http://www.hdstvision.org/contact daily 0.75 2018-11-08 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435234244527-LOZ1E271RJ07PSFYDPGC/aura-logo-grey.png Contact http://www.hdstvision.org/news-events daily 0.75 2016-02-03 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1436362530818-QD4Z682CP5G038O21TXW/amnh-hdst-panel.jpg Events HOST: Neil deGrasse Tyson, PANEL (left to right): Michael Shara, Jason Tumlinson, Marc Postman, David Schiminovich, Julianne Dalcanton, and Sara Seager Image credit: AMNH http://www.hdstvision.org/release-text daily 0.75 2015-07-06 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435760367522-9E62SXHT22O6VQAA8W2M/Solar+System+twin+simulation Release Text A simulated image of a solar system twin as seen with the proposed High Definition Space Telescope (HDST). The star and its planetary system are shown as they would be seen from a distance of 45 light years. The image here shows the expected data that HDST would produce in a 40-hour exposure in three filters (blue, green, and red). Three planets in this simulated twin solar system – Venus, Earth, and Jupiter - are readily detected. The Earth’s blue color is clearly detected. The color of Venus is distorted slightly because the planet is not seen in the reddest image. The image is based on a state-of-the-art design for a high-performance coronagraph (that blocks out starlight) that is compatible for use with a segmented aperture space telescope. Image credit: L. Pueyo, M. N’Diaye (STScI) https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435760521509-JI4L7IG7O93FXJ8TWJDM/simulated+spiral+galaxy Release Text A simulated spiral galaxy as viewed by Hubble, and the proposed High Definition Space Telescope (HDST) at a lookback time of approximately 10 billion years (z = 2) The renderings show a one-hour observation for each space observatory. Hubble detects the bulge and disk, but only the high image quality of HDST resolves the galaxy’s star-forming regions and its dwarf satellite. The zoom shows the inner disk region, where only HDST can resolve the star-forming regions and separate them from the redder, more distributed old stellar population. Image credit: D. Ceverino, C. Moody, and G. Snyder, and Z. Levay (STScI) https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435777035232-X8C89U868KV6UP9ZOSDH/Mirror+comparison Release Text A direct, to-scale, comparison between the primary mirrors of the Hubble Space Telescope, James Webb Space Telescope, and the proposed High Definition Space Telescope (HDST). In this concept, the HDST primary is composed of 36 1.7 meter segments. Smaller segments could also be used. An 11 meter class aperture could be made from 54 1.3 meters segments. Image credit: C. Godfrey (STScI) http://www.hdstvision.org/gallery-ch4 daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435694006408-CDS0TUQ6018A8TUAW4G7/fig_4-3.jpg Gallery: Chapter 4 - Figure 4-1 Telescopes imaging at their diffraction limit offer high-definition views of the Universe across cosmic distances. Major resolution thresholds reached by HDST are marked in magenta and illustrated at left. For a 12 m aperture, the resolution element at HDST’s 0.5-micron diffraction limit corresponds to 100 parsecs or less at all cosmological distances in the observable Universe. The D = 2.4 m Hubble (black line) is diffraction limited at λ = 0.6 micron, and the 6.5 m JWST (red line) is diffraction limited at λ = 2 microns, such that their physical resolution elements (proportional to λ/D) are about the same. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693993206-42HM1LFA5I4J306S0NI7/fig_4-1.jpg Gallery: Chapter 4 - Figure 4-2 Angular resolution as a function of wavelength for current, planned, and possible future astronomical facilities. The HDST resolution is shown assuming a 12 m aperture, diffraction limited at 500 nm. The expected performances from facilities that are still in pre-construction or conceptual phases are shown as dashed lines. Some ground-based facilities have non-continuous wavelength coverage due to atmospheric absorption features. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435694002802-T2OOXP91MIH7HBCXN0K3/fig_4-2.jpg Gallery: Chapter 4 - Figure 4-3 The total integration time needed to reach a 10-sigma point-source limiting magnitude for the 38 m E-ELT and a 12 m HDST (assumed here to operate at 270 K). Computations are done for 3 different passbands: V, J, and K. Total system throughput and instrument characteristics (read noise, dark current) are adopted from the ESO E-ELT ETC website. The E-ELT is assumed to perform at its diffraction limit at wavelengths longer than 1 micron and seeing-limited (0.6 arcsec) for wavelengths below 1 micron. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435694220452-55QXLUKEXMX7FZ9XRIQS/fig_4-4.jpg Gallery: Chapter 4 - Figure 4-4 The path from Cosmic Birth to Living Earth, witnessed at a range of physical scales. Stars in the first galaxies produce the first heavy elements, which leave those galaxies and recycle into the larger galaxies they become. Mature galactic disks form later, composed of many star-forming regions at 50–100 parsec in size. Inside these regions form multiple star clusters, each of which includes massive stars that forge more heavy elements and low-mass stars that host protoplanetary disks. At 4.5 billion years ago, one such disk in our Milky Way formed the Earth and its siblings in the Solar System. