TMT.PSC.PRE.06.032.REL011 Science with TMT The Power of the Planned Instrument Components GSMT SWG August 10, 2006 Paul Hickson The authors gratefully

TMT.PSC.PRE.06.032.REL01 1

Science with TMTThe Power of the Planned Instrument Components

GSMT SWG

August 10, 2006

Paul Hickson

The authors gratefully acknowledge the support of the TMT partner institutions. They are the Association of Canadian Universities for Research in Astronomy (ACURA), the Association of Universities for Research in Astronomy (AURA), the California Institute of Technology and the University of California. This work was supported, as well, by the Canada Foundation for Innovation, the Gordon and Betty Moore Foundation, the National Optical Astronomy Observatory, which is operated by AURA under cooperative agreement with the National Science Foundation, the Ontario Ministry of Research and Innovation, and the National Research Council of Canada.


The TMT

UC, Caltech, AURA, ACURA

Draws from three ELT design studies

– GSMT

– CELT

– VLOT

Unique aspects:

– 30-m filled circular aperture

– Wide 20 arcmin FOV

– A broad complement of instruments

– Powerful adaptive-optics systems


Science and Instrument development

Science programs drawn from a wide community in the USA and Canada

12-member Science Advisory Committee

– identified 8 instruments and 4 AO modes

– Science Requirements Document

– Detailed Science Case

Instrument Feasibility Studies

– Independent teams develop designs and science programs for the SAC instruments

– Non-advocate reviews for each instrument and AO systems

TMT Conceptual Design Review - May 2006

– “This is a well-scoped project, technically challenging, yet within reach. It will enable a new era in astronomy that is seductive and highly motivating.”


TMT Aperture Advantage

Seeing-limited observations and observations of resolved sources

Background-limited AO observations of unresolved sources

High-contrast AO observations of unresolved sources

High-contrast ExAO observations of unresolved sources

Sensitivity ∝ ηD2 (~ 14 × 8m)

Sensitivity ∝ ηS2D4 (~ 200 × 8m)

Sensitivity ∝ η S21−SD4 (~ 200 × 8m)

Contrast ∝ D2 (~ 14 × 8m)Sensitivity ∝ ηD6 (~ 3000 × 8m)

Sensitivity=1/ time required to reach a given s/n ratioη= throughput, S= Strehl ratio. D= aperture diameter


TMT Adaptive Optics Modes

NFIRAOS - Narrow-field infrared adaptive optics system

– LGS MCAO system - two DMs and asterism of seven laser stars

– Diffraction-limited over 30 arcsec FOV

– 2 arcmin FOV for AO-sharpened tip-tilt & focus stars

– S ~ 0.5 at 1 um (S ~ 0.3 at first light)

– Passed conceptual design review, May 2006

TMT NFIRAOS Team



ExAO - Extreme adaptive optics

– High-order AO system

– Diffraction suppression system - two-stage nulling interferometer

– Speckle suppression system

108 contrast achieved on a simulated G5 star at 30 pc in 1 hr. (TMT PFI team)



MIRAO - Mid-infrared adaptive optics

– Conventional high-Strehl laser AO system

MOAO - Multi-object adaptive optics

– Deployable probes with MEMS deformable mirrors

– Open-loop correction determined from LGS asterism

GLAO - Ground-layer adaptive optics

– Image ‘sharpening’ (low-order correction) over a wide field of view


IRIS

Near-infrared imaging spectrometer

– ~ 15-arcsec FOV diffraction-limited imager (4 mas pixels)

– 0.8 - 2.5 um

– On-axis R ~ 4000 IFU spectrometer

– Employs NFIRAOS MCAO system

TMT IRIS Team


IRMOS

Infrared multi-object spectrometer

– Multiple IFUs accessing a 2 - 5 arcmin FOV

– 0.8 - 2.5 um

– R ~ 2000 - 10000

– Employs MOAO to give near-diffraction-limited resolution

CIT IRMOS Team


WFOS

Wide-field optical spectrometer

– 0.3 - 1.2 um

– R ~ 150 - 6000

– 8 - 20 arcmin FOV

– GLAO capable

TMT WFOS Team


HROS

High-resolution optical spectrometer

– 0.3 - 1 um

– R ~ 20,000 - 100,000

– Fiber feed MOS option

UC HROS Team


MIRES

Mid-IR Echelle spectrometer

– 5 - 28 um

– R ~ 5000 - 100,000 spectrometer

– MIR slit-viewer / science imager

– Employs MIRAO system


NIRES

Near-infrared Echelle spectrometer

– bNIRES: 1 - 2.5 um

– rNIRES: 2.9 - 5 um

– diffraction-limited

– R ~ 20,000 - 100,000


PFI

Planet formation instrument

– high-contrast (~ 108) ExAO

– 1 - 5 um 2” x 2” imager and IFU spectrometer (R ~ 70 - 700)

