Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.stsci.edu/institute/conference/hsl/Mould.PDF Äàòà èçìåíåíèÿ: Tue Apr 11 00:24:43 2006 Äàòà èíäåêñèðîâàíèÿ: Sat Dec 22 11:28:41 2007 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: massive stars

HST++ Summary

Jeremy Mould
National Optical Astronomy Observatory


What is the discovery space for HST++ ?

· · · ·

UV 2.5 mag beyond COS 8 meter Optical 2.5 mag beyond ACS Resolution a few mas Field larger than ACS (>1 Gpx)

Instrumental gains beyond this if science drivers are identified


HST++ will complement ALMA, NGST, GSMT and SIM

10 mas at 1.6µ


SUVO

·

Evolution of IGM
ü ü ü ü

FUSE, COS ü equation of state of baryons Legacy

survey hot gas measure its large scale structure how do galaxies interact with this environment ? chemical evolution: light elements and Hubble Legacy heavies
watch for LSST

· ·

Weak lensing Supernova cosmology


· · · ·

LSST, a digital survey of the sky each week
Weak lensing mass map of the Universe 100,000 supernovae per year z (1,2) Earth crossing asteroids 10,000 primordial transNeptunian objects
View of the LSST telescope structure in the Steward Observatory straw man design. The primary mirror is at the center, and the secondary and tertiary are almost equidistant from the primary. The detectors are just ahead of the central hole in the primary (see: http://dmtelescope.org/ design.html)


IGM "killer apps" for HST++

UV HRS

·

Large scale structure of IGM @ z < 1.65
ü ü ü ü ü

evolution of Ly forest and its large scale structure many QSOs => many sight lines damped Ly systems = baryon reservoir for all z chemical evolution of IGM to present day relate structure to galaxies
( groundbased zs )


Stellar pops "killer apps" for HST++

·

Galaxy formation

Don't descope ü unfilled dark halos this WF camera ü first generation of stars &below a Gpx IMF
ü

forming stellar halos by accretion

·

H0 : Cepheids in Coma + SNIa zeropoint
ü ü

w is also an LSST H/H ~ 2% with SIM recalibration goal

with Planck, constrain the dark energy "equation of state of the Universe" w ~ 0.01


Global parameters: the Hubble Constant
Is H0 > 60 km/sec/Mpc ?


Jim Peebles' ruling


HST++ complementary to GSMT

·

Star formation histories in Virgo
MS Population I (to 108 years) with HST++ AGB 108 to 1010 years with GSMT

·

z = 6 Universe
molecular clouds ­ ALMA SFR from H ­ NGST kinematics of galaxy formation ­ GSMT starburst Ly emission ­ HST++

·

Large scale structure of IGM @ z < 1.65


Some HST programs
plane
van Dokkum et al

GSMT

e.g. Evolution of the fundamental

· ·

Currently, z = .5 to 1.5
Structure from HST Kinematics from Keck

Future, z = 2 to 3.5
Structure and kinematics from GSMT Mg lines 517 nm redshift to 1.6 ­ 2.3µ


The Fundamental Plane at z>0
Jorgensen et al '96 Kelson et al '00 van D & Franx `96

Kelson et al '97

van D et al `98

Slide courtesy of Pieter van Dokkum


HST programs
e.g. Extending the stellar

GSMT HST++

populations laboratory

·

Star formation histories of
M31 Leo ellipticals
Projects possibly accessible from the ground not included here among killer applications


WFPC2 and SFH of LMC
Just count stars at base of red giant branch => SFR(t)


Star formation histories with GSMT or HST++
· Basic assumption: IMF is robust
ü ü

verified by HST studies of local dwarfs maybe inapplicable to Pop.III

· In all Local Group galaxies, full Star
Formation History is on display
ü ü

CMDs show number of stars formed each Gyr in the Hertzsprung gap just count the stars as they cross !


Black hole environments ·HST++ 10 mas 200nm 4
Intermediate mass black holes in globular clusters

meter ·SIM ·GSMT ·NGST ·ALMA

10 10 300 10

mas mas mas mas

600nm 1.6µ 10µ 1mm
M31 nucleus 10 µas astrometry will probe dynamics [Spergel]

M87 jet 10 mas = 1 pc
wfpc2


Resolving stars

· · · ·

OVI inner disk in CVs Surface features of cool stars Globular cluster cores Star formation.....summary part II


Non-science notes

· · ·

Ground based co-program should be designed at the outset National Astronomy and Astrophysics Committee NSF/NASA cooperation Inter Agency Consultative Group NASA/ESA cooperation


The search for identity

· · · · · · · ·

SUVO LOST ALOT arbitrarily large Guinness HST++ HST II NHST followed by NIST, NJST... TPF

Ask for ALOT or we may not get MUCH


end


Comparative performance of a 30m GSMT with a 6.5m NGST
Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration
10
R=5 R=1,000 R=10,000

R = 10,000 R = 1,000 R= 5

S/N Gain (GSMT / NGST)

1

0.1

0.01

1E-3

1

10
S/NGain(GSMT/NGST)

NGST advantage

GSMT advantage

10 1 0.1 0.01 1 10 Wavelength (microns)

R=10,000 R=1,000 R=5

Wavelength (microns)