@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:33728423,
	title = {Searching for Supernovae in HETDEX Data Release 3},
	url = {https://m2.mtmt.hu/api/publication/33728423},
	author = {Vinkó, József and Thomas, B.P. and Wheeler, J.C. and Ho, A.Y.Q. and Cooper, E.M. and Gebhardt, K. and Ciardullo, R. and Farrow, D.J. and Hill, G.J. and Jäger, Zoltán and Kollatschny, W. and Liu, C. and Regős, Enikő and Sárneczky, Krisztián},
	doi = {10.3847/1538-4357/acbfa8},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {946},
	unique-id = {33728423},
	issn = {1538-4357},
	year = {2023},
	eissn = {0004-637X},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:33603304,
	title = {Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope},
	url = {https://m2.mtmt.hu/api/publication/33603304},
	author = {Kecskemethy, Viktoria and Kiss, Csaba and Szakáts, Róbert and Pál, András and Szabó M., Gyula and Molnár, László and Sárneczky, Krisztián and Vinkó, József and Szabó, Róbert and Marton, Gábor and Takácsné Farkas, Anikó and Kalup, Csilla and Kiss, L. László},
	doi = {10.3847/1538-4365/ac9c67},
	journal-iso = {ASTROPHYS J SUPPL S},
	journal = {ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES},
	volume = {264},
	unique-id = {33603304},
	issn = {0067-0049},
	abstract = {The K2 mission of the Kepler Space Telescope allowed the observations of light curves of small solar system bodies throughout the whole solar system. In this paper, we present the results of a collection of K2 trans-Neptunian object observations between campaigns C03 (2014 November-2015 February) and C19 (2018 August-September), which includes 66 targets. Due to the faintness of our targets, the detectability rate of a light-curve period is similar to 56%, notably lower than in the case of other small-body populations, like Hildas or Jovian Trojans. We managed to obtain light-curve periods with an acceptable confidence for 37 targets; the majority of these cases are new identifications. We were able to give light-curve amplitude upper limits for the other 29 targets. Several of the newly detected light-curve periods are longer than similar to 24 hr, in many cases close to similar to 80 hr; i.e., these targets are slow rotators. This relative abundance of slowly rotating objects is similar to that observed among Hildas, Jovian Trojans, and Centaurs in the K2 mission, as well as among main belt asteroids measured with the TESS space telescope. Trans-Neptunian objects show notably higher light-curve amplitudes at large (D greater than or similar to 300 km) sizes than found among large main belt asteroids, in contrast to the general expectation that due to their lower compressive strength, they reach hydrostatic equilibrium at smaller sizes than their inner solar system counterparts.},
	year = {2023},
	eissn = {1538-4365},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Vinkó, József/0000-0001-8764-7832; Szabó, Róbert/0000-0002-3258-1909; Kiss, L. László/0000-0002-3234-1374}
}

@CONFERENCE{MTMT:33364891,
	title = {Rotational properties of Kuiper belt objects as seen by the K2 mission},
	url = {https://m2.mtmt.hu/api/publication/33364891},
	author = {Kecskeméthy, Viktória and Kiss, Csaba and Szakáts, Róbert and Pál, András and Szabó M., Gyula and Molnár, László and Sárneczky, Krisztián and Vinkó, József and Szabó, Róbert and Marton, Gábor and Takácsné Farkas, Anikó and Kalup, Csilla and Kiss, L. László},
	booktitle = {16th Europlanet Science Congress 2022},
	doi = {10.5194/epsc2022-677},
	unique-id = {33364891},
	abstract = {Earlier reviews of trans-Neptunian light curves reported mean rotation periods of P = 7-8 h (Duffard et al., 2009), and it was also found that the binary trans-Neptunian population rotates slower (Thirouin & Sheppard, 2014), and objects in the cold classical population have larger variability and rotate slower than the non-cold classical TNOs (Benecchi et al., 2013,Thirouin & Sheppard, 2019). While ground-based observations have obvious limitations in detecting long-period light curves the K2 mission of the Kepler Space Telescope allowed long (up to ~80 days), uninterrupted observations of many Solar system objects, including main belt asteroids, Hildas, Jovian trojans, and also the irregular satellites of giant planets. Light curves were also published for a few, selected trans-Neptunian objects based on K2 observations (see Kiss et al., 2020, for a summary). A common outcome of the studies of larger samples, across all dynamical classes, was the identification of an increased number of targets with long rotation periods compared to previous ground-based studies. A similar trend is observed among the data of nearly 10 000 main belt asteroids obtained by the TESS Space Telescope (Pál et al., 2020), and asteroids with long rotation periods were identified in other surveys like the Asteroid Terrestrial-impact Last Alert System (ATLAS), the