Presentation on theme: "1 Massimo Stiavelli Space Telescope Science Institute Studying the First Galaxies with the Hubble and the Webb Space Telescopes Hubble Science Briefing."— Presentation transcript:
1 Massimo Stiavelli Space Telescope Science Institute Studying the First Galaxies with the Hubble and the Webb Space Telescopes Hubble Science Briefing
4 Perturbations z=18 z=0 z=1.4 z=5.7 Redshift z : 1+z gives the ratio of the radius of the Universe today and that at a given epoch in the past. It also gives the ratio of the wavelength we observe over the one that was emitted. Computer simulations show the growth of structure
5 Growth of perturbations Underdensities grow like miniature Universes. They expand becoming rounder. Overdensities collapse and can become flattened or filamentary. This is the origin of the filamentary structures seen in simulations. Galaxies form along filaments. Clusters of galaxies at the intersection of filaments.
6 Growth of perturbations From random initial conditions it is “easy” to study the evolution of dark matter through computer simulations. The reason is that dark matter interacts only by gravity. It is much more difficult to study the evolution of ordinary matter (gas) since its interactions are much more complex. Thus the formation of stars and galaxies share the complexity of weather forecast. We think the first galaxies form at a redshift between 6 and 15 but there are many uncertainties. Thus, the input from observations is essential.
16 Studying the sources responsible for reionization was the main goal of the Hubble Ultra Deep Field. Today we know more z=6 objects than we knew at z=4 ten years ago. Ionizing flux from z=6 tantalizing close to what is needed for reionization but not quite enough. Possibilities: – z=6 do the job because they are at very low metallicity and hence their stars are hotter and produce more UV light – z=6 do the job because LF has many dwarf galaxies too faint to be seen in the HUDF – z=6 don’t do the job alone look at z=7+ Reionization
17 Possible deficit of z>7 galaxies The Luminosity Function (LF) is defined as the number density of objects (galaxies, stars) with a given luminosity. The analysis of all deep fields observed with Hubble, finds evidence for a rapid change in the Luminosity Function of galaxies going from 6 to 7+. The significance is not very high due to small number statistics. However, if this result is confirmed it would imply that reionization is indeed completed between 6 and 7 and that some combination low metallicity and a dwarf-rich LF does the job.
18 Some examples HST NICMOSHST ACS <-- Probably not real 3 candidates Detected in the IR but not in the visible
19 Future Hubble observations Objects at z>7 are faint and relatively rare. In order to obtain a significant sample we need a better instrument : the IR channel of the Wide Field Camera 3 which was installed on Hubble in May during Servicing Mission 4. WFC3/IR can cover the same area as NICMOS Cam3 to the same depth in one tenth of the time.
21 Hubble Ultra Deep Field 2009 Our group has been awarded a total of 336 HST orbits to study the population of galaxies at redshift 7 or higher using the WFC3. Most of these orbits will be spent revisiting the original HUDF and the first followup (HUDF05). = NICP12 = NICP34
23 Reionization vs First Galaxies Reionization is not necessarily completed by the First Galaxies. However, the First Galaxies must have formed before the completion of reionization.
24 Indication from observations Above a redshift of 5, as the redshift increases galaxies seems to become fainter and rarer. Number evolution z=4 z=5 z=6 z=7 Luminosity evolution
25 Indication from theory The observed trend are in good agreement with the expectations with theory. Models predict that the first galaxies might form around redshift 15 but they will be faint and rare. Thus, they might be outside the capability of Hubble.
26 Cooling In our everyday experience cooling generally occurs by thermal conduction to a colder object. Heat flows from the warm to the cold object and the warm object cools. However, an object can cool radiatively, emitting light (e.g. infrared light). In our homes normal light bulbs cool radiatively. The filament heats because of its resistivity to an electric current and cools radiatively. Indeed, the filament is in vacuum (otherwise it would burn). Thus, unlike thermal conduction, radiative cooling can happen in vacuum and is the most important cooling mechanism in space. Gas that is enriched with metal is a more effective coolant.
27 A star is born Density and temperature of gas around a first star. From left to right the images refer to a time 0, 1, 2.7, and 8 Myrs after its formation.
28 Paving the way for the first galaxies The first stars will enrich the Universe with heavier chemical elements (“metals”) and will produce the first black holes. After the first and possibly second generation of stars gas in the Universe begins to have metallicities different from primordial. The additional metals change the way gas cools and make the formation of smaller mass stars easier.
