Five New Extrasolar Planets

Marcy, Geoffrey W.; Butler, R. Paul; Vogt, Steven S.; Fischer, Debra A.; Henry, Gregory W.; Laughlin, G.; Wright, Jason T.; Johnson, John Asher

doi:10.1086/426384

Cited by 192 publications

(212 citation statements)

References 62 publications

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“…In four cases there are major updates to previously published orbital parameters, which we detail below. Marcy et al (2005) announced an M sin i = 3.7 M Jup planet in a 634-day, eccentric (e = 0.4) orbit around HD 183263, a G2 IV star, and pointed out a strong residual linear trend of 32 m s −1 yr −1 . Wright et al (2007) showed that by 2007 the residuals had significant curvature, but could not constrain the minimum mass of the outer companion.…”

Section: New and Updated Multiplanet Systemsmentioning

confidence: 99%

Ten New and Updated Multiplanet Systems and a Survey of Exoplanetary Systems

Wright

Upadhyay

Marcy

et al. 2009

ApJ

350

290

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We present the latest velocities for ten multiplanet systems, including a re-analysis of archival Keck and Lick data, resulting in improved velocities that supersede our previously published measurements. We derive updated orbital fits for 10 Lick and Keck systems, including two systems (HD 11964, HD 183263) for which we provide confirmation of second planets only tentatively identified elsewhere, and two others (HD 187123 and HD 217107) for which we provide a major revision of the outer planet's orbit. We compile orbital elements from the literature to generate a catalog of the 28 published multiple-planet systems around stars within 200 pc. From this catalog we find several intriguing patterns emerging: (1) including those systems with long-term radial velocity trends, at least 28% of known planetary systems appear to contain multiple planets; (2) planets in multipleplanet systems have somewhat smaller eccentricities than single planets; and (3) the distribution of orbital distances of planets in multiplanet systems and single planets are inconsistent: single-planet systems show a pileup at P ∼ 3 days and a jump near 1 AU, while multiplanet systems show a more uniform distribution in log-period. In addition, among all planetary systems we find the following. (1) There may be an emerging, positive correlation between stellar mass and giant-planet semimajor axis. (2) Exoplanets with M sin i > 1 M Jup more massive than Jupiter have eccentricities broadly distributed across 0 < e < 0.5, while lower mass exoplanets exhibit a distribution peaked near e = 0.

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Section: New and Updated Multiplanet Systemsmentioning

confidence: 99%

Ten New and Updated Multiplanet Systems and a Survey of Exoplanetary Systems

Wright

Upadhyay

Marcy

et al. 2009

ApJ

350

290

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“…The selection criteria for the target stars were described in Marcy et al (2005). The stars were drawn from the Hipparcos catalog (ESA 1997) with criteria that they have B À V > 0:55, have decl: > À35 , be older than 2 Gyr, and reside within 3 mag of the main sequence.…”

Section: The Target Stars and Doppler Techniquementioning

confidence: 99%

“…The sixth column gives the mass of the star, as determined above from the Girardi et al (2002) models. The seventh column gives the logarithm of the fraction of the stellar luminosity that emerges as chromospheric emission at the Ca ii H and K lines, namely, log R 0 HK , and the eighth column gives the resulting photospheric jitter in m s À1 , estimated as described in Marcy et al (2005) and Wright et al (2005). The ninth and tenth columns give the expected rotation period and age of the star based on R 0 HK from Wright et al (2004) and Noyes et al (1984).…”

Section: The Target Stars and Doppler Techniquementioning

confidence: 99%

“…At most a few observations have been made with this new detector. Representative ''null'' stars that show no Doppler variation above those errors are presented in many past papers such as Marcy et al (2005), and additional null stars are provided here in Figure 2. Stars of spectral type FGK exhibit intrinsic velocity ''jitter'' due to acoustic p-modes, turbulent convection, starspots, and flows in magnetic regions.…”

Section: The Target Stars and Doppler Techniquementioning

confidence: 99%

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Five New Multicomponent Planetary Systems

