@article{MTMT:34493612,
	title = {Orbit determination for the binary Cepheid V1344 Aql},
	url = {https://m2.mtmt.hu/api/publication/34493612},
	author = {Cseh, Borbála and Csörnyei, Géza and Szabados, László and Csák, Balázs and Kovács, József and Kriskovics, Levente and Pál, András},
	doi = {10.1051/0004-6361/202347360},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {680},
	unique-id = {34493612},
	issn = {0004-6361},
	abstract = {Context. Binary Cepheids play an important role in the investigation of the calibration of the classical Cepheid period-luminosity relationship. Therefore, a thorough study of individual Cepheids belonging to binary systems is necessary. Aims: Our aim is to determine the orbit of the binary system V1344 Aql using newly observed and earlier published spectroscopic and photometric data. Methods: We collected new radial velocity observations using medium resolution (R ≈ 11 000 and R ⪅ 20 000) spectrographs, and we updated the pulsation period of the Cepheid based on available photometric observations using an O − C diagram. Separating the pulsational and orbital radial velocity variations for each observational season (year), we determined the orbital solution for the system using χ2 minimisation. Results: The updated pulsation period of the Cepheid estimated for the epoch of HJD 2458955.83 is 7.476826 days. We determined orbital elements for the first time in the literature. The orbital period of the system is about 34.6 yr, with an eccentricity of e = 0.22. Reduced spectra are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A89},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; binaries: spectroscopic; stars: variables: Cepheids; stars: individual: V1344 Aql},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Kovács, József/0000-0002-1883-9555}
}

@article{MTMT:34232492,
	title = {SN 2021gno: a calcium-rich transient with double-peaked light curves},
	url = {https://m2.mtmt.hu/api/publication/34232492},
	author = {Ertini, K. and Folatelli, G. and Martinez, L. and Bersten, M. C. and Anderson, J. P. and Ashall, C. and Baron, E. and Bose, S. and Brown, P. J. and Burns, C. and DerKacy, J. M. and Ferrari, L. and Galbany, L. and Hsiao, E. and Kumar, S. and Lu, J. and Mazzali, P. and Morrell, N. and Orellana, M. and Pessi, P. J. and Phillips, M. M. and Piro, A. L. and Polin, A. and Shahbandeh, M. and Shappee, B. J. and Stritzinger, M. and Suntzeff, N. B. and Tucker, M. and Elias-Rosa, N. and Kuncarayakti, H. and Gutiérrez, C. P. and Kozyreva, A. and Müller-Bravo, T. E. and Chen, T. -W. and Hinkle, J. T. and Payne, A. V. and Székely, Péter and Szalai, Tamás and Barna, Barnabás and Könyves-Tóth, Réka and Bánhidi, D. and Bíró, I. B. and Csányi, István and Kriskovics, Levente and Pál, András and Szabó, Zs and Szakáts, Róbert and Vida, Krisztián and Vinkó, József and Gromadzki, M. and Harvey, L. and Nicholl, M. and Paraskeva, E. and Young, D. R. and Englert, B.},
	doi = {10.1093/mnras/stad2705},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {526},
	unique-id = {34232492},
	issn = {0035-8711},
	abstract = {We present extensive ultraviolet (UV) and optical photometric and optical spectroscopic follow-up of supernova (SN) 2021gno by the 'Precision Observations of Infant Supernova Explosions' (POISE) project, starting less than 2 d after the explosion. Given its intermediate luminosity, fast photometric evolution, and quick transition to the nebular phase with spectra dominated by [Ca II] lines, SN 2021gno belongs to the small family of Calcium-rich transients. Moreover, it shows double-peaked light curves, a phenomenon shared with only four other Calcium-rich events. The projected distance from the centre of the host galaxy is not as large as other objects in this family. The initial optical light-curve peaks coincide with a very quick decline of the