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Title: A HIGH-ECCENTRICITY COMPONENT IN THE DOUBLE-PLANET SYSTEM AROUND HD 163607 AND A PLANET AROUND HD 164509

Abstract

We report the detection of three new exoplanets from Keck Observatory. HD 163607 is a metal-rich G5IV star with two planets. The inner planet has an observed orbital period of 75.29 {+-} 0.02 days, a semi-amplitude of 51.1 {+-} 1.4 m s{sup -1}, an eccentricity of 0.73 {+-} 0.02, and a derived minimum mass of M{sub P} sin i = 0.77 {+-} 0.02 M{sub Jup}. This is the largest eccentricity of any known planet in a multi-planet system. The argument of periastron passage is 78.7 {+-} 2.{sup 0}0; consequently, the planet's closest approach to its parent star is very near the line of sight, leading to a relatively high transit probability of 8%. The outer planet has an orbital period of 3.60 {+-} 0.02 years, an orbital eccentricity of 0.12 {+-} 0.06, and a semi-amplitude of 40.4 {+-} 1.3 m s{sup -1}. The minimum mass is M{sub P} sin i = 2.29 {+-} 0.16 M{sub Jup}. HD 164509 is a metal-rich G5V star with a planet in an orbital period of 282.4 {+-} 3.8 days and an eccentricity of 0.26 {+-} 0.14. The semi-amplitude of 14.2 {+-} 2.7 m s{sup -1} implies a minimum mass of 0.48 {+-} 0.09 M{submore » Jup}. The radial velocities (RVs) of HD 164509 also exhibit a residual linear trend of -5.1 {+-} 0.7 m s{sup -1} year{sup -1}, indicating the presence of an additional longer period companion in the system. Photometric observations demonstrate that HD 163607 and HD 164509 are constant in brightness to submillimagnitude levels on their RV periods. This provides strong support for planetary reflex motion as the cause of the RV variations.« less

Authors:
; ;  [1]; ; ;  [2];  [3];  [4];  [5];  [6]
  1. Department of Astronomy, Yale University, 260 Whitney Ave., New Haven, CT 06511 (United States)
  2. Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720 (United States)
  3. Department of Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125 (United States)
  4. Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209 (United States)
  5. Department of Astronomy, 525 Davey Lab, The Pennsylvania State University, University Park, PA 16802 (United States)
  6. Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States)
Publication Date:
OSTI Identifier:
22004373
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 744; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; METALS; PLANETS; PROBABILITY; RADIAL VELOCITY; STARS

Citation Formats

Giguere, Matthew J, Fischer, Debra A, Spronck, Julien, Howard, Andrew W, Marcy, Geoffrey W, Isaacson, Howard T, Johnson, John A, Henry, Gregory W, Wright, Jason T, and Fengji, Hou. A HIGH-ECCENTRICITY COMPONENT IN THE DOUBLE-PLANET SYSTEM AROUND HD 163607 AND A PLANET AROUND HD 164509. United States: N. p., 2012. Web. doi:10.1088/0004-637X/744/1/4.
Giguere, Matthew J, Fischer, Debra A, Spronck, Julien, Howard, Andrew W, Marcy, Geoffrey W, Isaacson, Howard T, Johnson, John A, Henry, Gregory W, Wright, Jason T, & Fengji, Hou. A HIGH-ECCENTRICITY COMPONENT IN THE DOUBLE-PLANET SYSTEM AROUND HD 163607 AND A PLANET AROUND HD 164509. United States. https://doi.org/10.1088/0004-637X/744/1/4
Giguere, Matthew J, Fischer, Debra A, Spronck, Julien, Howard, Andrew W, Marcy, Geoffrey W, Isaacson, Howard T, Johnson, John A, Henry, Gregory W, Wright, Jason T, and Fengji, Hou. 2012. "A HIGH-ECCENTRICITY COMPONENT IN THE DOUBLE-PLANET SYSTEM AROUND HD 163607 AND A PLANET AROUND HD 164509". United States. https://doi.org/10.1088/0004-637X/744/1/4.
@article{osti_22004373,
title = {A HIGH-ECCENTRICITY COMPONENT IN THE DOUBLE-PLANET SYSTEM AROUND HD 163607 AND A PLANET AROUND HD 164509},
author = {Giguere, Matthew J and Fischer, Debra A and Spronck, Julien and Howard, Andrew W and Marcy, Geoffrey W and Isaacson, Howard T and Johnson, John A and Henry, Gregory W and Wright, Jason T and Fengji, Hou},
abstractNote = {We report the detection of three new exoplanets from Keck Observatory. HD 163607 is a metal-rich G5IV star with two planets. The inner planet has an observed orbital period of 75.29 {+-} 0.02 days, a semi-amplitude of 51.1 {+-} 1.4 m s{sup -1}, an eccentricity of 0.73 {+-} 0.02, and a derived minimum mass of M{sub P} sin i = 0.77 {+-} 0.02 M{sub Jup}. This is the largest eccentricity of any known planet in a multi-planet system. The argument of periastron passage is 78.7 {+-} 2.{sup 0}0; consequently, the planet's closest approach to its parent star is very near the line of sight, leading to a relatively high transit probability of 8%. The outer planet has an orbital period of 3.60 {+-} 0.02 years, an orbital eccentricity of 0.12 {+-} 0.06, and a semi-amplitude of 40.4 {+-} 1.3 m s{sup -1}. The minimum mass is M{sub P} sin i = 2.29 {+-} 0.16 M{sub Jup}. HD 164509 is a metal-rich G5V star with a planet in an orbital period of 282.4 {+-} 3.8 days and an eccentricity of 0.26 {+-} 0.14. The semi-amplitude of 14.2 {+-} 2.7 m s{sup -1} implies a minimum mass of 0.48 {+-} 0.09 M{sub Jup}. The radial velocities (RVs) of HD 164509 also exhibit a residual linear trend of -5.1 {+-} 0.7 m s{sup -1} year{sup -1}, indicating the presence of an additional longer period companion in the system. Photometric observations demonstrate that HD 163607 and HD 164509 are constant in brightness to submillimagnitude levels on their RV periods. This provides strong support for planetary reflex motion as the cause of the RV variations.},
doi = {10.1088/0004-637X/744/1/4},
url = {https://www.osti.gov/biblio/22004373}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 744,
place = {United States},
year = {Sun Jan 01 00:00:00 EST 2012},
month = {Sun Jan 01 00:00:00 EST 2012}
}