SIRTF Speakers Bureau Charts - August 2001 Edition
| Page(s) | Chart Subject | Powerpoint | |
|---|---|---|---|
| 1-2 | Title Chart for Talk | p1-2.ppt | p1-2.pdf |
| 3-5 | Background in IR Astronomy; Need for Space | p3-5.ppt | p3-5.pdf |
| 6-11 | Overviews of SIRTF Mission, pictures and words | p6-11.ppt | p6-11.pdf |
| 12-23 | Drawings and Photographs of CTA and S/C hardware, including assembled CTA, MIC with three instruments, description of warm launch, heat map, etc. | p12-23.ppt | p12-23.pdf |
| 24-27 | Operational features, orbit, viewing windows, etc. | p24-27.ppt | p24-27.pdf |
| 28-32 | Defining scientific programs for SIRTF, recent progress in key areas, SIRTF in context of Great Observatories and Origins Program | p28-32.ppt | p28-32.pdf |
| 33-37 | SIRTF science utilization, timeline, interactions with SSC, summary of Legacy program. | p33-37.ppt | p33-37.pdf |
| 38-45 | SIRTF instrumentation overviews, sensitivity comparisons, summaries of functionality, etc. | p38-45.ppt | p38-45.pdf |
| 46-52 | IRAC - overview, hardware, science themes, HDF simulations, etc. Test image data shown as well | p46-52.ppt | p46-52.pdf |
| 53-58 | IRS - overview, hardware, science themes, stimulations, test data, etc. | p53-58.ppt | p53-58.pdf |
| 59-66 | MIPS - overview, hardware, science themes, simulations etc. | p59-66.ppt | p59-66.pdf |
| 67-86 | SIRTF extragalactic science, including Legacy and GTO programs, and relationship of SIRTF to other major NASA programs in this area | p67-86.ppt | p67-86.pdf |
| 87-97 | SIRTF galactic science, including Legacy and GTO programs | p87-97.ppt | p87-97.pdf |
| 98-99 | SIRTF and the Kuiper Belt | p98-99.ppt | p98-99.pdf |
| 100 | The SIRTF Science Center building | p100.ppt | p100.pdf |
| No. | Chart Subject | Powerpoint | |
|---|---|---|---|
| Title Slides | |||
| 1. | Speakers’ Bureau Title | p1.ppt | p1.pdf |
| 2. | Title Chart for Talk, including SIRTF Logos and Timeline | p2.ppt | p2.pdf |
| 3. | Themes of Infrared Astronomy | p3.ppt | p3.pdf |
| 4. | The Advantages of Space - illustrates low background and high transmission | p4.ppt | p4.pdf |
| 5. | The Infrared Array Revolution - strip chart and array images of the Galactic Center in the near infrared, illustrating progress between 1960’s and 1990’s | p5.ppt | p5.pdf |
| 6. | Artist’s conception of SIRTF in Solar Orbit | p6.ppt | p6.pdf |
| 7. | Artist’s conception of SIRTF in Solar Orbit with logos and title | p7.ppt | p7.pdf |
| 8. | SIRTF Summary - Summary table with artist’s conception | p8.ppt | p8.pdf |
| 9. | SIRTF Overview - word chart | p9.ppt | p9.pdf |
| 10. | SIRTF Status and Upcoming Highlights - word chart | p10.ppt | p10.pdf |
| 11. | SIRTF System Architecture and Team Members - Cartoon ground system with observatory cut away | p11.ppt | p11.pdf |
| 12. | Observatory Configuration - external view of entire SIRTF observatory with callouts | p12.ppt | p12.pdf |
| 13. | Observatory Cutaway - cutaway view of entire SIRTF observatory with callouts | p13.ppt | p13.pdf |
| 14. | Cryogenic Telescope Assembly completed at Ball Aerospace - color picture of assembled CTA | p14.ppt | p14.pdf |
| 15. | SIRTF Family Portrait - The three cold instrument assemblies installed on the MIC baseplate, with callouts | p15.ppt | p15.pdf |
| 16. | SIRTF Telescope Installation - Ball technician fastening telescope to cryostat | p16.ppt | p16.pdf |
| 17. | Completed Cryostat - SIRTF Cryostat with man for scale | p17.ppt | p17.pdf |
| 18. | Primary Mirror Prior to Integration Into Chamber - flight primary and associated mounting hardware on cold plate | p18.ppt | p18.pdf |
| 19. | SIRTF Flight Primary Exceeds Cold Figure Requirements - surface figure as measured cold compared to requirement | p19.ppt | p19.pdf |
| 20. | Warm Launch Architecture - Cutaway view of entire CTA with text quantifying improved performance vis-à-vis ISO | p20.ppt | p20.pdf |
