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A survey for variable young stars with small telescopes – IV. Rotation periods of YSOs in IC 5070

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Date
01/10/2021
Author
Froebrich, Dirk
Derezea, Efthymia
Scholz, Aleks
Eislöffel, Jochen
Vanaverbeke, Siegfried
Kume, Alfred
Herbert, Carys
Campbell-White, Justyn
Miller, Niall
Stecklum, Bringfried
Makin, Sally V
Urtly, Thomas
Soldán Alfaro, Francisco C
Schwendeman, Erik
Stone, Geoffrey
Phillips, Mark
Fleming, George
Gonzalez Farfán, Rafael
Vanmunster, Tonny
Heald, Michael A
Fernández Mañanes, Esteban
Nelson, Tim
Eggenstein, Heinz-Bernd
Dubois, Franky
Logie, Ludwig
Rau, Steve
Wiersema, Klaas
Quinn, Nick
Rodriguez, Diego
Castillo García, Rafael
Killestein, Thomas
Vale, Tony
Licchelli, Domenico
Deldem, Marc
Piehler, Georg
Moździerski, Dawid
Kotysz, Krzysztof
Kowalska, Katarzyna
Mikołajczyk, Przemysław
Futcher, Stephen R L
Long, Timothy P
Morales Aimar, Mario
Merrikin, Barry
Johnstone, Stephen
Dubovský, Pavol A
Kudzej, Igor
Pickard, Roger
Billington, Samuel J
Dover, Lord
Zegmott, Tarik
Evitts, Jack J
Traspas Munia, Alejandra
Price, Mark C
Keywords
Stars: formation
Stars: pre-main-sequence
Stars: rotation
Stars: variables: T Tauri
Herbig Ae/Be
QB Astronomy
QC Physics
3rd-DAS
MCC
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Abstract
Studying rotational variability of young stars is enabling us to investigate a multitude of properties of young star-disc systems. We utilize high cadence, multiwavelength optical time series data from the Hunting Outbursting Young Stars citizen science project to identify periodic variables in the Pelican Nebula (IC 5070). A double blind study using nine different period-finding algorithms was conducted and a sample of 59 periodic variables was identified. We find that a combination of four period finding algorithms can achieve a completeness of 85 per cent and a contamination of 30 per cent in identifying periods in inhomogeneous data sets. The best performing methods are periodograms that rely on fitting a sine curve. Utilizing Gaia EDR3 data, we have identified an unbiased sample of 40 periodic young stellar objects (YSOs), without using any colour or magnitude selections. With a 98.9 per cent probability, we can exclude a homogeneous YSO period distribution. Instead, we find a bi-modal distribution with peaks at 3 and 8 d. The sample has a disc fraction of 50 per cent, and its statistical properties are in agreement with other similarly aged YSOs populations. In particular, we confirm that the presence of the disc is linked to predominantly slow rotation and find a probability of 4.8 × 10−3 that the observed relation between period and presence of a disc has occurred by chance. In our sample of periodic variables, we also find pulsating giants, an eclipsing binary, and potential YSOs in the foreground of IC 5070.
Citation
Froebrich , D , Derezea , E , Scholz , A , Eislöffel , J , Vanaverbeke , S , Kume , A , Herbert , C , Campbell-White , J , Miller , N , Stecklum , B , Makin , S V , Urtly , T , Soldán Alfaro , F C , Schwendeman , E , Stone , G , Phillips , M , Fleming , G , Gonzalez Farfán , R , Vanmunster , T , Heald , M A , Fernández Mañanes , E , Nelson , T , Eggenstein , H-B , Dubois , F , Logie , L , Rau , S , Wiersema , K , Quinn , N , Rodriguez , D , Castillo García , R , Killestein , T , Vale , T , Licchelli , D , Deldem , M , Piehler , G , Moździerski , D , Kotysz , K , Kowalska , K , Mikołajczyk , P , Futcher , S R L , Long , T P , Morales Aimar , M , Merrikin , B , Johnstone , S , Dubovský , P A , Kudzej , I , Pickard , R , Billington , S J , Dover , L , Zegmott , T , Evitts , J J , Traspas Munia , A & Price , M C 2021 , ' A survey for variable young stars with small telescopes – IV. Rotation periods of YSOs in IC 5070 ' , Monthly Notices of the Royal Astronomical Society , vol. 506 , no. 4 , pp. 5989-6000 . https://doi.org/10.1093/mnras/stab2082
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stab2082
ISSN
0035-8711
Type
Journal article
Rights
Copyright 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stab2082.
Description
Funding: AS acknowledges support through STFC grant ST/R000824/1. JCW acknowledges support through STFC grant ST/S000399/1. This research was partially supported by the supercomputing infrastructure of the National Laboratory for High Performance Computing (NLHPC) (ECM-02).
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/24057

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