Galaxy disk masses from stellar kinematics - physics.ox.ac.uk · Galaxy Masses, Oxford, 21-25 July...
Transcript of Galaxy disk masses from stellar kinematics - physics.ox.ac.uk · Galaxy Masses, Oxford, 21-25 July...
Galaxy Masses, Oxford, 21-25 July 2014
Marc Verheijen!Kapteyn Astronomical Institute
• Motivation!
• The DiskMass Survey!
• Sample & data!
• From σz to M✶/LK!
• Baryon fractions and DM haloes!
• stellar M/L and SSP models!
• Disk Mass from Asymmetric Drift !
• Concluding remarks
Outline
Galaxy disk masses from stellar kinematics!highlights from the DiskMass Survey!
Bershady, Verheijen, Westfall, Martinsson, Swaters, Andersen
Galaxy Masses, Oxford, 21-25 July 2014
SparsePak - I! PPak - I ! SparsePak - II! PPak - II!!I. overview!II. error budget!III. XC technique!IV. UGC 463!V. disks are sub-maximal!VI. PPak data!VII. RC decompositions!VIII. Disk stability and SF!IX. HI observations!……
Bershady et al, 2004!Verheijen et al, 2004!Bershady et al, 2005!Kelz et al, 2006!!Bershady et al, 2010!Bershady et al, 2010!Westfall et al, 2011!Westfall et al, 2011!Bershady et al, 2011!Martinsson et al, 2013!Martinsson et al, 2013!Westfall et al, 2014!Martinsson et al, 2014
Martinsson, PhD thesis! Groningen
DiskMass Survey - Publications
http://dissertations.ub.rug.nl/faculties/science/2011/t.p.k.martinsson/thesis_martinsson.pdf
Instrumentation :
Galaxy Masses, Oxford, 21-25 July 2014
Motivation
Extended HI rotation curves:
Acurate measure of Mdyn(r),!often reaching far into DM halo.
Rotation curve decomposition !is highly degenerate,!even with 2-param halo models.
Requires independent measure !of stellar mass to determine!Mbar/Mdyn , ρDM(r) , Jz , etc
Two approaches:!‣ SPS modeling!‣ stellar kinematics
‣ break the disk-halo degeneracy →ρ (R)!‣ dynamical calibration of SSP models
DM
Galaxy Masses, Oxford, 21-25 July 2014
Use statistical measure of disk thickness hz from edge-on galaxies... ...apply relation to face-on galaxies!
for which σz can be measured.
* 1.5<k<2 for exp, sech sech2
Dynamical disk mass surface density
vertical distribution*
disk!thickness
vertical oscillations
Σdyn = 100 k hz σz
1.5 444 pc 30 km/s
-1 -1 2M⦿ pc-2⎞
⎠⎝⎛
⎝⎛
⎝⎛⎞⎠
⎞⎠
For a collisionless, isothermal disk in equilibrium:
A dynamical measure of disk mass
disk
Galaxy Masses, Oxford, 21-25 July 2014
disk scale height and scale length
From surveys of edge-ons :
Schwarzkopf & Dettmar 2000!Kregel+ 02, 04!Xilouris+ 97, 99 Log(hR/hz) = 0.367 Log(hR/kpc) + 0.708 ± 0.095
Galaxy Masses, Oxford, 21-25 July 2014
The DiskMass Survey
• Two custom-built, large-fiber, wide-field! fiber bundles on 3.5m telescopes.!
• Phase A:!• 145 Hα velocity fields!• UBVRI, JHK images!
➞ Kinematic inclinations (i≥15)!➞ Tully-Fisher and asymmetry studies !
• Phase B:!• 40 stellar σlos measurements ! ➞ MgIb & CaII at R≈7.500-10.000!• Spitzer 4.5, 8, 24, 70 μm images! ➞ SFR & proxy for molecular gas!• HI aperture synthesis imaging (VLA, WSRT, GMRT)!