UV flux, indicating a fast initial cooling phase. Through hydrodynamical modelling of the bolometric light curve and line velocity evolution, we found that the observations are compatible with the explosion of a highly stripped massive star with an ejecta mass of $0.8\\, M_\\odot$ and a 56Ni mass of 0.024 M⊙. The initial cooling phase (first light-curve peak) is explained by the presence of an extended circumstellar material comprising ~$10^{-2}\\, {\\rm M}_{\\odot }$ with an extension of $1100\\, R_{\\odot }$. We discuss if hydrogen features are present in both maximum-light and nebular spectra, and their implications in terms of the proposed progenitor scenarios for Calcium-rich transients.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; supernovae: general; Astrophysics - High Energy Astrophysical Phenomena; stars: massive; supernovae: individual: SN 2021gno},
	year = {2023},
	eissn = {1365-2966},
	pages = {279-298},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34221293,
	title = {Three is the magic number: Distance measurement of NGC 3147 using SN 2021hpr and its siblings},
	url = {https://m2.mtmt.hu/api/publication/34221293},
	author = {Barna, Barnabás and Nagy, Andrea and Bora, Zs. and Czavalinga, Donát Róbert and Könyves-Tóth, Réka and Szalai, Tamás and Székely, Péter and Zsíros, Szanna and Banhidi, D. and Biro, I. B. and Csanyi, I. and Kriskovics, Levente and Pál, András and Szabo, Zs. M. and Szakáts, Róbert and Vida, Krisztián and Bodola, Zsófia Réka and Vinkó, József},
	doi = {10.1051/0004-6361/202346395},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {677},
	unique-id = {34221293},
	issn = {0004-6361},
	abstract = {Context. The nearby spiral galaxy NGC 3147 hosted three Type Ia supernovae (SNe Ia) in the past decades that have been the subjects of intense follow-up observations. Simultaneous analysis of their data provides a unique opportunity for testing different methods of light curve fitting and distance estimation.Aims. The detailed optical follow-up of SN 2021hpr allows us to revise the previous distance estimations to NGC 3147 and compare the widely used light curve fitting algorithms to each other. After the combination of the available and newly published data of SN 2021hpr, its physical properties can also be estimated with higher accuracy.Methods. We present and analyse new BVgriz and Swift photometry of SN 2021hpr to constrain its general physical properties. Together with its siblings, SNe 1997bq and 2008fv, we cross-compared the individual distance estimates of these three SNe given by the Spectral Adaptive Lightcurve Template (SALT) code, and we also checked their consistency with the results from the Multi-Color Light Curve Shape (MLCS) code. The early spectral series of SN 2021hpr was also fit with the radiative spectral code TARDIS to verify the explosion properties and constrain the chemical distribution of the outer ejecta.Results. After combining the distance estimates for the three SNe, the mean distance to their host galaxy, NGC 3127, is 42.5 +/- 1.0 Mpc, which matches with the distance inferred by the most up-to-date light curve fitters, SALT3 and BayeSN. We confirm that SN 2021hpr is a Branch-normal Type Ia SN that ejected -1.12 +/- 0.28 M-circle dot from its progenitor white dwarf and synthesized -0.44 +/- 0.14 M-circle dot of radioactive Ni-56.},
	keywords = {radiative transfer; supernovae: general; Galaxies: distances and redshifts; supernovae: individual: SN 2021hpr},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34053151,
	title = {EI Eridani: A star under the influence. The effect of magnetic activity in the short and long term},
	url = {https://m2.mtmt.hu/api/publication/34053151},
	author = {Kriskovics, Levente and Kővári, Zsolt and Seli, Bálint Attila and Oláh, Katalin Ilona and Vida, Krisztián and Henry, G. W. and Granzer, T. and Görgei, A.},
