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Evolution of Kinematic Properties ofEarly-Type Galaxies Investigated bySurface Photometry
満田 和真
Kazuma Mitsuda
Tohoku University (PD)

Galaxy Evolution Workshop 2018/06/08

!2 / 22Outline❶ Introduction
Kinematics of Early-Type Galaxies (ETGs)❷ Relation between kinematics and surface brightness
profilesLocal ETGs with IFS data

❸ Surface photometry at z~1 and 0
Cluster ETG samples at z~1 and 0❹ Evolution of Kinematics from Surface photometry
Spin down of ETGs at z < 1
Galaxy Evolution Workshop 2018/06/08

!3 / 22Outline❶ Introduction
Kinematics of Early-Type Galaxies (ETGs)❷ Relation between kinematics and surface brightness
profilesLocal ETGs with IFS data

❸ Surface photometry at z~1 and 0
Cluster ETG samples at z~1 and 0❹ Evolution of Kinematics from Surface photometry
Spin down of ETGs at z < 1
Galaxy Evolution Workshop 2018/06/08

1. Introduction!4 / 22

Galaxy Formation & Evolution
Before Quenching
Star-forming (SF) galaxies
After Quenching
Quiescent or Early-Type Galaxies‣ Quenching of SF‣ Mass & size growth‣ EV of Morphology‣ EV of Kinematics (spin-down)

Cosmic Star Formation History; Bouwens+10

0 Early- and late-type galaxies
Early-type Galaxies (ETGs)
EllipticalS0Late-type Galaxies
SabScdGalaxy Evolution Workshop 2018/06/08

1. Introduction!5 / 22

Kinematics of ETGs by Integral Field Spectroscopy
degree of galaxy spin

Quantified with spin parameter λFast v.s. Slow Rotators

i: i-th pixel
Fi: flux
Ri: galactocentric distance
Vi: line-of-sight velocity
σi: velocity dispersion

Krajnovic et al., 2011

NGC4660

blue shift
red shift

Emsellem et al., 2007

✽ λ < 0.3 : Slow Rot, λ>0.3 Fast RotHow do ETGs obtain suchλ ofkinematic
260 local ETGsproperties?

Photometry

Velocity Field

Photometry

Velocity Field

Dispersion dominated= slow rotators

rotowSl

NGC4486λe

Krajnovic et al., 2011

rh [kpc](Half-light radius)

Rotation dominated= fastrotators
What
are the spin-down mechanisms of slow rots?

Fast rot

M＊ [M⦿] (stellar mass) Capperalli et al., 2013a● Only massive end = Slow Rot
Galaxy Evolution Workshop 2018/06/08

1. Introduction!6 / 22

Latest Cosmological Simulations● Spin-down history in a cosmological context●IfAmountof spin
down in majormerger, minor
etc…
we canobserve
kinematics(λmerger,parameter)● Not perfect (e.g., different results between different simulations)

λλmajor merger

nSpin dow

Stellar mass M✽ [1010 M⦿]of high-redshift ETGs, the results can be compared
Two examples from 15k simulated ETGs
Statistics with 3-5k simulated ETGs
with simulations.
But, observation is unfeasible with current facility
Need (←)highspatialresolution(e.g.,0.1”)
M
Need long, long integration for spatially-resolvedλ (→)
absorption
line spectroscopy
Indirectmeasurement
onlywithimagingdataRedshift z
Redshift zcolor: prob. density

Penoyre et al., 2017λλ✽

Choi et al., 2018
Galaxy Evolution Workshop 2018/06/08

!8 / 22Outline❶ Introduction
Kinematics of Early-type galaxies (ETGs)❷ Relation between kinematics and surface brightness
profilesLocal ETGs with IFS data

❸ Surface photometry at z~1 and 0
Cluster ETG samples at z~1 and 0❹ Evolution of Kinematics from Surface photometry
Spin down of ETGs at z < 1
Galaxy Evolution Workshop 2018/06/08

2. Kinematics and Surface Brightness Profiles of Local ETGs

!9 / 223DATLAS Data and Non-barred ETG Sample
ATLAS3D: Volume-limited, mass complete IFS survey(Cappellari et al., 2011)● D < 42 Mpc (Northern Hemisphere)● MK < -21.5 mag (M✽ > 6x109 M⦿)● Morphological selection by eye (absence of spiral arms)▸ 260 ETGs

Sample in this study: Non-barred ETGs with SDSS images● No bar, ring, and shell ⇐ Inspected by ATLAS3D team (Krajnovic et al., 2011)● Galaxies with Sloan Digital Sky Survey (SDSS) Images▸ 166 ETGs(Cappellari et al., 2011)

Examples of the non-barred ETG sample

Galaxy Evolution Workshop 2018/06/08

2. Kinematics and Surface Brightness Profiles of Local ETGs

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Relation between ΔSlope and λProbability
from random

Smaller ΔSlope (extended) → Smaller λ (slow rotators)

prank=4e-11

prank=1e-8● Significant correlation revealed by rank correlation tests● Best photometric parameter for kinematics (compared to, e.g., Sersic index)
Galaxy Evolution Workshop 2018/06/08

!15 / 22Outline❶ Introduction
Early-type galaxies (ETGs)❷ Relation between kinematics and surface brightness
profilesLocal ETGs with IFS data❸ Surface photometry at z~1 and 0
Cluster ETG samples at z~1 and 0❹ Evolution of Kinematics from Surface photometry
Spin down of ETGs at z < 1
Galaxy Evolution Workshop 2018/06/08

