Variability in IC5070: Two Young Stars with Deep Recurring Eclipses*

Froebrich, D.; Scholz, A.; Campbell-White, J.; Crumpton, James; D'Arcy, Emma; Makin, S. V.; Zegmott, Tarik; Billington, S. J.; Hibbert, R.; Newport, Robert J.; Fisher, Callum

doi:10.3847/2515-5172/aacd48

Cited by 5 publications

(5 citation statements)

References 9 publications

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“…C1, C2 in Appendix C in the online supplementary material. We can identify that V1490 Cyg exhibits a clear quasi-periodic behaviour for the broadband filters V, R c and I c , with a period of approximately 31.5 days, in agreement with Froebrich et al (2018a).…”

Section: Resultssupporting

confidence: 83%

“…It has been classified as a low mass YSO and emission studied by Ibryamov et al (2018), who do not report any periodicity. Froebrich et al (2018a) investigate the source and determine a period of approximately 31.8 days in the V-Band. In the analysis of HOYS data by Froebrich et al (2018b) it was classified as one of the most variable sources, grouped into the extreme dipper category.…”

Section: Resultsmentioning

confidence: 99%

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A survey for variable young stars with small telescopes: II -- Mapping a protoplanetary disk with stable structures at 0.15 AU

Evitts,

Froebrich,

Scholz

et al. 2020

Preprint

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The HOYS citizen science project conducts long term, multifilter, high cadence monitoring of large YSO samples with a wide variety of professional and amateur telescopes. We present the analysis of the light curve of V1490 Cyg in the Pelican Nebula. We show that colour terms in the diverse photometric data can be calibrated out to achieve a median photometric accuracy of 0.02 mag in broadband filters, allowing detailed investigations into a variety of variability amplitudes over timescales from hours to several years. Using Gaia DR2 we estimate the distance to the Pelican Nebula to be 870 +70 −55 pc. V1490 Cyg is a quasi-periodic dipper with a period of 31.447 ± 0.011 d. The obscuring dust has homogeneous properties, and grains larger than those typical in the ISM. Larger variability on short timescales is observed in U and R c −Hα, with U-amplitudes reaching 3 mag on timescales of hours, indicating the source is accreting. The Hα equivalent width and NIR/MIR colours place V1490 Cyg between CTTS/WTTS and transition disk objects. The material responsible for the dipping is located in a warped inner disk, about 0.15 AU from the star. This mass reservoir can be filled and emptied on time scales shorter than the period at a rate of up to 10 −10 M /yr, consistent with low levels of accretion in other T Tauri stars. Most likely the warp at this separation from the star is induced by a protoplanet in the inner accretion disk. However, we cannot fully rule out the possibility of an AA Tau-like warp, or occultations by the Hill sphere around a forming planet.

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Section: Resultssupporting

confidence: 83%

Section: Resultsmentioning

confidence: 99%

A survey for variable young stars with small telescopes: II -- Mapping a protoplanetary disk with stable structures at 0.15 AU

Evitts,

Froebrich,

Scholz

et al. 2020

Preprint

Self Cite

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“…The variable YSO sample with long-term time-series photometry in IC5070 is very limited (Findeisen et al 2013;Poljančić et al 2014;Ibryamov et al 2018;Froebrich et al 2018, as discussed in Section 1). Therefore, a number of our targets are new variable sources identified in the IC 5070.…”

Section: Variability Search and Period Determinationmentioning

confidence: 99%

“…However, the long-term optical photometric studies of PMS stars in these regions are available only for a limited sample (Kóspál et al 2011;Findeisen et al 2013;Poljančić et al 2014;Ibryamov et al 2018, and references within). The BVRI photometry for a sample of 17 PMS objects was presented by Poljančić et al (2014) in the field of North American and Pelican Nebulae while Froebrich et al (2018) found two new low-mass young stars with deep recurring eclipses in IC 5070.…”

