satoshi hamano (university of tokyo) collaborator:

Detection of Most Distant Type-Ia Supernova Remnant Shell as Absorption Lines in the Spectra of Gravitationally Lensed QSO B1422+231

Satoshi Hamano (University of Tokyo)

Collaborator:N. Kobayashi (Univ. of Tokyo), S. Kondo (Kyoto Sangyo Univ.), T. Tsujimoto (NAOJ), K. Okoshi (Tokyo Univ. of Science), T. Shigeyama (Univ. of Tokyo, RESCUE)

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Table of Contents1. Introduction

◦ QSO absorption-line systems◦ Gravitationally lensed QSOs

2. Observation◦ Target: B1422+231◦ Observation with Subaru IRCS

3. Results & Discussion◦ MgII absorption lines at z=3.54◦ The origin: type-Ia supernova remnant ?

4. Summary & Future Prospects◦ Preliminary results of our recent observation using

AO188

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1. Introduction

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QSO absorption-line systems

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“QSO absorption-line systems” are gas clouds that give rise to absorption lines in the spectrum of background quasars.

They are an only tool that can trace high-z gas clouds without bias of luminosity. 4

MgII systemsDoublet absorption lines of MgII (λλ2796, 2803) is the best lines to trace gas clouds associated with high-z galaxies. MgII systems can be detected in wide redshift range. MgII systems can trace various type of gas clouds in a wide

range of HI column density. 1015<N(HI)<1021 (Churchill+05)

MgII systems provide us precious information on the chemical and kinematical properties of high-z gas clouds. Processes of galaxy formation that stars are formed from

gas clouds are expected to be traced directly. (Kacprzak+11)

Complementary to the surveys of high-z galaxies with deep imaging.

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Difficulty of “single” line of sight of QSO

Observables from a set of absorption lines ◦ Column densities, temperature◦ Chemical abundances, metalicity

Non-observables because we observe them with just a single line of sight. ◦ Extent of gas clouds◦ Mass, volume density

The spatial structure of gas clouds is known to be one of a key parameters in galaxy formation theories. (Mo+99, Maller+04)


QSOObserver？ How large in

size or mass ?

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Lensing galaxy

QSO

Gas cloud

observer

“Multiple” lines of sight of gravitationally lensed QSOsMerits of gravitationally lensed QSOs (GLQSOs) Split of images

◦ We can observe multiple points of intervening gas clouds, which give us information of the spatial structure.

Magnification of images◦ We can resolve the structure of

gas clouds in small scale even at high redshift.


“Effective” spatial resolution reaches just １ mas ！

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Optical ←|MgII lines| →Near-infrared

observer

Spatial structure of MgII systems examined with GLQSOs


kpc-scale structure・ distribution of metal in halos/disks・ velocity field

lensing galaxy QSO

large separation

Past studies Our study

Possible with near-infrared high-dispersion spectroscopy Kobayashi+ (02), Hamano+ (12)

Many studies have been done by high-dispersion observation with optical and UV spectroscopy Rauch+ (00,01,02),Ellison+ (04) Lopez+(97,05),Monier+ (97,09), etc..

lower-z

small separation

higher-z

pc-scale structure・ geometry, size・ origin (HVC,SNR,HII region)

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z=2.5

Our purposeIn summary, our purpose is to investigate molecular clouds scale structure of high-z gas clouds traced by MgII systems at z>2.5 using multiple lines of sight of GLQSOs with near-infrared spectroscopy. In this talk, I will show you a first result of our on-going study of “GLQSO absorption-line systems” with Subaru IRCS. (Hamano+12)

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2. Observation

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TargetB1422+231 z=3.628 (Rauch+99) Four images and a lensing galaxy Have the 2nd brightest luminosity in NIR

among QSOs ever detected Known to have QSO absorption-line

systems at z>2.5 (Rauch+99, 00, 01). Due to the configuration, a very large

magnification can be achieved at higher redshift.

This object is the most appropriate for our study.

Closest images, A and B (AB=0.5 arcsec), are observed this time.


Lensing galaxy(z = 0.339,Tonry 98)

0”.5

Slitviewer image of B1422+231 obtained by Subaru IRCS w/ LGSAO188

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Telescope Subaru telescope

◦ 8.2 m diameter◦ Known to have excellent stellar

images among ground-based telescopes→ Best to resolve close lensed images of GLQSOs( ~ 0.5 arcsec)

IRCS(Infrared Camera and Spectrograph)◦ We used NIR echelle mode (high spectral resolution)

→MgII absorption lines at z>2.5 can be observed


IRCS

Subaru telescope

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Observation & Analysis Open-use observation by N.Kobayashi

◦ Wavelength : 1.01-1.38 μm (zJ & J bands)◦ Date : Feb. 13, 2003 ( zJ ),

Apr. 28, 2002 ( J )◦ AO36 was used only for zJ band observation.◦ Resolution : R=5,000 ( zJ ) , R=10,000 ( J )◦ Time : 9,000 sec ( zJ ) , 9,600 sec ( J )◦ Seeing : 0.3 arcsec (excellent !!)◦ Weather condition : photometric

Data was reduced with IRAF.


0”.5

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Obtained data

3. Results & Discussion

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Resolved spectra of B1422+231

Spectra of images A and B of B1422+231


Telluric absorption lines

z=3.54 MgII doublet

MgII emissionof QSO itself

Very small separation between images A and B :AB = 8pc @ z=3.54 corresponds to １ mas

z=3.54 FeII lines

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Resolved spectra of B1422+231Absorption lines at z=3.54 MgII absorption lines

◦ Two components are detected with separation of ~ 200 km/s for both images.