➞ extended rotation curves & atomic gas
SparsePak/WIYN PPak/Calar Alto
UGC 6918 Hα velocity field
Hα + HI!velocity field
➞ Measure Σdisk versus color, L, μ, SFR, etc!➞ Determine M★/L and ρDM
Galaxy Masses, Oxford, 21-25 July 2014
50x50 kpc - SDSS
a wide range in physical size, morphology, surface brightness and colour
DMS sample: physical sizes
Galaxy Masses, Oxford, 21-25 July 2014
2x2 arcmin - SDSS
a wide range in physical size, morphology, surface brightness and colour
DMS sample: morphologies
Galaxy Masses, Oxford, 21-25 July 2014
2x2 arcmin - SDSS & SparsePak Hα velocity fields
a wide range in physical size, morphology, surface brightness and colour
DMS sample: Hα velocity fields
Galaxy Masses, Oxford, 21-25 July 2014
40 nearly face-on spirals B-band 2.1m DSS Red Spitzer 8 μm Spitzer 24 μm SDSS (50x50 kpc)
a representative sample
Galaxy Masses, Oxford, 21-25 July 2014
40 nearly face-on spirals
x100 in luminosity x10 in surface-brightness 2 mags in B-K colour
a representative sample
Galaxy Masses, Oxford, 21-25 July 2014
λ = 4975−5375 Å R≈7500 Texp = 5−11 x 3600 sec
intensity observed VF model VF residual VF velocity disp. S/N
PPak IFU spectroscopy
Galaxy Masses, Oxford, 21-25 July 2014
continuum
EW [OIII]
σlos
σ starslos
σ gas
los
V gas
sin(i)c
V star
sin(i)c
V sin(i)c ✶ : stars!o : gas
✶ : stars!o : gas
PPak : stellar and gas kinematics
Galaxy Masses, Oxford, 21-25 July 2014
Radial σz(R) profiles follow expectations
For an exponential disk : hσ,z = 2 hR
Galaxy Masses, Oxford, 21-25 July 2014
HI 21cm spectral line aperture synthesis imaging
from VLA, WSRT, GMRT
Galaxy Masses, Oxford, 21-25 July 2014
HI 21cm spectral line aperture synthesis imaging
from VLA, WSRT, GMRT
Galaxy Masses, Oxford, 21-25 July 2014
MHI
ΣHI / ΣHImax vs R/RHI
DHI (kpc)
ΣHIave
MHI vs DHI at 1 M⦿/pc2
Log(MHI) = 1.72 Log(DHI) + 6.92
Resolved HI scaling relations
self-similar ΣHI(R) profiles
Galaxy Masses, Oxford, 21-25 July 2014
Vflat = 120−250 km/s Rmax = 4−10 hR
physical normalised & scaled
HSB !LSB
HSB !LSB
HI rotation curves
Galaxy Masses, Oxford, 21-25 July 2014
From μK and σz to Mdyn/L and M★/L
Radius (arcsec)
σ z (
km/s
)
Radius (arcsec)
Σ (M
⦿/p
c2 ) o: dyn!⦁:stellar
HI
H2
Σ★ = Σdyn − ΣHI − ΣH2
Σdyn = σz2 / π G k hz
Radius (arcsec)
M★/L
K
M★/LK = Σ★ / μK
Radius (arcsec)
μ K (
mag
/�)
bulge
maximum disk
Galaxy Masses, Oxford, 21-25 July 2014
V★,disk
V★,bulge
VHI+HeVmolec
VDM
Vc
cored pseudo-ISO cuspy NFW
Vc = V★,bulge + V★,disk + Vatom + Vmolec + VDM2 2 2 2 2 2
= Vbar + VDM2 2
Rotation curve decompositions with (M★/LK)dyn
VHαVHI
Galaxy Masses, Oxford, 21-25 July 2014
Baryon fraction!Fbar ≡ Vbar / Vc
Contribution of baryons to Vc
Maximum disk
Fb ≈ 0.4−0.7 at R>hR
Galaxy Masses, Oxford, 21-25 July 2014
DM halo parameters from RC decompositions
⦁ : based on (M/L)dyn !o : maximum disk
⦁ : based on (M/L)dyn !o : maximum disk
Bullock et al (2001)
Galaxy Masses, Oxford, 21-25 July 2014
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−iu−
g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−gτ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−iu−
g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Bruzual & Charlot 2003: Chabrier IMF, Padova’94 tracks, τ models for solar metallicity
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.3 Gyr