Zwicky Transient Facility (Erasmus et al., 2021) and the All-Sky Automated Survey for Supernovae (Hanus et al., 2021). We have collected the K2 trans-Neptunian object observations between Campaigns C03 (November 2014 -- February 2015) to C19 (August -- September, 2018), which includes 67 targets. Due to the faintness of our targets the detectability rate of a light curve period is ~57 %, notably lower than in the case of other small body populations, like Hildas or Jovian trojans. We managed to obtain light curve periods with an acceptable confidence for 36 targets; the majority of these cases are new identifications. We were able to give light curve amplitude upper limits for the other 31 targets. Several of the newly detected light curve periods are longer than ~24 h, in many cases close to ~100 h, i.e., slow rotators.There is a very significant difference between the rotation rates of the LCDB and K2 TNO samples (Figs. 1 and 2). The mean LCD spin frequency is 2.71 c/d (8.8 h), while it is 0.87 c/d (27.6 h) in the K2 sample which is more similar to the K2 Hilda and Jovian Trojan spin frequency distrbutions. Thirouin & Sheppard (2019) obtained 9.48±1.53 h and 8.45±0.58 h mean rotation periods for the cold classical and the non-cold classical TNOs. Our mean values for the same dynamical groups (but using different targets) are notably longer: 1.21+1.58-0.63 c/d (19.83 h) and 0.83+1.81-0.23 c/d (P=28.91 h), respectively. The K2 mean frequency is higher than that of the K2 Jovian Trojans and Hildas, but we could not detect the very long period targets that were observed in these other K2 samples. Figure 1: frequency distribution of asteroids. The cyan, magenta, green and blue colours represent the TNOs in the LCDB and Jovian trojans, Hildas and TNOs from K2, respectively. Figure 2: Frequency as a function of absolute magnitude. Big circles with error bars mark the median values standard deviations for the different samples. The horizontal dashed lines mark the spin frequencies of fast, slow, and very slow rotators (Pravec et al., 2002). While there are only three objects with D>500 km in our sample, there are a number of objects -- both with and without detected light curve periods -- that fall in the 300≤D≤500 km transitional zone where asphericity -- hence light curve amplitude -- is expected to drop assuming a single rotating body, assuming main belt composition. Main belt asteroids are already almost extinct in this size range, and so are Centaurs -- for these bodies irregular shapes are expected in most cases. While the general trend is that larger objects have smaller light curve amplitudes among TNOs -- a trend followed both by our sample and the LCDB TNOs -- there are a considerable number of TNOs with high asphericity in the 300≤D≤500 km size range. This contradiction could be resolved if TNOs had higher-than-expected compressive strength and become spherical for sizes larger than their main belt counterparts, and remain 'irregular' in the 300≤D≤500 km range. However, their general low density and high porosity point against this scenario. A notable fraction of contact or semi-contact binary systems in which the members themselves are in hydrostatical equlibrium could produce a population of high-amplitude light curves in this size range (Lacerda et al., 2006, 2014). As some authors pointed out, contact binaries may be very frequent, especially in the plutino population (Thirouin & Sheppard, 2018,2019). The long term stability of such systems against their tidal evolution, however, should be investigated to answer the reliability of this assumption. Finally, spherical (rotationally flattened) bodies with large albedo variegations could also explain the observed amplitudes. While the general expectation in most TNO light curve studies was a double peak light curve, in our sample most light curves were found to be single-peak, after comparing the single-peak and double-peak solutions.Fgiure 3: Light curve amplitude versus the estimated size of the targets in our sample. The region between the vertical dashed lines mark the irregular-to-spherical transition size range in the main belt. Blue and red symbols mark the K2 targets and K2 upper limits, small grey symbols correspond to main belt asteroids. Large gray symbols represent the theoretical maximum light curve amplitudes the of large main belt objects if it was solely caused by the elongated shape of a body with homogeneous albedo.},
	year = {2022},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Vinkó, József/0000-0001-8764-7832; Szabó, Róbert/0000-0002-3258-1909; Kiss, L. László/0000-0002-3234-1374}
}

@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}
}

@article{MTMT:33087067,
	title = {A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence},
	url = {https://m2.mtmt.hu/api/publication/33087067},
