New facilities for new science

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New facilities for new science

• Ewine van Dishoeck
• Leiden Observatory

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Overview

• Introduction
• X-ray telescopes
• Optical UV telescopes
• Infrared telescopes
• Submillimeter telescopes
• Radio telescopes
• Computational facilities
• Big physics facilities

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Introduction

• Astronomy and lab astrophysics have a long
  tradition together
• Sun (He, H-)
• Nebulae (atomic data)
• ISM (X-ogengt HCO)
• ..
• Golden age of astronomy
• Several billion /Eu/Yen facilities (about to
  come) on-line
• Challenges
• Make big telescopes a big scientific success
• Continue to convince astronomers about need for
  lab astro data for success
• Think transformational

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Where are molecules found?

• Interstellar medium
• Cold neutral medium, molecular clouds
• Star-forming regions
• Protoplanetary disks
• Envelopes of evolved stars
• Cometary atmospheres
• Planetary atmospheres, incl. Exo-planets
• Stellar atmospheres

Give just a few examples here of recent
developments and challenges, both gas and solid
state
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Molecules in Space
Based on Ehrenfreund Charnley 2000
Lifecycle of gas and dust raw material for
planetary systems
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Approach
Models
Observations
optical, IR, Millimeter,
Radiative transfer Source structure Gas-grain
chemistry
Laboratory
Gas-phase and solid state laboratory Quantum
chemical simulations
All information comes from spectroscopy of gas
and dust
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X-ray telescopes
XMM spectroscopy of supernova remnant

• Mostly highly-ionized atomic lines
• X-ray absorption of dusty regions
• Dust elemental composition, e.g., Si/Mg, Mg/Fe
  ratios
• Total H column
• Next big X-ray mission gt2020

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UV telescopes
R104

• Only technique to observe bulk of cold H2 and HD
  and their excitation directly
• Few other molecules, but constraints on dust
  from extinction curve incl. 2200 Å
• FUSE has extended studies to nearby galaxies and
  intergalactic medium
• successor probably the WSO-UV satellite
• - Cosmic Origins Spectrograph to be installed on
  HST (gt1200 Å)

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Optical telescopes
C60?

• Small molecules in diffuse and translucent
  clouds
• Diffuse interstellar bands carriers?

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Rapid response/robotic telescopes

• Optical spectra toward gamma-ray
• bursts need to take spectra within hrs
• Get spectra of ISM in host galaxy at
• high-z with same sensitivity as that of
• local O/B stars (e.g., zeta Oph)!
• UV spectrum red-shifted into optical
• wavelengths, including H2 lines
• Investigate different environments, e.g.
• low metallicity, high radiation, ..

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Extremely Large Telescopes

• Several ELTs in 20-42m range being
• planned across the globe
• Challenge adaptive optics to reach
• diffraction limited resolution of milliarcsec
• Extremely powerful, but instrument
• suite will be limited, especially for
• highest resolution spectroscopy
• Major goal imaging and spectroscopy
• of exoplanets

e-ELT concept 42 m
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First image of exoplanet
First Earth-like planet in habitable zone
Chauvin et al. 2005
Udry et al. 2007
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Probing exo-planetary atmospheres
HD 209458 transiting planet Detection
of H2O to be confirmed by infrared data
Barman 2007

• HST and Spitzer are starting to probe
  exo-planetary atmospheres
• Extremely rapidly developing field, but lab data
  needs not yet clear
• (besides opacities)

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From visible to infrared light
HH 46 star-forming region
Spitzer
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Star and planet formation
Jonlheid 2006
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NGC 1333 outflows Ha,
SII Walawender, Bally, Reipurth 2006
Spitzer/IRAC Jørgensen et al. 2006
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Infrared spectral features

• Embedded protostars
• Ices and silicates in absorption
• Gas phase molecules in absorption
• Atomic Ne II 12.8, S I 25.2 mm, H2 lines
  (extended emission from outflow)
• Protoplanetary disks
• Silicate and PAH emission
• Absorption if viewed close to edge-on
• H2 emission?
• Ne II, Fe I emission

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Spitzers potential for studying low-mass YSOs
From 105 to lt0.1 Lsun objects!
HH 46 solar-mass YSO
ISO
ISO
Spitzer
L1014 substellar YSO
Ground-based 8-m

• Spitzer can study objects gt100 times fainter
  than ISO
• Need 8-m class ground-based telescopes or AKARI
  to cover 3-5 mm range
• Limited spectral resolving power R600 from
  10-38 mm
• 
  R100 from 5-10 mm
• - Ice mapping!

