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Design Considerations for Directly Imaging Earth-like Exoplanets
содержание презентации «Design Considerations for Directly Imaging Earth-like Exoplanets.pptx»| Сл | Текст | Сл | Текст |
| 1 | Design Considerations for Directly | 34 | terrestrial planet in the HZ of HabCat |
| Imaging Earth-like Exoplanets. Garreth | stars. | ||
| Ruane gjr8334@rit.edu Chester F. Carlson | 35 | Detector Signal. . [Lyon and Clampin | |
| Center for Imaging Science Rochester | 2012]. | ||
| Institute of Technology. | 36 | Noise Sources. Noise sources: Shot | |
| 2 | Question: What telescope | noise of planet and star Zodiacal light | |
| specifications are necessary to directly | Exozodiacal light Background Dark current | ||
| image and characterize planets in the | Read noise. | ||
| “habitable zone” of nearby stars? | 37 | Noise Sources. . [Lyon and Clampin | |
| 3 | Outline. Introduction Exoplanetary | 2012]. | |
| Science Short history of direct imaging | 38 | Noise Sources. Exozodiacal Light | |
| High-contrast imaging technology Candidate | Subtraction will be necessary. Preliminary | ||
| stars Hipparcos Design specification | studies will allow better subtraction. | ||
| Conclusions. | Subtraction may cause significant noise. | ||
| 4 | Exoplanetary Science. Detections. | May be important for orbital | |
| Methods. 770 confirmed More than 2300 | determination. [Lyon and Clampin 2012]. | ||
| candidates. Radial velocities Planetary | 39 | Background Sources. Photometric | |
| transits Transit timing variation | measurements rule out background sources. | ||
| Gravitational microlensing Astrometry | 40 | Signal-to-Noise Ratio. . [Lyon and | |
| Pulsar timing Features in circumstellar | Clampin 2012]. | ||
| disks Direct imaging. Missions. Current | 41 | Integration Time. . Many HZ planets | |
| MOST (Canada) COROT (France) Kepler (NASA) | could be imaged at SNR = 5 under ideal | ||
| Under Development Gaia (ESA) JWST (NASA). | conditions and minimal noise. | ||
| 5 | History of Direct imaging. | 42 | Other performance considerations. |
| 6 | History of Direct Imaging. 2004: First | Aperture obstructions Optical surface | |
| direct image, 2M1207b 27 planetary systems | quality Polychromatic effects Pointing | ||
| have been imaged since 2004. VLT NACO (8 | Postprocessing. | ||
| m) J-band image of 2M1207 [Mohanty et. al. | 43 | Mission specifications. | |
| 2006]. VLT NACO (8 m) NIR image of 2M1207 | 44 | Mission design. . | |
| [ESO]. | 45 | Future missions. Photometric | |
| 7 | Beta Pictoris b (2008). [ESO/A.-M. | measurements Broadband (Spitzer: HD | |
| Lagrange et al. 2009]. | 189733b) Spectroscopy Atmosphere, | ||
| 8 | HR 8799 (2008/2010). Keck L’-band | biomarkers Polarimetry Oceans? Image | |
| image of HR 8799 [Marois et. al. 2010]. | credit: (left)Turnbull et. al. 2006 | ||
| 9 | LkCa 15 b (2011). [Kraus and Ireland | (right) ESO. | |
| 2011]. | 46 | Conclusions. It is possible to design | |
| 10 | What do these systems have in common? | a mission with current technology that is | |
| Large planets Large separation Low | likely to directly image at least one | ||
| contrast Hot Jupiters/Young? Emit in | earth-like planet. With state-of-the-art | ||
| infrared High contrast astronomical | starlight suppression JWST would have over | ||
| imaging seeks to resolve cool planets very | 200 viable HZ targets. Such a mission | ||
| close to bright stars. | would be capable of imaging most planets | ||
| 11 | High contrast imaging. | outside of the HZ. Later spectral types | |
| 12 | High-contrast imaging terminology. | are favored for contrast. These types have | |
| Contrast Inner working angle Outer working | very small HZs. Direct imaging opens doors | ||
| angle Discovery space. | to photometric, spectroscopic, | ||
| 13 | Contrast. [Lyon and Clampin 2012]. | polarimetric studies of exoplanets. | |
| 14 | Inner Working Angle. . [Lyon and | 47 | References. Kenworthy, M.A., Quanz, |
| Clampin 2012]. | S.P., Meyer, M.R., Kasper, M.E., Lenzen, | ||
| 15 | Outer Working Angle. Limited by the | R., Codona, J.L., Girard, J.H.V., Hinz, | |
| field of view of the optics Can be limited | P.M., 2010. An apodizing phase plate | ||
| by actuators. | coronagraph for VLT/NACO. arXiv:1007.3448. | ||
| 16 | Discovery Space. Field of view. IWA. | Kraus, A.L., Ireland, M.J., 2011. LkCa 15: | |
| Sky Angle. OWA. | A Young Exoplanet Caught at Formation? | ||
| 17 | High-contrast imaging technology. Lyot | arXiv:1110.3808. Lafreni?re, D., | |
| coronagraph. [Sivaramakrishnan et al. | Jayawardhana, R., van Kerkwijk, M.H., | ||
| 2001]. | 2008. Direct Imaging and Spectroscopy of a | ||