29 When stars fuse hydrogen into heavier elements, they produce both energy and metals. The role of metallicity The first stars have practically no metals but during their lifetime they produce metals. Some end their life as black holes others undergo a supernova explosion and enrich the Universe with metals.
30 Early in the life of the Universe when only few generations of stars had been formed the metallicity was very low. Each generation of stars incorporates metals produced by the previous generations. Once the metallicity is high enough stars form as in the Milky Way. Now High-z
31 If we assume that stars formed at a constant rate over the lifetime of the Universe, there were at z=6 only 7 per cent or less of the stars we see today. Thus, the mean metallicity of the Universe was also likely (much) less than 7 per cent of the present value. Now z=6 Age is only 7 per cent of present age
32 Metal poor stars are hotter and may have very different properties from present day stars. Detecting individual primordial stars is going to be very hard but it will be possible to detect primordial galaxies.
33 The First Galaxies might have higher metallicity if thet are formed from enriched gas. Primordial stars?Stars enriched by a SN?
34 JWST: Quick Facts Description Deployable cryogenic telescope - 6.5 meter ø, segmented adjustable primary mirror Launch on an ESA-supplied Ariane 5 to Sun-Earth L2 5-year science mission (10-year goal): launch 2013 Organization Mission Lead: Goddard Space Flight Center International collaboration with ESA & CSA Prime Contractor: Northrop Grumman Space Technology Instruments: Near Infrared Camera (NIRCam) – Univ. of Arizona Near Infrared Spectrograph (NIRSpec) – ESA Mid-Infrared Instrument (MIRI) – JPL/ESA Fine Guidance Sensor (FGS) – CSA Operations: Space Telescope Science Institute (STScI)
35 JWST Science Themes Patchy Absorption Redshift Wavelength Lyman Forest Absorption Black Gunn- Peterson trough z<z i z~z i z>z i Neutral IGM. What are the first galaxies? When did reionization occur? –Once or twice? What sources caused reionization?
36 JWST Science Themes Where and when did the Hubble Sequence form? How did the heavy elements form? Can we test hierarchical formation and global scaling relations? What about ultraluminous infrared galaxies and active galactic nuclei?
37 JWST Science Themes The Eagle Nebula as seen in the infrared How do clouds collapse? How does environment affect star-formation? –Vice-versa? What is the low-mass initial mass function?
38 JWST Science Themes Fomalhaut (SST): Stapelfeldt et al 2004 Fomalhaut (ACS): Kalas, Graham & Clampin 2005 How do planets form? How are circumstellar disks like our Solar System? How are habitable zones established?
40 z = 0.0 – 0.5 Probing the Early Universe in the Infrared with a 6m Space Telescope z = 0.5 – 1.6 z = 1.6 – 6.0 z = 1.6 – 6.0 JWST simulation, 10,000 seconds per infrared band, 2.2 m, 3.5 m, 5.8 m 1,000,000 seconds integration with HST
41 JWST-Spitzer image comparison Spitzer, 25 hour per band (GOODS collaboration) 1’x1’ region in the UDF – 3.5 to 5.8 m JWST, 1000s per band (simulated) (simulation by S. Casertano)
42 The James Webb & Hubble to same scale JWST is 7 tons and fits inside an Ariane V shroud This is enabled by: Ultra-lightweight optics (~20 kg/m 2 ) Deployed, segmented primary Multi-layered, deployed sunshade L2 Orbit allowing open design/passive cooling Astronaut
44 EDU Mirror - Figuring Process Pathfinder Today Concept DevelopmentDesign, Fabrication, Assembly and Test Formulation Authorization NAR (Program Commitment)Launch science operations... ICR [Long Lead Approval] Phase A Phase B Phase C/D Phase E Formulation Implementation … T-NAR
46 Technology Milestones met ✔ Sunshield Material April 2005 Mid-IR Detectors July 2005 ✔✔ ✔ ✔ ✔ ✔ ✔ ✔ ✔
47 Space science infrastructure and facilities only astronomers need Chandra’s X-Ray (cryogenic) calibration facility
48 Hardware progress JWST_ISIM.May.QSR/48 Optical Telescope Element Sun Shield Spacecraft Bus Integrated SI Module Thermal model test Model for membrane management tests Engineering Segment and Flight Segment Engineering Development Unit
49 Launch Configuration Long Fairing 17m Upper stage H155 Core stage P230 Solid Propellant booster Stowed Configuration JWST is folded into stowed position to fit into the payload fairing of the Ariane V launch vehicle