TMT PFI Team


Key advances enabled by TMT

Fundamental physics

– 10x improvement in search for variations of fundamental constants

First light

– Detect first-light objects and study their physical properties

Intergalactic medium

– Map ionization and chemistry from first-light to present

– Tomographic structure of IGM and gas-galaxy connection

Galaxy formation/evolution

– Determine morphology, kinematics, dynamics, chemistry of galaxies at all redshifts with 5x the resolution of JWST

– Probe the dark matter distribution in elliptical galaxies

Black holes

– Study BH’s in all galaxy types and resolve the sphere of influence to z ~ 0.4

– Determine properties of the Galactic BH, the DM distribution, and test GR


Key advances enabled by TMT

Stellar populations

– Determine the star formation history in galaxies as far as the Virgo cluster

Star and planet formation

– Measure the IMF over the full range of mass in a variety of environments

– Resolve bipolar outflows and study feedback to the IGM

– Measure accretion rates and relationship to mass of protostars

– High-resolution observations of planets and protoplanetary disks

Exoplanets

– 30x increase in Doppler detection of exoplanets

– Detect terrestrial planets in the habitable zones of M stars by Doppler shift

– Detect planets by reflected light

– Direct spectroscopy of massive planets

– Characterize exoplanet atmospheres by absorption spectroscopy

The Solar System

– Direct detection of sub-km TNOs

– Atmospheric and surface chemistry of outer solar system objects


What is Dark Matter and Dark Energy?

Many theories - some predict variation of fundamental parameters.

Wavelengths in multiplets of redshifted UV lines in quasar spectra are sensitive to and to .

A decade of study with 10m-class telescopes has hinted at variations:

– Mixed results for variation of .

– Tentative (3.5) evidence for variability of .

HROS will provide a definitive resolution.

Cosmology and Fundamental Physics- The nature of dark matter and dark energy

=e2 / hc=mp /me

Wavelength residuals seen in QSO spectra vs. sensitivity coefficient. Positive slope indicates variation of . (Reinhold et al. 2006)


The Early Universe and First Light- The first luminous objects

TMT should detect the first luminous objects - and will study the physics of objects found with JWST:

– Detection of He II emission would confirm the primordial nature of these objects.

– With IRIS and IRMOS, we will be able to study the flux distribution of sources, and the size and topology of the ionization region.

– IRMOS will reach ~ 2x10-20 erg s-1 cm-2 for 25 mas sources in 4 hrs (an order of magnitude fainter than JWST)

Schaerer 2002


The Intergalactic Medium- Probing beyond z ~ 7

NIRES will use adaptive optics and infrared spectroscopy to probe the evolution of the IGM beyond z ~ 7:

– CIV, OI, CII lines are not affected by the Lyman- forest.

– Gamma ray bursts could provide high redshift beacons.CIVSiIVCIISiII

Ly

Ly forest

Lyman limit Ly

NV

SiIVCIV

Lyem

Ly SiII


The Intergalactic Medium- Tomography of the baryonic structure

WFOS will use multi-object spectroscopy of background galaxies to map the structure of IGM during the peak epoch of galaxy formation (z ~ 2 - 3.5).

– This will elucidate the relationship between galaxies and the IGM.

Simulation of dark matter structure at z = 3. (R. Cen, Princeton Univ.)

Simulated TMT observation with R = 24 source galaxy (WFOS-HIA team).


Galaxy Formation and Evolution- Detecting the first galaxies

IRMOS will be able to detect galaxies at very high redshift:

– Ly- detectable to z > 12.

– z ~ 15 should be detectable by placing IFUs on caustics of gravitational lens systems.

