Radial Velocity Jitter in Stars from the California and Carnegie Planet Search at Keck Observatory

By Jason T. Wright. 2005

281 citations recorded by the source corpus.

I present an empirical model for predicting a star’s radial velocity jitter from its B - V color, activity level, and absolute magnitude. This model is based on observations of ∼450 well‐observed stars from Keck Observatory for the California and Carnegie Planet Search Program. The model includes noise from both astrophysical sources and systematic errors, and describes jitter as generally increasing with a star’s activity and height above the main sequence.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/84d40ff25a72b516d948bf76e8c44a2a08b99049

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Citations in the corpus

RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS (2009, methodology): “…velocity measurements were first combined into two-hour bins and the total measurement errors were estimated by adding 5 m s−1 to the internal measurement errors, in quadrature, to account for the moderate jitter level of typical subgiants (Fischer et al. 2003; Wright 2005; Johnson et al. 2007b).”
Retired A Stars and Their Companions: Exoplanets Orbiting Three Intermediate-Mass Subgiants (2007, background): “Measuring precise Doppler shifts of early–type dwarfs is complicated by their rotation- ally broadened spectral features, high surface temperatures, and high levels of excess radial velocity noise, or “jitter” (Saar et al. 1998; Wright 2005).”
Five Planets Orbiting 55 Cancri (2007, methodology): “The weights assigned to each Doppler measurement are the inverse square of each measurement’s uncertainty, which are approximated as the quadrature sum of the internal uncertainty in the Doppler measurement and the “jitter” that stems from photospheric motions and instrumental errors (Wright 2005).”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “Following Wright (2005), and based on the values of SHK, MV , and B − V , we estimate σjitter for each of the stars (Table 3).”
THE LICK–CARNEGIE EXOPLANET SURVEY: A 3.1 M⊕ PLANET IN THE HABITABLE ZONE OF THE NEARBY M3V STAR GLIESE 581 (2010, methodology): “Our measurement of logR′hk = −5.39 leads to an estimate (Wright 2005) of 1.9 ms−1 for the expected RV jitter due to stellar surface activity and an age estimate of 4.3 Gyr.”
TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “Wright et al. (2007) cautioned that the low amplitude of this prospective 38 d planet meant that it would require more observations for confirmation, especially given the higher levels . of jitter seen in subgiant stars (Wright 2005; Johnson et al. 2007b).”
CHROMOSPHERIC ACTIVITY AND JITTER MEASUREMENTS FOR 2630 STARS ON THE CALIFORNIA PLANET SEARCH (2010, methodology): “Chromospheric activity is monitored in the stellar spectra used to derive precision radial velocities for stars on many Doppler planet searches (Saar, Butler, Marcy 1998; Saar & Fischer 1999; Paulson et al. 2002; Wright et al. 2004; Wright 2005; Johnson et al. 2007).”
Binarity in carbon-enhanced metal-poor stars (2014, unknown): “Considering the precision of this study, this so-called radial velocity “jitter” – although theoretically poorly understood – is expected to (only) manifest itself clearly at the ip of the red giant branch (e.g. Gunn & Griffin 1979; Setiawan et al. 2003; Wright 2005; Carney et al. 2008).”
A New Planet around an M Dwarf: Revealing a Correlation between Exoplanets and Stellar Mass (2007, methodology): “…have rotationally broadened absorption features (do Nascimento et al. 2003; Galland et al. 2005), have fewer spectral lines due to high surface temperatures, and display a large amount of excess velocity scatter due to surface inhomogeneities and pulsation (“jitter”; Saar et al. 1998; Wright 2005).”
The HARPS search for southern extra-solar planets IX. Exoplanets orbiting HD 100777, HD 190647, and HD 221287 (2007, background): “This matches the lowest value expected for this star from the Santos et al. (2000) and Wright (2005) studies.”
Improving the Efficiency of Markov Chain Monte Carlo for Analyzing the Orbits of Extrasolar Planets (2005, background): “Indeed, the quoted uncertainties in the radial velocity observations have been demonstrated to be quite accurate for some chromosphically inactive stars with no signs of planets (Wright 2005).”
AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “In fact, inactive K and early M stars have weaker P-mode oscillations and lower Doppler noise (“jitter”) than their F or G counterparts (Wright 2005; Isaacson & Fischer 2011).”
Barycentric Corrections at 1 cm s-1 for Precise Doppler Velocities (2014, background): “…that they can be treated as linear perturbations or ignored for many purposes, and at any rate, the motions and inhomogeneities of stellar atmospheres (i.e., jitter, e.g. Wright 2005) limit the precision of Doppler work to levels that do not require the rigor provided by, for instance, TEMPO2.”
METALLICITY AND TEMPERATURE INDICATORS IN M DWARF K-BAND SPECTRA: TESTING NEW AND UPDATED CALIBRATIONS WITH OBSERVATIONS OF 133 SOLAR NEIGHBORHOOD M DWARFS (2011, background): “• Inactive: The activity of M dwarfs can also cause false positives (e.g. starspot-crossing events; Carter et al. (2011)) and can cause radial velocity and photometric jitter (Wright 2005; Berta et al. 2011).”
HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, methodology): “For this value the calibration by Wright (2005) predicts velocity jitter ranging from 8 to 16m s−1.”