The Gaia Parallax Discrepancy for the Cluster Pismis 19 and Separating δ Scutis from Cepheids

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dc.contributor.authorMajaess, Daniel
dc.contributor.authorBonatto, Charles J.
dc.contributor.authorTurner, David G
dc.contributor.authorSaito, Roberto K
dc.contributor.authorMinniti, Dante
dc.contributor.authorMoni Bidin, Christian
dc.contributor.authorGonzález-Díaz, Danilo
dc.contributor.authorAlonso-Garcia, Javier
dc.contributor.authorBono, Giuseppe
dc.contributor.authorBraga, Vittorio F.
dc.contributor.authorNavarro, Maria G
dc.contributor.authorCarraro, Giovanni
dc.date.accessioned2025-04-16T16:59:24Z
dc.date.available2025-04-16T16:59:24Z
dc.date.issued0025
dc.descriptionINDEXACION SCOPUS
dc.description.abstractPre-Gaia distances for the open cluster Pismis 19 disagree with Gaia parallaxes. A Two Micron All Sky Survey (2MASS) JKs red clump distance was therefore established for Pismis 19 (2.90 ± 0.15 kpc), which reaffirms that zero-point corrections for Gaia are required. OGLE GD-CEP-1864 is confirmed as a member of Pismis 19 on the basis of DR3 proper motions and its 2MASS+Vista Variables in the Vía Láctea color-magnitude position near the tip of the turnoff. That 0.3 day variable star is likely a δ Scuti rather than a classical Cepheid. The case revealed a pertinent criterion to segregate those two populations in tandem with the break in the Wesenheit Leavitt Law (≃0.5 day). Just shortward of that period discontinuity are δ Scutis, whereas beyond the break lie first overtone classical Cepheids mostly observed beyond the first crossing of the instability strip. © 2025. The Author(s). Published by the American Astronomical Society.
dc.identifier.issn0004637X
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/64210
dc.language.isoen
dc.publisherInstitute of Physics
dc.titleThe Gaia Parallax Discrepancy for the Cluster Pismis 19 and Separating δ Scutis from Cepheids
dc.typeArtículo
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