– Adaptive optics is critical for these small objects.

There are potentially many objects per TMT field of view, depending on the transparency of the intergalactic medium. TMT IRMOS-UFHIA team


Galaxy Formation and Evolution- Detailed mapping of high-redshift galaxies

IRIS and IRMOS will probe chemistry and dynamics of high-redshift galaxies and study the assembly of galaxies with 100 pc resolution.

Multiple deployable IFUs will provide statistically significant samples.

Key questions:

– How does the age of the stellar population compare to the dynamical age of the galaxy?

– How do star formation modes relate to the dynamical state?

– How do massive galaxies of old stellar populations form and evolve?

– How does the Hubble sequence arise?

– How do bars, bulges,disks form?

– How important is feedback?

J. Larkin


Galaxy Formation and Evolution- Physics of galaxy formation

IRIS and IRMOS will map the physical state of galaxies over the redshift range where the bulk of galaxy assembly occurs:

– Star formation rate

– Metallicity maps

– Extinction maps

– Dynamical Masses

– Gas kinematics

Synergy with ALMA:

– Molecular emission

z = 0

z = 2.5

z = 5.5

TMT IRMOS-UFHIA team


Galaxy Formation and Evolution- Dark matter distribution

WFOS can measure radial velocities for virtually all globular clusters in Virgo cluster elliptical galaxies.

This will allow us to probe the dark matter distribution in these massive galaxies.

Keck

TMT

M49 M49

TMT WFOS-HIA team


Black holes and Active Galactic Nuclei- Evolution and the galaxy - BH connection

IRIS will determine black hole masses over a wide range of galaxy types, masses and redshifts:

– It can resolve the region of influence of a 109 M BH to z ~ 0.4 using adaptive optics.

Key questions:

– When did the first super-massive BHs form?

– How do BH properties and growth rate depend on the environment?

– How do BHs evolve dynamically?

– How do BHs feed?

CFA Redshift Survey galaxies


Black Holes and Active Galactic Nuclei- The galactic center

IRIS will map stellar orbits in the galactic center with exquisite precision:

– This will allow us to probe the gravitational potential and study the nature of dark matter on small scales.

– It will provide a precise measurement of the black hole mass, galactic constants, and will detect relativistic effects.

A. Ghez, UCLA


Stellar Populations in the Local Universe- Stellar archaeology

IRIS and HROS will determine the star formation history in galaxies out to the Virgo cluster:

– Adaptive optics will allow photometry of resolved stellar populations in crowded fields.

– This will give star-formation history and metallicity in a wide range of environments.

– High-resolution spectroscopy will provide element abundances.

– Complimentary to high-z galaxy studies.

Simulated M32 CMD with TMT MCAO. The red, blue and green lines represent three input stellar populations. (K. Olsen, NOAO)


Stellar Populations in the Local Universe- Dynamics of halo stars

HROS will use multi-object spectroscopy of thousands of stars to map the dynamical states of stellar populations:

– This will allow us to test theories of structure formation on sub-galactic scales.

– By comparison with models, one can infer the merger history of nearby galaxies.

N-body simulations of satellite accretion (TMT WFOS-HIA team, Bullock & Johnstone 2005).


Evolution of Star Clusters and the IMF

IRIS will allow us to determine the initial mass function in star clusters from < 1 to 100 M in a range of stellar environments:

– IFU imaging/spectroscopy at the diffraction limit with MCAO.

AO image of star field in M31 from Gemini/Altair. TMT’s MCAO will provide better psf uniformity, higher Strehl ratios, 4x sharper images and ~ 20x deeper imaging (TMT IRIS team).


Physics of Star and Planet Formation- Bipolar outflows

IRMOS will allow us to study the physical conditions in star-forming regions:

– Resolve bipolar outflows using adaptive optics and study their interaction with the ISM in galactic star-forming regions.

– Investigate feedback from protostars to the molecular cloud.

– Study many Herbig Haro objects at a time using deployable IFUs.

– Will compliment submm observations with ALMA.

Perseus star-forming region (TMT IRMOS-CIT team)


Physics of Star and Planet Formation- Young stellar objects

NIRES will be able to characterize essentially all young stellar objects in nearby star-forming complexes:

– High-resolution spectra of the CO fundamental line will allow mass accretion rates to be derived.

