Institution
Search for extraterrestrial intelligence
Nonprofit•Mountain View, California, United States•
About: Search for extraterrestrial intelligence is a nonprofit organization based out in Mountain View, California, United States. It is known for research contribution in the topics: Planet & Exoplanet. The organization has 671 authors who have published 2857 publications receiving 126819 citations. The organization is also known as: Search for extraterrestrial intelligence & SETI.
Topics: Planet, Exoplanet, Stars, Mars Exploration Program, Planetary system
Papers published on a yearly basis
Papers
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Ames Research Center1, University of California, Berkeley2, San Jose State University3, Las Cumbres Observatory Global Telescope Network4, Search for extraterrestrial intelligence5, York University6, Aarhus University7, University of Texas at Austin8, Lowell Observatory9, Harvard University10, California Institute of Technology11, Space Telescope Science Institute12, Lawrence Hall of Science13, Goddard Space Flight Center14, United States Department of the Navy15, Carnegie Institution for Science16, University of Washington17, University of Hawaii at Hilo18, University of California, Santa Cruz19, Massachusetts Institute of Technology20, Fermilab21, San Diego State University22, Southern Connecticut State University23, Planetary Science Institute24, Yale University25, Marshall Space Flight Center26, The Catholic University of America27, University of Idaho28, Villanova University29
TL;DR: The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars, which is the region where planetary temperatures are suitable for water to exist on a planet's surface.
Abstract: The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet’s surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets (~0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets.
3,663 citations
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Shadab Alam1, Franco D. Albareti2, Carlos Allende Prieto3, Carlos Allende Prieto4 +360 more•Institutions (102)
TL;DR: The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrogram, and a novel optical interferometer.
Abstract: The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 sq. deg of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-Object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include measured abundances of 15 different elements for each star. In total, SDSS-III added 2350 sq. deg of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 sq. deg; 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5,513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra.
2,471 citations
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TL;DR: The K2 mission as discussed by the authors uses an innovative way of operating the Kepler spacecraft to observe target fields along the ecliptic for the next 2-3 years, with an estimated photometric precision near 400 ppm in a single 30 minute observation.
Abstract: The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hr photometric precision of 80 ppm (both at V = 12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75 days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers pre-launch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology.
1,672 citations
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San Jose State University1, Ames Research Center2, Las Cumbres Observatory Global Telescope Network3, Harvard University4, University of California, Santa Cruz5, University of Florida6, Pennsylvania State University7, University of California, Berkeley8, Georgia State University9, California Institute of Technology10, Carnegie Institution for Science11, University of Copenhagen12, Aarhus University13, University of Texas at Austin14, Massachusetts Institute of Technology15, Search for extraterrestrial intelligence16, Lawrence Hall of Science17, University of Hertfordshire18, Villanova University19, Fermilab20, Princeton University21, San Diego State University22
TL;DR: In this paper, the authors verified nearly 5000 periodic transit-like signals against astrophysical and instrumental false positives yielding 1108 viable new transiting planet candidates, bringing the total count up to over 2300.
Abstract: New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T_0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R_P/R_★), reduced semimajor axis (d/R_★), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2 R_⊕ compared to 53% for candidates larger than 2 R_⊕) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant.
1,271 citations
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Ames Research Center1, University of California, Berkeley2, San Jose State University3, Las Cumbres Observatory Global Telescope Network4, Search for extraterrestrial intelligence5, Aarhus University6, University of Texas at Austin7, Lowell Observatory8, California Institute of Technology9, Harvard University10, Space Telescope Science Institute11, Lawrence Hall of Science12, Carnegie Institution for Science13, University of Florida14, University of California, Santa Cruz15, Massachusetts Institute of Technology16, Fermilab17, San Diego State University18, Southern Connecticut State University19, Marshall Space Flight Center20, University of Arizona21, University of Hertfordshire22, Centre National D'Etudes Spatiales23, Villanova University24
TL;DR: In this article, the Kepler mission released data for 156,453 stars observed from the beginning of the science observations on 2009 May 2 through September 16, and there are 1235 planetary candidates with transit-like signatures detected in this period.
Abstract: On 2011 February 1 the Kepler mission released data for 156,453 stars observed from the beginning of the science observations on 2009 May 2 through September 16. There are 1235 planetary candidates with transit-like signatures detected in this period. These are associated with 997 host stars. Distributions of the characteristics of the planetary candidates are separated into five class sizes: 68 candidates of approximately Earth-size (R_p < 1.25 R_⊕), 288 super-Earth-size (1.25 R_⊕ ≤ R_p < 2 R_⊕), 662 Neptune-size (2 R_⊕ ≤ R_p < 6 R_⊕), 165 Jupiter-size (6 R_⊕ ≤ R_p < 15 R_⊕), and 19 up to twice the size of Jupiter (15 R_⊕ ≤ R_p < 22 R_⊕). In the temperature range appropriate for the habitable zone, 54 candidates are found with sizes ranging from Earth-size to larger than that of Jupiter. Six are less than twice the size of the Earth. Over 74% of the planetary candidates are smaller than Neptune. The observed number versus size distribution of planetary candidates increases to a peak at two to three times the Earth-size and then declines inversely proportional to the area of the candidate. Our current best estimates of the intrinsic frequencies of planetary candidates, after correcting for geometric and sensitivity biases, are 5% for Earth-size candidates, 8% for super-Earth-size candidates, 18% for Neptune-size candidates, 2% for Jupiter-size candidates, and 0.1% for very large candidates; a total of 0.34 candidates per star. Multi-candidate, transiting systems are frequent; 17% of the host stars have multi-candidate systems, and 34% of all the candidates are part of multi-candidate systems.
1,241 citations
Authors
Showing all 685 results
Name | H-index | Papers | Citations |
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Jon M. Jenkins | 126 | 581 | 62929 |
Jonathan J. Fortney | 123 | 435 | 55006 |
Jon A. Holtzman | 120 | 415 | 73942 |
Jack J. Lissauer | 113 | 478 | 54673 |
Daniel Huber | 111 | 538 | 40216 |
Jason F. Rowe | 110 | 374 | 44387 |
Douglas A. Caldwell | 90 | 267 | 36802 |
David Hollenbach | 87 | 251 | 32315 |
Joseph D. Twicken | 81 | 213 | 33686 |
Jessie L. Christiansen | 80 | 302 | 28457 |
Louis J. Allamandola | 79 | 254 | 20541 |
Jie Li | 76 | 843 | 32221 |
Peter Tenenbaum | 73 | 157 | 27071 |
Timothy J. Lee | 66 | 313 | 15878 |
Susan E. Thompson | 64 | 187 | 18077 |