Circum-galactic Medium Around Local Spiral Galaxies – A N - PowerPoint Presentation

Slide1

Circum-galactic Medium Around Local Spiral Galaxies – A New Window to Understand Galaxy Evolution

Li Jiang-Tao

1. Service d’Astrophysique, CEA, Saclay, France

2.

Department

of

Astronomy

,

University

of Michigan, Ann Arbor, USASlide2

Outline

1. Introduction

2. Diffuse X-ray

observation

s

of

the

hot

CGM

2.1.

The s

ample

2.2. X-ray scaling relations

2

.

3

.

Compare

to

cosmological

simulations

2.4. Massive spiral galaxies

3.

UV

absorption line

observations of the cool CGM

4. Radio observations

5. Summary and ProspectSlide3

What do we study of galaxy formation and evolution?

AGN

Star formation (SF)

Stellar component (

bulge+disk

)

Dark matter halo

What we still don’t know well?

The gaseous halo or the

circumgalactic

medium (CGM), compared to intergalactic or

intracluster

medium (IGM or ICM).

A typical spiral galaxy

1. IntroductionSlide4

Missing satellite problem

Why the number of dwarf galaxies is much less than predicted?

Overcooling problem

Why the gas cooling rate is much less than predicted?

How feedback works?

What are the temperature,

metallcity

, mass, ionization state, and velocity of the outflows?

Where they interact with the accreted gas?

Could feedback efficiently stop accretion and quench SF?

Missing baryon problem

…

Some big puzzles of galaxy evolution:

Why it is important to study the CGM?

Role of CGM in galaxy evolution

: Gas

reservoir

to continue SF

and

depository

of chemical and mechanical feedback

.

Studying CGM help us to understand the environment of galaxies, or the

galactic ecosystem

.Slide5

Why it is difficult to study the CGM?Theoretically

, adding

hydrodynamics

over large range of physical scale (from single SN to at least cluster of galaxies) is very time consuming.

Observationally

, the multi-phase CGM is always too faint to detect.

Could we study the CGM now?

Yes!Slide6

What

is the CGM gas comprised of

?

Metal line

radiative

cooling curve

Sutherland &

Dopita

1993, ApJS

, 88, 253

Hot; >106K or 0.1keV; X-ray emitting

Warm; 104-5

K; UV emitting

Cold; <104K; HI or COSlide7

What kind of observations do we need?

1.

X

-ray

observations

of

the

hot

CGM.

2. UV absorption line

studies of background AGNs to study

warm-hot intergalactic medium (WHIM)

and cold gas

around foreground

galaxies.

3. Radio observations of the cold molecular and atomic gases.Slide8

2. Diffuse X-ray observation of the hot CGM

2.1.

The s

ample

Li & Wang 2013a,b, MNRAS, 428, 2085; 435, 3071

Chandra

sample

of

53:

Nearby : distance<30MpcEdge-on :

inclination>60◦Disk

 galaxy: S0/spiral (-3<

TC<9)Moderate

size : 1’<D

25<16’ Low Extinction : N

H<8e20cm^-2No X-ray

bright

AGN

Subsample

definition

:

Starburst

(

f

60

/f

100

>0.4

and L

IR

>3e43erg/s) vs

non-

starburst

Clustered

(ρ>0.6) vs

field

Early

-type

(TC<1.5) vs late-typeSlide9

2.2.

X-ray scaling relations

L

X

has a

linear correlation

with Ė

SN

. The X-ray radiation efficiency

η≡

L

X

/Ė

SN~0.4%.

NGC4438

: 87ks XMM-Newton Cycle 13 observation (PI: Jiang-Tao Li, but as Priority C) plus many multi-wavelength observations.

NGC660: 50ks Suzaku Cycle 9 observation (

PI: Jiang-Tao Li

, but as

Priority C

).

Not the end!Slide10

L

X

L

X

v

rot

M

200

M

200

L

X

SFR

M

*

Abundance

matching

(

Leauthaud

et al. 2012,

ApJ

, 744, 159

).

2

.

3

.

Compare with cosmological

simulations

Li, Crain, & Wang, 2014, MNRAS, 440, 859

GIMIC

well

reproduce

both

the

range

and

scatter

of the corona

luminosity

for L* galaxies.

