A Lack of Planets in 47 Tucanae from a Hubble Space Telescope Search

By R. Gilliland, T. Brown, P. Guhathakurta, A. Sarajedini, E. Milone, M. Albrow, N. Baliber, H. Bruntt, Adam Burrows, D. Charbonneau and 14 more. 2000

220 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/12bb6bd727de9033e5001864e1fc054f888c3fea

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In Astronomy and Astrophysics

1. D. Charbonneau
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7. Andrew W. Howard
8. Sara Seager

Citations in the corpus

• Simulation of a Space-based Microlensing Survey for Terrestrial Extrasolar Planets (2000, background): “The only pointing variation needed during the ∼ 8 month Galactic bulge season would be a subpixel scale dither pattern needed to ensure that the photometric accuracy remains very close to the photon noise limit (Lauer 1999; Gilliland et al. 2000).”
• TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, background): “…the transit duration from the central crossing time by a factor of π/4 for its expectation assuming a uniform distribution of cos i for the orbital inclination (Gilliland et al. 2000; Seager & Mallén-Ornelas 2003), and include the expected dependence on the transit duration with e (Burke 2008).”
• The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, unknown): “Gilliland et al. (2000) conducted an important early transit search with HST, which targeted 47 Tucanae ([Fe/H] = −0.78 dex).”
• Planet formation and migration (2005, methodology): “Note that no short–period planets were found in the metal poor globular cluster 47 Tucanae in which about 34,000 stars were monitored by HST. Simulations had shown that about 17 hot Jupiters should have been detected by photometric transit signals if the frequency of these objects were the same in t”
• Some Tests to Establish Confidence in Planets Discovered by Transit Photometry (2002, background): “…from the ground (see, e.g., Borucki et al. 2001 ; Brown & Charbonneau 2000 ; Henry et al. 2000 ; Howell et al. 2000), while others are using spaceborne instruments including the Hubble Space Telescope (Gilliland et al. 2000 ; Brown et al. 2001) and the Hipparcos data archive (Laughlin 2000).”
• Spectroscopic Binaries, Velocity Jitter, and Rotation in Field Metal-poor Red Giant and Red Horizontal-Branch Stars (2003, background): “Gilliland et al. estimated that they should have detected transits by 17 ‘‘ hot Jupiters ’’ if the frequency in 47 Tuc was the same as has been observed for solar-type stars in the solar neighborhood.”
• Hubble Space Telescope Time-Series Photometry of the Transiting Planet of HD 209458 (2001, result): “This process was analogous to that used to search for transiting planets in observations of the eclipsing binary CM Dra (Doyle et al. 2000), and in HST time-series photometry of the globular cluster 47 Tucanae (Gilliland et al. 2000; Brown et al. 2001).”
• Difference imaging photometry of blended gravitational microlensing events with a numerical kernel (2009, methodology): “This approach is similar to that employed in R. Gilliland’s code for difference-imaging of undersampled HST WFPC2 images (Gilliland et al. 2000; Albrow et al. 2001d).”
• The Impact of Solar-like Variability on the Detectability of Transiting Terrestrial Planets (2002, methodology): “…from the ground (see, e.g., Borucki et al. 2001; Brown & Charbonneau 2000; Henry et al. 2000; Everett et al. 2000), while others are using spaceborne instruments, including the Hubble Space Telescope (HST) (Gilliland et al. 2000; Brown et al. 2001) and theHipparcos data archive (Laughlin 2000).”
• Detection of an Extrasolar Planet Atmosphere (2001, background): “Furthermore, the observed lack of close-in giant planets in the globular cluster 47 Tuc (Gilliland et al. 2000) may be due, in part, to a reduced planet formation rate caused by the low metallicity of the globular cluster.”
• Stellar Proper Motions in the Galactic Bulge from Deep Hubble Space Telescope ACS WFC Photometry (2008, methodology): “We remind the reader that this is probably a conservative upper limit, as no such false positives were found in the similar 47 Tuc analysis (Gilliland et al. 2000; for further discussion of this issue see Sahu et al. 2006).”
• A Deep Chandra Survey of the Globular Cluster 47 Tucanae: Catalog of Point Sources (2005, unknown): “Definitive identifications became possible using Chandra positions and HST data (especially the exceptional GO-8267 8.3 day time series; Gilliland et al. 2000) to search for variability and unusual colors (G01a; Edmonds et al. 2001, 2002a, 2002b, 2003a, 2003b).”
• Young Massive Star Clusters (2010, background): “Old globular clusters seem to be deficient in planets (e.g. 47 Tuc, Gilliland et al. 2000), possibly because of their low metallicities (Weldrake et al. 2005).”
• The effect of red noise on planetary transit detection (2006, background): “An obvious solution to the problem of photometric systematics is to move into space, as was indeed done soon after the discovery of 51 Peg with the Hubble Space Telescope (HST) in the globular cluster 47 Tuc (Gilliland et al. 2000).”