Vogt

Butler

Marcy

et al. 2005

ApJ

Self Cite

234

274

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We report Doppler measurements for six nearby G-and K-type main-sequence stars that show multiple low-mass companions, at least one of which has planetary mass. One system has three planets, the fourth triple-planet system known around a normal star, and another has an extremely low minimum mass of 18 M È . HD 128311 ( K0 V ) has two planets (one previously known) with minimum masses (M sin i) of 2.18M J and 3.21M J and orbital periods of 1.26 and 2.54 yr, suggesting a possible 2:1 resonance. For HD 108874 (G5 V ), the velocities reveal two planets (one previously known) having minimum masses and periods of (M sin i b ¼ 1:36M J , P b ¼ 1:08 yr) and (M sin i c ¼ 1:02M J , P c ¼ 4:4 yr). HD 50499 (G1 V ) has a planet with P ¼ 6:8 yr and M sin i ¼ 1:7M J , and the velocity residuals exhibit a trend of À4.8 m s À1 yr À1 , indicating a more distant companion with P > 10 yr and minimum mass of 2M J . HD 37124 (G4 IV-V ) has three planets, one having M sin i ¼ 0:61M J and P ¼ 154:5 days, as previously known. We find two plausible triple-planet models that fit the data, both having a second planet near P ¼ 840 days, with the more likely model having its third planet in a 6 yr orbit and the other one in a 29 day orbit. For HD 190360, we confirm the planet having P ¼ 7:9 yr and M sin i ¼ 1:5M J as found by the Geneva team, but we find a distinctly noncircular orbit with e ¼ 0:36 AE 0:03, rendering this not an analog of Jupiter as had been reported. Our velocities also reveal a second planet with P ¼ 17:1 days and M sin i ¼ 18:1 M È . HD 217107 (G8 IV) has a previously known ''hot Jupiter'' with M sin i ¼ 1:4M J and P ¼ 7:13 days, and we confirm its high eccentricity, e ¼ 0:13. The velocity residuals reveal an outer companion in an eccentric orbit, having minimum mass of M sin i > 2M J , eccentricity e $ 0:5, and a period P > 8 yr, implying a semimajor axis a > 4 AU and providing an opportunity for direct detection. We have obtained high-precision photometry of five of the six planetary host stars with three of the automated telescopes at Fairborn Observatory. We can rule out significant brightness variations in phase with the radial velocities in most cases, thus supporting planetary reflex motion as the cause of the velocity variations. Transits are ruled out to very shallow limits for HD 217107 and are also shown to be unlikely for the prospective inner planets of the HD 37124 and HD 108874 systems. HD 128311 is photometrically variable with an amplitude of 0.03 mag and a period of 11.53 days, which is much shorter than the orbital periods of its two planetary companions. This rotation period explains the origin of periodic velocity residuals to the two-planet model of this star. All of the planetary systems here would be further constrained with astrometry by the Space Interferometry Mission.

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“…These simulations were performed for all stars in the Anglo-Australian and Keck Planet Searches (for samples see Jones et al 2002;Marcy et al 2005;Butler et al 2006 and references therein), which show a long term radial-velocity profile consistent with an orbiting low-mass companion.…”

Section: Target Selectionmentioning

confidence: 99%

NACO-SDI imaging of known companion host stars from the AAPS and Keck planet search surveys

Jenkins¹,

Jones

Biller³

et al. 2010

A&A

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Context. Direct imaging of brown dwarfs as companions to solar-type stars can provide a wealth of well-constrained data to "benchmark" the physics of such objects, since quantities like metallicity and age can be determined from their well-studied primaries. Aims. We present results from an adaptive optics imaging program on stars drawn from the Anglo-Australian and Keck Planet Search projects, with the aim of directly imaging known cool companions. Methods. Simulations have modeled the expected contrast ratios and separations of known companions using estimates of orbital parameters available from current radial-velocity data and then a selection of the best case objects were followed-up with high contrast imaging to attempt to directly image these companions. Results. These simulations suggest that only a very small number of radial-velocity detected exoplanets with consistent velocity fits and age estimates could potentially be directly imaged using the VLT's Simultaneous Differential Imaging system and only under favorable conditions. We also present detectability confidence limits from the radial-velocity data sets and show how these can be used to gain a better understanding of these systems when combined with the imaging data. For HD32778 and HD91204 the detectabilities help little in constraining the companion and hence almost all our knowledge is drawn from the SDI images. Therefore, we can say that these stars do not host cool methane objects, out to on-sky separations of ∼2 , with contrasts less than 10−11 mag. However, for HD25874, HD120780 and HD145825, the contrasts and detectabilities can rule out a number of possible solutions, particularly at low angular separations, and for the best case, down to strong methane masses of 40 M J at 1 separation. The contrast curves constructed for these five stars show 5σ contrasts (ΔF1) of ∼9.2-11.5 mag at separations of ≥0.6 , which correspond to contrasts of ∼9.7-12.0 mag for companions of mid-T spectral type. Such limits allow us to reach down to 40 M J around fairly old field dwarfs that typically constitute high precision radial-velocity programs. Finally, the analysis performed here can serve as a template for future projects that will employ extreme-AO systems to directly image planets already indirectly discovered by the radial-velocity method.

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Five New Extrasolar Planets

Cited by 192 publications

References 62 publications

Ten New and Updated Multiplanet Systems and a Survey of Exoplanetary Systems

Ten New and Updated Multiplanet Systems and a Survey of Exoplanetary Systems

Five New Multicomponent Planetary Systems

NACO-SDI imaging of known companion host stars from the AAPS and Keck planet search surveys

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