Observations

of

massive spiral galaxies

from

the

literature

(

blue

).

Galaxies-

Intergalactic

Medium Interaction

Calculation

(

GIMIC

) (

green;

Crain

et al. 2009, MNRAS, 399, 1773

 ;

2010, MNRAS, 407, 1403

).

However, GIMIC has:

No AGN feedback

Constant

SNe

feedback parameters (wind velocity and mass loading factor).

Single phase ISM, so no cool-hot gas interaction below the numerical resolution.Slide11

OWLS & GIMIC projects taught us much about physical modeling, so major physical improvements by Eagle:

(1) Non-constant wind velocity, wind remain hydrodynamically coupled.

(2) Switching to thermal SNII feedback,

parametrized

by heating temperature and energy fraction.

(3) AGN feedback, seed black holes of mass (10

5

M

sun

) are injected into FOF haloes of a threshold mass.

Tuning the EAGLE Universe to match the galaxy stellar mass function (GSMF) and further perform comparisons with:

(1) X-ray scaling relations and abundances

(2) Local Tully-Fisher relation(3) Cosmic SNIa

rate(4) Local specific star formation rates(5) Local gas phase and stellar

metallicities(6) Local alpha/Fe abundance

Looking forward to the results from new simulations.The first EAGLE paper is already on astro

-ph!

and collaborators from many other institutes.Slide12

Why

massive galaxies

above

a transition

mass of ~2X10

11

M

ʘ

are X-ray

brighter

(

higher L

X/M

*)?

(a)

Stronger

thermal/ram-pressure

confinement

(

Dalla

Vecchia

&

Schaye

2008, MNRAS, 387, 1431

;

Lu & Wang 2011, MNRAS, 413, 347

).

(b) Major

accretion

mode

changing

from

cold-mode to hot-mode (e.g.,

Keres

et al. 2005, MNRAS, 363, 2

).

(c)

Steeper

density

profile

due to

hydrostatic

or

inflow

state (

Ciotti

et al. 1991,

ApJ

, 376, 380

;

O’Sullivan

et al. 2003, MNRAS, 340, 1375

).

We need

more

deep X-ray observations

of

massive galaxies

around or above the transition mass to confirm the existence of such a L

X

-M

*

slope change.2.4. Massive spiral galaxies

Most of the X-ray emission is produced by the high-density, high-metallicity gas directly related to stellar feedback. It is more important to search for X-ray emission from externally accreted gas, which is expected to be strong in isolated SF-inactive massive spiral galaxies. Slide13

XMM-Newton

Cycle 13 Large program (

490ks of 5 galaxies;

PI: Jiang-Tao Li

)

Selection

criteria

:

Massive:

v

maxg

≳300km/s and

M

∗

≳2×10

11 M

⊙

.

Quiescent:

SFR/M

∗

<0.05

Gyr

−1

.

Isolated

:

no

bright

companion

within

30' (600

kpc

at

a distance of 70

Mpc

).

Optimized

for X-ray observation:

N

H

<10

21

cm

−2

;

distance

<100Mpc.

Add

archival

data:

4 galaxies

in the table, and

another

two

(NGC6011, 45ks and NGC7490, 41ks by Akos Bogdan

also

in

this

cycle)?

Major

scientific

goals:

Better constrain

the metallicity

.

Radial distribution to

larger radii (plus (1) to measure the baryon content).

X-ray scaling relations with more galaxies around/above

the transition mass.NASA ADAP 3 year funding; Science PI: Jiang-Tao Li (UMich), Program PI: Joel N. Bregman (UMich); Co-I: Q. Daniel Wang (UMASS)Slide14

3. UV absorption line observations of the cool CGM

Bregman

2007, ARA&A, 45, 221

AGN UV absorption line observations

is

one of the

primary

scientific

objective of HST.

(

Bahcall

&

Spitzer

1969,

ApJ

, 156, 63

)

AGN UV absorption line

is

the best

way

to

study

the warm-hot

intergalactic

medium (

WHIM

).

1.

Strong

extinction and

usually

too

faint

for UV

imaging

(

Hodges

-Kluck &

Bregman

2014,

ApJ

, 789, 131

).

