t=
0)
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
What else quenches the fertility?
• supernova explosions • jets from active galactic nuclei
(powered by supermassive black holes)
12
Internal processes:
heat up OR mechanically remove (ram pressure) cold gas supply
Dekel & Silk 86
Silk & Rees 98
see Dashyan+17 (in revision) for analytical comparison of mechanical feedback in AGN vs SNe
AGN feedback can be positive!Begeman & Cioffi 89; Rees 89; Gaibler+12; Bieri+15,16
heat up OR mechanically remove (ram pressure) cold gas supply
Dekel & Silk 86
Silk & Rees 98
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
What else quenches the fertility?
13
External processes:
Prevent gas from falling into galaxy:low mass: entropy (temperature) is too highhigh mass: infall is supersonic
Rees 86Birnboim & Dekel 03
independent of environment
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Fertility quenching by nurture (environment)
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gas infall
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 15
gas infall
Ram pressure from cluster gas suppresses: infall & possibly interstellar molecular clouds
Gunn & Gott 72
Cluster tides suppress infallLarson+80
Fertility quenching by nurture (environment)
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Tidal Stripping for Elongated Orbits
shell of tidal radius has zero energy singular isothermal profiles for galaxy & cluster
16
neglect spin & resonances Mamon 00, astro-ph/9911333; Tollet, Cattaneo, GM+17 more complicated schemes: Gnedin+95; D’Onghia+10
orbit pericenter
mgalaxy
(r)
mvir
galaxy
⇡
Vperi
Vcirc
(Rperi
)
�M
cluster
(Rperi
)
Mvir
cluster
fraction of retained mass
independent of mstars/Mcluster!
�vstar ⇡ atide(Rperi)
✓Rperi
Vperi
◆velocity impulse
atide = �a ⇡ GM(R)
R3r
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Ram Pressure Stripping for Elongated Orbits
singular isothermal profiles for galaxy & cluster
17
P = ⇢ICM(R)V 2cos ✓ram pressure
�v ⇡ P ⌃gasRperi
Vperivelocity impulse
orbit mass ratio pericenter
mgas
(r)
mvir
gas
⇡Vcirc
(Rperi
)
Vperi
�"⇢(R
peri
)V 2
peri
h⇢(R)V 2(R)iorbit
# mvir
galaxy
Mvir
cluster
!2/3
Mcluster
(Rperi
)
Mvir
cluster
fraction of retained gas mass
see also McCarthy+08, Ruggiero & Lima Neto 16
~ (mstars/Mgroup)2/3
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Ram Pressure beats Tides (in removing gas)!
18
-3.5
-3-2.5
-2.5
-2
-2
-2
-1.5
-1.5
-1.5
-1.5
-1.5-1
-1
-1
-1
-1-0.5
-0.5
-0.5
-0.5
0
0
0
0
Log M ret,rp /M ret,td
mgal /Mcluster
10 -4 10 -3 10 -2 10 -1 10 0
Rp/Ra
0.1
0.2
0.5
1
typical orbit elongations
Ram pressure dominates
Tides dominate
log (fraction-gas-mass-retained-RPS/fraction-total-mass-retained-TS)
Irina DVORKIN
peric
ente
r / a
poce
nter
galaxy mass / cluster mass
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Hydrodynamical simulation
19
Horizon-AGN
log Mstars/Mgroup < –4.5 –4.5 < log Mstars/Mgroup < –3.5 log Mstars/Mgroup > –3.5
orbital phase orbital phaseorbital phase
r/rvi
r(t)
mga
scold/m
axsS
FR
cold gas lost in single (several) orbit(s) for extreme (moderate) mass ratiossSFR drops in single (several) orbit(s) for extreme (moderate) mass ratios
Vladan Markov (M2 student)
extreme moderate
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Environmental quenching of fertility ⇒ segregation
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Segregation by nature
21
assembly bias: early collapsing halos: old stars
DM
con
cent
ratio
n
log stellar mass
Wojtak & Mamon 13
high density peaks collapse 1stt ~ (G ρ)–1/2
early assembling halos:more concentrated Wechsler+02
clustergalaxies
totalthreshold for red galaxies
red galaxies more frequent in & near clusters
see Kaiser 84; Evrard+90
primordial density field
galactic conformity to large distances?
