General General AstrophysicsAstrophysicswith TPF-Cwith TPF-C

David SpergelDavid Spergel

PrincetonPrinceton

Please, Chas….Please, Chas….

Ability to point at alternative targetsAbility to point at alternative targets Wide (but not ultra-wide field imaging)Wide (but not ultra-wide field imaging)

5’ x 5’5’ x 5’ Astrometry well-sampled pixelsAstrometry well-sampled pixels Variable Objects (SN) large area/near-IRVariable Objects (SN) large area/near-IR

Ability to observe in parallel mode while doing Ability to observe in parallel mode while doing planet finding (control of scattered light)planet finding (control of scattered light)

GRISM capability?GRISM capability?

Division of Focal PlaneDivision of Focal Plane

GENERAL ASTROPHYSICS

Planet finding

Discovery SpaceDiscovery Space

UNIQUE CAPABILITYUNIQUE CAPABILITY CoronagraphyCoronagraphy PolarimetryPolarimetry High resolution/wide High resolution/wide

field (10 mas/5’)field (10 mas/5’) IFU + high spatial IFU + high spatial

resolutionresolution Stable PSFStable PSF

AstrometryAstrometry PhotometryPhotometry

OTHER INSTRUMENTSOTHER INSTRUMENTS JWSTJWST SIMSIM GAIAGAIA Ground-based 20/30-Ground-based 20/30-

mm LSSTLSST Many 8-m class Many 8-m class

telescopestelescopes

Astrometric CapabilitiesAstrometric Capabilities Able to get 30-100 Able to get 30-100

as astrometry for as astrometry for faint objectsfaint objects Tie to SIM Tie to SIM

referencesreferences Distance to faint Distance to faint

galactic objects galactic objects Proper motions for Proper motions for

main sequence main sequence stars in Baade’s stars in Baade’s window and in tidal window and in tidal tailstails

Key Science QuestionsKey Science Questions What is the dark energy?What is the dark energy? What is the dark matter?What is the dark matter? How do black holes form? What feeds them? How do black holes form? What feeds them?

How do they affect their environment?How do they affect their environment? How do galaxies form and evolve?How do galaxies form and evolve? How do stars and planetary systems form How do stars and planetary systems form

and evolve?and evolve? Explore diversity of worlds that might Explore diversity of worlds that might

harbor lifeharbor life

What is the dark energy?What is the dark energy? Measure angular diameter distanceMeasure angular diameter distance

Supernova as standard candlesSupernova as standard candlesSearch for supernova in parallel observing mode Search for supernova in parallel observing mode

(and other variable objects)(and other variable objects)TPF-C has ~8 x collecting area of SNAPTPF-C has ~8 x collecting area of SNAP

Growth rate of structureGrowth rate of structure Strong lensing (Survey rich cluster arcs to Strong lensing (Survey rich cluster arcs to

measure their mass). Much higher arc density measure their mass). Much higher arc density that ACS+HST [see Dedeo’s talk]that ACS+HST [see Dedeo’s talk]

Weak lensing of galaxies observed in parallel Weak lensing of galaxies observed in parallel mode (50-100 pencil beams)mode (50-100 pencil beams)

Parallel Extreme Deep Parallel Extreme Deep FieldsFields

50 target stars (50% of time [5 yr 50 target stars (50% of time [5 yr mission])mission]) 18 days of integration per field with 6 x 18 days of integration per field with 6 x

HST collecting area > UDF sensitivity on 50 HST collecting area > UDF sensitivity on 50 fieldsfields

Multiple visits: variability studiesMultiple visits: variability studies Very complementary to LSST programVery complementary to LSST program

Complement with repeat return visits?Complement with repeat return visits? 200 comparative planetology targets 200 comparative planetology targets

(25% of mission time)(25% of mission time) 3 days of integration ~ HDF sensitivity3 days of integration ~ HDF sensitivity

NICMOS + ACS JWST + TPF-C

Comparison with HST Comparison with HST Supernova searchSupernova search

HST study HST study Riess et al. 2004Riess et al. 2004 5 epochs at intervals of 5 epochs at intervals of

45 days (0.1 square 45 days (0.1 square degrees) in Z band degrees) in Z band (2000 s exposures)(2000 s exposures)

Limiting mag of 26Limiting mag of 26 Parallel fieldsParallel fields

10x area (50 5’ x5’ field)10x area (50 5’ x5’ field) Longer time-baselineLonger time-baseline Out to 1.7 micron, SNIa Out to 1.7 micron, SNIa

to z~3 (SNII to higher z)to z~3 (SNII to higher z) ~100 x HST Supernova ~100 x HST Supernova

samplesample

Riess et al. 2004

What is the dark matter?What is the dark matter?

