Confirmation of Color-dependent Centroid Shift Measured After 1.8 Years with HST

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dc.citation.issue5
dc.citation.volume165
dc.contributor.authorBhattacharya A
dc.contributor.authorBennett DP
dc.contributor.authorBeaulieu JP
dc.contributor.authorBond IA
dc.contributor.authorKoshimoto N
dc.contributor.authorLu JR
dc.contributor.authorBlackman JW
dc.contributor.authorRanc C
dc.contributor.authorVandorou A
dc.contributor.authorTerry SK
dc.contributor.authorMarquette JB
dc.contributor.authorCole AA
dc.contributor.authorFukui A
dc.date.accessioned2024-05-09T02:32:09Z
dc.date.available2024-05-09T02:32:09Z
dc.date.issued2023-04-19
dc.description.abstractWe measured the precise masses of the host and planet in the OGLE-2003-BLG-235 system, when the lens and source were resolving, with 2018 Keck high resolution images. This measurement is in agreement with the observation taken in 2005 with the Hubble Space Telescope (HST). In the 2005 data, the lens and sources were not resolved and the measurement was made using color-dependent centroid shift only. The Nancy Grace Roman Space Telescope will measure masses using data typically taken within 3-4 yr of the peak of the event, which is a much shorter baseline when compared to most of the mass measurements to date. Hence, the color-dependent centroid shift will be one of the primary methods of mass measurements for the Roman telescope. Yet, mass measurements of only two events (OGLE-2003-BLG-235 and OGLE-2005-BLG-071) have been done using the color-dependent centroid shift method so far. The accuracy of the measurements using this method are neither completely known nor well studied. The agreement of the Keck and HST results, as shown in this paper, is very important because this agreement confirms the accuracy of the mass measurements determined at a small lens-source separation using the color-dependent centroid shift method. It also shows that with >100 high resolution images, the Roman telescope will be able to use color-dependent centroid shift at a 3-4 yr time baseline and produce mass measurements. We find that OGLE-2003-BLG-235 is a planetary system that consists of a 2.34 ± 0.43M Jup planet orbiting a 0.56 ± 0.06M ⊙ K-dwarf host star at a distance of 5.26 ± 0.71 kpc from the Sun.
dc.description.confidentialfalse
dc.edition.editionMay 2023
dc.identifier.citationBhattacharya A, Bennett DP, Beaulieu JP, Bond IA, Koshimoto N, Lu JR, Blackman JW, Ranc C, Vandorou A, Terry SK, Marquette JB, Cole AA, Fukui A. (2023). Confirmation of Color-dependent Centroid Shift Measured After 1.8 Years with HST. Astronomical Journal. 165. 5.
dc.identifier.doi10.3847/1538-3881/acc85e
dc.identifier.eissn1538-3881
dc.identifier.elements-typejournal-article
dc.identifier.issn0004-6256
dc.identifier.number206
dc.identifier.urihttps://mro.massey.ac.nz/handle/10179/69536
dc.languageEnglish
dc.publisherAmerican Astronomical Society
dc.publisher.urihttps://iopscience.iop.org/article/10.3847/1538-3881/acc85e
dc.relation.isPartOfAstronomical Journal
dc.rights(c) 2023 The Author/s
dc.rightsCC BY 4.0
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titleConfirmation of Color-dependent Centroid Shift Measured After 1.8 Years with HST
dc.typeJournal article
pubs.elements-id461302
pubs.organisational-groupOther
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