	author = {Szabó, Zs. M. and Kóspál, Ágnes and Ábrahám, Péter and Park, Sunkyung and Siwak, Michal and Green, J. D. and Pál, András and Acosta-Pulido, J. A. and Lee, J. -E. and Ibrahimov, M. and Grankin, K. and Kovács, B. and Bora, Zs. and Bódi, Attila and Cseh, Borbála and Csörnyei, Géza and Dróżdż, Marek and Hanyecz, O. and Ignácz, B. and Kalup, Csilla and Könyves-Tóth, Réka and Krezinger, Máté and Kriskovics, Levente and Ogłoza, Waldemar and Ordasi, A. and Sárneczky, Krisztián and Seli, Bálint Attila and Szakáts, Róbert and Sódor, Ádám and Szing, A. and Vida, Krisztián and Vinkó, József},
	doi = {10.3847/1538-4357/ac82f5},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {936},
	unique-id = {33087067},
	issn = {1538-4357},
	abstract = {Historically, FU Orionis-type stars are low-mass, pre-main-sequence stars. The members of this class experience powerful accretion outbursts and remain in an enhanced accretion state for decades or centuries. V1515 Cyg, a classical FUor, started brightening in the 1940s and reached its peak brightness in the late 1970s. Following a sudden decrease in brightness, it stayed in a minimum state for a few months, then started brightening for several years. We present the results of our ground-based photometric monitoring complemented with optical/near-infrared spectroscopic monitoring. Our light curves show a long-term fading with strong variability on weekly and monthly timescales. The optical spectra show P Cygni profiles and broad blueshifted absorption lines, common properties of FUors. However, V1515 Cyg lacks the P Cygni profile in the Ca II 8498 Å line, a part of the Ca infrared triplet, formed by an outflowing wind, suggesting that the absorbing gas in the wind is optically thin. The newly obtained near-infrared spectrum shows the strengthening of the CO bandhead and the FeH molecular band, indicating that the disk has become cooler since the last spectroscopic observation in 2015. The current luminosity of the accretion disk dropped from the peak value of 138 L ⊙ to about 45 L ⊙, suggesting that the long-term fading is also partly caused by the dropping of the accretion rate.},
	keywords = {SPECTROSCOPY; photometry; Astrophysics - Solar and Stellar Astrophysics; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; INFRARED ASTRONOMY; FU Orionis stars; 1834; 553; 1558; optical astronomy; 1234; 235; 786; 1776},
	year = {2022},
	eissn = {0004-637X},
	orcid-numbers = {Bódi, Attila/0000-0002-8585-4544; Seli, Bálint Attila/0000-0002-3658-2175; Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:32826398,
	title = {Rotation periods and shape asphericity in asteroid families based on TESS S1-S13 observations},
	url = {https://m2.mtmt.hu/api/publication/32826398},
	author = {Szabó M., Gyula and Pál, András and Szigeti, László and Sódorné Bognár, Zsófia and Bódi, Attila and Kalup, Csilla and Jäger, Zoltán and Kiss, L. László and Kiss, Csaba and Kovács, József and Marton, Gábor and Molnár, László and Plachy, Emese and Sárneczky, Krisztián and Szakáts, Róbert and Szabó, Róbert},
	doi = {10.1051/0004-6361/202142223},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {661},
	unique-id = {32826398},
	issn = {0004-6361},
	abstract = {Here we present the analysis of the distribution of rotation periods and light curve amplitudes based on 2859 family asteroids in 16 Main Belt families based on 9912 TESS asteroid light curves in the TSSYS-DR1 asteroid light curve database. We found that the distribution of the light curve properties follow a family-specific character in some asteroid families, including the Hungaria, Maria, Juno, Eos, Eucharis, and Alauda families. While in other large families, these distributions are in general very similar to each other. We confirm that older families tend to contain a larger fraction of more spheroidal, low-amplitude asteroids. We found that rotation period distributions are different in the cores and outskirts of the Flora and Maria families, while the Vesta, Eos, and Eunomia families lack this feature. We also confirm that very fast spinning asteroids are close to spherical (or spinning top shapes), and minor planets rotating slower than approximate to 11 h are also more spherical than asteroids in the 4-8 h period range and this group is expected to contain the most elongated bodies.},
	keywords = {ASTEROIDS; General; MINOR PLANETS},
	year = {2022},
	eissn = {1432-0746},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Szigeti, László/0000-0002-6540-380X; Bódi, Attila/0000-0002-8585-4544; Kiss, L. László/0000-0002-3234-1374; Kovács, József/0000-0002-1883-9555; Szabó, Róbert/0000-0002-3258-1909}
}

@article{MTMT:32725386,
	title = {Study of changes in the pulsation period of 148 Galactic Cepheid variables},
	url = {https://m2.mtmt.hu/api/publication/32725386},
	author = {Csörnyei, Géza and Szabados, László and Molnár, László and Cseh, Borbála and Egei, N. and Kalup, Csilla and Kecskemethy, V and Könyves-Tóth, Réka and Sárneczky, Krisztián and Szakáts, Róbert},