2. Correct

temperature

range and

lower

column

density

(

than

X-ray).Slide15

Probing

Warm-Hot

Intergalactic

Gas

at

0.5 < z < 1.3

with

a Blind Survey for O VI, Ne VIII, Mg X, and Si XII Absorption

Systems

Cycle 17 ; PI : Todd Tripp

 ; 137

orbits

How

Galaxies

Acquire

their

Gas

: A

Map

of

Multiphase

Accretion

and Feedback in

Gaseous

Galaxy

Halos

Cycle

17 ; PI : Jason

Tumlinson

 ;

134

orbits

 ;

COS-Halos

A

COS

Snapshot

Survey for z < 1.25

Lyman

Limit

Systems

Cycle

18 ; PI : J.

Howk

 ;

140

orbits

How

Dwarf

Galaxies

Got

That

Way

:

Mapping

Multiphase

Gaseous

Halos and

Galactic

Winds Below L*

Cycle 18 ; PI : Jason Tumlinson ; 129 orbits ;

COS-Dwarfs Understanding the Gas

Cycle in Galaxies: Probing the

Circumgalactic

Medium

Cycle

19 ; PI : Timothy

Heckman

 ;

119

orbits

A

Breakaway

from

Incremental

Science: Full

Characterization

of the z<1 CGM and

Testing

Galaxy

Evolution

Theory

Cycle

21 ; PI : Christopher Churchill ;

110

orbits

The

COS Absorption Survey of Baryon

Harbors

(

CASBaH): Probing the Circumgalactic Media of Galaxies from z = 0 to z = 1.5 Cycle 22 ; PI : Todd Tripp ; 99 orbits

Some HST large projects studying AGN absorption lines since COS (the Cosmic Origins Spectrograph) was installed in May 2009:

Limitation

: Most of the absorbers are at

z>0.1

, in order to include the important

OVI

λλ

1032,1037 lines

in the COS range (e.g.,

Tumlinson

et al. 2011, Science, 334, 948

).Slide16

Sightline

map

of COS-Halos

1.

Associate

the absorber to the host galaxies.

2.

Detail

host

galaxy

properties

(e.g., distribution of SF in the

galactic

disk

)

3. The cold and hot CGM.

We

are

focusing

on

local

galaxies

already

have or

potentially

easy

to propose

high

quality

multi-

wavelength

observations

!

What

is

difficult

to do

with

the

current

data?

Bregman

et al. 2013,

ApJ

, 766, 57Slide17

Evidence for magnetic confinement (

Wang et al. 2001,

ApJL

, 555, 99

)?

4. Radio observations

CHANG-ES

:

C

ontinuum HAlos in

Nearby Galaxies — an E

VLA Survey (PI: Judith A. Irwin

). 405 hours

of EVLA observations of 35

nearby edge-on galaxies over two wide bandwidths centered at 1.5 and 6 GHz and in three (B, C and D) array configurations.

L-band (1.5GHz) contour overlaid on X-ray image (Irwin et al. 2012, AJ, 144, 44)

The relation between X-ray and radio halo remains to be investigated!

>20 CHANG-ES galaxies have high quality X-ray data, and we are working to obtain more (e.g.,

XMM-Newton

AO-10 program;

56ks

taken

, 37ks

Priority

C;

PI: Jiang-Tao Li

)

.

NGC 4631

CHANG-ES Paper IV (

van

Vliet

Wiegert

et al. 2015

) on D-array observations of extended radio halo is coming!Slide18

5. Summary and Prospect

Baryon budget of a

fiducial

COS-Halos galaxy;

Werk

et al. 2014,

ApJ

, 792, 8

1. In addition to the stellar component (through optical or IR observations), we are now ready to study

the multi-phase gaseous CGM around local galaxies (through X-ray, UV, and radio observations), which finally close the box of the baryon budget and greatly help to constrain the

galaxy evolution models.2. Theoretical works are also accurate enough to quantitative compare with observations.

3. It is even possible to study other phases of the CGM (in addition to the stars, gases, and dark matter), such as the magnetic field and

cosmic ray. It is also time to consider their roles in galaxy evolution (e.g., Pakmor et al. 2014,

ApJ, 783, 20).Slide19

Thank

you very much

!

We are on the way to fully understand the whole baryonic Universe

……………………