| 21. | Heat Flow Map and Steady State Temperatures for Nominal Parameters - Chart showing temperatures and heat flows illustrating radiative cooling and operation of warm-launch architecture | p21.ppt | p21.pdf |
| 22. | Spacecraft Assembly at Lockheed Martin - Photo of spacecraft in middle of harness and avionics installation | p22.ppt | p22.pdf |
| 23. | Building up the Spacecraft Attitude Reference Bench - Lockheed technician working on Inertial Reference Unit/Startracker assembly, with partially completed spacecraft in the background | p23.ppt | p23.pdf |
| 24. | SIRTF - Operational Features - summary of operational features, emphasizing simplicity | p24.ppt | p24.pdf |
| 25. | Solar Orbit - view looking down on solar orbit in earth-sun rotating frame, illustrating drift of SIRTF away from Earth | p25.ppt | p25.pdf |
| 26. | SIRTF Instantaneous Sky Visibility - figure illustrates sky accessible from SIRTF at one instant, emphasizing constant viewing zones at pole, operational pointing zone, avoidance zones, etc. | p26.ppt | p26.pdf |
| 27. | Inertial Target Viewing Statistics - sky visibility over a year in ecliptic, equatorial, and galactic coordinates | p27.ppt | p27.pdf |
| 28. | Defining Scientific Programs for SIRTF - word chart listing “big four” themes, Bahcall report, discovery potential, etc. | p28.ppt | p28.pdf |
| 29. | SIRTF Science Update - word chart summarizing recent developments in SIRTF science areas, highlighting scientific priority of SIRTF | p29.ppt | p29.pdf |
| 30. | Great Observatories Imaging Sensitivity - panchromatic gamma ray to radio spectral energy distribution of blazar with sensitivities of space and ground-based astronomical facilities indicated | p30.ppt | p30.pdf |
| 31. | SIRTF - A Cornerstone of the Origins Program - Summarizes SIRTF in the context of Origins, with figure showing SIRTF pixel at Alpha Centauri | p31.ppt | p31.pdf |
| 32. | SIRTF Science Utilization - word chart summarizing allocation of Community Time, GTO time, Discretionary Time, etc. | p32.ppt | p32.pdf |
| 33. | SIRTF Science Timeline - word chart listing milestones from November, 2000 to December, 2003. Note that all future milestones shown are tied to the launch date. | p33.ppt | p33.pdf |
| 34. | How You Will Use SIRTF for General Observer Science - word chart summarizing proposal input, evaluation, implementation, program funding, for General Observers | p34.ppt | p34.pdf |
| 35. | SIRTF Legacy Science - word chart summarizing requirements and scope of Legacy Science programs | p35.ppt | p35.pdf |
| 36. | SIRTF Legacy Science - quote from TAC Chair John Bahcall indicating that selected Legacy program fulfills Bahcall Committee/CAA expectations for SIRTF | p36.ppt | p36.pdf |
| 37. | The Legacy Science Program - Tabular listing of six selected Legacy Teams, including acronyms or short names used on following charts. | p37.ppt | p37.pdf |
| 38. | SIRTF Instrumentation Overview - word chart summarizing functionality of three instruments | p38.ppt | p38.pdf |
| 39. | SIRTF Measurement Functionality - Imaging - Pictorial representation of SIRTF fields of view and array sizes vs. wavelength | p39.ppt | p39.pdf |
| 40. | SIRTF Measurement Functionality - Spectroscopy - Pictorial representation of SIRTF spectral resolving power as a function of wavelength | p40.ppt | p40.pdf |
| 41. | SIRTF Focal Plane Apertures - Diagram showing SIRTF fields of view projected onto sky | p41.ppt | p41.pdf |
| 42. | SIRTF Instrumentation Summary - Table summarizing fields of view, wavelength bands, array sizes, sensitivities, etc. | p42.ppt | p42.pdf |
| 43. | SIRTF Performance Comparison - Detailed chart comparing SIRTF with IRAS and other facilities, together with brightnesses of typical SIRTF targets - all as a function of wavelength. Both imaging and spectroscopic performance illustrated for SIRTF, and confusion estimates are included. | p43.ppt | p43.pdf |