Section: Introductionmentioning

confidence: 99%

Variability of young stellar objects in the star-forming region Pelican Nebula

Bhardwaj

Panwar

Herczeg

et al. 2019

A&A

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Context. Pre-main-sequence variability characteristics are useful to probe the physical processes leading to the formation and initial evolution of both stars and planets. Aims. Photometric variability of pre-main-sequence stars is studied at optical wavelengths to explore star-disk interactions, accretion, spots and other physical mechanisms associated with young stellar objects. Methods. We observed a field of 16 × 16 in the star-forming region Pelican Nebula (IC 5070) at BVRI wavelengths for 90 nights spread over one year in 2012-2013. More than 250 epochs in VRI-bands are used to identify and classify variables up to V ∼ 21 mag. Their physical association with the cluster IC 5070 is established based on the parallaxes and proper motions from the Gaia second data release. Multiwavelength photometric data are used to estimate physical parameters based on the isochrone fitting and spectral energy distributions. Results. We present a catalogue of optical time-series photometry with periods, mean-magnitudes and classifications for 95 variable stars including 67 pre-main-sequence variables towards star-forming region IC 5070. The pre-main-sequence variables are further classified as candidate classical T Tauri and weak-line T Tauri stars based on their light curve variations and the locations on the color-color and color-magnitude diagrams using optical and infrared data together with Gaia DR2 astrometry. Classical T Tauri stars display variability amplitudes up to three times the maximum fluctuation in disk-free weak-line T Tauri stars, which show strong periodic variations. Short-term variability is missed in our photometry within single nights. Several classical T Tauri stars display long-lasting (≥ 10 days) single or multiple fading and brightening events up to a couple of magnitudes at optical wavelengths. The typical mass and age of the pre-main-sequence variables from the isochrone-fitting and spectral energy distributions are estimated to be ≤ 1 M and ∼ 2 Myr, respectively. We do not find any correlation between the optical amplitudes or periods with the physical parameters (mass and age) of pre-main-sequence stars. Conclusions. The low-mass pre-main-sequence stars in the Pelican Nebula region display distinct variability and color trends and nearly 30% variables exhibit strong periodic signatures attributed to cold spot modulations. In case of accretion bursts and extinction events, the average amplitudes are larger than one magnitude at optical wavelengths. These optical magnitude fluctuations are stable over the year-long time-scale.

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“…The Gulf of Mexico is located in the active star-forming complex NGC 7000/IC 5070 and contains many young stellar objects as emission line stars, flare stars, T Tauri variables, and Herbig Ae/Be stars. Results from recent studies of objects in the complex NGC 7000/IC 5070 have been published in Armond et al (2011), Findeisen et al (2013), Bally et al (2014), Poljančić Beljan et al (2014, Ibryamov et al (2015a), Semkov et al (2017), Giannini et al (2018), Ibryamov et al (2018a), Ibryamov et al (2018b), Froebrich et al (2018, Bhardwaj et al (2019), etc.…”

Section: Introductionmentioning

confidence: 99%

New four-color optical photometry of the young stars V521 Cyg and FHO 27

Ibryamov,

Semkov

2019

Preprint

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Results from new BV RI photometric observations of the pre-MS stars V521 Cyg and FHO 27 collected during the period from February 2015 to July 2019 are presented. These stars are embedded in the LDN 935, dubbed "The Gulf of Mexico" in the active star-forming complex NGC 7000/IC 5070. Previous studies revealed them as variables with large amplitude brightness variations. Our new observations show that the stars continue to exhibit strong photometric variability and fading events in the brightness. On the basis of the new data received and the data available in the literature, we were able to specify the periodicity in the brightness variations of V521 Cyg. In the case of FHO 27, we found a significant peak in its periodogram corresponding to 893 days period.

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Variability in IC5070: Two Young Stars with Deep Recurring Eclipses*

Cited by 5 publications

References 9 publications

A survey for variable young stars with small telescopes: II -- Mapping a protoplanetary disk with stable structures at 0.15 AU

A survey for variable young stars with small telescopes: II -- Mapping a protoplanetary disk with stable structures at 0.15 AU

Variability of young stellar objects in the star-forming region Pelican Nebula

New four-color optical photometry of the young stars V521 Cyg and FHO 27

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