Measure clustering properties of Measure clustering properties of dark matterdark matter In our own Galaxy: Tidal tails--- extend In our own Galaxy: Tidal tails--- extend

SIM tidal tail program by obtaining SIM tidal tail program by obtaining proper motions for stars in tidal proper motions for stars in tidal streams (requirement: 10 km/s at 20 streams (requirement: 10 km/s at 20 kpc -> 100 kpc -> 100 as)as)

In clusters of galaxies: strong lensingIn clusters of galaxies: strong lensing

Strong Lensing: Detailed Strong Lensing: Detailed Studies of ArcsStudies of Arcs

Resolve substructure Resolve substructure in arcsin arcs

Detect many more Detect many more arcsarcs

Use surface Use surface brightness constraints brightness constraints to limit lens modelsto limit lens models

Use features in arcs to Use features in arcs to constrain lumpiness in constrain lumpiness in cluster halos cluster halos

= 0.01 (M/10= 0.01 (M/1066 Msun) Msun)1/21/2

See Dedeo’s talk

How Are Galaxies How Are Galaxies Assembled?Assembled?

Galaxies far awayGalaxies far away Extreme deep field imaging (complemented by Extreme deep field imaging (complemented by

JWST imaging of same fields and spectroscopy JWST imaging of same fields and spectroscopy with the 20/30-meters)with the 20/30-meters)

Galaxies nearbyGalaxies nearby Stellar population studies in M31Stellar population studies in M31 White dwarf sequences in GCs [M4 study can White dwarf sequences in GCs [M4 study can

be extended further out and combined with be extended further out and combined with SIM distances]SIM distances]

Orbits for stars down to main sequence in Orbits for stars down to main sequence in Baade’s window [SIM astrometry + multi-epoch Baade’s window [SIM astrometry + multi-epoch imaging] (e.g., Kuijken & Rich’s HST program)imaging] (e.g., Kuijken & Rich’s HST program)

Black Holes and Their Black Holes and Their EnvironmentsEnvironments

Extend studies of black hole properties in Extend studies of black hole properties in nearby galaxies (IFU with higher nearby galaxies (IFU with higher resolution?)resolution?)

Coronagraphic Imaging of Host GalaxiesCoronagraphic Imaging of Host Galaxies Image M31 nucleusImage M31 nucleus

Resolve nature of double nucleusResolve nature of double nucleus Follow orbits around black holeFollow orbits around black hole

Probe black holes near “hang-up radius” Probe black holes near “hang-up radius” (Yu 2002)(Yu 2002) Imaging or astrometryImaging or astrometry

Imaging of fine details of low surface Imaging of fine details of low surface brightness host/lens galaxies of brightness host/lens galaxies of gravitationally lensed quasarsgravitationally lensed quasarsHost galaxy

of a bright &low redshiftquasar. ---->Change withredshift?

<---- Optical EinsteinRing gravitational lens.

Reconstructed 0.01”resolution image of ahigh z star formationburst galaxy. ---->

The details of low surface brightness resolved objects are often key to constraining lens models but nearly superimposed bright quasar images make their detection difficult.

E. Turner 4/14/04 TPF Ancillary Science

RequirementsRequirements

Pointing without bright target starPointing without bright target star Parallel mode operation (data Parallel mode operation (data

download + scattered starlight)download + scattered starlight) Wide field imaging capability (5’x5’)?Wide field imaging capability (5’x5’)?

Small pixels on some of field for better Small pixels on some of field for better astrometric capabilityastrometric capability

Spectroscopy? GRISMSpectroscopy? GRISM

THE END

Origins RoadmapOrigins Roadmap