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dc.contributor.authorMontano, John W.
dc.contributor.authorGuo, Hengxiao
dc.contributor.authorBarth, Aaron J.
dc.contributor.authorU, Vivian
dc.contributor.authorRemigio, Raymond
dc.contributor.authorGonzález-Buitrago, Diego H.
dc.contributor.authorHernández Santisteban, Juan V.
dc.date.accessioned2022-11-18T16:30:06Z
dc.date.available2022-11-18T16:30:06Z
dc.date.issued2022-08-04
dc.identifier282199504
dc.identifier208eea40-ff42-4356-83d7-d19b11e609dd
dc.identifier85135723309
dc.identifier000835956500001
dc.identifier.citationMontano , J W , Guo , H , Barth , A J , U , V , Remigio , R , González-Buitrago , D H & Hernández Santisteban , J V 2022 , ' Optical continuum reverberation in the dwarf Seyfert nucleus of NGC 4395 ' , Astrophysical Journal Letters , vol. 934 , no. 2 , L37 . https://doi.org/10.3847/2041-8213/ac7e54en
dc.identifier.issn2041-8205
dc.identifier.otherRIS: urn:2EA0328DA8FDCCB34032A5C60F144A5B
dc.identifier.otherORCID: /0000-0002-6733-5556/work/123196916
dc.identifier.urihttps://hdl.handle.net/10023/26437
dc.descriptionFunding information: LCO telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This Letter is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. Research at UC Irvine was supported by NSF grant AST-1907290. D.H.G.-B. acknowledges CONACYT support #319800. J.V.H.S. acknowledges support from STFC grant ST/R000824/1.en
dc.description.abstractIn order to constrain the size of the optical continuum emission region in the dwarf Seyfert 1 galaxy NGC 4395 through reverberation mapping, we carried out high-cadence photometric monitoring in the griz filter bands on two consecutive nights in 2022 April using the four-channel MuSCAT3 camera on the Faulkes Telescope North at Haleakalā Observatory. Correlated variability across the griz bands is clearly detected, and the r-, i-, and z-band light curves show lags of - + 7.72 +1.01 -1.09, 14.16 +1.22-1.25, and 20.78  +1.99-2.09 minutes with respect to the g band when measured using the full-duration light curves. When lags are measured for each night separately, the Night 2 data exhibit lower cross-correlation amplitudes and shorter lags than the Night 1 light curves. Using the full-duration lags, we find that the lag–wavelength relationship is consistent with the τ ∝ λ4/3 dependence found for more luminous active galactic nuclei. Combining our results with continuum lags measured for other objects, the lag between g and z band scales with optical continuum luminosity as τgz ∝ L0.56±0.05, similar to the scaling of broad-line region size with luminosity, reinforcing recent evidence that diffuse continuum emission from the broad-line region may contribute substantially to optical continuum variability and reverberation lags.
dc.format.extent6
dc.format.extent675333
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectDASen
dc.subjectMCCen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleOptical continuum reverberation in the dwarf Seyfert nucleus of NGC 4395en
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.3847/2041-8213/ac7e54
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/R00824/1en


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