Infrared radial velocities of vB 10

Osorio, M. R. Zapatero; Martín, E. L.; Burgo, C. del; Deshpande, Rohit; Rodler, F.; Montgomery, M. M.

doi:10.1051/0004-6361/200912869

Cited by 15 publications

(2 citation statements)

References 29 publications

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“…The dispersions of our nightly RV measurements are 143 m s −1 and 351 m s −1 for GJ 752 A and GJ 752 B, respectively (see Figure 3). The scatter in our NIRSPEC RV measurements is smaller than the measurements of Zapatero Osorio et al (2009), which reached an amplitude of 1 km s −1 . Our RV dispersion for GJ 752 B is larger than the 10 m s −1 reached by Bean et al (2009) and could be due the smaller spectral resolution of NIRSPEC compared with CRIRES (R = 24,000 for NIRSPEC versus R = 50,000 for CRIRES).…”

Section: Gj 752 Bcontrasting

confidence: 71%

Keck Nirspec Radial Velocity Observations of Late-M Dwarfs

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White

Bailey

et al. 2012

ApJS

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We present the results of an infrared spectroscopic survey of 23 late-M dwarfs with the NIRSPEC echelle spectrometer on the Keck II telescope. Using telluric lines for wavelength calibration, we are able to achieve measurement precisions of down to 45 m s −1 for our late-M dwarfs over a one-to four-year long baseline. Our sample contains two stars with radial velocity (RV) variations of >1000 m s −1. While we require more measurements to determine whether these RV variations are due to unseen planetary or stellar companions or are the result of starspots known to plague the surface of M dwarfs, we can place upper limits of <40 M J sin i on the masses of any companions around those two M dwarfs with RV variations of <160 m s −1 at orbital periods of 10-100 days. We have also measured the rotational velocities for all the stars in our late-M dwarf sample and offer our multiorder, high-resolution spectra over 2.0-2.4 μm to the atmospheric modeling community to better understand the atmospheres of late-M dwarfs.

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Section: Gj 752 Bcontrasting

confidence: 71%

Keck Nirspec Radial Velocity Observations of Late-M Dwarfs

Tanner

White

Bailey

et al. 2012

ApJS

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“…More recently, an ammonia gas cell has been employed to achieve ∼5 m s −1 precision (Bean et al 2010b) over 6 month time‐scales with CRIRES operating at K ‐band wavelengths. This survey (Bean et al 2010a) has not found evidence for the massive planet claimed to be orbiting the low‐mass M dwarf VB 10 (Pravdo & Shaklan 2009; Zapatero Osorio et al 2009).…”

Section: Introductionmentioning

confidence: 89%

The effect of M dwarf starspot activity on low-mass planet detection thresholds

Barnes

Jeffers

Jones

2011

Monthly Notices of the Royal Astronomical Society

105

104

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???The definitive version is available at www3.interscience.wiley.com Copyright Royal Astronomical SocietyIn light of the growing interest in searching for low mass, rocky planets, we investigate the impact of starspots on radial velocity searches for earth-mass planets in orbit about M dwarf stars. Since new surveys targeting M dwarfs will likely be carried out at infrared wavelengths, a comparison between V and Y band starspot-induced jitter is made, indicating a reduction of up to an order of magnitude when observing in the Y band. The exact reduction in jitter is dependent on the photosphere to spot contrast ratio, with greater improvements at smaller contrasts. We extrapolate a model used to describe solar spot distributions to simulate the spot patterns that we expect to find on M dwarfs. Under the assumption that M dwarfs are near or fully convective, we randomly place starspots on the stellar surface, simulating different levels of spot coverage. Line profiles distorted by spots are derived and are used to investigate the starspot-induced jitter. By making assumptions about the degree of spot activity, detection limits for earth-mass planets in habitable zones are simulated for between 10 and 500 observation epochs. We find that < 50 epochs are required to detect 1-2 planets (with < 1 per cent false alarm probability) orbiting slowly rotating 0.1 and 0.2 M-circle dot stars. This sensitivity decreases when typical rotation velocities and activity levels for each stellar mass/spectral type are considered. No detections of below 20 planets are expected for < 500 observations for the most active stars with v sin i >= 20 km s-1 and dark spots

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The Radial Velocity Method for the Detection of Exoplanets

Hatzes

2016

Methods of Detecting Exoplanets

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Infrared radial velocities of vB 10

Cited by 15 publications

References 29 publications

Keck Nirspec Radial Velocity Observations of Late-M Dwarfs

Keck Nirspec Radial Velocity Observations of Late-M Dwarfs

The effect of M dwarf starspot activity on low-mass planet detection thresholds

The Radial Velocity Method for the Detection of Exoplanets

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