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Questions• Are environmental trends = f(group finder)?
• Do our imperfect measures of environment blur/bias the environmental effects
• Is quenching fast OR slow?
• How far do environmental effects act on galaxy fertility?
• Is observed segregation caused by Nurture (environment) OR Nature (initial conditions)?
22
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Global environment: group mass
Local environment: galaxy position in group (central, inner/outer satellite)
Large-scale environment: filament/field
galaxies like MW = groups (w LMC/SMC, dwarf spheroidals…)?
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
How do we measure environment?
23
central galaxy
satellite galaxy
group
cluster clusterfilament
field
group/clustergalaxy
LEGEND
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
How to extract real-space groups from redshift-space data?
GM, Biviano & Murante 10
rmax
rvir
=
r�
2
✓�v
vv
◆' 11� 18
+κ σv
–κ σv
Dlos / r200
v los / v
200
∆ = overdensity / critical density
1993MNRAS.261..827M
real space
redshift space
Moore, Frenk & White 93
cz = H0D + vpec
redshiftdistortions
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Group finders for spectroscopic galaxy samples
• Frequentist • Friends-of-Friends • Voronoi Tessellation • Dendrograms
25
Huchra & Geller 82
Marinoni+02
• Prior-based • Matched Filter • Yang • MAGGIE
Kepner+99
Yang, Mo, van den Bosch +05, 07
Duarte & Mamon 15
incomplete list!
Tully 87
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Friends of Friends (FoF)
26
survey edge
survey edge
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Friends of Friends (FoF)
27
line-of-sight linking length
trans
vers
e lin
king
leng
th
Dimensionless linking lengths in terms ofmean nearest neighbor separation: b = LL/⟨n(z)⟩–1/3
Optimal linking lengths (analytical + tests on mocks)b⟂ = 0.07 & b// = 1.1 Duarte & Mamon 14
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Yang et al.’s Halo-based Group Finder
28
Yang, Mo & van den Bosch 04; Yang+07Domínguez Romero, García Lambas & Muriel 12
g(R, vz) = ⌃NFW(R) exp
✓� v2z2�2
LOS
◆> 10
c ⇢Univ
H0
group masses (hence virial radii) from: • FoF group luminosities (1st pass: M=300L) • Halo Abundance Matching on group luminosity (next passes)
• LOS velocity dispersion profile should be convex in log-log (not cst)• LOS velocity distributions not Maxwellian (outer radial vel. anisotropy)• ad hoc threshold for membership (10)• imprecise correction for lum. incompleteness (for SDSS flux-limited sample)• hard group assignment is unstable
weaknesses
Accurate group masses (global environment), BGG at center (local environment)
surfacedensity
density in projected phase spaceR = projected radius
vz = line-of-sight velocity
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
MAGGIE: Models & Algorithms for
Galaxy Groups, Interlopers & Environment
29
Duarte & Mamon 15
P (R, vz) =ghalo
(R, vz)
ghalo
(R, vz) + gilop
(R, vz)halo interlopersinterlopers
probabilistic
more realistic ghalo from ΛCDM 3D model with anisotropic velocitiesNFW
z
z
z
3D tracer density
σr(r) from solving Jeans equation β(r) from cosmo simulations
zz
3D LOSvelocity distrib.
= 1 – σθ2/σr2 = velocity anisotropy
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 30
Duarte & Mamon 15MAGGIE: interlopers
Mamon, Biviano & Murante 10
DM particles in HD simulation: Borgani+04
Duarte & Mamon 15
SAM: Guo+11
P (R, vz) =ghalo
(R, vz)
ghalo
(R, vz) + gilop
(R, vz)
zz
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
MAGGIE: Models & Algorithms for
Galaxy Groups, Interlopers & Environment
31
Mamon & Duarte 15
• group masses by Halo Abundance Matching‣ on central galaxy luminosity or stellar mass (1st pass)‣ on total group luminosity or stellar mass (next passes)
• groups extracted from D- & L-complete subsamples
• group properties = sums weighted by probabilities
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Testing Group Finders
32
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Tests on mocks: group fragmentationmocks: SDSS-like galaxy catalog with errors on luminosities (0.08 dex) & stellar masses (0.2 dex)
matching extracted & true groups bymost luminous (L) or massive in stars (M) member
FoF clusters: high probability of being secondary fragment!