TMT flux limit (500s, R=100,000, s/n = 50)

TMT NIRES team


Physics of Star and Planet Formation- Protoplanetary disks

MIRES will resolve the inner regions of protoplanetary disks to study abundances, chemistry, kinematics and planet formation dynamics:

– Determine physical properties of the disk and detect gaps produced by planets

– Synergy with ALMA, JWST.

G. BrydenG. Bryden & J. Najita


Physics of Star and Planet Formation- Planet formation

MIRES will be able to image protoplanetary disks and detect features produced by planets:

– TMT will have 5x the resolution of JWST.

Simulation of Solar System protoplanetary disk (Liou & Zook 1999)


Doppler Detection of Extrasolar Planets

HROS will expand the number of host stars accessible to Doppler spectroscopy by a

factor of ~ 30, and provide sensitivity to lower-mass stars

R. P. Butler


Characterization of Extrasolar Planets - Doppler detection

HROS will be able to detect Earth-mass planets in habitable zones around nearby M stars:

– M stars are the most common stars in the galaxy. Their habitable zone is 0.01 - 0.3 AU.

Kasting et al 1993


Characterization of Extrasolar Planets - Direct detection

PFI will directly image young planets near low-mass stars using high-order adaptive optics (ExAO)

– Arguably the most technically challenging (and rewarding) of all the TMT technologies

4 MJ planet orbiting a brown dwarf

~80 MJ planet orbiting an old K star


Characterizing Extrasolar Planets- Extreme adaptive optics

TMTs large aperture will allow detection of planets closer to their host stars:

– Detection of planets by reflected light.

– Probe scales comparable to inner Solar System.

– Detect planets forming in circumstellar disks.

TMT PFI team


Characterizing Extrasolar Planets- Properties of exoplanets

TMT will provide:

– Doppler follow-up of transit detections (HROS).

– Absorption spectroscopy of atmospheres of transiting planets (HROS).

– Reflected light spectroscopy of “hot jupiters” (PFI).

– Direct spectroscopy of massive planets (PFI).

GJ 876d: 7.5 M

Lynette Cook


Characterization of Extrasolar Planets- Atmospheres of massive planets

MIRES will be able to measure the spectra of massive planets in the mid-infrared:– Contrast is lower in the

mid-infrared.

– Strong molecular lines characterize the atmospheric composition.

– Spectral deconvolution can reveal the planetary spectrum

TMT MIRES team


Characterization of Extrasolar Planets- Atmospheres of terrestrial planets

TMT will detect the absorption signatures of gases in the atmosphere in transiting planets.

– Na, K, He, will be easily detectable with TMT

HROS should be able to detect O2 in the atmosphere of an Earth-like planet orbiting in the habitable zone of an M star

– s/n ~ 30,000 per 6 km/s resolution element - achievable by TMT in ~ 3 hrs.

Webb & Wormleaton 2001

O2 A-band


Solar System Studies

TMT will extend studies of the outer Solar System:

– IRIS will be able to detect a 1 km TNO at 50 AU in 15 min.

IRIS and MIRES will provide a capability for high-spatial resolution imaging and spectroscopy of planets and satellites of the solar system:

– high-resolution spectra of features on outer Solar System bodies will allow studies of atmospheric physics and atmospheric and surface chemistry

– Regular monitoring will allow TMT to study transient phenomena, weather, volcanic activity, etc.

Europa at the resolution of TMT

adaptive optics (M. Brown, CIT)


Solar System Studies-Atmospheric chemistry

MIRES will be able to study the atmospheric physics of the outer planets and their satellites by mapping them at high spectral and spatial resolution using adaptive optics

– This resolution is well beyond what has been achieved by planetary space missions.

High-resolution spectra of Titan. (Roe et al. 2003)


Summary

TMT will open new frontiers over a broad range of science areas.

This will be enabled by an ambitious complement of instruments and sophisticated adaptive optics systems.

D4 gain will provide a 100-fold increase in sensitivity compared to 8 - 10 m telescopes, opening vast new discovery space.

Documents

TMT.PSC.PRE.06.032.REL011 Science with TMT The Power of the Planned Instrument Components GSMT SWG August 10, 2006 Paul Hickson The authors gratefully