The Tables

Mermilliod, J. C.; Mermilliod, Monique

doi:10.1007/978-1-4613-8436-6_2

Cited by 6 publications

(5 citation statements)

References 1,041 publications

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“…The sole exception was NGC 6705, where the magnitudes and colors came from Johnson, Sandage, & Wahlquist (1956). Other sources of cluster photometry are Hagen (1970) and Mermilliod (1976). In all, three sets of cluster observations were taken in the , , , and passbands, which are sum-…”

Section: Taking the Observationsmentioning

confidence: 99%

A New Method for Computing Differential Color Refraction

Stone

2002

PUBL ASTRON SOC PAC

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A new method for computing differential color refraction (DCR) is presented in this paper that uses observations taken through a conventional filter as well as through a narrowband interference filter that serves as a template for the reductions. The method is tested with observations taken through Johnson BV and Cousins RI filters, and, in general, there is good agreement (excellent in all but one case) between observed and predicted values of DCR. A full description of the method is given as well as a discussion of the refraction model used to make the predictions. As expected, DCR is strongest in the B passband and weakest in the I band because of the wavelength dependence of atmospheric refraction. Furthermore, the common practice of calibrating DCR against a stellar color is investigated, finding that the procedure is justified, albeit the intrinsic scatter in the calibration can vary widely with the choice for the color. This scatter can be minimized with a judicious choice for the color system, and examples are given for the BVRI passbands considered in the paper. Nonetheless, there will always be some remaining error caused by the calibrating process, which will affect mostly star positions determined at large zenith distances. Further gains in positional accuracy are possible by choosing a passband for which the DCR is very small. Two such passbands are the Cousins I band (FWHM p 1900 A ˚) and the passband (FWHM p 630 A ˚) chosen for the USNO CCD Astrograph Catalog project. The ranges in the DCR for these passbands are, respectively, only 19 and 12 mas at a zenith distance of ZD p 60Њ. When calibrated against stellar color, remaining errors in the DCR calibrations for both of these passbands are expected to be under 5 mas. In the final section of the paper, numerical results are given for other possible passbands with small ranges (≤20 mas) in DCR.

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Section: Taking the Observationsmentioning

confidence: 99%

A New Method for Computing Differential Color Refraction

Stone

2002

PUBL ASTRON SOC PAC

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“…Lovis et al (2011) detect a magnetic activity cycle of P cyc = 3792 +806 −566 d and predict the rotation period to be P rot = 43.7±4.9 d based on the their estimate of the star's mean chromospheric activity (log R HK = -4.996). Combining the star's mean chromospheric activity levels (log R HK = -4.993) recently reported by Meunier et al (2017), with its color (B − V = 0.884 ;Mermilliod 2006) and the rotation-activity relations from Mamajek & Hillenbrand (2008), one predicts the star's rotation to be approximately P rot 48 d.…”

Section: Hd 192310 (Gj 785)mentioning

confidence: 91%

Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions

Laliotis¹,

Burt²,

Mamajek³

et al. 2023

Preprint

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Directly imaging temperate rocky planets orbiting nearby, Sun-like stars with a 6-m-class IR/O/UV space telescope, recently dubbed the Habitable Worlds Observatory, is a high priority goal of the Astro2020 Decadal Survey. To prepare for future direct imaging surveys, the list of potential targets should be thoroughly vetted to maximize efficiency and scientific yield. We present an analysis of archival radial velocity data for southern stars from the NASA/NSF Extreme Precision Radial Velocity Working Group's list of high priority target stars for future direct imaging missions (drawn from the HabEx, LUVOIR, and Starshade Rendezvous studies). For each star, we constrain the region of companion mass and period parameter space we are already sensitive to based on the observational baseline, sampling, and precision of the archival RV data. Additionally, for some of the targets we report new estimates of magnetic activity cycle periods, rotation periods, improved orbital parameters for previously known exoplanets, and new candidate planet signals that require further vetting or observations to confirm. Our results show that for many of these stars we are not yet sensitive to even Saturn-mass planets in the habitable zone, let alone smaller planets, highlighting the need for future EPRV vetting efforts before the launch of a direct imaging mission. We present evidence that the

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“…VOSA allowed us to collect all the photometry available in the Virtual Observatory (VO) for our list of 201 stars (including the nine stars from V1 and V2 with an indirect θ LD ) and to convert magnitudes into fluxes thanks to an exhaustive description of all the existing filters. We only kept the photometry from the VO catalogues that contain at least fifty of our targets, namely 2MASS (Cutri et al 2003), AKARI (Yamamura et al 2010), Gaia DR3 (Gaia Collaboration 2023c), GALEX (Bianchi et al 2017), Strömgren photometric catalogues (Hauck & Mermilliod 1998;Paunzen 2015), Johnson UBV (Mermilliod 1987), IRAS (Neugebauer et al 1984), HIPPARCOS (ESA 1997), Tycho-2 (Høg et al 2000) and WISE (Cutri et al 2021).…”

Section: Compilation Of Magnitudes and Fluxesmentioning

confidence: 99%

Gaia FGK benchmark stars: Fundamental T_eff and log g of the third version

Soubiran,

Creevey,

Lagarde

et al. 2024

A&A

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Large spectroscopic surveys devoted to the study of the Milky Way, including Gaia, use automated pipelines to determine the atmospheric parameters of millions of stars. The Gaia FGK benchmark stars are reference stars with and derived through fundamental relations, independently of spectroscopy, to be used as anchors for the parameter scale. The first and second versions of the sample have been extensively used for that purpose, and more generally to help constrain stellar models. We provide the third version of the Gaia FGK benchmark stars, an extended set intended to improve the calibration of spectroscopic surveys, and their interconnection. We have compiled about 200 candidates that have precise measurements of angular diameters and parallaxes. We determined their bolometric fluxes by fitting their spectral energy distribution. Masses were determined using two sets of stellar evolution models. In a companion paper, we describe the determination of metallicities and detailed abundances. We provide a new set of 192 Gaia FGK benchmark stars with their fundamental and and with uncertainties lower than 2<!PCT!> for most stars. Compared to the previous versions, the homogeneity and accuracy of the fundamental parameters are significantly improved thanks to the high quality of the Gaia photometric and astrometric data.

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The Tables

Cited by 6 publications

References 1,041 publications

A New Method for Computing Differential Color Refraction

A New Method for Computing Differential Color Refraction

Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions

Gaia FGK benchmark stars: Fundamental T_eff and log g of the third version

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The Tables

Cited by 6 publications

References 1,041 publications

A New Method for Computing Differential Color Refraction

A New Method for Computing Differential Color Refraction

Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions

Gaia FGK benchmark stars: Fundamental Teff and log g of the third version

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Product

Resources

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Gaia FGK benchmark stars: Fundamental T_eff and log g of the third version