Noriega-Crespo et al. 2004 Boogert et al. 2004,
2007 Young et al. 2004
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Silicate grain growth and crystallization in
disks first step in planet
formation
Serpens core
Kessler-Silacci et al. 2006
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From dust to planets
Observable with DARWIN TPF etc.
Observable in visual, infrared and (sub-)mm
?
1?m
1km
1000km
1mm
1m
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Grain growth in lab and theory
Experiments Blum Wurm 2000. Icarus 143, 146
Theory Dominik Tielens 1997. ApJ 480, 647
Low impact energy hit-and-stick collisions
Intermediate impact energy compaction
High impact energyfragmentation
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Polycyclic Aromatic Hydrocarbons
- Challenge for lab larger PAHs
PAHN N-containing PAHs
Hudgins et al. 2005
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PAHs in disks
PAHs
Large grains
spectrum
8.6
11.3
PSF

• Separation of small and large grains
• Large grains have inner hole
• Very small grains, PAHs present inside hole

Geers et al. 2007
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Carbonaceous material
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Mid-infrared James Webb Space Telescope
Launch 2013
6 m
Medium resolution R1000-3000 spectroscopy 1-28 mm
NIRSPEC, MIRI
Sensitivity 1-3 orders of magnitude better than
ground or Spitzer
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JWST-MIRI hot water in inner disk
H2O abundance 10-5
Spitzer
Lahuis et al. 2006

• Prediction for H2O absorption toward IRS46 with
  MIRI
• Detection of hot CH4 and other organics should
  also be feasible
• Search for H2O emission in face-on disks

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Characterizing atmospheres of exoplanets

• JWST giant planets
• Darwin, TPF
• Earth-like planets
• gt2020

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SOFIA

• 2.5m telescope in B747 airplane
• US-German collaboration
• Good spectroscopic capabilities at
• long wavelengths

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Herschel Space Observatory

• HIFI heterodyne spectrometer R106
• 480- 1250 1410-1910 GHz
• 500-200 mm, 158 mm
• PACS imaging spectrometer R1500
• 60-200 mm
• SPIRE FTS spectrometer Rlt1000
• 200-670 mm

2008
H2O and other hydrides, Complete spectral
scans, Low-frequency modes of chains and PAHs,
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H2O from low-mass Class 0 sources to disks
ISO-LWS

• What is origin of strong H2O emission?
• - What is H2O abundance in disks?

Nisini et al. 1999 Ceccarelli et al. 1998
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Submillimeter telescopes
ODIN
IRAM30m
O2?!
Nobeyama 45m
APEX
CARMA
SMAJCMTCSO
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Dust and CO at 0.5 billion yr!
Z6.4
Optical image
Bertoldi et al.
CO lines
Contours dust

• Chemistry at high redshift HCN, HCO, ..
• Dust at high redshift formed by supernovae?
  composition and properties?

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Hot cores complex chemistry
G327 with APEX
Orion-KL 690 GHz spectra SMA

• How are complex molecules formed?
• on grains or in gas-phase?

Beuther et al. in prep Blake et al. 1987, Ohishi
et al. 1995, Wright et al. 1996, Schilke et al.
1997, 2001, White et al. 2003, Comito et al.
2005, .
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Some complex organic molecules
Not (yet) detected
Detected
Acetic acid
Di-methyl ether
Purine
Glycine
Ethanol
Sugar
Methyl cyanide
Methyl formate
Pyrimidine
Caffeine
How far does chemical complexity go? Can we find
pre-biotic molecules?
Based on Ehrenfreund 2003
Benzene
Ethyl cyanide
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Atacama Large Millimeter/Submillimeter Array
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Atmospheric transmission on good day
Bands 3, 6, 7 and 9 4 and 8 installed initially
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Atacama Large Millimeter/Submillimeter
Array
Chili 5000 m Chajnantor
50 x 12m antennas with zoom-lens
capability through configurations from 150 m to
15 km gt 1 to 0.01 12 x 7m ACA to fill in
short spacings 4 X 12m single dish total power
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Low frequency radio telescopes(up to 25 GHz)
Possible SKA design(s)

• Low frequency arrays well suited for searches for
  largest complex
• molecules

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Conclusions

• Incredible wealth in new facilities, many of
  which are well suited for studying molecules
• Puts responsibility on all of us to make the best
  use of them
• New areas of astrochemistry highest z galaxies,
  disks, exo-planets, .
• Need continued close interaction between
  laboratory and observations to define the right
  questions