J/A+A/545/A97ivo://CDS.VizieR/J/A+A/545/A97doi:10.26093/cds/vizier.35450097CDSCrossfield I.J.M.2017-07-03T14:27:08Z2012-09-12T13:42:11ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsg-starssolar-system-planetsspectroscopyThe ACME Spectra project provides absolutely calibrated, mostly empirical spectra of exoplanet host stars for use in analysis of the stars and their planets. Spectra are obtained from ground-based telescopes and are tied directly to calibrated ground- and space-based photometry. The spectra remain only "mostly" empirical because of telluric absorption, but interpolation of stellar models over the gaps in wavelength coverage provides continuous stellar spectra. Among other uses, the spectra are suitable for precisely converting observed secondary eclipses (occultations) into absolute flux units with minimal recourse to models. In this paper, I introduce ACME's methods and present a calibrated spectrum of the nearby, super-Earth hosting star 55 Cancri that spans the range from 0.81-5.05um.2012A&A...545A..97Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/545/A97CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/533/A114 : Transit of super-Earth 55 Cnc e (Demory+, 2011)J/A+A/539/A28 : New transit photometry for super-Earth 55 Cnc e (Gillon+ 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/545/A97https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/545/A97http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/545/A97https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/545/A97https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/545/A97http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/545/A97GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/545/A97/55cancri55 Cancri spectrumrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[0.8/6] Wavelength (microns)umem.wldoublelog(Flux)Flux F_{lambda}_ , in W/m^2^/{mu}mlog(W.m**-2.um**-1)phot.flux;em.line.HalphadoubleerrFractional error in Fluxstat.errorfloat