	doi = {10.1051/0004-6361/202245767},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {674},
	unique-id = {34053151},
	issn = {0004-6361},
	abstract = {Context. Homogeneous photometric time series spanning decades provide a unique opportunity to study the long-term cyclic behavior of active spotted stars such as our target EI Eridani. In addition, with ultraprecise space photometry data, it is possible to investigate the accompanying flare activity in detail. However, the rotation period of ≈2 days for EI Eri makes it impossible to achieve time-resolved surface images from a single ground-based observing site. Therefore, for this purpose, spectroscopic data from a multi-site observing campaign are needed.},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Kővári, Zsolt/0000-0001-5160-307X; Seli, Bálint Attila/0000-0002-3658-2175; Görgei, A./0009-0002-1289-7946}
}

@misc{MTMT:33729197,
	title = {VizieR Online Data Catalog: Opt-to-IR monitoring obs. of V1057 Cyg (Szabo+, 2021)},
	url = {https://m2.mtmt.hu/api/publication/33729197},
	author = {Szabo, Z. M. and Kóspál, Ágnes and Ábrahám, Péter and Park, Sunkyung and Siwak, Michal and Green, J. D. and Moór, Attila and Pál, András and Acosta-Pulido, J. A. and Lee, J. -E. and Cseh, B. and Csornyei, G. and Hanyecz, O. and Könyves-Tóth, Réka and Krezinger, M. and Kriskovics, Levente and Ordasi, A. and Sárneczky, Krisztián and Seli, B. and Szakáts, Róbert and Szing, A. and Vida, Krisztián},
	unique-id = {33729197},
	abstract = {We performed the majority of our photometric observations in B, V, RC, IC , g', r', and i' filters at the Piszkesteto Mountain Station of Konkoly Observatory (Hungary) between 2005 and 2021. Three telescopes with three slightly different optical systems were used: the 1m Ritchey-Chretien-coude (RCC) telescope, the 60/90/180cm Schmidt telescope and the Astro Systeme Austria AZ800 alt-azimuth direct drive 80cm Ritchey-Chretien (RC80) telescope; see Section 2.1. In addition to our national facilities, we occasionally used other telescopes. On 2006 July 20 and 2012 October 13 we obtained B, V, RJ, and IJ images of V1057 Cyg with the IAC80 telescope of the Instituto de Astrofisica de Canarias located at Teide Observatory (Canary Islands, Spain). During 2019 August-September, in parallel with TESS, we additionally observed V1057 Cyg at the Northern Skies Observatory (NSO). We used the 0.4m telescope equipped with BVI filters. We also observed V1057 Cyg with the 2.56m Nordic Optical Telescope (NOT) at the Roque de los Muchachos Observatory, La Palma, in the Canary Islands (Plan ID 61-414, PI: Zs. M. Szabo). For optical imaging we used the Alhambra Faint Object Spectrograph and Camera (ALFOSC) on 2020 August 17. The Bessel BVR filter set was supplemented by an i interference filter, which is similar to the SLOAN i', but with a slightly longer effective wavelength of λeff=0.789um. We obtained NIR images in the J, H, and Ks bands at six epochs between 2006 July 15 and 2012 October 13 using the 1.52m Telescopio Carlos Sanchez (TCS) at the Teide Observatory. We also used the NOTCam instrument on the NOT on 2020 August 29. See Section 2.3. We obtained a new optical spectrum of V1057 Cyg with the high-resolution FIbre-fed Echelle Spectrograph (FIES) instrument on the NOT on 2020 August 17. We used a fiber with a larger entrance aperture of 2.5", which provided a spectral resolution R=25000, covering the 370-900nm wavelength range. V1057 Cyg was also observed with the Bohyunsan Optical Echelle Spectrograph (BOES) installed on the 1.8m telescope at the Bohyunsan Optical Astronomy Observatory (BOAO). It provides R=30000 in the wavelength range ~400-900nm. The first spectrum was obtained on 2012-September-11 and the last on 2018-December-18. See Section 2.4. On 2020 August 29, we used the NOTCam on the NOT to