Discovery of three very distant M and L dwarfs

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dc.contributor.authorWolf, C.en
dc.contributor.authorMundt, R.en
dc.contributor.authorThompson, D.en
dc.contributor.authorChaffee, F.en
dc.contributor.authorBeckwith, S. V.W.en
dc.contributor.authorFockenbrock, R.en
dc.contributor.authorFried, J.en
dc.contributor.authorHippelein, H.en
dc.contributor.authorHuang, J. S.en
dc.contributor.authorVon Kuhlmann, B.en
dc.contributor.authorLeinert, C.en
dc.contributor.authorMeisenheimer, K.en
dc.contributor.authorPhleps, S.en
dc.contributor.authorRöser, H. J.en
dc.contributor.authorThommes, E.en
dc.date.accessioned2026-01-04T11:41:31Z
dc.date.available2026-01-04T11:41:31Z
dc.date.issued1998en
dc.description.abstractWe report the serendipitous discovery of three very cool distant late type dwarfs. These low-mass stars were found in the 9h- and 16h-fields of the Calar Alto Deep Imaging Survey (CADIS) and named CA09-LMS1, CA16-LMS1 and CA16-LMS2. CA16-LMS1 is the latest object and has a spectral type of >M10 (L1 in the new spectral class L). The other two stars have spectral types of about M9 (CA16-LMS2) and M6.5 (CA09-LMS1). We derive distances of 1150±300pc for CA09-LMS1, 330±80 pc for CA16-LMS1, and 120±30 pc for CA16-LMS2. The first two of these three objects are probably the most distant late-type M dwarfs for which optical spectra have been obtained.en
dc.description.statusPeer-revieweden
dc.format.extent5en
dc.identifier.issn0004-6361en
dc.identifier.otherORCID:/0000-0002-4569-016X/work/189310614en
dc.identifier.scopus0043028086en
dc.identifier.urihttps://hdl.handle.net/1885/733803511
dc.language.isoenen
dc.sourceAstronomy and Astrophysicsen
dc.subjectStars: individual: CA09-LMS1 (J0913.5+4611); CA16-LMS1 (J1625.0+5544); CA16-LMS2 (J1623.9+5546)en
dc.subjectStars: low-mass, brown dwarfsen
dc.titleDiscovery of three very distant M and L dwarfsen
dc.typeJournal articleen
dspace.entity.typePublicationen
local.bibliographicCitation.lastpage131en
local.bibliographicCitation.startpage127en
local.contributor.affiliationWolf, C.; Max Planck Institute for Astronomyen
local.contributor.affiliationMundt, R.; Max Planck Institute for Astronomyen
local.contributor.affiliationThompson, D.; Max Planck Institute for Astronomyen
local.contributor.affiliationChaffee, F.; W. M. Keck Observatoryen
local.contributor.affiliationBeckwith, S. V.W.; Max Planck Institute for Astronomyen
local.contributor.affiliationFockenbrock, R.; Max Planck Institute for Astronomyen
local.contributor.affiliationFried, J.; Max Planck Institute for Astronomyen
local.contributor.affiliationHippelein, H.; Max Planck Institute for Astronomyen
local.contributor.affiliationHuang, J. S.; Max Planck Institute for Astronomyen
local.contributor.affiliationVon Kuhlmann, B.; Max Planck Institute for Astronomyen
local.contributor.affiliationLeinert, C.; Max Planck Institute for Astronomyen
local.contributor.affiliationMeisenheimer, K.; Max Planck Institute for Astronomyen
local.contributor.affiliationPhleps, S.; Max Planck Institute for Astronomyen
local.contributor.affiliationRöser, H. J.; Max Planck Institute for Astronomyen
local.contributor.affiliationThommes, E.; Royal Observatoryen
local.identifier.citationvolume338en
local.identifier.pure44b3b87e-8ba9-45fc-bf2a-9bf4379d0c1aen
local.identifier.urlhttps://www.scopus.com/pages/publications/0043028086en
local.identifier.urlhttps://articles.adsabs.harvard.edu/pdf/1998A%26A...338..127Wen
local.identifier.urlhttps://articles.adsabs.harvard.edu/full/1998A%26A...338..127Wen
local.type.statusPublisheden

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