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dc.contributor.authorTanaka, M-
dc.contributor.authorMorokuma, T-
dc.contributor.authorItoh, R-
dc.contributor.authorAkitaya, H-
dc.contributor.authorTominaga, N-
dc.contributor.authorSaito, Y-
dc.contributor.authorStawarz, L-
dc.contributor.authorTanaka, Y, T-
dc.contributor.authorGandhi, P-
dc.contributor.authorAli, G-
dc.contributor.authorAoki, T-
dc.contributor.authorContreras, C-
dc.contributor.authorDoi, M-
dc.contributor.authorEssam, A-
dc.contributor.authorHamed, G-
dc.contributor.authorHsiao, E. Y-
dc.contributor.authorIwata, I-
dc.contributor.authorKawabata, K. S-
dc.contributor.authorKawai, N-
dc.contributor.authorKikuchi, Y-
dc.contributor.authorKobayashi, N-
dc.contributor.authorKuroda, D-
dc.contributor.authorMaehara, H-
dc.contributor.authorMatsumoto, E-
dc.contributor.authorMazzali, P. A-
dc.contributor.authorMinezaki, T-
dc.contributor.authorMito, H-
dc.contributor.authorMiyata, T-
dc.contributor.authorMiyazaki, S-
dc.contributor.authorMori, K-
dc.contributor.authorMoritani, Y-
dc.contributor.authorMorokuma-Matsui, Kana-
dc.contributor.authorMorrell, N-
dc.contributor.authorNagao, T-
dc.contributor.authorNakada, Y-
dc.contributor.authorNakata, F-
dc.contributor.authorNoma, C-
dc.contributor.authorOhsuga, K-
dc.contributor.authorOkada, N-
dc.contributor.authorPhillips, M. M-
dc.contributor.authorPian, E-
dc.contributor.authorRichmond, M. W-
dc.contributor.authorSahu, D. K-
dc.contributor.authorSako, S-
dc.contributor.authorSarugaku, Y-
dc.contributor.authorShibata, T-
dc.contributor.authorSoyano, T-
dc.contributor.authorStritzinger, M. D-
dc.contributor.authorTachibana, Y-
dc.contributor.authorTaddia, F-
dc.contributor.authorTakaki, K-
dc.contributor.authorTakey, Ali-
dc.contributor.authorTarusawa, K-
dc.contributor.authorUi, T-
dc.contributor.authorUkita, N-
dc.contributor.authorUrata, Y-
dc.contributor.authorWalker, E. S-
dc.contributor.authorYoshii, T-
dc.identifier.citationThe Astrophysical Journal Letters, Vol. 793, No. 2, L26en
dc.descriptionRestricted Accessen
dc.description.abstractWe present our discovery of dramatic variability in SDSS J1100+4421 by the high-cadence transient survey Kiso Supernova Survey. The source brightened in the optical by at least a factor of three within about half a day. Spectroscopic observations suggest that this object is likely a narrow-line Seyfert 1 galaxy (NLS1) at z = 0.840, however, with unusually strong narrow emission lines. The estimated black hole mass of ~107 M ☉ implies bolometric nuclear luminosity close to the Eddington limit. SDSS J1100+4421 is also extremely radio-loud, with a radio loudness parameter of R sime 4 × 102-3 × 103, which implies the presence of relativistic jets. Rapid and large-amplitude optical variability of the target, reminiscent of that found in a few radio- and γ-ray-loud NLS1s, is therefore produced most likely in a blazar-like core. The 1.4 GHz radio image of the source shows an extended structure with a linear size of about 100 kpc. If SDSS J1100+4421 is a genuine NLS1, as suggested here, this radio structure would then be the largest ever discovered in this type of active galaxies.en
dc.publisherIOP Publishingen
dc.rights© IOP Publishingen
dc.subjectGalaxies: activeen
dc.subjectGalaxies: individual (SDSS J110006.07+442144.3)en
dc.subjectGalaxies: jetsen
dc.subjectGalaxies: Seyferten
dc.titleDiscovery of Dramatic Optical Variability in SDSS J1100+4421: A Peculiar Radio-loud Narrow-line Seyfert 1 Galaxy?en
Appears in Collections:IIAP Publications

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