obtain new NIR spectra of V1057 Cyg and Iot Cyg (A5 V) as our telluric standard star in the JHKs bands. We used the low-resolution camera mode (R=2500). See Section 2.5. On 2018 September 6, we observed V1057 Cyg with the Stratospheric Observatory for Infrared Astronomy (SOFIA) using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST). We obtained mid-infrared imaging in a series of short exposures in band F111 (10.6-11.6um) totaling ~30s, a single exposure in F056 (5.6um) for 37s and F077 (7.5-8um) for 42s, and R~100-200 spectra with G063 (5-8um) and G227 (17-27um) (Plan ID 06_062, PI: J. D. Green). See Section 2.6. (2 data files).},
	keywords = {stars: pre-main sequence; Photometry: UBVRI; Spectra: infrared},
	year = {2023}
}

@article{MTMT:33720970,
	title = {Glancing through the debris disk: Photometric analysis of DE Boo with CHEOPS},
	url = {https://m2.mtmt.hu/api/publication/33720970},
	author = {Boldog, Ádám and Szabó M., Gyula and Kriskovics, Levente and Brandeker, A. and Kiefer, F. and Bekkelien, A. and Guterman, P. and Olofsson, G. and Simon, A. E. and Gandolfi, D. and Serrano, L. M. and Wilson, T. G. and Sousa, S. G. and Lecavelier, des Etangs A. and Alibert, Y. and Alonso, R. and Anglada, G. and Bandy, T. and Bárczy, T. and Barrado, D. and Barros, S. C. C. and Baumjohann, W. and Beck, M. and Beck, T. and Benz, W. and Billot, N. and Bonfils, X. and Broeg, C. and Buder, M. and Cabrera, J. and Charnoz, S. and Collier, Cameron A. and Corral, van Damme C. and Csizmadia, Sz. and Davies, M. B. and Deline, A. and Deleuil, M. and Delrez, L. and Demangeon, O. D. S. and Demory, B. -O. and Ehrenreich, D. and Erikson, A. and Farinato, J. and Fortier, A. and Fossati, L. and Fridlund, M. and Gillon, M. and Güdel, M. and Heng, K. and Hoyer, S. and Isaak, K. G. and Kiss, L. László and Laskar, J. and Lendl, M. and Lovis, C. and Magrin, D. and Maxted, P. F. L. and Mecina, M. and Nascimbeni, V. and Ottensamer, R. and Pagano, I. and Pallé, E. and Peter, G. and Piotto, G. and Pollacco, D. and Queloz, D. and Ragazzoni, R. and Rando, N. and Rauer, H. and Ribas, I. and Santos, N. C. and Scandariato, G. and Ségransan, D. and Smith, A. M. S. and Steller, M. and Thomas, N. and Udry, S. and Van, Grootel V. and Walton, N. A.},
	doi = {10.1051/0004-6361/202245101},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {671},
	unique-id = {33720970},
	issn = {0004-6361},
	abstract = {Aims: DE Boo is a unique system, with an edge-on view through the debris disk around the star. The disk, which is analogous to the Kuiper belt in the Solar System, was reported to extend from 74 to 84 AU from the central star. The high photometric precision of the Characterising Exoplanet Satellite (CHEOPS) provided an exceptional opportunity to observe small variations in the light curve due to transiting material in the disk. This is a unique chance to investigate processes in the debris disk. Methods: Photometric observations of DE Boo of a total of four days were carried out with CHEOPS. Photometric variations due to spots on the stellar surface were subtracted from the light curves by applying a two-spot model and a fourth-order polynomial. The photometric observations were accompanied by spectroscopic measurements with the 1m RCC telescope at Piszkésteto and with the SOPHIE spectrograph in order to refine the astrophysical parameters of DE Boo. Results: We present a detailed analysis of the photometric observation of DE Boo. We report the presence of nonperiodic transient features in the residual light curves with a transit duration of 0.3-0.8 days. We calculated the maximum distance of the material responsible for these variations to be 2.47 AU from the central star, much closer than most of the mass of the debris disk. Furthermore, we report the first observation of flaring events in this system. Conclusions: We interpreted the transient features as the result of scattering in an inner debris disk around DE Boo. The processes responsible for these variations were investigated in the context of interactions between planetesimals in the system. This article uses data from CHEOPS programme CH_PR100010.},
