학술논문

The First Post-Kepler Brightness Dips of KIC 8462852
Document Type
Working Paper
Author
Boyajian, Tabetha S.Alonso, RoiAmmerman, AlexArmstrong, DavidRamos, A. AsensioBarkaoui, K.Beatty, Thomas G.Benkhaldoun, Z.Benni, PaulBentley, RoryBerdyugin, AndreiBerdyugina, SvetlanaBergeron, SergeBieryla, AllysonBlain, Michaela G.Blanco, Alicia CapetilloBodman, Eva H. L.Boucher, AnneBradley, MarkBrincat, Stephen M.Brink, Thomas G.Briol, JohnBrown, David J. A.Budaj, J.Burdanov, A.Cale, B.Carbo, Miguel AznarGarcia, R. CastilloClark, Wendy JClayton, Geoffrey C.Clem, James L.Coker, Phillip HCook, Evan M.Copperwheat, Chris M.Curtis, J.Cutri, R. M.Cseh, B.Cynamon, C. H.Daniels, Alex J.Davenport, James R. A.Deeg, Hans J.De Lorenzo, RobertoDe Jaeger, ThomasDesrosiers, Jean-BrunoDolan, JohnDowhos, D. J.Dubois, FrankyDurkee, R.Dvorak, ShawnEasley, LynnEdwards, N.Ellis, Tyler G.Erdelyi, EmeryErtel, SteveFarfán, Rafael. G.Farihi, J.Filippenko, Alexei V.Foxell, EmmaGandolfi, DavideGarcia, FaustinoGiddens, F.Gillon, M.González-Carballo, Juan-LuisGonzález-Fernández, C.Hernández, J. I. GonzálezGraham, Keith A.Greene, Kenton A.Gregorio, J.Hallakoun, Na'amaHanyecz, OttóHarp, G. R.Henry, Gregory W.Herrero, E.Hildbold, Caleb F.Hinzel, D.Holgado, G.Ignácz, BernadettIvanov, Valentin D.Jehin, E.Jermak, Helen E.Johnston, SteveKafka, S.Kalup, CsillaKardasis, EmmanuelKaspi, ShaiKennedy, Grant M.Kiefer, F.Kielty, C. L.Kessler, DennisKiiskinen, H.Killestein, T. L.King, Ronald A.Kollar, V.Korhonen, H.Kotnik, C.Könyves-Tóth, RékaKriskovics, LeventeKrumm, NathanKrushinsky, VadimKundra, E.Lachapelle, Francois-ReneLacourse, D.Lake, P.Lam, KristineLamb, Gavin P.Lane, DaveLau, Marie WingyeeLewin, PabloLintott, ChrisLisse, CareyLogie, LudwigLongeard, NicolasVillanueva, M. LopezLudington, E. WhitMainzer, A.Malo, LisonMaloney, ChrisMann, A.Mantero, A.Marengo, MassimoMarchant, JonGonzález, M. J. MartinezMasiero, Joseph R.Mauerhan, Jon C.Mccormac, JamesMcneely, AaronMeng, Huan Y. A.Miller, MikeMolnar, Lawrence A.Morales, J. C.Morris, Brett M.Muterspaugh, Matthew W.Nespral, DavidNugent, C. R.Nugent, Katherine M.Odasso, A.O'keeffe, DerekOksanen, A.O'meara, John M.Ordasi, AndrásOsborn, HughOtt, John J.Parks, J. R.Perez, Diego RodriguezPetriew, VancePickard, R.Pál, AndrásPlavchan, P.Plaza, C. WestendorpPollacco, DonNuñez, F. PozoPozuelos, F. J.Rau, SteveRedfield, SethRelles, HowardRibas, I.Richards, JonSaario, Joonas L. O.Safron, Emily J.Sallai, J. MartinSárneczky, KrisztiánSchaefer, Bradley E.Schumer, Clea F.Schwartzendruber, MadisonSiegel, Michael H.Siemion, Andrew P. V.Simmons, Brooke D.Simon, Joshua D.Simón-Diaz, S.Sitko, Michael L.Socas-Navarro, HectorSódor, Á.Starkey, DonnSteele, Iain A.Stone, GeoffStreet, R. A.Sullivan, TriciaSuomela, J.Swift, J. J.Szabó, Gyula M.Szabó, RóbertSzakáts, RóbertSzalai, TamásTanner, Angelle M.Toledo-Padrón, B.Tordai, TamásTriaud, Amaury H. M. J.Turner, Jake D.Ulowetz, Joseph H.Urbanik, MarianVanaverbeke, SiegfriedVanderburg, AndrewVida, KrisztiánVietje, Brad P.Vinkó, JózsefVon Braun, K.Waagen, Elizabeth O.Walsh, DanWatson, Christopher A.Weir, R. C.Wenzel, KlausWilliamson, Michael W.Wright, Jason T.Wyatt, M. C.Zheng, WeikangZsidi, Gabriella
Source
Subject
Astrophysics - Solar and Stellar Astrophysics
Astrophysics - Earth and Planetary Astrophysics
Language
Abstract
We present a photometric detection of the first brightness dips of the unique variable star KIC 8462852 since the end of the Kepler space mission in 2013 May. Our regular photometric surveillance started in October 2015, and a sequence of dipping began in 2017 May continuing on through the end of 2017, when the star was no longer visible from Earth. We distinguish four main 1-2.5% dips, named "Elsie," "Celeste," "Skara Brae," and "Angkor", which persist on timescales from several days to weeks. Our main results so far are: (i) there are no apparent changes of the stellar spectrum or polarization during the dips; (ii) the multiband photometry of the dips shows differential reddening favoring non-grey extinction. Therefore, our data are inconsistent with dip models that invoke optically thick material, but rather they are in-line with predictions for an occulter consisting primarily of ordinary dust, where much of the material must be optically thin with a size scale <<1um, and may also be consistent with models invoking variations intrinsic to the stellar photosphere. Notably, our data do not place constraints on the color of the longer-term "secular" dimming, which may be caused by independent processes, or probe different regimes of a single process.
Comment: 19 pages, 8 figures, accepted for publication in ApJL