Hiroshi TERADA Probing Proto- /Exo-Planetary Atmosphere with RAVEN/IRCS - (I) Organic Molecules in Protoplanetary Disks
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Probing
Proto-‐/Exo-‐Planetary
Atmosphere
with
RAVEN/IRCS
Hiroshi TERADA
(Subaru Telescope, NAOJ)
(I) Organic Molecules in Protoplanetary Disks
(II) Exo-Planetary Atmosphere in Transiting Systems
Basic
Concept
~
Mul&plicity
vs.
Simultaneity
~
✓-‐-‐>
More
efficient
“survey
capability”
Mul%ple
Observa%on
=>
Very
important
towards
more
mul%plicity
than
“2”
(30-‐m
class
MOAO).
✓
Simultaneous
Observa%on
-‐-‐>
Simultaneity
could
be
essen%al
for
some
science
cases.
=>
Should
be
unique
even
with
“2”
science
paths.
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )
Advantage
of
RAVEN:
“Simultaneity”
Keyword:
Atmospheric
Calibra%on
at
IR
1
0.9
For
atmospheric
correc%on,
0.8
a
reference
star
is
observed
with
similar
airmass,
loca%on
J
0.7
0.6
on
the
sky,
and
close
%me
H interval.
K
0.5
0.4
Simultaneous
observa%on
of
0.3
the
reference
star
is
ul%mate
0.2
L methodology
for
perfect
0.1
M cancella%on
of
the
0
0.951 1.5 2 2.5 3 3.5 4 4.5 5 5.5 atmosphere
condi%on..
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )
(I) Organic Molecules in Protoplanetary Disks
Annu. Rev. Astro. Astrophys. 2010.48:205-239. Downloaded from www
by KOKURITSU-TENMONDAI LIBRARY on 09/19/10. For pers
large dynamic range that is involved: the outer radius of a protoplanetary disk can be anywhere
from a few tens of astronomical units up to 1,000 AU or more, whereas the inner disk radius is
(I)
Organic
Molecule
in
Protoplanetary
Disks typically just a few stellar radii, i.e., of the order of 0.02 AU. This spans a factor of 104 –105 in
spatial scale. For each orbit of the outer disk, we have up to ten million orbits of the inner edge
General
View
of
Protoplanetary
Disks ALMA
Direct imaging (HST or 8-meter ground-based)
Diffrac%on
Limits
(1-‐-‐3um)
(sub-)mm: continuum
Nearest
High-‐maa
starforming
region
(Orion) + molecular rotation lines
Nearby
molecular
cloud
(ex.
Taurus,
Near-IRρ
Ointerferometry
ph,,,)
cu l a r
regi on
Nearest
starforming
region
(ex.
TW
Hya) ol e
Warm
M
Mid-IR interferometry
Magnetospheric
accretion
Pure gas disk Dust inner rim
Planet-forming Cold
mid-‐plane Outer disk
region (mass reservoir)
(Ice)
0.03AU
0.03 AU 0.1--1AU
0.1 .. 1 AU
Near IR: continuum
10 AU
10AU
UV continuum, + atomic andNear-IR
molecular
dust lines
H-recombination lines continuum
Near-IR continuum Mid IR: continuum Mid-IR: (Sub)millimeter:
(origin unclear so far) dust continuum
+ molecular lines dust continuum 100 AU
100AU
IRCS + AO188 [NGS] @ + atomic
Orionlines (Br–γ) + molecular lines + molecular rot-lines
+ occasional molecular (H2O, CO2, ... )
lines (H2O, CO, OH) N
J,H,K’ L’ E
Ground-‐based
AO
works
well
Figure 1
in
Pictogram of the structure and spatial scales of a protoplanetary disk. Note that the radial scale onN IR
the r
x-axisegion.
is not linear. Above the
pictogram shows which techniques can spatially resolve which scales. Below shows which kind of emission arises from which parts of
the disk.
=>
Spectro-‐Astrometry
w/
AO
206 Dullemond · Monnier
is
a
hope
to
probe
the
inner
0”.2 (88AU) region..