	keywords = {methods: data analysis; Astrophysics - Solar and Stellar Astrophysics; circumstellar matter; techniques: photometric; starspots; Astrophysics - Earth and Planetary Astrophysics; stars: flare},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Kiss, L. László/0000-0002-3234-1374}
}

@article{MTMT:33538419,
	title = {Characteristics of flares on giant stars},
	url = {https://m2.mtmt.hu/api/publication/33538419},
	author = {Oláh, Katalin Ilona and Seli, Bálint Attila and Kővári, Zsolt and Kriskovics, Levente and Vida, Krisztián},
	doi = {10.1051/0004-6361/202243789},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {668},
	unique-id = {33538419},
	issn = {0004-6361},
	abstract = {Context. Although late-type dwarfs and giant stars are substantially different, their flares are thought to originate in similar physical processes and differ only by a scale factor in the energy levels. We study the validity of this approach.},
	year = {2022},
	eissn = {1432-0746},
	orcid-numbers = {Seli, Bálint Attila/0000-0002-3658-2175; Kővári, Zsolt/0000-0001-5160-307X}
}

@article{MTMT:33537935,
	title = {Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct},
	url = {https://m2.mtmt.hu/api/publication/33537935},
	author = {Park, Sunkyung and Kóspál, Ágnes and Ábrahám, Péter and Fernando, Cruz-Saenz de Miera and Fiorellino, Elenonora and Siwak, Michal and Nagy, Zsófia and Giannini, Teresa and Carini, Roberta and Szabó, Zsófia Marianna and Lee, Jeong-Eun and Lee, Jae-Joon and Vitali, Fabrizio and Kun, Mária and Cseh, Borbála and Krezinger, Máté and Kriskovics, Levente and Ordasi, András and Pál, András and Szakáts, Róbert and Vida, Krisztián and Vinkó, József},
	doi = {10.3847/1538-4357/aca01e},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {941},
	unique-id = {33537935},
	issn = {1538-4357},
	abstract = {Gaia19fct is one of the Gaia-alerted eruptive young stars that has undergone several brightening events. We conducted monitoring observations using multifilter optical and near-infrared photometry, as well as near-infrared spectroscopy, to understand the physical properties of Gaia19fct and investigate whether it fits into the historically defined two classes. We present the analyses of light curves, color variations, spectral lines, and CO modeling. The light curves show at least five brightening events since 2015, and the multifilter color evolutions are mostly gray. The gray evolution indicates that bursts are triggered by mechanisms other than extinction. Our near-infrared spectra exhibit both absorption and emission lines and show time variability throughout our observations. We found lower rotational velocity and lower temperature from the near-infrared atomic absorption lines than from the optical lines, suggesting that Gaia19fct has a Keplerian rotating disk. The CO overtone features show a superposition of absorption and emission components, which is unlike other young stellar objects. We modeled the CO lines, and the result suggests that the emission and absorption components are formed in different regions. We found that although Gaia19fct exhibits characteristics of both types of eruptive young stars, FU Orionis–type objects and EX Lupi–type objects, it shows more similarity with EXors in general.},
	year = {2022},
	eissn = {0004-637X},
	orcid-numbers = {Giannini, Teresa/0000-0002-7035-8513; Carini, Roberta/0000-0003-1604-2064; Szabó, Zsófia Marianna/0000-0001-9830-3509; Lee, Jeong-Eun/0000-0003-3119-2087; Lee, Jae-Joon/0000-0003-0894-7824; Vitali, Fabrizio/0000-0001-8332-4227; Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:33108812,
