Chromospheric Ca II Emission in Nearby F, G, K, and M Stars

By Jason T. Wright, G. Marcy, R. P. Butler, S. Vogt. 2004

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We present chromospheric Ca II H and K activity measurements, rotation periods, and ages for ∼1200 F, G, K, and M type main-sequence stars from ∼18,000 archival spectra taken at Keck and Lick Observatories as a part of the California and Carnegie Planet Search Project. We have calibrated our chromospheric S-values against the Mount Wilson chromospheric activity data. From these measurements we have calculated median activity levels and derived R, stellar ages, and rotation periods from general parameterizations for 1228 stars, ∼1000 of which have no previously published S-values. We also present precise time series of activity measurements for these stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c81b4c622e0cca4b6d0a487397ae4f118ba3808e

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Citations in the corpus

Hot Jupiters and Hot Spots: The Short- and Long-Term Chromospheric Activity on Stars with Giant Planets (2004, unknown): “The chromospheric contibutions R′HK are from Wright et al. (2004).”
How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars (2004, methodology): “The Keck and Lick target lists are those of Nidever et al. (2002), since � 7% of the targets in Wright et al. (2004) have not been observed over the full 5 year baseline used in this analysis.”
FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, methodology): “We used the standard HIRES setup and reduction pipeline employed by the California Planet Search (CPS) consortium (Wright et al. 2004; Howard et al. 2009; Johnson et al. 2010).”
Metallicity of M dwarfs - I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence (2005, background): “…or http://dx.doi.org/10.1051/0004-6361:20053046 planets are Gl 876 (Delfosse et al. 1998; Marcy et al. 1998, 2001) and Gl 436 (Butler et al. 2004), but a number of ongoing surveys are looking for more (e.g. Bonfils et al. 2004; Endl et al. 2003; Kuerster et al. 2003; Wright et al. 2004).”
Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first Super-Earth with measured radius (2009, unknown): “Using the relations in Wright et al. (2004), we derive a chromospheric age estimate of 1.4± 0.40 Gyr and a rotational period of 23± 3 days.”
Five New Multicomponent Planetary Systems (2005, methodology): “Analysis of our HIRES spectra shows that ½Fe/H ¼þ0:21, TeA ¼ 5551 K, V sin i¼ 2:2 km s 1, log R0HK ¼ 5:09, andProt ¼ 40 days, implying an age of 7–10Gyr (Valenti & Fischer 2005; Wright et al. 2004).”
Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, background): “Wright et al. (2004) estimated an age of 5.9 Gyr from its chromospheric activity and Valenti & Fischer (2005) reported an isochronal age of 8.2+4.3 −5.2 Gyr.”
Limits on Planetary Companions from Doppler Surveys of Nearby Stars (2016, background): “Selection of the target stars is described in Wright et al. (2004) and Marcy et al. (2005b).”
Catalog of Nearby Exoplanets (2006, background): “…& Mayor (2004) and Santos et al. (2005), Column 15 lists Mount Wilson S-values for many of the stars, most of which are drawn from Wright et al. (2004), Tinney et al. (2002), and Jenkins et al. (2005), but some of which are new to this work, measured in the manner described in Wright et al. (2004).”
ELODIE metallicity-biased search for transiting Hot Jupiters. II. A very hot Jupiter transiting the bright K star HD 189733 (2005, methodology): “The chromospheric activity indexS based on the relative flux level on CaII H and K lines was measured by Wright et al. (2004).”
A CORRELATION BETWEEN STELLAR ACTIVITY AND HOT JUPITER EMISSION SPECTRA (2010, methodology): “We used the standard HIRES setup employed by the California Planet Search (CPS) group (Wright et al. 2004; Howard et al. 2009).”
The HARPS search for southern extra-solar planets - VI. A Neptune-mass planet around the nearby M dwarf Gl 581 (2005, background): “Nonetheless, several teams (Wright et al., 2004; Endl et al., 2003; Delfosse et al., 1998a) collectively monitor over 200 M dwarfs with sufficient precision to detect a Jupiter-mass planet out to at least 2 AU.”
Frequency of Debris Disks around Solar-Type Stars: First Results from a Spitzer MIPS Survey (2005, methodology): “Whenever possible we adopt ages from the compilation of Wright et al. (2004), which provides a uniform tabulation for 1200 stars based on Ca II H&K line strengths.”
Five New Extrasolar Planets (2005, methodology): “It is chromospherically quiet, with S ¼ 0:15 and log R0HK ¼ 5:05 (Wright et al. 2004).”
The Ages of Stars (2007, background): “Multiple, extended measurements of chromospherically-quiet stars show a scatter of about 6% (Wright et al. 2004); this represents the floor to inherent variation in the best cases.”
The Transit Light Curve Project. V. System Parameters and Stellar Rotation Period of HD 189733 (2006, background): “The parent star is relatively active, with a chromospheric activity index S ¼ 0:525 (Wright et al. 2004) and log R0HK ¼ 4:4, raising the possibility of measuring the rotation period through starspot-induced quasi-periodic flux variations.”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “We also measure the chromospheric emission in the Ca II H & K line cores, providing SHK values (Isaacson 2009; Wright et al. 2004) on the Mt. Wilson system.”