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dc.contributor.authorKruszyńska, Katarzyna
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorRybicki, K. A.
dc.contributor.authorMaskoliūnas, M.
dc.contributor.authorBachelet, E.
dc.contributor.authorRattenbury, N.
dc.contributor.authorMróz, P.
dc.contributor.authorZieliński, P.
dc.contributor.authorHowil, K.
dc.contributor.authorKaczmarek, Z.
dc.contributor.authorHodgkin, S. T.
dc.contributor.authorIhanec, N.
dc.contributor.authorGezer, I.
dc.contributor.authorGromadzki, M.
dc.contributor.authorMikołajczyk, P.
dc.contributor.authorStankevičiūtė, A.
dc.contributor.authorČepas, V.
dc.contributor.authorPakštienė, E.
dc.contributor.authorŠiškauskaitė, K.
dc.contributor.authorZdanavičius, J.
dc.contributor.authorBozza, V.
dc.contributor.authorDominik, M.
dc.contributor.authorFiguera Jaimes, R.
dc.contributor.authorFukui, A.
dc.contributor.authorHundertmark, M.
dc.contributor.authorNarita, N.
dc.contributor.authorStreet, R.
dc.contributor.authorTsapras, Y.
dc.contributor.authorBronikowski, M.
dc.contributor.authorJabłońska, M.
dc.contributor.authorJabłonowska, A.
dc.contributor.authorZiółkowska, O.
dc.date.accessioned2022-07-28T16:30:13Z
dc.date.available2022-07-28T16:30:13Z
dc.date.issued2022-06-30
dc.identifier.citationKruszyńska , K , Wyrzykowski , Ł , Rybicki , K A , Maskoliūnas , M , Bachelet , E , Rattenbury , N , Mróz , P , Zieliński , P , Howil , K , Kaczmarek , Z , Hodgkin , S T , Ihanec , N , Gezer , I , Gromadzki , M , Mikołajczyk , P , Stankevičiūtė , A , Čepas , V , Pakštienė , E , Šiškauskaitė , K , Zdanavičius , J , Bozza , V , Dominik , M , Figuera Jaimes , R , Fukui , A , Hundertmark , M , Narita , N , Street , R , Tsapras , Y , Bronikowski , M , Jabłońska , M , Jabłonowska , A & Ziółkowska , O 2022 , ' Lens parameters for Gaia18cbf : a long gravitational microlensing event in the Galactic plane ' , Astronomy & Astrophysics , vol. 662 , A59 . https://doi.org/10.1051/0004-6361/202142602en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 279564957
dc.identifier.otherPURE UUID: dd89bae2-17d7-47fa-aab8-925c865cc540
dc.identifier.otherBibCode: 2021arXiv211108337K
dc.identifier.otherORCID: /0000-0002-3202-0343/work/116598430
dc.identifier.otherScopus: 85132378864
dc.identifier.urihttp://hdl.handle.net/10023/25746
dc.descriptionFunding: This work was supported from the Polish NCN grants: Harmonia No. 2018/30/M/ST9/00311, Daina No. 2017/27/L/ST9/03221, MNiSW grant DIR/WK/2018/12 and NCBiR grant within POWER program nr POWR.03.02.00-00-l001/16-00. We acknowledge Research Council of Lithuania grant No S-LL-19-2 and European Commission’s H2020 OPTICON grant No. 730890 as well as OPTICON RadioNet Pilot grant No. 101004719. YT acknowledges the support of DFG priority program SPP 1992 “Exploring the Diversity of Extrasolar Planets” (TS 356/3-1). This work is partly supported by JSPS KAKENHI Grant Number JP18H05439, and the Astrobiology Center of National Institutes of Natural Sciences (NINS) (Grant Number AB031010).en
dc.description.abstractContext: The timescale of a microlensing event scales as a square root of a lens mass. Therefore, long-lasting events are important candidates for massive lenses, including black holes. Aims: Here, we present the analysis of the Gaia18cbf microlensing event reported by the Gaia Science Alerts system. It exhibited a long timescale and features that are common for the annual microlensing parallax effect. We deduce the parameters of the lens based on the derived best fitting model. Methods: We used photometric data collected by the Gaia satellite as well as the follow-up data gathered by the ground-based observatories. We investigated the range of microlensing models and used them to derive the most probable mass and distance to the lens using a Galactic model as a prior. Using known mass-brightness relation we determined how likely it is that the lens is a main-sequence (MS) star. Results: This event is one of the longest ever detected, with the Einstein timescale of tE=491.41+128.31-84.94 days for the best solution and tE=453.74+178.69-105.74 days for the second-best. Assuming Galaxy priors, this translates to the most probable lens mass of ML = 2.65+5.09-1.48 M⊙ and ML = 1.71+3.78-1.06 M⊙, respectively. The limits on the blended light suggest that this event was most likely not caused by a MS star, but rather by a dark remnant of stellar evolution.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © 2022 ESO. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/202142602.en
dc.subjectGravitational lensing: microen
dc.subjectTechniques: photometricen
dc.subjectWhite dwarfsen
dc.subjectStars: neutronen
dc.subjectStars: black holesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subjectMCCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleLens parameters for Gaia18cbf : a long gravitational microlensing event in the Galactic planeen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Commissionen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202142602
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2111.08337en
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2021arXiv211108337Ken
dc.identifier.grantnumber730890en


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