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435699209962-652G7XZ85B7HFEEILXWV/fig_4-5-report.jpg Gallery: Chapter 4 - Figure 4-5 A simulated galaxy viewed by Hubble, JWST, and HDST at z = 2. The renderings show a one-hour observation (VIH for Hubble and HDST, zJH for JWST). Hubble and JWST detect the bulge and disk, but only the exquisite image quality of HDST resolves the galaxy’s star-forming regions and its dwarf satellite. The zoom shows the inner disk region, where only HDST can resolve the star-forming regions and separate them from the redder, more distributed old stellar population. Image credit: D. Ceverino, C. Moody, and G. Snyder. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435694236787-IBKYE8QCE4K6BJK3MO9R/fig_4-6.jpg Gallery: Chapter 4 - Figure 4-6 A comparison of present and future observatories and sky surveys in terms of “information content,” defined as the number of spatial resolution elements in the observed field. This figure of merit increases toward the upper right, perpendicular to the diagonal lines. Current facilities are marked with filled symbols and future facilities with open symbols. All-sky ground-based surveys cluster around the horizontal line, which marks the entire sky observed at 1ʺ resolution. Space-based narrow/deep fields cluster at lower right. Large ground-based telescopes achieve high resolution, but over relatively small fields of view (~1 arcmin), and are limited in depth by sky backgrounds. WFIRST/AFTA will expand Hubble-like imaging and depth to much larger areas, moving toward the upper right. Though it observes smaller fields, its exquisite spatial resolution means that HDST will surpass WFIRST/AFTA in information content on galaxies. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695207679-JTVJQSGT29Z0SZFSGQ31/fig_4-7.jpg Gallery: Chapter 4 - Figure 4-7 A visualization of the Circumgalactic Medium (CGM) gas fueling a Milky-Way-like galaxy. The color renders the strength of UV emission by triply ionized Carbon (C IV) in the CGM gas surrounding a Milky-Way-analog galaxy at z ~ 0.25. HDST should be able to directly detect gas emission from infalling filaments (green regions) and absorption from C IV and many other species in absorption at all densities. Image credit: Joung, Fernandez, Bryan, Putman & Corlies (2012, 2015). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695211980-BSQ6LUWM52C2CIQNNDWE/fig_4-8.jpg Gallery: Chapter 4 - Figure 4-8 The availability of physical line diagnostics versus lookback time and redshift. Rest wavelengths are marked where lines touch the axis at left (z = 0). The line density of available diagnostics increases sharply toward the rest-frame UV. All the important diagnostics of H I (magenta) and hot and/or high ionization gas (blue) lie in the UV at 8–12 Gyr lookback time, and do not cross the 3100 Å atmospheric cutoff until z ≳ 1.5–2. While a few low-ionization lines (orange) are available from the ground at low redshift, over most of cosmic time the measurement of physical conditions and elemental abundances in multiphase gas and stellar populations requires access to observed-frame UV wavelengths. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695216955-KGBWGVT7P73VACEC7OZ8/fig_4-9.jpg Gallery: Chapter 4 - Figure 4-9 The energy/timescale parameter space for the transient sky. In single-night visits, LSST will reach events at the luminosity limits shown by the pink bands, e.g., events at Mv ~ –19 will be detected out to z = 0.5–1, and HDST will localize these events to within 50–100 parsec precision within their host galaxies. Localization becomes 10 parsec or better, the size of a single molecular cloud region, for events detected out to 100 Mpc. Credit: M. Kasliwal (Caltech). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695371653-ICDYYNSEDE6RTQVI7780/fig_4-10.jpg Gallery: Chapter 4 - Figure 4-10 Dissecting galaxy outflow and inflow requires UV multi-object spectroscopy. A UV MOS mode with 50–100 objects observable at once in a 3–5' FOV will enable efficient studies of young stellar clusters, ISM gas, and energetic feedback for thousands of clusters in dozens of galaxies in the nearby Universe. Together with star-formation histories and halo gas, these observations will dissect the past evolution and current activity of nearby galaxies. This capability will also enable intensive studies of the circumgalactic medium, young stars in Galactic clusters, and many other frontier science problems. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695374161-K3E3LSWQQ783VPHDKGWZ/fig_4-11.jpg Gallery: Chapter 4 - Figure 4-11 Most stars form in clusters like these. Hubble can resolve individual stars in the nearest massive star-formation region to Earth (Orion, at bottom). As shown in the zoom-in panel at right, dense clusters in the low-metallicity Magellanic Clouds, which better resemble conditions in the early history of the Milky Way, cannot be resolved into individual stars for star-count IMFs or UV-derived mass-accretion rates. HDST will fully resolve such clusters and directly measure the shape and causes of the IMF in these chemically primitive environments. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695377621-EKHSZD4SB61PDLV9MBY8/fig_4-12.jpg Gallery: Chapter 4 - Figure 4-12 A visualization of HDST’s imaging performance for weather and atmospherics dynamics in the outer planets. This example using Neptune shows that HDST will resolve cloud patterns with 300-km resolution. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695449955-E2JN0Z571DYQR9TG5GLX/fig_4-13.jpg Gallery: Chapter 4 - Figure 4-13 Two views of the Galilean satellite Europa, including visible band images at left and UV-band emission-line images of water vapor ejecta with Hubble/STIS and re-simulated at HDST resolution. At the orbit of Jupiter, HDST’s spatial resolution is 35 km. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695454018-5ZT911VZ4K6RXMRXZHXS/fig_4-14.jpg Gallery: Chapter 4 - Figure 4-14 The minimum size detection limit (in km) for Kuiper Belt Objects and Trans Neptunian Objects at various heliocentric distances extending into the inner Oort cloud. The limits provided assume a 4% albedo and negligible contribution from thermal emission. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695457743-J17XXNIT9R7WOMATLO65/fig_4-15.jpg Gallery: Chapter 4 - Figure 4-15 Two views of Pluto and Charon. At bottom, Hubble images that span the two bodies by only a few pixels. At top, a simulated HDST views that resolves surface features as small as 300 km. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695464753-0QLEUVRXTLYWEMSWSU43/fig_4-16.jpg Gallery: Chapter 4 - Figure 4-16 The 10-sigma limiting sensitivities as a function of wavelength are shown for various facilities in the near-IR and mid-IR for a 10 ksec broadband imaging integration. HDST sensitivities are shown for two different operating temperatures. Even without operating at cryogenic temperatures, HDST is competitive with JWST and the ELTs at wavelengths of less than 2 microns, and with Spitzer at longer wavelengths. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695469750-5WD48L8AFMCJNJEO3UMO/fig_4-17.jpg Gallery: Chapter 4 - Figure 4-17 The ratio of integration time needed to reach an SNR = 10 on a 38 m E-ELT to that needed on HDST as a function of wavelength for point sources. Four different spectral resolutions (R = 5, 100, 2000, and 20,000) are shown for sources with AB mag of 30, 28, 26.5, and 24, respectively. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435702350083-2DOAIFDU7CSV6I9FKQSD/table_4-1.jpg Gallery: Chapter 4 - Table 4-1 Conceptual Astrophysics Treasury Programs with HDST http://www.hdstvision.org/resources daily 0.75 2015-08-14 http://www.hdstvision.org/gallery-ch6 daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696315753-SU98H8QVB70MEKA4J8M3/fig_6-1.jpg Gallery: Chapter 6 - Figure 6-1 A coronagraph designed to yield high contrast with an HDST-type segmented, obscured aperture (M. N’Diaye et al., in preparation). This design combines shaped pupil and Lyot coronagraph techniques to obtain 1 × 10^-10 raw contrast or better, for an IWA of 3.6 λ/D. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435703368877-QAUS74T661Q64CBK7L3B/table_6-1a.jpg Gallery: Chapter 6 - Table 6-1a Starlight Suppression Goals and Status https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435703373837-ES51EE19NTOGHVGFKOMC/table_6-1b.jpg Gallery: Chapter 6 - Table 6-1b Starlight Suppression Goals and Status (continued) https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435704127312-4ZWY428SWN5QBPYJBR5R/table_6-2.jpg Gallery: Chapter 6 - Table 6-2 Critical technologies, prioritized https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435704130015-PK2TU3YAQANNYBB9VLQ5/table_6-3.jpg Gallery: Chapter 6 - Table 6-3 Key architecture-specific, device, and science technologies https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435761454393-FI0HCCGO3YVSGOY9QKCD/table_6-4.jpg Gallery: Chapter 6 - Table 6-4 Key Starshade Technologies https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435761693575-F79J1EDX1OGZCEIIQBUU/table_6-5.jpg Gallery: Chapter 6 - Table 6-5 Key Far-Term Technologies http://www.hdstvision.org/in-the-news daily 0.75 2016-07-22 http://www.hdstvision.org/gallery-ch5 daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435702445984-A1A24Q5PNXBZN2DPI5YA/table_5-1.jpg Gallery: Chapter 5 - Table 5-1 Examples of general astrophysics drivers across cosmic epoch (Chapter 4) for three key HDST capability requirements: aperture diameter, efficient ultraviolet imaging and spectroscopy, and near-IR imaging and spectroscopy. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435702457613-NPAHM0119JZHN20S250U/table_5-2.jpg Gallery: Chapter 5 - Table 5-2 This science traceability matrix links HDST science investigations to key capability and instrument requirements (Exo-Im, Exo-Sp – Exoplanet discovery instrument imager and spectrograph; UV – High-resolution ultraviolet spectrograph; PI – Panoramic imager; MOS – Multi-object spectrograph). Detector capability requirement includes Photon counting (PC) and High dynamic range (Dyn Rg). The rightmost column provides a “typical” minimum count rate (in counts per second) per telescope or instrument resolution element (angular and spectral; not per detector pixel). Those observations requiring photon counting or high dynamic range are in bold. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435695728790-XFGB624V9GDUVL8364Z1/fig_5-1.jpg Gallery: Chapter 5 - Figure 5-1 A direct, to-scale, comparison between the primary mirrors of Hubble, JWST, and HDST. In this concept, the HDST primary is composed of 36 1.7 m segments. Smaller segments could also be used. An 11 m class aperture could be made from 54 1.3 m segments. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435699789225-177EL5YCYK6O41LD47EG/fig_5-2.jpg Gallery: Chapter 5 - Figure 5-2 A folded 11 m primary mirror, constructed with 54 1.3 m segments, is shown inside a Delta 4-H shroud. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696202841-QEID7U43EB8YZVEQUR3J/fig_5-3.jpg Gallery: Chapter 5 - Figure 5-3 Comparison of physical sizes of existing and planned detectors with possible “usable” size of the full focal plane of HDST. Several channels of wide-field instruments (e.g., panoramic imager with 0.5–1 Gpix detectors and multi-object spectrograph; both with ~6' FOV) will share the focal plane of HDST. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435702696239-S4MGNRJQX76PS90I6RWR/table_5-3.jpg Gallery: Chapter 5 - TABLE 5-3 HDST Summary of Capability Requirements and Comparison with Hubble and JWST http://www.hdstvision.org/early-release daily 0.75 2015-07-29 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435763788590-V296ZXKUA7MBZUDZ4U8S/kepler-69c.jpg Early Release An artist’s rendition of the exoplanet Kepler-69c, which is 1.7 times larger than the Earth. Credit: NASA/Ames/JPL-Caltech https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435765090068-5Q4N0KJ5D08E29O3R37Q/hdst-folded.jpg Early Release HDST folded within an EELV or SLS-1 shroud https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435764388434-X8P330HM673A7OEMJIU9/hdst-survey-map.jpg Early Release A map of the nearly 600 stars that would be surveyed with HDST to find dozens of exoEarths, given approximately two years of observing time. The stars are plotted on a projection of a sphere with radius 35 parsecs. Star colors and sizes correspond to star type and relative luminosity. Only a large 12-m telescope can survey hundreds of stars to find dozens of exoEarths. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435764675265-5B14ZB8J7AZ4GWLD9R2Y/galaxy-simulation.jpg Early Release The 5× gain in angular resolution from Hubble (left) to HDST (right) is demonstrated in this simulated image of a galaxy 10 billion light-years away. Hubble detects the galaxy’s bulge and disk but only HDST resolves the galaxy’s star forming regions and its nearby dwarf satellite. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435758942970-2912RLRYRNNRHVR7ZI5A/AURA%27s+HDST+draft+report+cover Early Release http://www.hdstvision.org/gallery-index daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435697738679-WKM8TXF59IOUB7R1YHT1/fig_3-17.jpg Gallery Index A simulated image of a solar system twin as seen with the proposed High Definition Space Telescope (HDST). The star and its planetary system are shown as they would be seen from a distance of 45 light years. The image here shows the expected data that HDST would produce in a 40-hour exposure in three filters (blue, green, and red). Three planets in this simulated twin solar system - Venus, Earth, and Jupiter - are readily detected. The Earth’s blue color is clearly detected. The color of Venus is distorted slightly becuase the planet is not seen in the reddest image. The image is based on a state-of-the-art design for a high-performance coronagraph (that blocks out starlight) that is compatible for use with a segmented aperture space telescope. Image credit: L. Pueyo, M. N’Diaye (STScI) https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435697719063-V3MQEXDBLXCKOA057MVQ/fig_4-5.jpg Gallery Index A simulated spiral galaxy as viewed by Hubble, and the proposed High Definition Space Telescope (HDST) at a lookback time of approximately 10 billion years (z = 2) The renderings show a one-hour observation for each space observatory. Hubble detects the bulge and disk, but only the high image quality of HDST resolves the galaxy’s star-forming regions and its dwarf satellite. The zoom shows the inner disk region, where only HDST can resolve the star-forming regions and separate them from the redder, more distributed old stellar population. Image credit: D. Ceverino, C. Moody, G. Snyder, and Z. Levay (STScI) https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435701796033-I91LOSBQWZE0OTJKT67K/fig_5-1-website.jpg Gallery Index A direct, to-scale, comparison between the primary mirrors of the Hubble Space Telescope, James Webb Space Telescope, and the proposed High Definition Space Telescope (HDST). In this concept, the HDST primary is composed of 36 1.7 meter segments. Smaller segments could also be used. An 11 meter class aperture could be made from 54 1.3 meters segments. Image credit: C. Godfrey (STScI) http://www.hdstvision.org/gallery-ch3 daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435684301042-AR3EZD9RGBUUT1X9O99L/fig_3-1.jpg Gallery: Chapter 3 - Figure 3-1 Image of a dark, star-filled sky including a view of the stately disk of the Milky Way. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435685728263-F5PWHFUKRHPNAI1ZEDUV/fig_3-2a.jpg Gallery: Chapter 3 - Figure 3-2a Kepler-11b, the iconic compact multiple planet system, with six planets orbiting interior to where Venus’ orbit would be. Credit: NASA. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435684481025-06T4VUBVY7PP6XEFFPKL/fig_3-2b.jpg Gallery: Chapter 3 - Figure 3-2b The Moon-sized exoplanet Kepler-37b in comparison to other small planets. Credit: NASA. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435685769433-1LJDV6JTP97O5UMNXV5O/fig_3-2c.jpg Gallery: Chapter 3 - Figure 3-2c The circumbinary planet Kepler-16b from an overhead view. The eccentric orbits of the two stars Kepler 16A and 16B are also shown. Credit: NASA. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435685803774-5Z0MKS2OZQOWWDY1XNSJ/fig_3-2d.jpg Gallery: Chapter 3 - Figure 3-2d Comparison of the planets in our inner Solar System to those in Kepler 186, a five-planet star system with an M dwarf host star, a star that is half the size and mass of the Sun. Credit: NASA. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435688338596-GS17RAERAWIBDONSUVUF/fig_3-3.jpg Gallery: Chapter 3 - Figure 3-3 Exoplanet discovery space as of 2014. Data points are color-coded according to the planet discovery technique. Plotted as mass vs. orbital period (left) but excluding Kepler discoveries. Plotted as radius vs. orbital period (right, using a simplified mass-radius relationship to transform planet mass to radius where needed). A large number of exoplanets and planet candidates are known, but the Earth-size exoplanets in Earth-like orbits still reside in an open part of discovery space. Figure from Batalha (2014). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435688632561-9Y3JKL372DEP07TAMX8P/fig_3-4.jpg Gallery: Chapter 3 - Figure 3-4 Planets in the habitable zone. The Solar System planets are shown with images. Known super-Earths (here planets with a mass or minimum mass less than 10 Earth masses; taken from Rein 2012) are shown as color-coded data points. The light blue region depicts the “conventional” habitable zone for N₂-CO₂-H₂O atmospheres. The habitable zone could indeed be much wider, depending on the planet’s atmospheric properties. The red region shows the habitable zone as extended inward for dry planets, with minimal surface water, a low water-vapor atmospheric abundance, and low atmospheric relative humidity and hence a smaller greenhouse effect. The brown region shows the outer extension of the habitable zone for planets that are massive and cold enough to hold onto molecular hydrogen—a potent greenhouse gas. The habitable zone might even extend out to free-floating planets with no host star. Figure from Seager (2013). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435688737967-L5AIJU8V3Y4WTRHO7WKZ/fig_3-5.jpg Gallery: Chapter 3 - Figure 3-5 The variety of exoplanets as illustrated by their masses and orbital semi-major axes. Different exoplanet-finding techniques’ discovery spaces and discovered planets are indicated by colors. Many more exoplanets are known that do not have measured masses (see Figure 3-3). The anticipated parameter space accessible with HDST is shown in dark green. Figure adapted from Gaudi and Henderson (private communication) and Wright and Gaudi (2013). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435688762498-DYV9PWG0SMDYRID7IA5Q/fig_3-6.jpg Gallery: Chapter 3 - Figure 3-6 Direct imaging contrast capabilities of current and future instrumentation. Shown are the 5-σ contrast limits after post-processing one hour’s worth of data for various coronagraph instruments. As can be seen in the plot, there are roughly three groupings of curves: 1) state-of-the art instruments in the early 2010s, as represented by Keck near-IRC2, the Palomar Well-Corrected Subaperture, and VLT-NaCo; 2) newly operational state-of-the-art instruments, represented by P1640, GPI, and VLTI-SPHERE; and 3) future extremely large telescopes, represented by TMT PFI and E-ELT EPICS. The contrast curves for JWST NIRCam and Hubble/ACS are shown for reference. On the top right of the figure are plotted the K-band contrasts of some of the giant exoplanets imaged to date. In the lower part of the figure are plotted our Solar System planets as they would appear in reflected light around a Sun-like star at a distance of 10 pc. The left side of the plot shows the corresponding RMS wavefront error for a coronagraph using a 64 × 64 element deformable mirror. The region above the solid red line would be probed by HDST. The gray region in the lower left of the figure shows the predicted locus of terrestrial habitable zone planets for F-G-K (Solar-like) stars. Figure and caption adapted from Lawson et al. (2012), Mawet et al. (2012), and Stapelfeldt (private communication 2015). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435689096436-JT7AT5ZAPVFUEO8XMY5Q/fig_3-7.jpg Gallery: Chapter 3 - Figure 3-7 Schematic of a transiting exoplanet. Figure credit: D. Beckner. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435689230159-XK3FHSKJKKWQ2EZOAEL8/fig_3-8.jpg Gallery: Chapter 3 - Figure 3-8 Earth’s observed reflectance spectrum at visible and near-IR wavelengths. From Earthshine measurements (Turnbull et al. 2006), the spectrum is disk-integrated, i.e., spatially unresolved and shows what Earth would like to a distant observer. The reflectance is normalized to one; the relatively high continuum and the presence of water vapor, oxygen, and ozone at visible wavelengths are relevant. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435689326098-WZZHBW7FMDA2NGYWGT31/fig_3-9.jpg Gallery: Chapter 3 - Figure 3-9 Simulated spectra of small planets orbiting a Sun-like star. The Earth, Venus, Archean Earth, and super-Earth models are from the Virtual Planet Laboratory. The sub-Neptune model is from R. Hu (personal communication). The Earth, super-Earth, and Archean Earth are at 1 AU. Venus is at its 0.75 AU. The sub Neptune is at 2 AU. The spectra have been convolved to R = 70 spectral resolution and re-binned onto a wavelength grid with 11 nanometer bins. Figure courtesy of A. Roberge. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435770793591-EH6KEKAPAM3GLS5DXC7G/fig_3-10.jpg Gallery: Chapter 3 - Figure 3-10 The exoEarth sample size, NEC, required to ensure detection of at least one exoEarth with evidence for habitability (or even biosignature gases) as a function of the fraction of exoEarths with such detectable features.These results are computed using the binomial theorem (see equation in figure) where C is the probability of detecting at least one life-bearing exoEarth in the sample, η⊕ is the eta Earth value (taken to be 0.1 for this computation), and ηx is the fraction of exoEarths with detectable biosignature gases. Shown are the lines for three commonly used probabilities: 68%, 95%, and 99.7%. Image credit: C. Stark https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693199171-EQ0RSM7RE3C86G4Z54JZ/fig_3-11.jpg Gallery: Chapter 3 - Figure 3-11 Planet occurrence as a function of planet size and planet orbital period. Kepler-detected small planets are shown by red circles. While the detected planets show the transit discovery technique’s bias towards larger, shorter-period planets, the occurrence rates provided in each bin are corrected for biases. Figure adapted from Petigura et al. (2013). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435843464063-JR1JN6E1WEI2ZKS784FJ/table_3-1.jpg Gallery: Chapter 3 - Table 3-1 Values of ηEarth for Sun-like stars under different HZ and Earth-size radius assumptions. Note that functional form extrapolations for planet occurrence rates as a function of orbital period may also differ. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693250898-5JQJ61IY525JOPVLT1UE/fig_3-12.jpg Gallery: Chapter 3 - Figure 3-12 Illustration of the origins of obscurational and photometric incompleteness in direct imaging surveys. Image credit: C. Stark. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693292162-YGS0G4TG05T20BIWXBZM/fig_3-13.jpg Gallery: Chapter 3 - Figure 3-13 Schematic description of the input ingredients to the exoEarth yield calculations. Image credit: C. Stark. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435698676140-31YVZLXHP2K4R9P6VQZ5/fig_3-14.jpg Gallery: Chapter 3 - Figure 3-14 Star positions and properties for an exoplanet survey considering visible wavelengths and an internal coronagraph. Telescope and coronagraph values are consistent with those described in the text for the exoEarth yield simulations. Plotted are: stars surveyed to optimize exoEarth yield for a 4 m aperture (74 stars, top); 8 m aperture (291 stars, middle); and 12 m aperture (582 stars, bottom) telescope given 1 total year of integration time (with 100% overheads) and including spectral characterization. Stars are plotted on a projection of a sphere with radius 35 parsecs. Star colors correspond to their B-V color and star size corresponds to the stellar luminosity with respect to Solar. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693386221-1IXHFZ11RWXAP454X0PH/fig_3-15.jpg Gallery: Chapter 3 - Figure 3-15 The number of candidate exoEarths that can be detected in the habitable zones of Sun-like stars as a function of telescope aperture diameter, assuming one year of on-sky observations, and including time to acquire R=70 spectra centered at 550 nm. Results are shown for two IWA values and for two values of ηEarth. Black curves are for an assumed exozodi background of 3 zodi. Gray curves show the impact of increasing exozodi levels to 5, 10, 50, and 100 zodi. If the same one year of observing time is spent only on discovery and not spectra, the yields may increase by as much as 40%. Image credit: C. Stark. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693390414-EDEX5LV6Z7W88JXV8HU2/fig_3-16.jpg Gallery: Chapter 3 - Figure 3-16 The number of planets discovered at 500 nm (black curve) that could also be detected at longer wavelengths (colored curves), as desired for spectroscopic observations, as a function of telescope aperture size and for two different assumed inner working angles. In other words, these plots show the number of planets that are visible at some point during their orbit, for a range of different wavelengths. Figure courtesy of C. Stark. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693495980-RTBMORKW4J72BANTEWO5/fig_3-17.jpg Gallery: Chapter 3 - Figure 3-17 Simulation of a Solar System twin at a distance of 13.5 pc as seen with HDST (12 m space telescope) and a binary apodized-pupil coronagraph, optimized using the methods described in N’Diaye et al. (2015). The image here simulates a 40-hour exposure in 3 filters with 10% bandwidths centered at 400, 500, and 600 nm. The inner and outer working angles used in this simulation are 4 λ/D and 30 λ/D, respectively. The coronagraph design can support smaller inner working angles and larger outer working angles. Perfect PSF subtraction has been assumed (i.e., no wavefront drifts between target star and calibrator star). The Earth and its blue color are easily detected. The color of Venus is biased because that planet lies inside the inner working angle in the reddest exposure. The image employs a linear stretch to the outer working angle and a logarithmic stretch beyond that (where the purple-colored ring begins). Image credit: L. Pueyo, M. N’Diaye. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693533347-M8RDCSOQMYKQMH605ZJ0/fig_3-18.jpg Gallery: Chapter 3 - Figure 3-18 Simulated near-IR (1.6 μm, 20% band) image of a solar system twin at a distance of 13.5 pc as seen by HDST (12 m space telescope) with a 2 day exposure. The pupil geometry adopted for this simulation is shown in the lower right. A Phase- Induced Amplitude Apodization Complex Mask Coronagraph (PIAACMC), offering small IWA (1.25 λ/D), is used here to overcome the larger angular resolution at longer wavelength. Earth, at 2.65 λ/D separation, is largely unattenuated, while Venus, at 1.22 λ/D, is partially attenuated by the coronagraph mask. At this wavelength, the wavefront control system (assumed here to use 64 x 64 actuator deformable mirrors) offers a larger high contrast field of view, allowing Saturn to be imaged in reflected light. This simulation assumes PSF subtraction to photon noise sensitivity. In the stellar image prior to PSF subtraction, the largest light contribution near the coronagraph IWA is due to finite stellar angular size (0.77 mas diameter stellar disk). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435693588747-OHMV82ILZAFXDO7UVIAG/fig_3-19.jpg Gallery: Chapter 3 - Figure 3-19 Simulated false-color (450–850 nm) image of a planetary system around a nearby G star (Beta Cvn) seen by a 12 m optical space telescope equipped with a free-flying ~100 m diameter starshade. Imperfections in the starshade scatter some starlight and sunlight into the center of the image, yielding a contrast of 4 × 10-11 at 1 AU, but twins of Venus, Earth, Jupiter and Saturn stand out clearly from the PSF wings on either side of the starshade. A Mars twin may also be detectable in one-day exposures like this one with some careful calibration. The large aperture easily separates planets from background galaxies and local and external zodiacal dust (all included), but still senses the narrow dust ring at 3.5 AU in this model, 10× fainter than any other current or upcoming missions can reach. Credit: M. Kuchner. http://www.hdstvision.org/report daily 0.75 2015-07-29 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435764675265-5B14ZB8J7AZ4GWLD9R2Y/galaxy-simulation.jpg AURA Report The 5× gain in angular resolution from Hubble (left) to HDST (right) is demonstrated in this simulated image of a galaxy 10 billion light-years away. Hubble detects the galaxy’s bulge and disk but only HDST resolves the galaxy’s star forming regions and its nearby dwarf satellite. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435765090068-5Q4N0KJ5D08E29O3R37Q/hdst-folded.jpg AURA Report HDST folded within an EELV or SLS-1 shroud https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1436202954153-C1FL3767Y23PYQ6EI59D/AURA%27s+HDST+draft+report+cover AURA Report https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435763788590-V296ZXKUA7MBZUDZ4U8S/kepler-69c.jpg AURA Report An artist’s rendition of the exoplanet Kepler-69c, which is 1.7 times larger than the Earth. Credit: NASA/Ames/JPL-Caltech https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435764388434-X8P330HM673A7OEMJIU9/hdst-survey-map.jpg AURA Report A map of the nearly 600 stars that would be surveyed with HDST to find dozens of exoEarths, given approximately two years of observing time. The stars are plotted on a projection of a sphere with radius 35 parsecs. Star colors and sizes correspond to star type and relative luminosity. Only