The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties

Eleonora Fiorellino; Péter  Ábrahám; Ágnes Kóspál; Mária Kun; Juan M. Alcalá; Alessio Caratti o Garatti; Fernando Cruz-Sáenz de Miera; David García-Álvarez; Teresa Giannini; Sunkyung Park; Michal  Siwak; Máté Szilágyi; Elvira Covino; Gabor Marton; Zsófia Nagy; Brunella Nisini; Zsofia Marianna Szabo; Zsófia Bora; Borbála Cseh; Csilla Kalup; Máté Krezinger; Levente Kriskovics; Waldemar  Ogłoza; András Pál; Ádám Sódor; Eda Sonbas; Róbert  Szakáts; Krisztián Vida; József Vinkó; Lukasz Wyrzykowski; Pawel Zielinski

doi:10.1051/0004-6361/202347777

The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties

Eleonora Fiorellino^*, Péter Ábrahám, Ágnes Kóspál, Mária Kun, Juan M. Alcalá, Alessio Caratti o Garatti, Fernando Cruz-Sáenz de Miera, David García-Álvarez, Teresa Giannini, Sunkyung Park, Michal Siwak, Máté Szilágyi, Elvira Covino, Gabor Marton, Zsófia Nagy, Brunella Nisini, Zsofia Marianna Szabo, Zsófia Bora, Borbála Cseh, Csilla KalupMáté Krezinger, Levente Kriskovics, Waldemar Ogłoza, András Pál, Ádám Sódor, Eda Sonbas, Róbert Szakáts, Krisztián Vida, József Vinkó, Lukasz Wyrzykowski, Pawel Zielinski

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

Context. Gaia18cjb is one of the Gaia-alerted eruptive young star candidates that has been experiencing a slow and strong brightening during the last 13 years, similarly to some FU Orionis-type objects.
Aims. The aim of this work is to derive the young stellar nature of Gaia18cjb and determine its physical and accretion properties to classify its variability.
Methods. We conducted monitoring observations using multi-filter optical and near-infrared (NIR) photometry, as well as NIR spectroscopy. We present an analysis of pre-outburst and outburst optical and IR light curves, color-magnitude diagrams in different bands, the detection of NIR spectral lines, and estimates of both stellar and accretion parameters during the burst.
Results. The optical light curve shows an unusually long (over 8 years) brightening event of 5 mag in the last 13 years, before reaching a plateau indicating that the burst is still ongoing, suggesting a FU Orionis-like (FUor-like) nature. The same outburst is less strong in the IR light curves. The NIR spectra, obtained during the outburst, exhibit emission lines typical of highly accreting low-intermediate mass young stars with typical EX Lupi-type (EXor) features. The spectral index of Gaia18cjb SED classifies it as a Class I in the pre-burst stage and a flat-spectrum young stellar object (YSO) during the burst.
Conclusions. Gaia18cjb is an eruptive YSO that exhibits FUor-like photometric features (in terms of brightening amplitude and length of the burst) as well as EXor-like spectroscopic features and accretion rate. Its nature appears similar to that of V350 Cep and V1647 Ori, which have been classified as objects in between FUors and EXors.

Original language	English
Article number	A160
Number of pages	19
Journal	Astronomy & Astrophysics
Volume	686
Early online date	6 Jun 2024
DOIs	https://doi.org/10.1051/0004-6361/202347777
Publication status	Published - Jun 2024

Keywords

Accretion
Accretion disks
Techniques: imaging spectroscopy
Stars: formation
Stars: low-mass
Stars: pre-main sequence
Stars: protostars

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Fiorellino_2024_AandA_Enigma-of-Gaia18cjb-hybrid-FUor-EXor_CC
Copyright © The Authors 2024. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 1.19 MBLicence: CC BY

https://arxiv.org/abs/2403.08698Licence: CC BY

Gaia18cjb LT, LBT, NTT and GTC spectra
Fiorellino, E. (Creator), Abraham, P. (Creator), Kospal, A. (Creator), Kun, M. (Creator), Alcala, J. M. (Creator), Caratti O Garatti, A. (Creator), Cruz-Saenz De Miera, F. (Creator), Garcia-Alvarez, D. (Creator), Giannini, T. (Creator), Park, S. (Creator), Siwak, M. (Creator), Szilagyi, M. (Creator), Covino, E. (Creator), Marton, G. (Creator), Nagy, Z. (Creator), Nisini, B. (Creator), Szabo, Z. M. (Creator), Bora, Z. (Creator), Cseh, B. (Creator), Kalup, C. (Creator), Krezinger, M. (Creator), Kriskovics, L. (Creator), Ogloza, W. (Creator), Pal, A. (Creator), Sodor, A. (Creator), Sonbas, E. (Creator), Szakats, R. (Creator), Vida, K. (Creator), Vinko, J. (Creator), Wyrzykowski, L. (Creator) & Zielinski, P. (Creator), Centre de Donnees Strasbourg (CDS), 2024
DOI: 10.26093/cds/vizier.36860160
Dataset