Terada+
2012
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )direct Hubble Space Telescope images of such objects in silhouette against the background light in
(I)
Organic
Molecule
in
Protoplanetary
Disks
the Orion Nebula (McCaughrean & O’Dell 1996), the observational and theoretical study of these
planetary birthplaces has experienced an enormous thrust, leading to a much better understanding
of what they are, what they look like, how they evolve, how they are formed, and how they are
Previous
Detec%ons
eventually dissipated. Although none of these aspects has yet been firmly understood in detail,
there is a consensus on the big picture. It is clear that protoplanetary disks are the remnants of
Spitzer
the star-formation process. Excess angular momentum of the original parent cloud has to be shed Herschel
before most matter can assemble into a “tiny” object such as a star. Protostellar accretion disks (see
H2 HI NeII C2H2 HCN OH CO2
e.g., Hartmann 2009, for a review) are the most natural medium by which this angular momentum
Keck
NIRSPEC
Annu. Rev. Astro. Astrophys. 2010.48:205-239. Downloaded from www.annualreviews.org
can be extracted from the infalling material. When the star is mostly “finished” and makes its way
DK Tau
toward the main sequence, the remainder of this protostellar accretion disk is what constitutes a
by KOKURITSU-TENMONDAI LIBRARY on 09/19/10. For personal use only.
protoplanetary disk: the cradle of a future planetary system.
RW Aur / 2
Protoplanetary disks have a rich structure, with very different physics playing a role in different
GI Tau
regions of the disk. A pictographic representation is shown in Figure 1. One can see the strikingly
BP Tau
large dynamic range that is involved: the outer radius of a protoplanetary disk can be anywhere
AA Tau
from a few tens of astronomical units up to 1,000 AU or more, whereas the inner disk radius is
GK Tau
typically just a few stellar radii, i.e., of the order of 0.02 AU. This spans a factor of 104 –105 in
spatial scale. For each orbit of the outer disk, we have up to ten million orbits of the inner edge
UY Aur
DO Tau
DG Tau / 2
ALMA
Direct imaging (HST or 8-meter ground-based)Hogerheijde+
2011
V1331 Cyg
AS 353A
(sub-)mm: continuum
Carr+
2011 + molecular rotation lines
Near-IR interferometry
Salyk+
2008
u l a r
regi on
Mid-IR interferometry
a rm
M olec
Magnetospheric
W
accretion
Pure gas disk Dust inner rim
Planet-forming Cold
mid-‐plane Outer disk
region (mass reservoir)
(Ice)
0.03 AU
0.03AU 0.1 .. 1 AU
0.1--1AU
Near IR: continuum
10 AU
10AU
UV continuum, + atomic andNear-IR
molecular
dust lines
H-recombination lines continuum
Near-IR continuum Mid IR: continuum Mid-IR: (Sub)millimeter:
(origin unclear so far) dust continuum
+ molecular lines dust continuum 100AU
100 AU
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25
+ atomic lines (Br–γ) + molecular lines + molecular rot-lines Hiroshi TERADA ( Subaru Telescope )(I)
Organic
Molecule
in
Protoplanetary
Disks:
Near
IR
(~3um)
Wavelengths
Example of a Single IRCS Echelle Setting
Suitable for tracing
warm molecular volatile
gases.
Sensitive for temperature
(100--100K)
==>(I)
Organic
Molecule
in
Protoplanetary
Disks:
Difficul%es
in
Detec%on
DR Tau - NIRSPEC
Sect. 1
0.10
Tell. Mod. x 1/33
0.05
Flux (Jy)
0.00
Final Resids
1-sigma Noise
-0.05
2.950 2.955 2.960 2.965
Wavelength (µm)
Sect. 2
0.10
H2O, 900 K Combined Model
0.05 OH, 900 K
Flux (Jy)
HCN, 900 K
C2H2, 900 K
0.00
-0.05
2.970 2.975 2.980 2.985
Wavelength (µm)
Mandell+
2012
Gibb+
2007
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(I)
Organic
Molecule
in
Protoplanetary
Disks:
Example
of
IRCS
Result
(b) PDS 144N
PDS 144N 1
2006-02-07-UT
2008-02-18-UT
0.5
2008-06-12-UT
3 3.2 3.4 3.6 3.8 4
Terada+
2013
in
prep.
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(I)
Organic
Molecule
in
Protoplanetary
Disks:
Concept
for
Detec%on
On-sky
NGS IRCS Slit (Echelle)
4”
4”
4” 4”
• Simultaneous
spectroscopy
NGS • PA
can
be
selected
independently
NGS • Foreground
contribu%on
can
be
excluded
when
the
reference
is
in
the
same
cloud....
3.’5
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(I)
Organic
Molecule
in
Protoplanetary
Disks:
Example
of
Actual
Target
d294-606 R~8.15@58”
1”.28 x 1”.28 R~6.41@64”
Several
more
targets
are
available
in
HST / ACS F658N
2”.06x 2”.06
this
region!!
R~9.47@22”
IRCS+AO188 K’
VISTA
J,H,Ks
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(I)
Organic
Molecule
in
Protoplanetary
Disks:
Resolving
the
wavelength
issue...
