Ia Supernova Remnant Shell as Absorption Lines in the Spectra of Gravitationally Lensed QSO B1422231 Satoshi Hamano University of Tokyo Collaborator N Kobayashi Univ of Tokyo ID: 386267
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Slide1
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)
2013.01.15-17 Subaru UM @ NAOJ
1Slide2
Table of ContentsIntroductionQSO absorption-line systemsGravitationally lensed QSOsObservation
Target: B1422+231Observation with Subaru IRCSResults & DiscussionMgII absorption lines at z=3.54The origin: type-Ia supernova remnant ?Summary & Future ProspectsPreliminary results of our recent observation using AO188
2013.01.15-17 Subaru UM @ NAOJ
2Slide3
1. Introduction2013.01.15-17 Subaru UM @ NAOJ
3Slide4
QSO absorption-line systems2013.01.15-17 Subaru UM @ NAOJ“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.
4Slide5
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.
2013.01.15-17 Subaru UM @ NAOJ
5Slide6
Difficulty of “single” line of sight of QSOObservables from a set of absorption lines Column densities, temperatureChemical abundances,
metalicityNon-observables because we observe them with just a single line of sight. Extent of gas cloudsMass, volume densityThe spatial structure of gas clouds is known to be one of a key parameters in galaxy formation theories. (Mo+99, Maller+04)2013.01.15-17 Subaru UM @ NAOJ
QSO
Observer
？
How large in
size or mass ?
6Slide7
Lensing
galaxy
QSO
Gas cloud
observer
“Multiple” lines of sight of gravitationally lensed QSOs
Merits 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
W
e
can resolve the structure of
gas
clouds in
small scale
even at
high redshift.
2013.01.15-17 Subaru UM @ NAOJ
“Effective” spatial resolution reaches just
１
mas
！
7Slide8
Optical ←|MgII lines| →Near-infrared
observerSpatial structure of MgII systems examined with GLQSOs2013.01.15-17 Subaru UM @ NAOJ
kpc
-
scale structure
・
distribution of metal
in halos/disks
・
velocity field
lensing galaxy
QSO
l
arge
separation
Past studies
Our study
Possible with near-infrared high-dispersion spectroscopy
Kobayashi+ (02
), Hamano+ (12)
Molecular cloud scale structure
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)
Galactic scale structure
MgII
CIV
z~1
8
z
=2.5Slide9
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) 2013.01.15-17 Subaru UM @ NAOJ9Slide10
2. Observation2013.01.15-17 Subaru UM @ NAOJ
10Slide11
TargetB1422+231
z=3.628 (Rauch+99)Four images and a lensing galaxyHave the 2nd brightest luminosity in NIRamong QSOs ever detectedKnown 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
.
T
his
object is the most appropriate
for
our
study.
Closest images
, A and
B (AB=0.5 arcsec),
are
observed
this
time.
2013.01.15-17 Subaru UM @ NAOJ
Lensing galaxy
(z
= 0.339,Tonry 98)
0
”.5
Slitviewer
image of B1422+231
obtained by Subaru IRCS
w/ LGSAO18811Slide12
TelescopeSubaru telescope8.2 m diameterKnown 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 observed2013.01.15-17 Subaru UM @ NAOJ
IRCS
Subaru telescope
12Slide13
Observation & AnalysisOpen-use observation by N.KobayashiWavelength : 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 : photometricData was reduced with IRAF.2013.01.15-17 Subaru UM @ NAOJ
0
”.5
13
Photo of data
PSF image
Obtained dataSlide14
3. Results & Discussion2013.01.15-17 Subaru UM @ NAOJ
14Slide15
Resolved spectra of B1422+231Spectra of images A and B of B1422+2312013.01.15-17 Subaru UM @ NAOJ
Telluric absorption lines
z=3.54 MgII
doublet
MgII emission
of 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 linesTwo 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 linesOnly one component of image A is detected
with large Doppler width.MgI
absorption lines
No detection
2013.01.15-17 Subaru UM @ NAOJ
16
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.
A
BSlide17
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 velocit
y 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
e
xpand symmetrically
from image A to image C
2013.01.15-17 Subaru UM @ NAOJ
By what type of gas clouds
are these unique profiles produced ?
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A
C
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
2013.01.15-17 Subaru UM @ NAOJ
A
C
B
Newly
observed
Is spectrum of image B
consistent with this model ?
Outer shel
l produces
stronger
lines with
smaller
velocities
Inn
er shel
l produces
weaker
lines with
larger
velocities
18
QSO
observerSlide19
Our observation2013.01.15-17 Subaru UM @ NAOJ
A
C
B
CII
C
A
A
,
B
：
MgII
C
：
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 Rauc
h+99, qualitatively.
19Slide20
3D spherically expanding shell model
In 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
.
2013.01.15-17 Subaru UM @ NAOJ
Two geometrical
equations
on
⊿
OAB, OBC
8 equations
9
v
ariables
：
(Rauch+ 02)
R(v
)
can be obtained
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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.
2013.01.15-17 Subaru UM @ NAOJ
(Koo+ 91)
Consistent with SNR
21
Images must be located
near the edge of the shell
The diameter must be
exactly equal
to the separation A-C.
Most likely!!Slide22
What is the z=3.54 system? (2)Estimate of fundamental parameters of the z=3.54 systemEstimate mass of shell using the value of MgII
column densityUnder the assumption that the z=3.54 system is a SNR, using sedov-phase solution,Age:Density of interstellar medium :Energy of supernova :2013.01.15-17 Subaru UM @ NAOJ
22
All of these parameters are consistent
with typical
values
of Galactic SNRs (Koo+91),
suggesting the z=3.54 system is truly a SNR.Slide23
Type of the SNR at z=3.54 (1)Abundance ratioComparison 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. 2013.01.15-17 Subaru UM @ NAOJ
z=3.54
system
MgII
column density
log[MgII/
FeII
]
Low-z MgII systems
solar
■
Confirmed
Fe-rich systems
FeII
rich
Type-
Ia
SN enrichment
(Rigby+02)
The z=3.54 system is a remnant
produced by a type-
Ia
supernova
23Slide24
Type of the SNR at z=3.54 (2)Gas kinematicsBroad FeII absorption lineb(FeII
) = 23±6 km/sb(MgII) = 9±1 km/s2013.01.15-17 Subaru UM @ NAOJ
Perturbed
FeII
-
rich gas
ejected by SN explosion.
Conclusion:
The z=3.54 system is the
most distant type-
Ia
SNR
24Slide25
4. Summary & Future Prospects2013.01.15-17 Subaru UM @ NAOJ
25Slide26
SummaryWe 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).
2013.01.15-17 Subaru UM @ NAOJ
26
See Hamano et al., (2012,
ApJ
, 754, 88) for
th
e detail of this study
.Slide27
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 slitWe selected 7 brighter GLQSOs as a first sample and we are observing them.
2013.01.15-17 Subaru UM @ NAOJ
27
LGSAO188 with Subaru.
(from NAOJ homepage)Slide28
Preliminary results2 GLQSOs (including B1422+231) have been already observed using guaranteed time of AO188.
2013.01.15-17 Subaru UM @ NAOJ28Detected!Profiles are
slightly
resolved!
Spectra of B1422+231 obtained
w/ 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
proceed
ing now!
R=10,000
R=20,000