a large 12-m telescope can survey hundreds of stars to find dozens of exoEarths. http://www.hdstvision.org/home daily 1.0 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435680919951-IBPOKVHIXTJFLI72PJZY/AURA+logo Home https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435680874086-EP8L4CSS66U7NEHGM9W9/Exoplanet+illustration Home https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435174174334-IX7UDEHZRNXK5EI00J1M/hdst-banner-2780x930.jpg Home http://www.hdstvision.org/gallery-ch7 daily 0.75 2015-06-30 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435702924610-DTLKXTBXIUFQKEXZMMBM/table_7-1.jpg Gallery: Chapter 7 - Table 7-1 Key Technology Heritages https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696465927-XHT7QUTO7XYPHJWFEAQB/fig_7-1.jpg Gallery: Chapter 7 - Figure 7-1 The possible range of exoEarth yields (left), given the uncertainties in astrophysical parameters (the earth occurrence rate, the level of exozodiacal light, and the planet albedo; right panels, top to bottom), for the nominal HDST 12 m, and the possible 9.2 m and 6.5 m descope options (assuming an IWA of 3 λ/D, and 1 year of on-sky integration including both detection and spectroscopic characterization). Histograms indicate the probability that a mission would find more than a given number of exoEarths. For a fixed telescope aperture and starlight suppression performance, there is a large range in possible yields that reflect how favorable the true astrophysical parameters are. Larger telescopes offer better protection against the possibility that astrophysical parameters are skewed to values that make exoEarth detection more difficult. Vertical dashed lines in the right panels indicate the median value of each astrophysical parameter. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696469442-3YV1RAL2A98G2IRTTXDZ/fig_7-2.jpg Gallery: Chapter 7 - Figure 7-2 The increase in the exposure time for a 10-sigma detection of a point source when descoping from a 12 m to a 9.2 m (purple line) or a 6.5 m (red line), as a function of magnitude. In the background limited regime (>29 mag), exposure times increase by a factor of 3 for a 9.2 m and by a factor of 12 for a 6.5 m. Light, medium, and dark lines are for the U, V, and J bands, respectively. A 4 m aperture (black line) is included for comparison. https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696472910-Z1PYFPM7UJXZMU6UIJJG/fig_7-3.jpg Gallery: Chapter 7 - Figure 7-3 The fraction of currently cataloged UV-bright QSOs in bins FUV magnitude (AB < 18.5 for Hubble, < 20.5 for a 6.5 m, 21 for a 9.2 m, and < 22 for a 12 m HDST; left panel) as a function of redshift. Larger telescopes access significantly more sources and provide the majority of the most valuable high-redshift sources that support the evolutionary studies of galaxies, the CGM and IGM, and AGN (Chapter 4). https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1435696630663-HHDD9MC92ZK6V9AY0K7S/fig_7-4.jpg Gallery: Chapter 7 - Figure 7-4 The change in limiting magnitude for crowding-limited observations of stellar populations when descoping from a 12 m to a 9.2 m or 6.5 m aperture. As shown from the stellar luminosity functions on the left, descoping to a smaller aperture restricts the observations to lower stellar surface densities, and thus to rarer, more luminous stars, leading to brighter limiting magnitudes. The top panel shows the impact on observations of an old stellar population that could resolve ~9 Gyr old main-sequence turnoffs with a 12 m HDST. The CMD on the right panel shows that a 9.2 m could no longer detect the old turnoff, and a 6.5 m could only detect much younger turnoffs and the red horizontal branch. The bottom panel shows the impact of smaller apertures on observations of young stellar populations, for which HDST could detect ~1.6 solar mass stars with ~2 Gyr lifetimes, while a 9.2 m and 6.5 m could only detect ~3 solar mass stars with 500 Myr lifetimes, and 5 solar mas stars with 100 Myr lifetimes, respectively. The rightmost axis gives apparent magnitudes at a distance of ~4 Mpc; there are many hundreds of galaxies within this volume. http://www.hdstvision.org/events daily 0.75 2015-07-08 https://images.squarespace-cdn.com/content/v1/558adc44e4b002a448a04c1a/1436362530818-QD4Z682CP5G038O21TXW/amnh-hdst-panel.jpg Events HOST: Neil deGrasse Tyson, PANEL (left to right): Michael Shara, Jason Tumlinson, Marc Postman, David Schiminovich, Julianne Dalcanton, and Sara Seager Image credit: AMNH http://www.hdstvision.org/response-to-elvis-2015-article daily 0.75 2015-11-05 http://www.hdstvision.org/deep-field-viewer daily 0.75 2016-03-18 http://www.hdstvision.org/read-me daily 0.75 2025-05-09 https://images.squarespace-cdn.com/content/v1/4ffee282e4b03755ffaefa81/1377028382592-IH9TYZ8LHZFIKU4UV0OP/ROBBIE+ROGERS+%2820130820%29.jpg Read Me https://images.squarespace-cdn.com/content/v1/4ffee282e4b03755ffaefa81/1377028469557-01IVM94AVBCGAXCH7XQU/More-Real+%2820130820%29.jpg Read Me https://images.squarespace-cdn.com/content/v1/4ffee282e4b03755ffaefa81/1377028382584-CNLHXXUTGDWV682OTOXK/Matthew+Cooper+%2820130820%29.jpg Read Me