General General Astrophysics Astrophysics with TPF-C with TPF-C David Spergel David Spergel Princeton Princeton
Jan 16, 2016
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