fract
ion
of e
xtra
cted
gro
ups
= se
cond
ary
fragm
ents
of t
rue
grou
ps
Duarte & Mamon 15
FoF-M (solid)FoF-L (dashed) Yang-MYang-LMAGGIE-MMAGGIE-L
only unflagged groups Ntrue≧3 & Nest≧3
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Tests on mocks: group total mass accuracy
34
FoF virial theorem masses biased low by 0.15 - 0.5 dex, 0.3 dex at hi mass
only unflagged primary-fragment groups Ntrue≧3 & Nest≧3
Duarte & Mamon 15 log distance
log
lum
inos
ity
flux li
mit
1 2
FoF-M (solid)FoF-L (dashed) Yang-MYang-LMAGGIE-MMAGGIE-L
![Page 35: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/35.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Tests on mocks: group total mass accuracy
35
FoF virial theorem masses biased low by 0.15 - 0.5 dex, 0.3 dex at hi mass@log M = 13: 0.35 (FoF), 0.32 (Yang), 0.28 (MAGGIE) @log M = 14: 0.2-0.4 (FoF), 0.23 (Yang), 0.20 (MAGGIE) mass accuracy (dex)
only unflagged primary-fragment groups Ntrue≧3 & Nest≧3
Duarte & Mamon 15
FoF-M (solid)FoF-L (dashed) Yang-MYang-LMAGGIE-MMAGGIE-L
log distance
log
lum
inos
ity
flux li
mit
1 2
![Page 36: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/36.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Observational diagnostics of fraction of fertile galaxies
vs. environment
36
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Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Effects of galaxy environment on red galaxy fraction
37
Peng+10: red fraction boosted at hi density (for lo Mstars) or hi Mstars (at lo density)
in stars
Peng+10
effe
ct o
f den
sity
effect of stellar mass
over
den
sity
(fro
m d
ista
nce
to 5
th n
eare
st n
eigh
bor)
Weinmann+06
spectral types
Weinmann+06: passive fraction boosted at hi group mass (less by position)& for innermost satellites (even at hi Mstars!)
![Page 38: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/38.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Fraction of infertile galaxies
38
increases with halo, stellar mass, inner position in group(complicated!)
Woo+13see Weinmann+06; Peng+10; von der Linden+10
log Mstars/M⦿lo
g R
/r vir
log
R/r v
ir
log Mhalo/M⦿
![Page 39: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/39.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Environmental effects as a function of group finder
39
Diego STALDERformer Doctoral student
INPE
in progress
![Page 40: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/40.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
fraction of fertile galaxies in SDSS
fblue(R) = f1R
R+ ablueKnobel+15
log stellar mass (M⦿)
log
sSFR
(Gyr
–1)
logistic regression (see Maria-Luiza Dantas talk)
ln
✓fquenched
1� fquenched
◆= a+ b log
✓R
rvir
◆� 1
clog
"✓Mstars
10
10.5
◆e c
+
✓Mstars
10
10.5
◆f c#+ d log
✓M
10
13
◆
formula chosen after comparison of ≠ ones with Bayesian evidence
![Page 41: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/41.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
strong variation with stellar mass
41
f SF
log stellar mass
especially at low end
![Page 42: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/42.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
≠ group finders on SDSS
42
radial trend sharpness of Mstars
hi-end trend of Mstars lo-end trend of Mstarstrend of Mgroup
ln
✓fquenched
1� fquenched
◆= a+ b log
✓R
rvir
◆� 1
clog
"✓Mstars
10
10.5
◆e c
+
✓Mstars
10
10.5
◆f c#+ d log
✓M
10
13
◆
FoFYangMAGGIE
Stalder, GM& Trevisan in prep.
–
quenching normalization
![Page 43: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/43.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
≠ group finders on SDSS
43
radial trend sharpness of Mstars
hi-end trend of Mstars lo-end trend of Mstarstrend of Mgroup
FoFYangMAGGIE
Stalder, GM& Trevisan in prep.
FoF: weaker trend with group mass, less quenching …
–
quenching normalization
![Page 44: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/44.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
≠ group finders on mock SAM
44
quenching normalization radial trend sharpness of Mstars
hi-end trend of Mstars lo-end trend of Mstarstrend of Mgroup
Henriques+15
MAGGIE: correct normalization & radial trend; too weak lo-end trend with Mstars vs SDSS: similar parameters, except slightly ≠ powers of Mstars
Stalder, GM& Trevisan in prep.