| 44. | SIRTF Performance Expectations - same as above with other facilities not shown | p44.ppt | p44.pdf |
| 45. | The Sensitivity of Infrared Telescopes - simplified version of #43 with only three lines - IRAS, SIRTF, and “Current State of the Art”, which includes large ground-based telescopes and SOFIA | p45.ppt | p45.pdf |
| 46. | Infrared Array Camera (IRAC) - word chart summarizing IRAC features and team | p46.ppt | p46.pdf |
| 47. | IRAC Conceptual Design - cartoon showing IRAC arrays, lenses, calibrators, etc. | p47.ppt | p47.pdf |
| 48. | IRAC Flight Unit - picture of IRAC flight instrument, including a few people who establish the scale | p48.ppt | p48.pdf |
| 49. | IRAC 3.6um Simulation - high latitude fields imaged by IRAC at 3.6um | p49.ppt | p49.pdf |
| 50. | IRAC Images at 3.6um - test images at center and two corners of array, with derived profiles inset | p50.ppt | p50.pdf |
| 51. | Simulated IRAC image of the HDF, provided by the GOODS team - This simulation of a 100-hour integration presumes image quality slightly better than that specified in the SIRTF Users’ Handbook but which might be realized based on better than specified optics, careful sampling, and using the HST image as a template [cf. Figure 84]. | p51.ppt | p51.pdf |
| 52. | Source Counts from IRAC Image - 8um sources extracted from simulated image showing agreement of input model and output data | p52.ppt | p52.pdf |
| 53. | Infrared Spectrograph (IRS) - word chart summarizing IRS features and team | p53.ppt | p53.pdf |
| 54. | IRS on MIC Baseplate - picture of all four IRS modules and circuit board installed on MIC baseplate for flight. | p54.ppt | p54.pdf |
| 55. | First Light in the Short-Low Module - Data illustrate short-low spectrum, wrap-around, and peak-up images | p55.ppt | p55.pdf |
| 56. | IRS H2O Long-High Spectrum - absorption lines of atmospheric water illustrate echelle format of long-high module | p56.ppt | p56.pdf |
| 57. | IRS Short High Simulated Spectrum -Extended source simulation, 64s of integration in echelle format, includes cosmic rays. NeII line clearly seen. Equivalent flux per point source along the slit is ~25mJy. | p57.ppt | p57.pdf |
| 58. | Simulated IRS Spectra of Distant Galaxies - lo resolution spectrum of galaxy at z=3; high resolution of galaxy at z=1 - broad and narrow spectral features clearly seen, including PAH features and NeII line at 12.8um, redshifted. | p58.ppt | p58.pdf |
| 59. | Multiband Imaging Photometer for SIRTF (MIPS) - word chart summarizing MIPS features and team | p59.ppt | p59.pdf |
| 60. | Integrated MIPS Provides Imaging/Surveying/Spectral Capabilities - side-by-side picture of assembled MIPS and line drawing showing optical paths | p60.ppt | p60.pdf |
| 61. | MIPS Critical Elements - pictures of arrays and scan mirror with accompanying text | p61.ppt | p61.pdf |
| 62. | Simulated MIPS 70 micron Scan Map Data - simulation of 35x35 arcmin field, including distant galaxies and foreground cirrus | p62.ppt | p62.pdf |
| 63. | Source Counts from MIPS Image at 70um - figure illustrating successful extraction of input source counts from simulated image | p63.ppt | p63.pdf |
| 64. | MIPS Simulated Photometry at 70um - simulated observation of bright-ish star, illustrating chops, nods, and stim flashes. Much fainter objects are seen in the vicinity | p64.ppt | p64.pdf |
| 65. | Simulated MIPS 24 and 70 Micron Observations of Circumstellar Disks - simulated images of disks with as little as 1% the amount of dust as Vega, around a star of Vega’s brightness. | p65.ppt | p65.pdf |
| 66. | MIPS flight array tests, showing stability of both 24 and 70um arrays from December 2000 to April 2001 | p66.ppt | p66.pdf |
| 67. | Planned SIRTF Surveys - Table listing Legacy, GTO, and FLS parameters, including sky coverage and limiting fluxes. Note that the faintest fluxes expected differ from one survey to another, due to uncertain models of source confusion. | p67.ppt | p67.pdf |