Cite this

Fiorellino, E., Ábrahám, P., Kóspál, Á., Kun, M., Alcalá, J. M., Caratti o Garatti, A., Cruz-Sáenz de Miera, F., García-Álvarez, D., Giannini, T., Park, S., Siwak, M., Szilágyi, M., Covino, E., Marton, G., Nagy, Z., Nisini, B., Szabo, Z. M., Bora, Z., Cseh, B., ... Zielinski, P. (2024). The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties. Astronomy & Astrophysics, 686, Article A160. https://doi.org/10.1051/0004-6361/202347777

@article{b89caba3e05740069a1d7828ee6fc4bf,

title = "The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties",

abstract = "Context. Gaia18cjb is one of the Gaia-alerted eruptive young star candidates that has been experiencing a slow and strong brightening during the last 13 years, similarly to some FU Orionis-type objects.Aims. The aim of this work is to derive the young stellar nature of Gaia18cjb and determine its physical and accretion properties to classify its variability.Methods. We conducted monitoring observations using multi-filter optical and near-infrared (NIR) photometry, as well as NIR spectroscopy. We present an analysis of pre-outburst and outburst optical and IR light curves, color-magnitude diagrams in different bands, the detection of NIR spectral lines, and estimates of both stellar and accretion parameters during the burst.Results. The optical light curve shows an unusually long (over 8 years) brightening event of 5 mag in the last 13 years, before reaching a plateau indicating that the burst is still ongoing, suggesting a FU Orionis-like (FUor-like) nature. The same outburst is less strong in the IR light curves. The NIR spectra, obtained during the outburst, exhibit emission lines typical of highly accreting low-intermediate mass young stars with typical EX Lupi-type (EXor) features. The spectral index of Gaia18cjb SED classifies it as a Class I in the pre-burst stage and a flat-spectrum young stellar object (YSO) during the burst.Conclusions. Gaia18cjb is an eruptive YSO that exhibits FUor-like photometric features (in terms of brightening amplitude and length of the burst) as well as EXor-like spectroscopic features and accretion rate. Its nature appears similar to that of V350 Cep and V1647 Ori, which have been classified as objects in between FUors and EXors.",

keywords = "Accretion, Accretion disks, Techniques: imaging spectroscopy, Stars: formation, Stars: low-mass, Stars: pre-main sequence, Stars: protostars",

author = "Eleonora Fiorellino and P{\'e}ter {\'A}brah{\'a}m and {\'A}gnes K{\'o}sp{\'a}l and M{\'a}ria Kun and Alcal{\'a}, {Juan M.} and {Caratti o Garatti}, Alessio and {Cruz-S{\'a}enz de Miera}, Fernando and David Garc{\'i}a-{\'A}lvarez and Teresa Giannini and Sunkyung Park and Michal Siwak and M{\'a}t{\'e} Szil{\'a}gyi and Elvira Covino and Gabor Marton and Zs{\'o}fia Nagy and Brunella Nisini and Szabo, {Zsofia Marianna} and Zs{\'o}fia Bora and Borb{\'a}la Cseh and Csilla Kalup and M{\'a}t{\'e} Krezinger and Levente Kriskovics and Waldemar Og{\l}oza and Andr{\'a}s P{\'a}l and {\'A}d{\'a}m S{\'o}dor and Eda Sonbas and R{\'o}bert Szak{\'a}ts and Kriszti{\'a}n Vida and J{\'o}zsef Vink{\'o} and Lukasz Wyrzykowski and Pawel Zielinski",

