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The Young Exoplanet Transit Initiative (YETI)
Neuhaeuser, R.1,2; Errmann, R.1,2; Berndt, A.1,2; Maciejewski, G.1,2,3; Takahashi, H.4; Chen, W. P.5; Dimitrov, D. P.6,12; Pribulla, T.1,2,7; Nikogossian, E. H.8; Jensen, E. L. N.9; Marschall, L.10; Wu, Z. -Y.11; Kellerer, A.13,14; Walter, F. M.15; Briceno, C.16; Chini, R.17,18; Fernandez, M.19; Raetz, St1,2; Torres, G.20; Latham, D. W.20; Quinn, S. N.20; Niedzielski, A.3; Bukowiecki, L.3; Nowak, G.3; Tomov, T.3; Tachihara, K.21,22; Hu, S. C. -L.5; Hung, L. W.5; Kjurkchieva, D. P.23; Radeva, V. S.23; Mihov, B. M.6,12; Slavcheva-Mihova, L.6,12; Bozhinova, I. N.6,12; Budaj, J.7; Vanko, M.7; Kundra, E.7; Hambalek, L.7; Krushevska, V.7,24; Movsessian, T.8; Harutyunyan, H.8; Downes, J. J.16; Hernandez, J.16; Hoffmeister, V. H.17; Cohen, D. H.9; Abel, I.9; Ahmad, R.9; Chapman, S.9; Eckert, S.9; Goodman, J.9; Guerard, A.9; Kim, H. M.9; Koontharana, A.9; Sokol, J.9; Trinh, J.9; Wang, Y.9; Zhou, X.11; Redmer, R.25; Kramm, U.25; Nettelmann, N.25; Mugrauer, M.1,2; Schmidt, J.1,2; Moualla, M.1,2; Ginski, C.1,2; Marka, C.1,2; Adam, C.1,2; Seeliger, M.1,2; Baar, S.1,2; Roell, T.1,2; Schmidt, T. O. B.1,2; Trepl, L.1,2; Eisenbeiss, T.1,2; Fiedler, S.1,2; Tetzlaff, N.1,2; Schmidt, E.1,2; Hohle, M. M.1,2,26; Kitze, M.1,2; Chakrova, N.27; Graefe, C.1,2,28; Schreyer, K.1,2; Hambaryan, V. V.1,2; Broeg, C. H.29; Koppenhoefer, J.26,30; Pandey, A. K.31
AbstractWe present the Young Exoplanet Transit Initiative (YETI), in which we use several 0.2 to 2.6-m telescopes around the world to monitor continuously young (<= 100 Myr), nearby (<= 1 kpc) stellar clusters mainly to detect young transiting planets (and to study other variability phenomena on time-scales from minutes to years). The telescope network enables us to observe the targets continuously for several days in order not to miss any transit. The runs are typically one to two weeks long, about three runs per year per cluster in two or three subsequent years for about ten clusters. There are thousands of stars detectable in each field with several hundred known cluster members, e. g. in the first cluster observed, Tr-37, a typical cluster for the YETI survey, there are at least 469 known young stars detected in YETI data down to R = 16.5 mag with sufficient precision of 50 millimag rms (5 mmag rms down to R = 14.5 mag) to detect transits, so that we can expect at least about one young transiting object in this cluster. If we observe similar to 10 similar clusters, we can expect to detect similar to 10 young transiting planets with radius determinations. The precision given above is for a typical telescope of the YETI network, namely the 60/90-cm Jena telescope (similar brightness limit, namely within +/-1 mag, for the others) so that planetary transits can be detected. For targets with a periodic transit-like light curve, we obtain spectroscopy to ensure that the star is young and that the transiting object can be sub-stellar; then, we obtain Adaptive Optics infrared images and spectra, to exclude other bright eclipsing stars in the (larger) optical PSF; we carry out other observations as needed to rule out other false positive scenarios; finally, we also perform spectroscopy to determine the mass of the transiting companion. For planets with mass and radius determinations, we can calculate the mean density and probe the internal structure. We aim to constrain planet formation models and their time-scales by discovering planets younger than similar to 100 Myr and determining not only their orbital parameters, but also measuring their true masses and radii, which is possible so far only by the transit method. Here, we present an overview and first results. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
KeywordPlanetary Systems Surveys Techniques: Photometric Techniques: Spectroscopic
Indexed BySCI
WOS IDWOS:000293271400001
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Cited Times:29[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Affiliation1.Inst Astrophys, D-07745 Jena, Germany
2.Univ Sternwarte, FSU Jena, D-07745 Jena, Germany
3.Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland
4.Gunma Astron Observ, Takayama, Gunma 3770702, Japan
5.Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan
6.Bulg Acad Sc, Inst Astron, Sofia 1784, Bulgaria
7.Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia
8.Byurakan Astrophys Observ, Byurakan 378433, Armenia
9.Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA
10.Gettysburg Coll Observ, Dept Phys, Gettysburg, PA 17325 USA
11.Chinese Acad Sci, Key Lab Opt Astron, NAO, Beijing 100012, Peoples R China
12.Bulg Acad Sc, NAO, Sofia 1784, Bulgaria
13.Univ Hawaii, Inst Astron, Hilo, HI 96720 USA
14.Big Bear Solar Observ, Big Bear City, CA 92314 USA
15.SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA
16.Ctr Invest Astron, Merida 5101, Venezuela
17.Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany
18.Univ Catolica Norte, Fac Ciencias, Antofagasta, Chile
19.CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain
20.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
21.Joint ALMA Observ, Santiago, Chile
22.Natl Astron Observ Japan, ALMA Project Off, Tokyo 1818588, Japan
23.Univ Shumen, Shumen 9700, Bulgaria
24.NAS Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine
25.Univ Rostock, Inst Phys, D-18051 Rostock, Germany
26.MPI Extraterr Phys, D-85740 Garching, Germany
27.FSU Jena, Inst Appl Phys, D-07743 Jena, Germany
28.Univ Kiel, D-24098 Kiel, Germany
29.Univ Bern, Inst Phys, CH-3012 Bern, Switzerland
30.Univ Sternwarte, D-81679 Munich, Germany
31.Aryabhatta Res Inst Observat Sci, Naini Tal 263129, Uttarakhand, India
Recommended Citation
GB/T 7714
Neuhaeuser, R.,Errmann, R.,Berndt, A.,et al. The Young Exoplanet Transit Initiative (YETI)[J]. ASTRONOMISCHE NACHRICHTEN,2011,332(6):547-561.
APA Neuhaeuser, R..,Errmann, R..,Berndt, A..,Maciejewski, G..,Takahashi, H..,...&Pandey, A. K..(2011).The Young Exoplanet Transit Initiative (YETI).ASTRONOMISCHE NACHRICHTEN,332(6),547-561.
MLA Neuhaeuser, R.,et al."The Young Exoplanet Transit Initiative (YETI)".ASTRONOMISCHE NACHRICHTEN 332.6(2011):547-561.
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