Optical Seti Observations of the Anomalous Star Kic 8462852

Schuetz, Marlin; Vakoch, Douglas A.; Shostak, Seth; Richards, J.

doi:10.3847/2041-8205/825/1/l5

Cited by 56 publications

(28 citation statements)

References 21 publications

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“…KIC 8462852 is a peculiar and intriguing source that caught a lot of attention from the astronomic community in the recent years (Boyajian et al 2016;Montet & Simon 2016;Lisse et al 2015;Wright & Sigurdsson 2016;Bodman & Quillen 2016;Harp et al 2016;Schaefer 2016;Makarov & Goldin 2016;Schuetz et al 2016;Thompson et al 2016;Abeysekara et al 2016;Marengo, et al 2015;Hippke et al 2016;Neslušan & Budaj 2017). KIC 8462852 is an F3V star located at about 454±35 pc away from us (Hippke et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Detection of a repeated transit signature in the light curve of the enigma star KIC 8462852: A possible 928-day period

Kiefer

Étangs

Vidal‐Madjar

et al. 2017

A&A

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As revealed by its peculiar Kepler light curve, the enigmatic star KIC 8462852 undergoes short and deep flux dimmings at a priori unrelated epochs. It presents nonetheless all other characteristics of a quiet 1 Gyr old F3V star. These dimmings resemble the absorption features expected for the transit of dust cometary tails. The exocomet scenario is therefore most commonly advocated. We reanalyzed the Kepler data and extracted a new high-quality light curve to allow for the search of shallow signature of single or a few exocomets. We discovered that among the 22 flux dimming events that we identified, two events present a striking similarity. These events occurred 928.25 days apart, lasted for 4.4 days with a drop of the star brightness by 1000 ppm. We show that the light curve of these events is well explained by the occultation of the star by a giant ring system, or the transit of a string of half a dozen of exocomets with a typical dust production rate of 10 5 -10 6 kg/s. Assuming that these two similar events are related to the transit of the same object, we derive a period of 928.25 days. The following transit was expected in March 2017 but bad weather prohibited us to detect it from ground-based spectroscopy. We predict that the next event will occur from the 3 rd to the 8 th of October 2019.

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Section: Introductionmentioning

confidence: 99%

Detection of a repeated transit signature in the light curve of the enigma star KIC 8462852: A possible 928-day period

Kiefer

Étangs

Vidal‐Madjar

et al. 2017

A&A

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show abstract

“…Therefore, the Harp et al (2016) and Schuetz et al (2016) limited observation times and wavelength coverage are not sufficient to produce firm conclusions on power beaming from KIC 8462852. Most applications would be seen in the radio-if transmissions were oriented in our direction at the proper time and at the frequencies observed-but are not.…”

Section: Power Beaming From Kic 8462852?mentioning

confidence: 98%

“…In addition to radio measurements, an optical SETI measurement has been conducted toward KIC 8462852 using the Boquete observatory (Schuetz et al 2016). Its photomultiplier detector has a detection threshold of 67 photons m −2 using a 25 ns gate time.…”

Section: Power Beaming From Kic 8462852?mentioning

confidence: 99%

Power Beaming Leakage Radiation as a Seti Observable

Benford

2016

ApJ

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The most observable leakage radiation from an advanced civilization may well be from the use of power beaming to transfer energy and accelerate spacecraft. Applications suggested for power beaming involve launching spacecraft to orbit, raising satellites to a higher orbit, and interplanetary concepts involving space-to-space transfers of cargo or passengers. We also quantify beam-driven launch to the outer solar system, interstellar precursors, and ultimately starships. We estimate the principal observable parameters of power beaming leakage. Extraterrestrial civilizations would know their power beams could be observed, and so could put a message on the power beam and broadcast it for our receipt at little additional energy or cost. By observing leakage from power beams we may find a message embedded on the beam. Recent observations of the anomalous star KIC 8462852 by the Allen Telescope Array (ATA) set some limits on extraterrestrial power beaming in that system. We show that most power beaming applications commensurate with those suggested for our solar system would be detectable if using the frequency range monitored by the ATA, and so the lack of detection is a meaningful, if modest, constraint on extraterrestrial power beaming in that system. Until more extensive observations are made, the limited observation time and frequency coverage are not sufficiently broad in frequency and duration to produce firm conclusions. Such beams would be visible over large interstellar distances. This implies a new approach to the SETI search: instead of focusing on narrowband beacon transmissions generated by another civilization, look for more powerful beams with much wider bandwidth. This requires a new approach for their discovery by telescopes on Earth. Further studies of power beaming applications should be performed, potentially broadening the parameter space of the observable features that we have discussed here.

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“…Observations have mostly focused on FGK stars and individual objects, such as the anomalous star KIC 8462852 (Schuetz et al 2016;Abeysekara et al 2016), and exoplanet host stars Trappist-1, GJ 422 and Wolf 1061 (Welsh et al 2018).…”

Section: Previous Searchesmentioning

confidence: 99%

Interstellar communication: Short pulse duration limits of optical SETI

Hippke

2018

J Astrophys Astron

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Previous and ongoing searches for extraterrestrial optical and infrared nanosecond laser pulses and narrow line-width continuous emissions have so far returned null results. At the commonly used observation cadence of ∼ 10 −9 s, sky-integrated starlight is a relevant noise source for large field-of-view surveys. This can be reduced with narrow bandwidth filters, multipixel detectors, or a shorter observation cadence. We examine the limits of short pulses set by the uncertainty principle, interstellar scattering, atmospheric scintillation, refraction, dispersion and receiver technology. We find that optimal laser pulses are time-bandwidth limited Gaussians with a duration of ∆t ≈ 10 −12 s at a wavelength λ 0 ≈ 1 µm, and a spectral width of ∆λ ≈ 1.5 nm. Shorter pulses are too strongly affected through Earth's atmosphere. Given certain technological advances, survey speed can be increased by three orders of magnitude when moving from ns to ps pulses. Faster (and/or parallel) signal processing would allow for an all-sky-at-once survey of lasers targeted at Earth.

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Optical Seti Observations of the Anomalous Star Kic 8462852

Cited by 56 publications

References 21 publications

Detection of a repeated transit signature in the light curve of the enigma star KIC 8462852: A possible 928-day period

Detection of a repeated transit signature in the light curve of the enigma star KIC 8462852: A possible 928-day period

Power Beaming Leakage Radiation as a Seti Observable

Interstellar communication: Short pulse duration limits of optical SETI

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