note = "Funding: This work has been supported by the project PRIN{\textquoteright}INAF 2019 “Spectroscopically Tracing the Disk Dispersal Evolution (STRADE)” and by the INAF Large Grant 2022 “YSOs Outflow, Disks and Accretion (YODA)”. This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme under grant agreement No 716155 (SACCRED). We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (https://gsaweb.ast.cam. ac.uk/alerts) This work is (partly) based on data obtained with the instrument EMIR, built by a Consortium led by the Instituto de Astrof{\'i}sica de Canarias. EMIR was funded by GRANTECAN and the National Plan of Astronomy and Astrophysics of the Spanish Government. This work is (partly) based on data obtained at the Mount Suhora Observatory, Krakow Pedagogical University, Poland. This work has been supported by the Hungarian National Research, Development and Innovation Office grants OTKA K131508, OTKA K138962, the {\'E}lvonal KKP-143986 and KKP-137523 {\textquoteleft}SeismoLab{\textquoteright} grants of the Hungarian Research, Development and Innovation Office (NKFIH). We acknowledge support from the ESA PRODEX contract nr. 4000132054. KV, LK, ZN, and GM are supported by the Bolyai J{\'a}nos Research Scholarship of the Hungarian Academy of Sciences, KV is supported by the Bolyai+ grant {\'U}NKP22-5-ELTE-1093. Authors acknowledge the financial support of the AustrianHungarian Action Foundation (112{\"o}u1). LK is supported by the Hungarian National Research, Development and Innovation Office grant PD-134784. G.M. acknowledges support from the European Union{\textquoteright}s Horizon 2020 research and innovation programme under grant agreement No. 101004141. This work is supported by the Polish MNiSW grant DIR/WK/2018/12 and the European Union{\textquoteright}s Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON-RadioNet Pilot). Zs.M.Sz. acknowledges funding from a St Leonards scholarship from the University of St Andrews. BZs is supported by the {\'U}NKP-22-2 New National Excellence Program of the Ministry for Culture and Innovation from the source of the National Research, Development and Innovation Fund. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. We acknowledge the Hungarian National Research, Development and Innovation Office grant OTKA FK 146023. FCSM received financial support from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (ERC Starting Grant “Chemtrip”, grant agreement No 949278). This work was also supported by the NKFIH excellence grant TKP2021-NKTA-64.",

year = "2024",

month = jun,

doi = "10.1051/0004-6361/202347777",

language = "English",

volume = "686",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Fiorellino, E, Ábrahám, P, Kóspál, Á, Kun, M, Alcalá, JM, Caratti o Garatti, A, Cruz-Sáenz de Miera, F, García-Álvarez, D, Giannini, T, Park, S, Siwak, M, Szilágyi, M, Covino, E, Marton, G, Nagy, Z, Nisini, B, Szabo, ZM, Bora, Z, Cseh, B, Kalup, C, Krezinger, M, Kriskovics, L, Ogłoza, W, Pál, A, Sódor, Á, Sonbas, E, Szakáts, R, Vida, K, Vinkó, J, Wyrzykowski, L & Zielinski, P 2024, 'The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties', Astronomy & Astrophysics, vol. 686, A160. https://doi.org/10.1051/0004-6361/202347777

TY - JOUR

T1 - The enigma of Gaia18cjb

T2 - a possible rare hybrid of FUor and EXor properties

AU - Fiorellino, Eleonora

AU - Ábrahám, Péter

AU - Kóspál, Ágnes

AU - Kun, Mária

AU - Alcalá, Juan M.