	title = {Mid-infrared time-domain study of recent dust production events in the extreme debris disc of TYC 4209-1322-1},
	url = {https://m2.mtmt.hu/api/publication/33108812},
	author = {Moór, Attila and Ábrahám, Péter and Kóspál, Ágnes and Su, Kate Y. L. and Rieke, George H. and Vida, Krisztián and Cataldi, Gianni and Bódi, Attila and Sódorné Bognár, Zsófia and Cseh, Borbála and Csörnyei, Géza and Egei, Nóra and Farkas, Anikó and Hanyecz, Ottó and Ignácz, Bernadett and Kalup, Csilla and Könyves-Tóth, Réka and Kriskovics, Levente and Mészáros, László and Pál, András and Ordasi, András and Sárneczky, Krisztián and Seli, Bálint Attila and Sódor, Ádám and Szakáts, Róbert and Vinkó, József and Zsidi, Gabriella},
	doi = {10.1093/mnras/stac2595},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {516},
	unique-id = {33108812},
	issn = {0035-8711},
	abstract = {Extreme debris discs are characterized by unusually strong mid-infrared excess emission, which often proves to be variable. The warm dust in these discs is of transient nature and is likely related to a recent giant collision occurring close to the star in the terrestrial region. Here we present the results of a 877 days long, gap-free photometric monitoring performed by the Spitzer Space Telescope of the recently discovered extreme debris disc around TYC 4209-1322-1. By combining these observations with other time-domain optical and mid-infrared data, we explore the disc variability of the last four decades, with particular emphasis on the last 12 years. During the latter interval the disc showed substantial changes, the most significant was the brightening and subsequent fading between 2014 and 2018 as outlined in WISE data. The Spitzer light curves outline the fading phase and a subsequent new brightening of the disc after 2018, revealing an additional flux modulation with a period of ~39 days on top of the long-term trend. We found that all these variations can be interpreted as the outcome of a giant collision that happened at an orbital radius of ~0.3 au sometime in 2014. Our analysis implies that a collision on a similar scale could have taken place around 2010, too. The fact that the disc was already peculiarly dust rich 40 years ago, as implied by IRAS data, suggests that these dust production events belong to a chain of large impacts triggered by an earlier even more catastrophic collision.},
	keywords = {infrared: planetary systems; (stars:) circumstellar matter; stars: individual: TYC 4209-1322-1},
	year = {2022},
	eissn = {1365-2966},
	pages = {5684-5701},
	orcid-numbers = {Bódi, Attila/0000-0002-8585-4544; Seli, Bálint Attila/0000-0002-3658-2175; Vinkó, József/0000-0001-8764-7832}
}

@misc{MTMT:33087177,
	title = {GRB220101A: optical afterglow detection from Konkoly Observatory},
	url = {https://m2.mtmt.hu/api/publication/33087177},
	author = {Vinkó, József and Pál, András and Kriskovics, Levente and Szakáts, Róbert and Vida, Krisztián},
	unique-id = {33087177},
	abstract = {We observed the field of GRB220101A (Tohuvavohu et al., GCN #31347; Arimoto et al., GCN #31350; AGILE Ursi et al., GCN #31354) with the RC80 robotic telescope at Piszkesteto Station of Konkoly Observatory on 2022 Jan 01 starting at 21:32:18 UT. A series of 5x300 sec frames were collected through Sloan r'- and i' bands. The bright optical afterglow (Kuin & Tohuvavohu, GCN #31351; Fu et al., GCN #31353; Hentunen et al., GCN #31356; Perley, GCN #31357; Ugarte Postigo et al. GCN #31358; Fynbo et al. GCN #31359) is clearly detected on the stacked frames with the following magnitudes, calibrated via nearby PS1 stars: Date UT-middle t-T0(hr) Exp(s) r'(AB-mag) i'(AB-mag) 2022-01-01 21:52:52 16.73 5x300 19.81 +/- 0.12 18.67 +/- 0.14},
	year = {2022},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}