“π of the Sky” – automated search for fast optical transients over the whole sky

Burd, Aleksander; Ćwiok, M.; Czyrkowski, H.; Dąbrowski, R.; Dominik, W.; Grajda, Marcin; Jegier, M.; Kasprowicz, G.; Mankiewicz, L.; Nawrocki, K.; Pilecki, B.; Piotrowski, L. W.; Poźniak, Krzysztof T.; Romaniuk, Ryszard S.; Salanski, Rafal; Sokołowski, M.; Stankiewicz, S.; Szczygiel, D.; Wrochna, G.

doi:10.1002/asna.200410327

Cited by 26 publications

(5 citation statements)

References 2 publications

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“…After a quick inspection, released data for CzeV502 from the Lincoln Near-Earth Asteroid Research (LINEAR, Sesar et al 2011) and Pi of the Sky databases (Burd et al 2004) were found to be unusable for our purpose due to poor quality; CzeV502 is probably too bright (LINEAR) or too faint (Pi of the sky). On the other hand, data in ASAS-3 12 (Pojmanski 2002), the Northern Sky Variability Survey (NSVS, Woźniak et al 2004), the Catalina Real-time Transient Survey (CRTS, Drake et al 2009), the Kamogata/Kiso/Kyoto Wide-field Survey (KWS) 13 , and ASAS-SN (Shappee et al 2014;Kochanek et al 2017) are quite homogeneous, and we identified several bright points which may indicate flares (one in ASAS-3, two in NSVS, eleven in CRTS, one in KWS, four in ASAS-SN).…”

Section: Sky Surveysmentioning

confidence: 99%

Czev502 – An M Dwarf Near the Leo Triplet With Very Strong Flares

Liška

Hudec

Mikulasek

et al. 2022

RMxAA

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Discovery of flares in the M dwarf CzeV502 and our follow-up results are presented. We classify it as a dMe eruptive variable of UV Ceti type due to the X-ray activity, measured B − V of 1.5 mag, Hα; emission, and flares. Our monitoring revealed only one reliable and one suspected superflare in 58 nights (210 hrs). The strongest flare with ΔR = 1.5 mag (ΔB ≈ 6-8 mag) could have a total energy of 3E+34 erg. The ASAS-SN data may contain 4 events up to ΔV of 0.43 mag and 12.55 d periodicity corresponding to the rotation or possible binarity. Other brightenings in sky survey (ASAS-3, CRTS, NSVS, and KWS) are doubtful. No event was unveiled on the 1 600 photographic plates. The upper rate limit of 1-2 superflares/1 640 hrs corresponds to activity several orders higher than for other M-dwarfs, especially, for the slow rotators. The low amplitude flares ( ΔB < 0.5 mag) may be common (1 flare/4 hrs).

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Section: Sky Surveysmentioning

confidence: 99%

Czev502 – An M Dwarf Near the Leo Triplet With Very Strong Flares

Liška

Hudec

Mikulasek

et al. 2022

RMxAA

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“…Burd et al 2004;Siudek et al 2011) to determine maximum timings from the individual well-covered nights.…”

Section: Other Sourcesmentioning

confidence: 99%

“…We used high-cadence measurements from the SuperWASP project (Pollacco et al 2006;Butters et al 2010) and Pi of the Sky project (e.g. Burd et al 2004;Siudek et al 2011) to determine maximum timings from the individual wellcovered nights.…”

Section: Other Sourcesmentioning

confidence: 99%

New analysis of the light time effect in TU Ursae Majoris

Liška

Skarka

Mikulášek

et al. 2016

A&A

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Context. Recent statistical studies prove that the percentage of RR Lyrae pulsators that are located in binaries or multiple stellar systems is considerably lower than might be expected. This can be better understood from an in-depth analysis of individual candidates. We investigate in detail the light time effect of the most probable binary candidate TU UMa. This is complicated because the pulsation period shows secular variation. Aims. We model possible light time effect of TU UMa using a new code applied on previously available and newly determined maxima timings to confirm binarity and refine parameters of the orbit of the RRab component in the binary system. The binary hypothesis is also tested using radial velocity measurements. Methods. We used new approach to determine brightness maxima timings based on template fitting. This can also be used on sparse or scattered data. This approach was successfully applied on measurements from different sources. To determine the orbital parameters of the double star TU UMa, we developed a new code to analyse light time effect that also includes secular variation in the pulsation period. Its usability was successfully tested on CL Aur, an eclipsing binary with mass-transfer in a triple system that shows similar changes in the O-C diagram. Since orbital motion would cause systematic shifts in mean radial velocities (dominated by pulsations), we computed and compared our model with centre-of-mass velocities. They were determined using high-quality templates of radial velocity curves of RRab stars. Results. Maxima timings adopted from the GEOS database (168) together with those newly determined from sky surveys and new measurements (85) were used to construct an O-C diagram spanning almost five proposed orbital cycles. This data set is three times larger than data sets used by previous authors. Modelling of the O-C dependence resulted in 23.3-yr orbital period, which translates into a minimum mass of the second component of about 0.33 M . Secular changes in the pulsation period of TU UMa over the whole O-C diagram were satisfactorily approximated by a parabolic trend with a rate of −2.2 ms yr −1 . To confirm binarity, we used radial velocity measurements from nine independent sources. Although our results are convincing, additional long-term monitoring is necessary to unambiguously confirm the binarity of TU UMa.

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“…SPIE. Wilga Symposium enjoys the patronage of Committee of Electronics and Telecommunications of the Polish Academy of Science [1] [2][3][4][5][6][7][8] has always several sessions on photonics [9][10][11][12][13][14][15][16], astronomy and astroparticle physics [17], large research experiments including high energy particle physics, hot plasma fusion energy, free electron lasers and large accelerator infrastructures [18][19][20][21][22][23][24][25][26]. R.S.Romaniuk is with the Institute of Electronic Systems, Warsaw University of Technology, Poland (e-mail: R.Romaniuk@ise.pw.edu.pl).…”

Section: Introductionmentioning

confidence: 99%

International Journal of Electronics and Telecommunications

Romaniuk

2018

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“π of the Sky” – automated search for fast optical transients over the whole sky

Cited by 26 publications

References 2 publications

Czev502 – An M Dwarf Near the Leo Triplet With Very Strong Flares

Czev502 – An M Dwarf Near the Leo Triplet With Very Strong Flares

New analysis of the light time effect in TU Ursae Majoris

International Journal of Electronics and Telecommunications

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