Extinction and the dimming of KIC 8462852

Huan Y.A. Meng, George Rieke, Franky Dubois, Grant Kennedy, Massimo Marengo, Michael Siegel, Kate Su, Nicolas Trueba, Mark Wyatt, Tabetha Boyajian, C. M. Lisse, Ludwig Logie, Steve Rau, Sigfried Vanaverbeke

Research output: Contribution to journalArticlepeer-review

Abstract

To test alternative hypotheses for the behavior of KIC 8462852, we obtained measurements of the star over a wide wavelength range from the UV to the mid-infrared from October 2015 through December 2016, using Swift, Spitzer and at AstroLAB IRIS. The star faded in a manner similar to the long-term fading seen in Kepler data about 1400 days previously. The dimming rate for the entire period reported is 22.1 ± 9.7 milli-mag yr1 in the Swift wavebands, with amounts of 21.0 ± 4.5 mmag in the groundbased B measurements, 14.0 ± 4.5 mmag in V , and 13.0 ± 4.5 in R, and a rate of 5.0 ± 1.2 mmag yr1 averaged over the two warm Spitzer bands. Although the dimming is small, it is seen at & 3 σ by three different observatories operating from the UV to the IR. The presence of long-term secular dimming means that previous SED models of the star based on photometric measurements taken years apart may not be accurate. We find that stellar models with Teff = 7000 - 7100 K and AV ∼ 0.73 best fit the Swift data from UV to optical. These models also show no excess in the near-simultaneous Spitzer photometry at 3.6 and 4.5 µm, although a longer wavelength excess from a substantial debris disk is still possible (e.g., as around Fomalhaut). The wavelength dependence of the fading favors a relatively neutral color (i.e., RV & 5, but not flat across all the bands) compared with the extinction law for the general ISM (RV = 3.1), suggesting that the dimming arises from circumstellar material.

Original languageEnglish (US)
JournalUnknown Journal
StatePublished - Aug 24 2017

Keywords

  • Circumstellar matter
  • Dust, extinction
  • Individual (KIC 8462852)
  • Peculiar — stars
  • Stars

ASJC Scopus subject areas

  • General

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