| 68. | What is the Role of Dust in Galaxy Formation? - Figure illustrating a number of blank field SCUBA sources, which show no optical counterpart down to ~26th magnitude at I. Text explains how SIRTF will find further examples and follow up spectroscopically. | p68.ppt | p68.pdf |
| 69. | IRS Modules Provide Diagnostic Capability out to High Redshift -- Spectrum of Circinus Galaxy from ISO with wavelength coverage of IRS modules superposed. Lines from solid materials and from a range of ionization states are seen, and, as illustrated also in #58, the IRS can trace the diagnostic features out to redshifts ~3 or beyond. | p69.ppt | p69.pdf |
| 70. | Arp 220 at High Redshift. - Figure illustrates that the SIRTF Deep Survey (cf. #67) could detect Arp 200 at z=1, and a ~15x more luminous analog at z=3. | p70.ppt | p70.pdf |
| 71. | The Groth Strip: Surveys by SIRTF and Others.- Roughly 200 hours of coordinated deep surveys with IRAC and MIPS are planned by SIRTF GTO's for a 2 degree long by 10 arcminute long region which includes the Groth strip. The background is a digitized Palomar Sky Survey image covering 2 degrees on a side, centered at approximately 14h19m +52d44' (J2000). The Groth strip (outlined in blue in the figure) is a series of 28 overlapping HST WFPC2 images in V and I, each 1 orbit. IRAC will map the inner red rectangle to a depth of 3 hours per position in all four bands, sufficient to detect L* galaxies at redshift 3 in rest frame K light (observed 8 microns). MIPS will observe the same region using scan maps with 20 minutes of exposure per position. The dashed red rectangle will also be surveyed by IRAC (for 500 seconds per position) and MIPS (for 20 minutes per position). The overlapping MIPS regions will receive a total of 40 minutes integration. A representative 5 x 5 arcminute MIPS/IRAC FOV is shown by the red square towards top left. A few additional individual MIPS photometry mode pointings at 24 microns of 1.5 hours duration are also planned. The white circle shows the 27 arcminute diameter of a planned deep XMM observation. Deep (200 ksec) Chandra observations within the region have also been approved. Intensive groundbased observations of this region are underway. The four purple rectangles show where the CFHT has obtained deep imaging in B,R, and I to select targets for the UC/Caltech Deep Evolutionary Extragalactic Probe, which will obtain tens of thousands of spectra within the yellow rectangle using the DEIMOS spectrograph on the Keck telescope. The region has also been a target for the Lyman Break Galaxy survey of Steidel et al and submm surveys with SCUBA (green square). Overall, this illustrates the important trend towards intensive multispectral studies of selected regions of the sky. | p71.ppt | p71.pdf |
| 72. | Extragalactic Science in the Legacy Program. Relationship of SINGS, SWIRE, and GOOD surveys illustrated in context of “Journey through Cosmic Time” figure. | p72.ppt | p72.pdf |
| 73. | Anchor Points in the Local Universe - Using Antennae and HDF as examples, shows how SINGS survey provides basis for interpreting observations of more distant galaxies. | p73.ppt | p73.pdf |
| 74. | History of Star Formation - Shows Madau type plots with range of estimate of effects of correcting for dust/extinction. The shading illustrates the redshift range to be probed by various SIRTF surveys. | p74.ppt | p74.pdf |
| 75. | SIRTF Fills the Gap - Shows how planned SIRTF surveys and spectroscopic follow-on capability fill 3-180um gap between near infrared and submillimeter data on SCUBA sources. | p75.ppt | p75.pdf |
