Tracking the year-to-year variation in the spectral energy distribution of the narrow-line Seyfert 1 galaxy Mrk 335

dc.contributorAalto Universityen
dc.contributor.authorTripathi, S.en_US
dc.contributor.authorMcGrath, K. M.en_US
dc.contributor.authorGallo, L. C.en_US
dc.contributor.authorGrupe, D.en_US
dc.contributor.authorKomossa, S.en_US
dc.contributor.authorBerton, M.en_US
dc.contributor.authorKriss, G.en_US
dc.contributor.authorLonginotti, A. L.en_US
dc.contributor.departmentMetsähovi Radio Observatoryen
dc.contributor.organizationSaint Mary's University Halifaxen_US
dc.contributor.organizationMorehead State Universityen_US
dc.contributor.organizationMax Planck Institute for Radio Astronomyen_US
dc.contributor.organizationSpace Telescope Science Instituteen_US
dc.contributor.organizationInstituto Nacional de Astrofísica, Óptica y Electrónicaen_US
dc.description.abstractMultiwavelength monitoring of Mrk 335 with Swift between 2007 and 2019 are used to construct annual spectral energy distributions (SEDs) and track year-to-year changes. Non-contemporaneous archival data prior to 2007 are used to build a bright state SED. In this work, the changes are examined and quantified to build the foundation for future SED modelling. The yearly SEDs trace a downward trend on the average, with the X-ray portion varying significantly and acquiring further lower values in the past two years when compared to the optical/UV portion of SED. The bolometric Eddington ratios derived using optical/UV to X-ray SEDs and the calculated X-ray luminosities show a gradual decrease over the monitoring period. Changes in the parameters over time are examined. Principal component analysis suggests that the primary variability is in the X-ray properties of Mrk 335. When looking at the broader picture of Mrk 335 and its behaviour, the X-rays, accounting most of the variability in the 13-yr data, are possibly driven by physical processes related to the corona or absorption whereas the modest optical-UV variations suggest their origin within the accretion disc. These results are consistent with the previous interpretation of Mrk 335 using the timing analyses on the monitoring data and spectral modelling of deep observations.en
dc.description.versionPeer revieweden
dc.identifier.citationTripathi, S, McGrath, K M, Gallo, L C, Grupe, D, Komossa, S, Berton, M, Kriss, G & Longinotti, A L 2020, ' Tracking the year-to-year variation in the spectral energy distribution of the narrow-line Seyfert 1 galaxy Mrk 335 ', Monthly Notices of the Royal Astronomical Society, vol. 499, no. 1, pp. 1266-1286 .
dc.identifier.otherPURE UUID: 08a28bdb-0b9b-47cf-a030-a2a9b4af015aen_US
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dc.relation.ispartofseriesMonthly Notices of the Royal Astronomical Societyen
dc.relation.ispartofseriesVolume 499, issue 1en
dc.subject.keywordGalaxies: activeen_US
dc.subject.keywordGalaxies: individual: Mrk 335en_US
dc.subject.keywordGalaxies: nucleien_US
dc.subject.keywordX-rays: galaxiesen_US
dc.titleTracking the year-to-year variation in the spectral energy distribution of the narrow-line Seyfert 1 galaxy Mrk 335en
dc.typeA1 Alkuperäisartikkeli tieteellisessä aikakauslehdessäfi