3. Surface Brightness Profiles of ETGs at z~1 and 0!16 / 22

Early-type Galaxy Samples at z~1 and 0

Cluster ETG Sample: Easy to follow evolution from z~1 to 0
● Galaxies remain in the cluster once they fall in it● Galaxy clusters: matching halo mass assuming mass evolution● ETGs: assuming passive evolution to select z~0 descendants of z~1 ETGs

High-z Sample (z~1)

Low-z Sample (z~0)

ETG@z~1● 25 clusters at z=0.9-1.5 (zmed=1.2) ● 9 clusters at z=0.02-0.05 (zmed=0.03)(Dawson et al., 2009)logM200/M⦿ = 14.2 - 14.9

logM200/M⦿ = 14.6 - 15.2

(Reiprich & Böringer 2002)● 692 ETGs with log(M✽/M⦿)>10● 621 ETGs with log(M✽/M⦿)>10

Selected by i, z color-mag diagram
Quantitative morphological selection

Selected by u, g color-mag diagram
Quantitative morphological selection● High-quality HST imaging (i, z)
PSF FWHM: 0.1 arcsec
Integration time: >10k sec (z)(Suzuki et al., 2012)● SDSS imaging
g-band: close to z-band
z~1kpc3” ~at24

Comparable PSF size to z~1 in physical scale
Galaxy Evolution Workshop 2018/06/08

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Mass Dependence of ΔSlope

3. Surface Brightness Profiles of ETGs at z~1 and 0● High-z (z~1) sample has larger ΔSlope (i.e., more truncated)

z~0 ETGsz~1 ETGs

Galaxy Evolution Workshop 2018/06/08

4. Discussion!18 / 22

Evolution of Kinematic Properties of ETGs
§3. ΔSlope of z~1 and 0 ETGs

λ of z~1 and 0 ETGs
z~1 ETGsz~0 ETGs§2. ΔSlope — λ relation● Spin down from z~1 to 0 by
Δλ~0.05 - 0.15
(compared at a fixed stellar mass)

Galaxy Evolution Workshop 2018/06/08

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SummarySection 2● We investigate the relation between kinematics and surface brightness profile witha local ETG sample from IFS survey ATLAS3D● We introduce the ΔSlope parameter, and show that ΔSlope is correlated with thespin parameter λ.
● Slow Rotator tend to have ΔSlope<0 (extended), while Fast Rotator tend to have
ΔSlope>0 (truncated)● ΔSlope is measured from imaging data and can be applied to high-redshift ETGsSection 3 and 4● We measure ΔSlope for large samples (>600) of ETGs at z~1 and 0● z~1 ETGs have larger ΔSlope● Assuming ΔSlope — λ relation, ETGs experience spin down by Δλ ~ 0.05 - 0.15
from z~1 to 0.

Galaxy Evolution Workshop 2018/06/08

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Kinematics of z > 2 Lensed ETGs
Lensed ETGs at z>2 provide
opportunities for direct
kinematic measurements● One ETG per 10 clusters▸ a few hundred by HSC

Multiple images

Newman et al., 2015

Galaxy Evolution Workshop 2018/06/08

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Direct observation of kinematics at z~1
Overcome spatial resolution with laser tomographic AO
on the Subaru telescope
Laser tomographic AO (LTAO)

Seeing limited

More information on the poster P15
Subaru Tomography Adaptive Optics to study cosmological0.5”

evolution of galaxy internal structures

Hajime Ogane, Kaoru Omoto, Masayuki Akiyama (Tohoku University)

Galaxy evolution workshop@Ehime University 2018/6/6-8

ABSTRACTNow the telescope which achieves the highest spatial resolution in the visible wavelength is the Hubble Space Telescope (0.05”). In order to resolve internal structure of disks and bulgesof the galaxies at high redshifts, we need higher spatial resolution in the wavelength range. For resolving this problem, we use a technology of Adaptive optics. Adaptive optics (AO) is atechnique for allowing observation at high spatial resolution on the ground by correcting wave distortion by turbulence in real time. In our laboratory, we are developing laser tomography
adaptive optics (LTAO) for the Subaru telescope to accomplish near diffraction limit with the 8.2-m Subaru telescope in the visible wavelength (0.02") which is higher spatial resolution thanHubble Space Telescope and JWST. It is expected that we can spatially resolve properties of high-redshift galaxies such as stellar kinematics and morphology. We report the predictedperformance with the LTAO on Subaru, and discuss current status of the development and future prospects of the project as well as science cases.

w/ LTAO

error
correction for● Wavefront
1. What is AdaptiveOptics?
multiple turbulence layers▸ Diffraction limit in optical
Spatial resolution = 0.02”
The eﬀect of atmospheric turbulence issevere in ground-based observations. Thisturbulence makes the wavefront from thestars distorted into bumpy surface andprevent us from carrying out observations athigh spatial resolution. AO is a technologythat measure the turbulence of wavefront ofreference stars and then recover theundistorted wavefront by using that

Schematic diagram of Adaptive Optics

HST (2.5m)-Laser589.2nm laser excites Na atoms at 90km

height. The Na atoms re-emit the visible light,
producing an artificial star.
-Deformable Mirror
The shape of mirror is controlled by actuators.
←Deformable mirror usedin Subaru currently

Galaxy Evolution Workshop 2018/06/08
Reference:Subaru Telescope(https://!22 / 22END
Galaxy Evolution Workshop 2018/06/08