| 76. | Nested Survey Strategy/Lifting the Mass-Age Degeneracy - Shows “nesting” of SIRTF surveys in transition from wide, shallow SWIRE survey to deep pencil beam of GOODS survey. Insets show plot from #74 and illustrate use of IRAC data to constrain age and mass of stellar population in distant galaxies by observing redshifted starlight. | p76.ppt | p76.pdf |
| 77. | Deep Survey: Redshift Distribution at 70um - Predicted distribution with redshift of galaxies to be detected in MIPS portion of DEEP survey (cf.#67) based on models of Devriendt et al (1999). | p77.ppt | p77.pdf |
| 78. | Predicted Galaxy Number Counts in the Far Infrared - Counts predicted by Tan et al (1999) at various wavelengths shown cut by lines giving areal density at which MIPS becomes confused at 10 beams/source. | p78.ppt | p78.pdf |
| 79. | MIPS Observations may Resolve the Infrared Background and 160um - simulated DIRBE, ISO, and MIPS/SIRTF observations of 160um sky, showing background partly resolved into point sources by ISO and much more completely resolved by SIRTF | p79.ppt | p79.pdf |
| 80. | Influence of Resolution on Deep Far Infrared Confusion-Limited Surveys - Simulations of 34’x34’ area at 70um, with IRAS, ISO, and MIPS resolution, based on models from Dole et al. No instrumental noise is included. | p80.ppt | p80.pdf |
| 81. | Influence of Resolution on Deep Far Infrared Confusion-Limited Surveys - Same as above, but at 160um, zoomed in to 6.7’x6.7’ subset of 34’x34’ area, again based on models from Dole et al | p81.ppt | p81.pdf |
| 82. | SIRTF and the Cosmic Infrared Background - Estimated flux in galaxies to be detected by MIPS at 24, 70, and 160um is shown in comparison to models (Tan et al) and data on the infrared background from 10-1000um. | p82.ppt | p82.pdf |
| 83. | Great Observatories Synergy. The deepest observations planned for SIRTF will be obtained by the Great Observatories Origins Deep Survey (GOODS) Legacy team. The targets of these observations are the Hubble Deep Field North (HDF-N) and Chandra Deep Field South (CDF-S). Both regions have received one million second exposures with the ACIS camera on Chandra (green outlines), which has a 16 arcminute FOV. Because the CDF-S data were obtained at a variety of position angles, the Chandra coverage here is shown as a circle. The region covered by the existing WFPC2 HDF-N data is outlined in white. The GOODS team will obtain IRAC coverage over 10 x 16 arcminute regions (shown in red) to a depth of 25 hours per positions. These observations will be taken at two epochs, 6 months apart, to maximize the uniformity and efficiency of coverage in the two IRAC fields of view. An overlapping region in the center (darker red) will receive 50 hours of integration. An additional set of two epoch/50 hour integrations in two individual IRAC 5 x 5 arcminute fields (deepest red) is planned for the HDF-N, pending demonstration that the data will produce useful additional gains. Deep 10 hour integrations of the same regions at 24 microns with MIPS photometry mode are also planned (blue), pending demonstration that these data will achieve at least twice the sensitivity of the 20 minute exposure MIPS GTO scan maps in these regions. | p83.ppt | p83.pdf |
| 84. | Comparing HST and SIRTF images of the HDF - Inset illustrates how knowledge of optical image at better than SIRTF resolution might be used to improve resolution of IRAC images of the HDF. | p84.ppt | p84.pdf |
| 85. | SIRTF and the X-ray Universe - z=0 and z=3 SEDs of Type 2 AGN over x-ray/visible/infrared bands are compared with limits to be achieved by GOODS team in coordinated program of deep x-ray/ultraviolet/optical/SIRTF imaging. This figure illustrates the real possibility that some objects might be detectable by Chandra and SIRTF but not in the visible band. | p85.ppt | p85.pdf |