RAVEN
1st
Science
Mee>ng
@
Tohoku
University • CaF2
Exit
relay
lens
designed/fabricated
(I),Organic,Molecule,in,Protoplanetary,Disks:
Issues!to!be!considered
Thanks,
Olivier!!
• Switch
the
relay
lens
RAVEN is not designed forthermal infrared bands (> 3.0um) only
when
thermal
# ,while IRCS covers 0.9--5.5um.
Table 1. Top Level Raven Requirements
Transmittance and emissivity
observa%ons
are
Parameter
AO System
Calibration System
Requirement
MOAO operation with tomographic reconstructor
Capable of testing MOAO during daytime and in lab
around 3.0um: unknown
planned.
• S%ll
needs
to
be
Science Instrument
Capable of feeding IRCS in imaging, grism and Might be worthy of trying observations
Echelle modes
Science spectral range 0.9-2.5 microns
at these wavelengths....
# of science channels 2
confirmed
for
the
# of WFS 3 NGS + 1 on-axis LGS
Field of Regard 3.5 arcminutes diameter
Science Field of View 4 arcseconds diameter per science pick-off
thermal
infrared
Delievered EE >30% in 140mas in H-band for r0=15 cm
>0.32 in H-band, telescope and IRCS excluded (80%
Throughput
of AO188 throughput) Only!hot!water!
Image rotation Ability to align each source to the IRCS slit emission
performance
because
Zenith angle(II) Exo-‐Planetary Atmosphere in Transi^ng Systems
(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Theory
for
Detec%on
Star
Transiting Planet
Molecular Atmosphere
around Planet
Required
Precision
~
10(-‐4)
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Observa%onal
Achievements
First
detec>on
w/
HST
STIS
NaD
line:
HD
209458
Ground-‐based
detec>on
w/
VLT
FORS
Op^cal
Spectroscopy
GJ
1214b
Charbonneau+
2002 Bean+
2010
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Ground-‐based
Trial
in
IR
Ground-‐based
IR
detec>on
w/
Magellan
+
MMIRS
Infrared
K-‐band
Spectroscopy
GJ
1214b
Bean+
2011
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Ground-‐based
Trial
in
IR
Miller-‐Ricci
Kempton,
Zahnle,
Fortney
2012
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Keys
to
Achieve
“10(-‐4)”
Especially for IR, it’s so difficult..
a. S%ck
the
target
exactly
at
the
same
loca%on
of
the
detector.
=>
Uncertainty
of
“ununiform
sensi%vity”
in
the
infrared
detector
has
to
be
eliminated.
b. Increase
the
S/N
using
over-‐sampling
of
the
object.
=>
Usually
defocused
image
is
used.
c. “Simultaneously”
observe
the
reference.
=>
Eliminate
variability
of
atmospheric
absorp%on
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Concept
for
Detec%on
1. Use AO to keep the star very effectively
at the same location of the infrared array.
=> atmospheric dispersion correction (software should be enough)
2. Too sharp image should lose S/N. +
Defocused image before the slit will lose the photon.
=> IRCS Prism is used.
=> After the slit, the photon will distribute over wider area of the array.
K
~50pix
L
Takato
&
Terada
2006
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
Example
of
Actual
Target
CoRoT-1b
R~13.3@67”
R~13.04@34”
R~12.21@30”
Many
targets
should
be
able
to
be
found
2MASS
J,H,Ks
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )(II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
S%ll
Require
Feasibility
Studies
RAVEN
1st
Science
Mee>ng
@
Tohoku
University
Currently
checking
•
(II),Exo7Planetary,Atmosphere,in,Transi[ng,System:,
CoRoT-‐1b
data.
In
one
Issues!and!Feasibility!Studies
month,
first
es%mate
No one has achieved yet such a high precision ~10(-4)
measurement in IR... will
come.
✴ Method!should!be!examined
I tried the feasibility study by using • HIP-‐HIP
binary
!!w/!on0sky!tes%ng
Hipparcos binary on Nov.17th, but
terrible weather prevented from tes%ng
w/
the
Prism
the successful testing.... Trial will continue.
✴ Close!((II)
Exo-‐Planetary
Atmosphere
in
Transi^ng
System:
S%ll
Require
Feasibility
Studies
CoRoT-1b
R~12.21@30”
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )Summary
✓Simultaneity:
A
key
for
showing
RAVEN’s
unique
science!
✓
To
detect
“Organic
Molecule
in
Protoplanetary
Disks”:
Wavelength
limita%ons
should
be
s%ll
carefully
inspected.
✓
“Exo-‐Planetary
Atmosphere
in
Transit”:
Feasibility
study
is
definitely
required.
RAVEN 2nd Science Meeting @ Waikoloa on 2013/07/25 Hiroshi TERADA ( Subaru Telescope )You can also read
