We use 3D models to make composite, intensity-weighted mock spectral lines, and then use MCMC to find the best fit V(RE), σ.

Internal galaxy structures

We find an trend of increasing V/σ with decreasing SSFR for both the galaxies with and without detected rotation. Our measurements are in excellent agreement with the trend found by Wisnioski et al. (2015).

This trend may be evidence for disk settling, with galaxies’ disks becoming thinner as a their gas fractions decrease.

�10.5 �10.0 �9.5 �9.0 �8.5 �8.0

log10(SSFRH↵/yr�1)

1

10

V2.

2/�

KMOS3D, z = 1KMOS3D, z = 2Unresolved,median

Resolved rotation, z⇠1.5Resolved rotation, z⇠2.3AGN

9.0 9.5 10.0 10.5 11.0 11.5

log10(M⇤/M�)

1

10

V2.

2/�

KMOS3D, z = 1KMOS3D, z = 2Unresolved,median

Specific SFR - V/σ

Wisnioski+15

Sedona H. Price1, Mariska Kriek1, Alice Shapley2, Naveen A. Reddy3,William R. Freeman3, Alison L. Coil4, Laura de Groot5, Irene Shivaei3, Brian Siana3,

Mojegan Azadi4, Guillermo Barro1, Bahram Mobasher3, Ryan L. Sanders2, Tom Zick1

1UC Berkeley, 2UCLA, 3UC Riverside, 4UCSD, 5Denison University

Kinematics of z~2 star-forming galaxies  with MOSDEF & CANDELS Price et al. 2016, ApJ, 819, 80

Galaxy structural evolution over cosmic time

We probe galaxy structures, masses, and kinematics to trace how star-forming galaxies grow over time. The MOSFIRE Deep Evolution Field Survey (MOSDEF; Kriek et al. 2015) is well-suited to study kinematics at z~2, as this survey provides rest-frame optical spectra for ~1500 galaxies in the CANDELS and 3D-HST fields at 1.4 ≤ z ≤ 3.8. We select a sample of 178 star-forming galaxies at 1.4 ≤ z ≤ 2.6. By combining the MOSFIRE and CANDELS data, we are able to constrain the internal kinematics even though rotation is only detected in 20% of our sample.

References: Grogin et al. 2011, ApJSS, 197, 35Kassin et al. 2007, ApJL, 660, L35Koekemoer et al. 2011, ApJSS, 197, 36 Kriek et al. 2015, ApJSS, 218, 15Skelton et al. 2014, ApJSS, 214, 24Wisnioski et al. 2015, ApJ, 799, 209

Contact: sedona@berkeley.edu

ΔPA = 0°

ΔPA = 45°

Velocity Line modelIntensity

ΔPA = 45°

σ = 0

σ = 0 V/σ = 2.1

ΔPA = 0°

V/σ = 2.1

Line model

Detected rotation: 2D kinematic models

AE

GIS

-174

37

1 kpc

HST/F160W image

1 kpc

Image, MOSFIRE res. Spec Model V(R

E)=

�186

+67

�48[km

/s],�

V,0

=98

+36

�42[km

/s]

Residual

CO

SM

OS

-137

01

1 kpc 1 kpc

V(R

E)=

163+

14

�20[km

/s],�

V,0

=31

+16

�19[km

/s]

UD

S-2

4412

1 kpc 1 kpc

V(R

E)=

162+

24

�25[km

/s],�

V,0

=52

+19

�29[km

/s]

CO

SM

OS

-161

41

1 kpc 1 kpcV

(RE

)=

374+

61

�90[km

/s],�

V,0

=33

+35

�17[km

/s]

HST/F160W Image, MOSFIRE res. Spectrum Best-fit model Residual

RE,projected

Masked

V(RE), σ Example kinematic best-fit model for a galaxy with detected rotation.

Kinematic models for misaligned slit spectra

Spectra taken with misaligned slits suffer from aperture losses and reduced rotation signals. However, detailed HST/CANDELS imaging shows how much of the galaxy falls outside of the slit, and allows us to measure the galaxy’s structural parameters. To measure kinematics from misaligned slits, we create 3D kinematic models with variable V and σ which account for the galaxy's size RE, Sérsic index n, and inclination, as well as seeing, instrument resolution, and aperture losses.

Unresolved or misaligned galaxies: 1D kinematic models

We assume a ratio V/σ, and then use the 3D models to calculate the aperture correction needed to convert the observed velocity dispersion σobs,1D to VRMS(RE).

Measuring baryonic and dynamical masses

We measure dynamical masses using the misaligned-slit kinematic models, infer stellar masses from stellar population synthesis models, and estimate gas masses from the dust-corrected Hα SFRs.

We find good agreement between baryonic and dynamical masses when we assume the galaxies without detected rotation have the same the median V/σ as those with detected rotation. 9 10 11 12

log10 (Mbaryon/M�)

9

10

11

12

log 1

0(M

dyn/M

�)

�RMS = 0.34� log10 M = 0.04

Unresolved,V/� = 2.1Resolved rotationH� non-detected

Mbar - Mdyn

Can we constrain V/σ for galaxies without detected rotation?

0.2 0.4 0.6 0.8 1.0

b/a

�1.5

�1.0

�0.5

0.0

0.5

1.0

1.5

log 1

0(M

dyn/M

bar

yon)

�RMS = 0.35� log10 M = 0.16

Assume pure disks

Unresolved, median binUnresolved, diskResolved rotationH� non � detected

0.2 0.4 0.6 0.8 1.0

b/a

�1.5

�1.0

�0.5

0.0

0.5

1.0

1.5

log 1

0(M

dyn/M

bar

yon)

�RMS = 0.34� log10 M = 0.04

Assume all disks, V/� = 2.1

Assume disks, V/σ = 2.1

23

Edge-on

25

Face-on

If we assume the unresolved and misaligned galaxies have no dispersion, there is an increasing trend of dynamical-baryonic mass difference with axis ratio b/a. We independently constrain the average V/σ for these galaxies by removing any b/a trend of ΔM, and find these galaxies have the same V/σ = 2.1.

0.2 0.4 0.6 0.8 1.0

b/a

�1.5

�1.0

�0.5

0.0

0.5

1.0

1.5

log 1

0(M

dyn/M

bar

yon)

�RMS = 0.35� log10 M = 0.16

Assume pure disks

Unresolved, median binUnresolved, diskResolved rotationH� non � detected

0.2 0.4 0.6 0.8 1.0

b/a

�1.5

�1.0

�0.5

0.0

0.5

1.0

1.5

log 1

0(M

dyn/M

bar

yon)

�RMS = 0.34� log10 M = 0.04

Assume all disks, V/� = 2.1

Assume pure disks

23

Edge-on

25

Face-on

σ2v,los

VRMS(RE)

Line σobs,1D

Hα

[NII][NII]

λ

Flux