| 86. | SIRTF’s Legacy to NGST. Figure illustrating that SIRTF sensitivity at 3.6um is intermediate between that of Keck and that projected for NGST; with possible source count models superposed. The vertical lines show sensitivity achievable from SIRTF for range of integration times and [at 3.6um] two choices of on-orbit image quality - the actual performance should lie between these limits. The green triangles and circles are the observed [optically] density of galaxies in the range 2.6<z<3.4 and 3.8<z<4.5, respectively, converted to IRAC fluxes using an SED model for a Luminous Blue Galaxy. | p86.ppt | p86.pdf |
| 87. | Overview: Galactic Science in the Legacy Program. The science thrusts of the GLIMPSE, FEPS, and Cores to Disks Legacy Programs are indicated on an Origins Program figure spanning the epochs from the Big Bang to the formation of DNA. | p87.ppt | p87.pdf |
| 88. | Sky Coverage and Potential Discoveries of the GLIMPSE Survey. Upper panel illustrates sky coverage of GLIMPSE, +/- 1 degree in galactic latitude over longitudes of 10-to-70 [extending beyond the borders of this figure]. Insets from 2-MASS album illustrate potential discoveries from GLIMPSE. | p88.ppt | p88.pdf |
| 89. | Protostellar Disks to Mature Planetary Systems (I) - Figures illustrating temporal, structural, and SED evolution from proplyds to solar zodiacal light. | p89.ppt | p89.pdf |
| 90. | Protostellar Disks to Mature Planetary Systems (II) - Same as above, with emphasis now on spectral evolution. | p90.ppt | p90.pdf |
| 91. | Molecular Clouds: Cradles of Starbirth - Figure from Cores to Disks team illustrating regions to be surveyed in Perseus Cloud and SEDs of embedded sources to be identified and studied with follow up spectroscopy, in comparison to sensitivity limits of survey. | p91.ppt | p91.pdf |
| 92. | Disk Survey of Young Cluster NGC2516: MIPS Scan Paths - Optical image of NGC2516, a young cluster about 30 arcmin in extent, showing tracks of MIPS scans superposed. The MIPS + IRAS survey of this object would take only a few hours. This cluster is about 100 million years old and at a distance of about 350pc. | p92.ppt | p92.pdf |
| 93. | Projected SIRTF Results for Young Cluster NGC2516 - Based on the observed luminosity function, the left axis and the histogram show how many objects would be detected in the cluster as a function of mass to well below the substellar limit, while the other axis shows the sensitivity of the survey - as a function of the stellar mass - to 25um excess indicative of a circumstellar disk. | p93.ppt | p93.pdf |
| 94. | What are the Conditions Under Which Planets Form? - HST image, cartoon, and predicted spectrum of a flared disk, illustrating surface layer which radiates strongly in the SIRTF band. | p94.ppt | p94.pdf |
| 95. | Debris Disks: Models and Images - Calculation by Ozernoy et al of structure of dust disk perturbed by embedded planet [square] compared with JCMT image of the dust around Vega and the MIPS 24 and 70um beam sizes. | p95.ppt | p95.pdf |
| 96. | Spectra of Dust Disk in HD100546 and of Comet Hale-Bopp - ISO data showing similar mineralogy in the two environments. SIRTF can obtain this type of data on many, many dust disks and in lots of comets, so that conditions in our solar system can be compared with those in material from which extrasolar planets may be forming or have formed. | p96.ppt | p96.pdf |
| 97. | Predicted spectrum of Brown Dwarf GL229B - The 5-15um spectrum is compared with the projected sensitivity of the IRS Short-Lo module. | p97.ppt | p97.pdf |
| 98. | KBOs: The Remants of Solar System Formation: Image from the Minor Planet Center showing the distribution in the plane of the Solar System of all KBO’s known as of November 2000. | p98.ppt | p98.pdf |
| 99. | KBO and Centaurs and SIRTF Detection Limits - Figure showing 24 and 70um flux of KBOs and Centaurs, indicating which objects would be detectable in which MIPS bands. | p99.ppt | p99.pdf |
| 100. | Keith Spalding Building, Caltech (home of the SIRTF Science Center) | p100.ppt | p100.pdf |
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