AU - Caratti o Garatti, Alessio

AU - Cruz-Sáenz de Miera, Fernando

AU - García-Álvarez, David

AU - Giannini, Teresa

AU - Park, Sunkyung

AU - Siwak, Michal

AU - Szilágyi, Máté

AU - Covino, Elvira

AU - Marton, Gabor

AU - Nagy, Zsófia

AU - Nisini, Brunella

AU - Szabo, Zsofia Marianna

AU - Bora, Zsófia

AU - Cseh, Borbála

AU - Kalup, Csilla

AU - Krezinger, Máté

AU - Kriskovics, Levente

AU - Ogłoza, Waldemar

AU - Pál, András

AU - Sódor, Ádám

AU - Sonbas, Eda

AU - Szakáts, Róbert

AU - Vida, Krisztián

AU - Vinkó, József

AU - Wyrzykowski, Lukasz

AU - Zielinski, Pawel

N1 - Funding: This work has been supported by the project PRIN’INAF 2019 “Spectroscopically Tracing the Disk Dispersal Evolution (STRADE)” and by the INAF Large Grant 2022 “YSOs Outflow, Disks and Accretion (YODA)”. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreement No 716155 (SACCRED). We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (https://gsaweb.ast.cam. ac.uk/alerts) This work is (partly) based on data obtained with the instrument EMIR, built by a Consortium led by the Instituto de Astrofísica de Canarias. EMIR was funded by GRANTECAN and the National Plan of Astronomy and Astrophysics of the Spanish Government. This work is (partly) based on data obtained at the Mount Suhora Observatory, Krakow Pedagogical University, Poland. This work has been supported by the Hungarian National Research, Development and Innovation Office grants OTKA K131508, OTKA K138962, the Élvonal KKP-143986 and KKP-137523 ‘SeismoLab’ grants of the Hungarian Research, Development and Innovation Office (NKFIH). We acknowledge support from the ESA PRODEX contract nr. 4000132054. KV, LK, ZN, and GM are supported by the Bolyai János Research Scholarship of the Hungarian Academy of Sciences, KV is supported by the Bolyai+ grant ÚNKP22-5-ELTE-1093. Authors acknowledge the financial support of the AustrianHungarian Action Foundation (112öu1). LK is supported by the Hungarian National Research, Development and Innovation Office grant PD-134784. G.M. acknowledges support from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004141. This work is supported by the Polish MNiSW grant DIR/WK/2018/12 and the European Union’s Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON-RadioNet Pilot). Zs.M.Sz. acknowledges funding from a St Leonards scholarship from the University of St Andrews. BZs is supported by the ÚNKP-22-2 New National Excellence Program of the Ministry for Culture and Innovation from the source of the National Research, Development and Innovation Fund. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. We acknowledge the Hungarian National Research, Development and Innovation Office grant OTKA FK 146023. FCSM received financial support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (ERC Starting Grant “Chemtrip”, grant agreement No 949278). This work was also supported by the NKFIH excellence grant TKP2021-NKTA-64.

PY - 2024/6

Y1 - 2024/6

N2 - Context. Gaia18cjb is one of the Gaia-alerted eruptive young star candidates that has been experiencing a slow and strong brightening during the last 13 years, similarly to some FU Orionis-type objects.Aims. The aim of this work is to derive the young stellar nature of Gaia18cjb and determine its physical and accretion properties to classify its variability.Methods. We conducted monitoring observations using multi-filter optical and near-infrared (NIR) photometry, as well as NIR spectroscopy. We present an analysis of pre-outburst and outburst optical and IR light curves, color-magnitude diagrams in different bands, the detection of NIR spectral lines, and estimates of both stellar and accretion parameters during the burst.Results. The optical light curve shows an unusually long (over 8 years) brightening event of 5 mag in the last 13 years, before reaching a plateau indicating that the burst is still ongoing, suggesting a FU Orionis-like (FUor-like) nature. The same outburst is less strong in the IR light curves. The NIR spectra, obtained during the outburst, exhibit emission lines typical of highly accreting low-intermediate mass young stars with typical EX Lupi-type (EXor) features. The spectral index of Gaia18cjb SED classifies it as a Class I in the pre-burst stage and a flat-spectrum young stellar object (YSO) during the burst.Conclusions. Gaia18cjb is an eruptive YSO that exhibits FUor-like photometric features (in terms of brightening amplitude and length of the burst) as well as EXor-like spectroscopic features and accretion rate. Its nature appears similar to that of V350 Cep and V1647 Ori, which have been classified as objects in between FUors and EXors.

AB - Context. Gaia18cjb is one of the Gaia-alerted eruptive young star candidates that has been experiencing a slow and strong brightening during the last 13 years, similarly to some FU Orionis-type objects.Aims. The aim of this work is to derive the young stellar nature of Gaia18cjb and determine its physical and accretion properties to classify its variability.Methods. We conducted monitoring observations using multi-filter optical and near-infrared (NIR) photometry, as well as NIR spectroscopy. We present an analysis of pre-outburst and outburst optical and IR light curves, color-magnitude diagrams in different bands, the detection of NIR spectral lines, and estimates of both stellar and accretion parameters during the burst.Results. The optical light curve shows an unusually long (over 8 years) brightening event of 5 mag in the last 13 years, before reaching a plateau indicating that the burst is still ongoing, suggesting a FU Orionis-like (FUor-like) nature. The same outburst is less strong in the IR light curves. The NIR spectra, obtained during the outburst, exhibit emission lines typical of highly accreting low-intermediate mass young stars with typical EX Lupi-type (EXor) features. The spectral index of Gaia18cjb SED classifies it as a Class I in the pre-burst stage and a flat-spectrum young stellar object (YSO) during the burst.Conclusions. Gaia18cjb is an eruptive YSO that exhibits FUor-like photometric features (in terms of brightening amplitude and length of the burst) as well as EXor-like spectroscopic features and accretion rate. Its nature appears similar to that of V350 Cep and V1647 Ori, which have been classified as objects in between FUors and EXors.

KW - Accretion

KW - Accretion disks

KW - Techniques: imaging spectroscopy

KW - Stars: formation

KW - Stars: low-mass

KW - Stars: pre-main sequence

KW - Stars: protostars

U2 - 10.1051/0004-6361/202347777

DO - 10.1051/0004-6361/202347777

M3 - Article

SN - 0004-6361

VL - 686

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A160

ER -

The enigma of Gaia18cjb: a possible rare hybrid of FUor and EXor properties

Abstract

Keywords

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Gaia18cjb LT, LBT, NTT and GTC spectra

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