Transiting Exoplanet Survey Satellite

被引：3236

作者：

Ricker, George R. ^{[1
]}

Winn, Joshua N. ^{[1
]}

Vanderspek, Roland ^{[1
]}

Latham, David W. ^{[2
]}

Bakos, Gaspar A. ^{[3
]}

Bean, Jacob L. ^{[4
]}

Berta-Thompson, Zachory K. ^{[1
]}

Brown, Timothy M. ^{[5
]}

Buchhave, Lars ^{[2
,6
]}

Butler, Nathaniel R. ^{[7
]}

Butler, R. Paul ^{[8
]}

Chaplin, William J. ^{[9
,10
]}

Charbonneau, David ^{[2
]}

Christensen-Dalsgaard, Jorgen ^{[10
]}

Clampin, Mark ^{[11
]}

Deming, Drake ^{[12
]}

Doty, John ^{[13
]}

De Lee, Nathan ^{[14
,15
]}

Dressing, Courtney ^{[2
]}

Dunham, Edward W. ^{[16
]}

Endl, Michael ^{[17
]}

Fressin, Francois ^{[2
]}

Ge, Jian ^{[18
]}

Henning, Thomas ^{[19
]}

Holman, Matthew J. ^{[2
]}

Howard, Andrew W. ^{[20
]}

Ida, Shigeru ^{[21
]}

Jenkins, Jon M. ^{[22
]}

Jernigan, Garrett ^{[23
]}

Johnson, John Asher ^{[2
]}

Kaltenegger, Lisa ^{[19
]}

Kawai, Nobuyuki ^{[21
]}

Kjeldsen, Hans ^{[10
]}

Laughlin, Gregory ^{[24
]}

Levine, Alan M. ^{[1
]}

Lin, Douglas ^{[24
]}

Lissauer, Jack J. ^{[22
]}

MacQueen, Phillip ^{[17
]}

Marcy, Geoffrey ^{[25
]}

McCullough, Peter R. ^{[26
,27
]}

Morton, Timothy D. ^{[3
]}

Narita, Norio ^{[28
]}

Paegert, Martin ^{[15
]}

Palle, Enric ^{[29
]}

Pepe, Francesco ^{[30
]}

Pepper, Joshua ^{[15
,31
]}

Quirrenbach, Andreas ^{[32
]}

Rinehart, Stephen A. ^{[11
]}

Sasselov, Dimitar ^{[2
]}

Sato, Bun'ei ^{[21
]}

机构：

[1] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[3] Princeton Univ, Princeton, NJ 08540 USA

[4] Univ Chicago, Chicago, IL 60611 USA

[5] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA

[6] Univ Copenhagen, DK-1165 Copenhagen, Denmark

[7] Arizona State Univ, Tempe, AZ 85004 USA

[8] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA

[9] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[10] Univ Aarhus, Stellar Astrophys Ctr, DK-8000 Aarhus, Denmark

[11] NASA, Goddard Space Flight Ctr, Green Belt, MD 20771 USA

[12] Univ Maryland, College Pk, MD 20742 USA

[13] Noqsi Aerosp Ltd, Pine, CO 80470 USA

[14] No Kentucky Univ, Highland Hts, KY 41099 USA

[15] Vanderbilt Univ, Nashville, TN 37235 USA

[16] Lowell Observ, Flagstaff, AZ 86001 USA

[17] McDonald Observ, Austin, TX 78712 USA

[18] Univ Florida, Gainesville, FL 32611 USA

[19] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[20] Univ Hawaii, Manoa, HI 96822 USA

[21] Tokyo Inst Technol, Tokyo 1528851, Japan

[22] NASA, Ames Res Ctr, Mountain View, CA 94035 USA

[23] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[24] UCO, Lick Observ, Santa Cruz, CA 95064 USA

[25] Univ Calif Berkeley, Berkeley, CA 94720 USA

[26] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[27] Johns Hopkins Univ, Baltimore, MD 21218 USA

[28] Natl Astron Observ Japan, Tokyo 1818588, Japan

[29] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain

[30] Observ Geneva, CH-1290 Versoix, Switzerland

[31] Lehigh Univ, Bethlehem, PA 18015 USA

[32] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany

[33] INAF, Osservatorio Astrofis Torino, I-10025 Turin, Italy

[34] Fisk Univ, Nashville, TN 37208 USA

来源：

JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS | 2015年 / 1卷 / 01期

基金：

美国国家科学基金会;

关键词：

exoplanet; extrasolar planet; photometry; satellite; transits; KEPLER; PLANETS; STARS; MISSION; SYSTEMS; CATALOG;

D O I：

10.1117/1.JATIS.1.1.014003

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I-C approximate to 4-13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

引用

页数：10

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