FoFYangMAGGIEPerfect
![Page 45: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/45.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Radial variations
45
stellar mass →
← g
roup
mas
s f S
F
R/rvir
![Page 46: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/46.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
When are galaxies quenched as they fall into
groups & clusters?
46
![Page 47: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/47.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Time for quenching star formation
47
virialized
infalling
backsplash
cluster
orbital classes of galaxies
virialized
infalling
backsplashcluster
orbital classes of galaxies fr
actio
n of
rec
ent
star
burs
ts
projected radius
Mahajan, GM & Raychaudhury 11
z=0 radial phase space of DM particlesMahajan+11
Galaxies only quenched when they reach virial radius on their way out
frac
tion
of r
ecen
t st
arbu
rsts
physical radius
Mahajan+11
A=infall
Time to rvir outwards: 2.5-3 Gyr from entry, 1.5-1.75 Gyr from pericenter Tollet, Cattaneo, GM+17
slow quenching!
![Page 48: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/48.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Slow or fast quenching by environment?
48
Haines+15z=0 radial phase space of DM particles
1.7 Gyr after entry≈ < 0.5 Gyr after pericenter≣ Fast Quenching
Haines+15
z=0 projected phase space of DM particles
Oman & Hudson 16
4.5 Gyr after entry in 2.5 rvir≈ 0.75 Gyr after pericenter≣ Fairly Fast Quenching
cells of z=0 projected phase space of DM particles
Time to rvir outwards: 2.5-3 Gyr from entry, 1.5-1.75 Gyr from pericenter≣ Slow Quenching Tollet, Cattaneo, GM+17
4 Gyr from entry≣ Slow fading then fast quenching Wetzel+13
![Page 49: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/49.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Slow quenching
49
Peng+15 (Nature)
4 Gyr
![Page 50: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/50.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
How far does the environment act on galaxy fertility?
Marina TREVISANPostdoc, IAP
in progress
![Page 51: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/51.jpg)
fract
ion
of s
pect
ral t
ypes
von der Linden+10
distance from BCG / r200
log Mstars: 9.6-10 log Mstars: 10-10.3 log Mstars: 10.3-10.5
log Mstars: 10.5-10.7 log Mstars > 10.7
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
How far does the environment act on galaxy fertility?
2 r200 for low mstars10 r200 for high mstars
![Page 52: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/52.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Explanations for large-scale environmental effects
• processing in filaments?
• backsplash galaxies?
• primordial density field?
• (pre-)processing in groups below mass threshold?
52
von der Linden+10
![Page 53: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/53.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Backsplash?
53
Mahajan, GM+11
z=0 radial phase space of DM particles
Backsplash galaxies:have crossed cluster at least once
How far can they go?2 to 2.5 r100
Balogh, Navarro & Morris 00Mamon+04Gill+05
sometimes out to 3-4 r100 Sales, Navarro+07Ludlow, Navarro+098 r100: 50% of particles are bound
require ~4.3 σv to escape that far (possible) time to reach 8 r100 ≈ 2.3 Hubble times!possible if start at z=2! (t0/4)
infall
backsplash
![Page 54: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/54.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Assigning galaxies to nearest group
54
von der Linden+10: d =
s✓R
r200
◆2
+
✓v
�v
◆2
(Yang+07):
redshift space
d = f
(b⌃
✓R
r200, c
◆exp
"�✓
v
�v
◆2#)
d =
s✓R
r200
◆2
+�
2
✓v
v200
◆2
surfacedensity
log (R / rvir)
v los
/ v
vir
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−1.0 −0.5 0.0 0.5 1.0
0.0
1.0
2.0
3.0
−0.45 −0.05 0.35 0.75 1.15−0.85 1.35
log (r3D / rvir)
Yangz-space
real space distances in redshift spacefrom cosmological simulation
Trevisan+ in prep.
![Page 55: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/55.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Assigning galaxies to nearest group
55
von der Linden+10: d =
s✓R
r200
◆2
+
✓v
�v
◆2
�
�
�
��
��
-��� -��� -��� -��� ��� ��� ����
�
�
�
�
��� �/����
v ���/v ���
von der Linden
Yangz-space
Trevisan+ in prep.