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 1 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 8 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
CSFR
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−gτ = 0.1 Gyr
Bruzual & Charlot 2003: Chabrier IMF, Padova’94 tracks, τ models for solar metallicity
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.3 Gyr
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 1 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 8 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
CSFR
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Bruzual & Charlot 2003: Chabrier IMF, Padova’94 tracks, τ models for solar metallicity
DMS
0 1 2
2
1
0
g−iu−
g
τ = 0.3 Gyr
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 1 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 8 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
CSFR
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Bruzual & Charlot 2003: Chabrier IMF, Padova’94 tracks, τ models for solar metallicity
DMS
0 1 2
2
1
0
g−iu−
g
τ = 0.3 Gyr
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 1 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 8 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
CSFR
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
g-i g-i g-i g-i
u-g
Bruzual & Charlot (2003): Chabrier IMF, Padova’94 tracks, solar metallicity, τ models :
DiskMass Survey : dynamical measurement of stellar M/L Bershady et al (2014)M★/LK from dynamical data and SPS models
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
g-i g-i g-i
u-g
Galaxy Masses, Oxford, 21-25 July 2014
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−iu−
g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−gτ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−i
u−g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
0 1 2
2
1
0
g−i
u−g
τ = 0.1 Gyr
Maraston 2005: Kroupa IMF, Geneva tracks, τ models for solar metallicity
DMS
AB=0.5
0 1 2
2
1
0
g−iu−
g
τ = 0.25 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 0.5 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 2 Gyr
DMS
0 1 2
2
1
0
g−i
u−g
τ = 5 Gyr
DMS
0 1 2
2
1
0
g−iu−
g
τ = 20 Gyr
Bershady et al. 2014
DMS
M/L*K
0.1
0.25
0.4
0.55
0.7
g-i g-i g-i g-i
u-g
Maraston (2005): Kroupa IMF, Fuel Consumption Theorem, solar metallicity, τ models :
DiskMass Survey : dynamical measurement of stellar M/L Bershady et al (2014)M★/LK from dynamical data and SPS models
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
.5 1 1.52
1.5
1
.5
g−i
u−g
DiskMass Survey: dynamical measurements of stellar M/L (Bershady et al. 2014)
0 1 2
2
1
0
g−i
u−g
0 1 2
2
1
0
g−i
u−g
AB=0.50.3
0.0
M/L*K
0.1
0.25
0.4
0.55
0.7
g-i g-i g-i
u-g
Galaxy Masses, Oxford, 21-25 July 2014
Dynamical Disk Masses using Asymmetric Drift
See poster by Kyle Westfall!(downstairs to left)
Example: UGC 448
Vga
sV
star
sσ s
tars
Disk mass using!asymmetric drift to infer σstars
Disk mass using σstars directly≈
Galaxy Masses, Oxford, 21-25 July 2014
Conclusions
• σz declines exponentially with radius (hσ,z ≈2 hR )!
• sub-maximal disks with 0.4<Fbar<0.7 for R>hR!
• consistent NFW pars for sub-maximal disks!
• (M★/LK)dyn consistent with Maraston’05 models! (Kroupa IMF, FCT, TP-AGB, τ≈few Gyr)
Questions / implications:!
‣ build-up of M★ over cosmic time?!
‣ baryonic Tully-Fisher relation?!
‣ disk stability?