dc.creator |
Majaess, Daniel J. |
|
dc.creator |
Turner, David Gerald, 1945- |
|
dc.creator |
Gieren, W. |
|
dc.date.accessioned |
2018-04-30T15:57:42Z |
|
dc.date.available |
2018-04-30T15:57:42Z |
|
dc.date.issued |
2011-11-10 |
|
dc.identifier.issn |
2041-8205 |
|
dc.identifier.uri |
http://library2.smu.ca/handle/01/27492 |
|
dc.description |
Publisher's Version/PDF |
|
dc.description.abstract |
Evidence is presented which supports findings that the classical Cepheid VI<sub>C</sub> period Wesenheit function is relatively insensitive to metallicity. The viability of a recently advocated strong metallicity dependence was evaluated by applying the proposed correction (γ = −0.8 mag dex<sup>−1</sup>) to distances established for the Magellanic Clouds via a Galactic VI<sub>C</sub> Wesenheit calibration, which is anchored to 10 nearby classical Cepheids with measured Hubble Space Telescope (HST) parallaxes. The resulting γ-corrected distances for the Magellanic Clouds (e.g., Small Magellanic Cloud, μ0,γ ∼ 18.3) are in significant disagreement with that established from a mean of >300 published estimates (NED-D), and a universal Wesenheit template featuring 11 δ Scuti, SX Phe, RR Lyrae, and Type II Cepheid variables with HST/Hipparcos parallaxes. Conversely, adopting a null correction (i.e., γ = 0 mag dex<sup>−1</sup>) consolidates the estimates. In tandem with existing evidence, the results imply that variations in chemical composition among Cepheids are a comparatively negligible source of uncertainty for W<sub>VIc</sub> -based extragalactic distances and determinations of H<sub>0</sub>. A new approach is described which aims to provide additional Galactic Cepheid calibrators to facilitate subsequent assessments of the VI<sub>C</sub> Wesenheit function's relative (in) sensitivity to abundance changes. VVV/UKIDSS/Two Micron All Sky Survey JHK<sub>s</sub> photometry for clusters in spiral arms shall be employed to establish a precise galactic longitude–distance relation, which can be applied in certain cases to determine the absolute Wesenheit magnitudes for younger Cepheids. |
en_CA |
dc.description.provenance |
Submitted by Betty McEachern (betty.mceachern@smu.ca) on 2018-04-30T15:57:42Z
No. of bitstreams: 1
Majaess_D_article_2011.pdf: 163699 bytes, checksum: fad9784e9a38087af2084eb9e7ecd380 (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2018-04-30T15:57:42Z (GMT). No. of bitstreams: 1
Majaess_D_article_2011.pdf: 163699 bytes, checksum: fad9784e9a38087af2084eb9e7ecd380 (MD5)
Previous issue date: 2011-11-10 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
IOP Publishing |
en_CA |
dc.relation.uri |
https://dx.doi.org/10.1088/2041-8205/741/2/L36 |
|
dc.rights |
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user. |
|
dc.subject.lcsh |
Cosmological distances |
|
dc.subject.lcsh |
Extragalactic distances |
|
dc.subject.lcsh |
Red shift |
|
dc.subject.lcsh |
Cepheids |
|
dc.title |
Concerning the classical Cepheid VI[subscript C] Wesenheit function's strong metallicity dependence |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal Letters 741(2), L36. (2011) |
en_CA |
Copyright statement:
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.