(Yang+07):
redshift space
d = f
(b⌃
✓R
r200, c
◆exp
"�✓
v
�v
◆2#)
d =
s✓R
r200
◆2
+�
2
✓v
v200
◆2
surfacedensity
which minimum group mass to assign galaxies?
![Page 56: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/56.jpg)
Gary Mamon (IAP), Galaxies far beyond the virial radius of groups and clusters: the role of nature in the fraction of fertile galaxies, 22 June 2017, RoE/IfA
1-halo density profile to 20 rvir
56
Trevisan, GM & Stalder 17
NFW to 13 rvir for optimal group assignment mass in real spaceNFW to 10 rvir for optimal group assignment mass in redshift space
real space
Universe
num
ber d
ensi
tyre
sidu
als
redshift space
resi
dual
ssu
rface
num
ber d
ensi
ty
![Page 57: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/57.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
NFW-optimal group assignment mass
57
Trevisan, GM & Stalder 17
log Massign=12.3 for log Msample=13
![Page 58: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/58.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Fraction of star forming galaxies with better galaxy assignment scheme
58
Knobel+15
log stellar mass (M⦿)
log
sSFR
(Gyr
–1)
![Page 59: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/59.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
min group assignment log mass = 13
59
600
600
●
log M stars, gal →
←lo
g M
grou
p13
− 1
4
0.0
0.4
0.8
10 − 10.5
600
600 ●
10.5 − 10.8
600
600
●
10.8 − 11.3
600
600
14 −
15
0.0
0.4
0.8
0.01 0.1 1.0 10
R / rvir
f SF
600
600
0.01 0.1 1.0 10600
600
●
0.01 0.1 1.0 10
stellar mass →
← g
roup
mas
s = centrals
fSF saturates at R ≈ 4 rvir
field fraction & quenching radius = independent of group mass
R90 where fSF(R90) = 0.9 fSF(∞)
![Page 60: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/60.jpg)
600
600
●
log M stars, gal →
←lo
g M
grou
p13
− 1
4
0.0
0.4
0.8
10 − 10.5
600
600 ●
10.5 − 10.8
600
600
●
10.8 − 11.3
600
600
14 −
15
0.0
0.4
0.8
0.01 0.1 1.0 10
R / rvir
f SF
600
600
0.01 0.1 1.0 10600
600
●
0.01 0.1 1.0 10
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
min group assignment log mass = 12.3
60
600
600
●
log M stars, gal →
←lo
g Mgr
oup
12.3 −
13
0.00.2
0.40.6
0.81.0
10 − 10.5
600
600 ●
10.5 − 10.8
600
600
●
10.8 − 11.3
600
600
●
13 −
14
0.00.2
0.40.6
0.81.0
f SF
600
600
●
600
600
●
600
600
14 −
15
0.00.2
0.40.6
0.81.0
0.01 0.1 1.0 10
R / rvir600
600
0.01 0.1 1.0 10600
600
●
0.01 0.1 1.0 10
= centrals
stellar mass →
← g
roup
mas
s
⇒ pre-processing in groups of mass 12.3 to 13!
jump of fSF at 2.5 rvir (hi Mstars): lose quiescent small groups
fSF saturates at R ≈ 2 rvir(except for hi stellar mass)
![Page 61: Galaxy fertility: nature versus nurture - SAB · Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017 Tidal Stripping for Elongated Orbits shell](https://reader030.fdocuments.in/reader030/viewer/2022041216/5e057664e72dda709e5bce97/html5/thumbnails/61.jpg)
Gary Mamon (IAP), SAB keynote: Galaxy fertility: nature vs. nurture, São Paulo, 7 Sep 2017
Conclusions
61
• Are environmental trends = f(group finder)? Yes to some extent: try different group finders
• Do our imperfect measures of environment blur/bias the environmental effects? Yes: compare to mocks
• Is quenching fast OR slow? Fast after merging or strong ram pressure (low Mstars/Mgroup) Slow after moderate ram pressure (high Mstars/Mgroup)
• How far does environment act on galaxy fertility? = f(group min assignment mass) up to 2.5 virial radii
• Observed segregation by: Nurture (environment) OR Nature (initial conditions)? Mainly nurture!