◦ Differences of absorption lines can be seen between A and B for both components.

FeII absorption lines◦ Only one component of image A

is detected with large Doppler width. MgI absorption lines

◦ No detection

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These absorption lines reflect pc-scale gaseous structure at high redshift.

Since now, we will discuss the structure and origin of the z=3.54 system.

AB

A

C

CII

Past study of the z=3.54 system

Rauch+99 Optical obs. w/ Keck HIRES (R~45,000)

◦ Images A and C are observed( AC=22pc @ z=3.54)

◦ 2 velocity components are detected with low-ionization absorption lines (CII, SiII, etc.)

Symmetric profiles◦ Unique feature◦ Much difference of column

densities between images A and C◦ Velocities expand symmetrically

from image A to image C


By what type of gas clouds are these unique profiles produced ?

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AC

CII

Past study of the z=3.54 system

Interpretation of the z=3.54 system by Rauch+99 Explanation of differences

by a expanding shell. Limit the expanding velocity


A

CB

Newly observed

skmv /98

Is spectrum of image B consistent with this model ?

Outer shell produces stronger lines with smaller velocitiesInner shell produces weaker lines with larger velocities

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QSOobserver

Our observation


A

CB

CII

C

AA,B ： MgIIC ： CII

MgII absorption lines in the spectrum of image B is found to have intermediate column densities and velocities of those of images A and C

Our observation supports the expanding shell model proposed by Rauch+99, qualitatively.

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3D spherically expanding shell modelIn order to constrain the size of the shell combining information from three images, we calculated a simple model of a 3-dimensional symmetric expanding shell with radius R and expanding velocity of v.


AA vv cos2

AA Rd sin

Two geometrical equations on ⊿OAB, OBC

8 equations9 variables ：

,,,,,,,, CBACBA dddvR

(Rauch+ 02)

R(v) can be obtained20

What is the z=3.54 system? (1)R-v relation of the z=3.54 system in comparison with Galactic objects having an expanding shell structure.


(Koo+ 91)

Consistent with SNR21

Images must be located near the edge of the shell

The diameter must be exactly equal to the separation A-C.

Most likely!!

What is the z=3.54 system? (2)Estimate of fundamental parameters of the z=3.54 system Estimate mass of shell using the value of MgII column

density

Under the assumption that the z=3.54 system is a SNR, using sedov-phase solution,◦ Age:◦ Density of interstellar medium :

◦ Energy of supernova :


oo MMM 18847

ergEerg 500

49 102.3108.3

yrtyr 55 102.2101.1

330

33 106.3108.1 cmncm

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All of these parameters are consistent with typical values of Galactic SNRs (Koo+91), suggesting the z=3.54 system is truly a SNR.

Type of the SNR at z=3.54 (1)Abundance ratio Comparison of [MgII/FeII]

with low-z MgII systems (Narayanan+07)

[MgII/FeII] of the z=3.54 system is near to those of Fe-rich systems.


z=3.54 system

MgII column density

log[MgII/

FeII]

Low-z MgII systems

solar

■Confirmed 　 Fe-rich systemsFeII rich

Type-Ia SN enrichment (Rigby+02)

The z=3.54 system is a remnant produced by a type-Ia supernova

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Type of the SNR at z=3.54 (2)Gas kinematics Broad FeII absorption line

◦ b(FeII) = 23±6 km/s◦ b(MgII) = 9±1 km/s


Perturbed FeII-rich gasejected by SN explosion.

Conclusion:The z=3.54 system is themost distant type-Ia SNR

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4. Summary & Future Prospects

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Summary We obtained spatially-resolved NIR spectra of images

A and B of a GLQSO, B1422+231 with Subaru IRCS. We detected MgII and FeII absorption lines at z=3.54

with systematical differences between images A and B, whose separation at the redshift is just an 8 pc.

From expanding shell model, we concluded that the z=3.54 system is a type-Ia supernova remnant. It is the first case to identify the origin of a specific QSO absorption-line system.

The z=3.54 system is the most distant type-Ia supernova (remnant) ever detected (Most distant type-Ia supernova detected with light is at z=1.55: Conley+11).

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See Hamano et al., (2012, ApJ, 754, 88) for the detail of this study .

Future plan ~ LGSAO188 ~ We are advancing the NIR survey of MgII systems in

the spectra of GLQSOs with Subaru IRCS/LGSAO188.◦ LGSAO188 enables us to obtain high-quality

(higher spectral-, spatial-resolution, throughput) spectra of GLQSOs.

More GLQSOs at z>2.5 can be observedw/ higher throughput of LGSAO188for the first time.◦ Improved stellar images increase flux in a slit◦ We selected 7 brighter GLQSOs as

a first sample and we are observing them.

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LGSAO188 with Subaru.(from NAOJ homepage)

Preliminary results 2 GLQSOs (including B1422+231) have been already

observed using guaranteed time of AO188.

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Detected!

Profiles are slightly resolved!

Spectra of B1422+231 obtainedw/ IRCS/AO188 (NGS & LGS)

Spectra obtained w/o AO(this study)

As for the other observed object, we also detected some MgII systems with spatial structures.Analysis and observation are proceeding now!

R=10,000 R=20,000

satoshi hamano (university of tokyo) collaborator:

Documents

best lines

line of sight

lensed qso b1422

subaru um

highz gas clouds

various type of gas

lensed qso kwz b1422

multiple lines of sight