| 18 | High-contrast imaging technology. | Planetary-Mass Candidate Companion to a | |
| Apodizing phase plate coronagraph. | Young Solar Analog. The Astrophysical | ||
| [Kenworthy et al. 2010]. | Journal 689, L153–L156. Lagrange, A.-M., | ||
| 19 | Instruments in use. VLT NACO/APP | Gratadour, D., Chauvin, G., Fusco, T., | |
| coronagraph Keck NIRC-2 Gemini NICI/Lyot | Ehrenreich, D., Mouillet, D., Rousset, G., | ||
| coronagraph HST NICMOS STIS ACS/HCR JWST | Rouan, D., Allard, F., Gendron, ?., | ||
| NIRCam. Image credit: ESO. | Charton, J., Mugnier, L., Rabou, P., | ||
| 20 | Next generation technology. NASA’s New | Montri, J., Lacombe, F., 2009. A probable | |
| Worlds Observer. 4-m telescope plus | giant planet imaged in the ? Pictoris | ||
| starshade has star:planet limiting | disk. Astronomy and Astrophysics 493, | ||
| contrast of 10-11 at IWA = 50 mas. | L21–L25. Lyon, R.G., Clampin, M., 2012. | ||
| [http://newworlds.colorado.edu]. | Space telescope sensitivity and controls | ||
| 21 | Next generation technology. Optical | for exoplanet imaging. Optical Engineering | |
| vortex coronagraph. z. Mask. PP1. Lyot | 51, 011002– 011002–15. Marois, C., | ||
| Stop. Detector. L3. L1. L2. ?’, ?’. r, ? | Macintosh, B., Barman, T., Zuckerman, B., | ||
| ?, ? O1. | Song, I.S., Patience, J., Lafreniere, D., | ||
| 22 | Next generation technology. Optical | Doyon, R., 2008. Direct Imaging of | |
| vortex coronagraph. z. Mask. PP1. Lyot | Multiple Planets Orbiting the Star HR | ||
| Stop. Detector. L3. L1. L2. ?’, ?’. r, ? | 8799. Science 322, 1348–1352. Marois, C., | ||
| ?, ? O1. | Zuckerman, B., Konopacky, Q.M., Macintosh, | ||
| 23 | Next generation technology. Vortex | B., Barman, T., 2010. Images of a fourth | |
| coronagraph. [Serabyn et al. 2010]. | planet orbiting HR 8799. Nature 468, | ||
| 24 | Candidate stars. | 1080–1083. Mohanty, S., Jayawardhana, R., | |
| 25 | “Habitable” Zone. Image credit: | Hu?lamo, N., Mamajek, E., 2007. The | |
| NASA/Ames/JPL-Caltech. | Planetary Mass Companion 2MASS 1207-3932B: | ||
| 26 | HabCat: A catalog of nearby | Temperature, Mass, and Evidence for an | |
| “habitable” systems. Originally targets | Edge-on Disk. The Astrophysical Journal | ||
| selected for SETI Derived from the | 657, 1064–1091. Serabyn, E., Mawet, D., | ||
| Hipparcos catalog 17,129 stars out of | Burruss, R., 2010. An image of an | ||
| about 118,218 Criteria for HabCat | exoplanet separated by two diffraction | ||
| Candidates Stars must be at least 3 Gyr | beamwidths from a star. Nature 464, | ||
| old. Stars must be non-variable. Stars | 1018–1020. Sivaramakrishnan, A., Koresko, | ||
| must be capable of harboring terrestrial | C.D., Makidon, R.B., Berkefeld, T., | ||
| planets (measured by [Fe/H]). Stars must | Kuchner, M.J., 2001. Ground?based | ||
| support a dynamically stable habitable | Coronagraphy with High?Order Adaptive | ||
| zone. [Turnbull et al. 2003]. | Optics. The Astrophysical Journal 552, | ||
| 27 | The HabCat catalog. | 397–408. Swartzlander, G.A., 2009. The | |
| 28 | Size of habitable zone. . [Turnbull | optical vortex coronagraph. Journal of | |
| et al. 2004]. | Optics a-Pure and Applied Optics 11. | ||
| 29 | Habitable Zone. . [Image Credit: | Turnbull, M., Glassman, T., Roberge, A., | |
| ESO]. | Lo, A., Cash, W., 2009. Looking for New | ||
| 30 | Can we resolve planets in the HZ? . | Earth in the Coming Decade with Direct | |
| Diameter [m]. IWA [mas]. # of HabCat | Imaging, in: Astro2010: The Astronomy and | ||
| Stars. 1. 226.9. 1. 2. 113.4. 9. 4. 56.7. | Astrophysics Decadal Survey. Presented at | ||
| 86. 8. 28.4. 1167. 16. 14.2. 9092. | the astro2010: The Astronomy and | ||
| 31 | Planet-Star Contrast. . [Lyon and | Astrophysics Decadal Survey, p. 299. | |
| Clampin 2012]. | Turnbull, M.C., Tarter, J.C., 2003a. | ||
| 32 | Luminosity Ratio of Earth-like planet. | Target Selection for SETI. I. A Catalog of | |
| . Plot of luminosity ratio of a | Nearby Habitable Stellar Systems. The | ||
| terrestrial planet in the HZ of HabCat | Astrophysical Journal Supplement Series | ||
| stars. | 145, 181–198. Turnbull, M.C., Tarter, | ||
| 33 | Aperture Flux. . [Lyon and Clampin | J.C., 2003b. Target Selection for SETI. | |
| 2012]. | II. Tycho?2 Dwarfs, Old Open Clusters, and | ||
| 34 | Aperture Flux of an Earth-like planet. | the Nearest 100 Stars. The Astrophysical | |
| Plot of aperture flux for a 6.5 m (JWST) | Journal Supplement Series 149, 423–436. | ||
| aperture in the J-band due to a | |||
| Design Considerations for Directly Imaging Earth-like Exoplanets.pptx | |||
Design Considerations for Directly Imaging Earth-like Exoplanets
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