	doi = {10.1093/mnras/stac115},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {511},
	unique-id = {32725386},
	issn = {0035-8711},
	abstract = {Investigating period changes of classical Cepheids through the framework of O - C diagrams provides a unique insight to the evolution and nature of these variable stars. In this work, the new or extended O - C diagrams for 148 Galactic classical Cepheids are presented. By correlating the calculated period change rates with the Gaia EDR3 colours, we obtain observational indications for the non-negligible dependence of the period change rate on the horizontal position within the instability strip. We find period fluctuations in 59 Cepheids with a confidence level of 99 per cent, which are distributed uniformly over the inspected period range. Correlating the fluctuation amplitude with the pulsation period yields a clear dependence, similar to the one valid for longer period pulsating variable stars. The non-negligible amount of Cepheids showing changes in their O - C diagrams that are not or not only of evolutionary origin points towards the need for further studies for the complete understanding of these effects. One such peculiar behaviour is the large amplitude period fluctuation in short period Cepheids, which occurs in a significant fraction of the investigated stars. The period dependence of the fluctuation strength and its minimum at the bump Cepheid region suggests a stability enhancing mechanism for this period range, which agrees with current pulsation models.},
	keywords = {stars: evolution; stars: oscillations; Binaries: General; stars: variables: Cepheids},
	year = {2022},
	eissn = {1365-2966},
	pages = {2125-2146}
}

@article{MTMT:32720651,
	title = {Probing into emission mechanisms of GRB 190530A using time-resolved spectra and polarization studies: synchrotron origin?},
	url = {https://m2.mtmt.hu/api/publication/32720651},
	author = {Gupta, Rahul and Gupta, S. and Chattopadhyay, T. and Lipunov, V and Castro-Tirado, A. J. and Bhattacharya, D. and Pandey, S. B. and Oates, S. R. and Kumar, Amit and Hu, Y-D and Valeev, A. F. and Minaev, P. Yu and Kumar, H. and Vinkó, József and Dimple, Dimple and Sharma, V and Aryan, A. and Castellon, A. and Gabovich, A. and Moskvitin, A. and Ordasi, A. and Pál, András and Pozanenko, A. and Zhang, B-B and Kumar, B. and Svinkin, D. and Saraogi, D. and Vlasenko, D. and Fernandez-Garcia, E. and Gorbovskoy, E. and Anupama, G. C. and Misra, K. and Sárneczky, Krisztián and Kriskovics, Levente and Castro-Tirado, M. A. and Caballero-Garcia, M. D. and Tiurina, N. and Balanutsa, P. and Lopez, R. R. and Sanchez-Ramirez, R. and Szakáts, Róbert and Belkin, S. and Guziy, S. and Iyyani, S. and Tiwari, S. N. and Vadawale, Santosh V. and Sun, T. and Bhalerao, V and Kornilov, V and Sokolov, V. V.},
	doi = {10.1093/mnras/stac015},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {511},
	unique-id = {32720651},
	issn = {0035-8711},
	abstract = {Multipulsed GRB 190530A, detected by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope onboard Fermi, is the sixth most fluent GBM burst detected so far. This paper presents the timing, spectral, and polarimetric analysis of the prompt emission observed using AstroSat and Fermi to provide insight into the prompt emission radiation mechanisms. The time-integrated spectrum shows conclusive proof of two breaks due to peak energy and a second lower energy break. Time-integrated (55.43 +/- 21.30 per cent) as well as time-resolved polarization measurements, made by the Cadmium Zinc Telluride Imager (CZTI) onboard AstroSat, show a hint of high degree of polarization. The presence of a hint of high degree of polarization and the values of low energy spectral index (alpha(pt)) do not run over the synchrotron limit for the first two pulses, supporting the synchrotron origin in an ordered magnetic field. However, during the third pulse, alpha(pt) exceeds the synchrotron line of death in few bins, and a thermal signature along with the synchrotron component in the time-resolved spectra is observed. Furthermore, we also report the earliest optical observations constraining afterglow polarization using the MASTER (P < 1.3 per cent) and the redshift measurement (z = 0.9386) obtained with the 10.4 m GTC (Gran Telescopio Canarias) telescopes. The broad-band afterglow can be described with a forward shock model for an ISM (interstellar medium)-like medium with a wide jet opening angle. We determine a circumburst density of n(0) similar to 7.41, kinetic energy E-K similar to 7.24 x 10(54) erg, and radiated gamma-ray energy E-gamma,E-iso similar to 6.05 x 10(54) erg.},
	keywords = {gamma-ray burst: general; gamma-ray burst: individual: GRB 190530A; polarization; methods: data analysis; telescopes},
	year = {2022},
	eissn = {1365-2966},
	pages = {1694-1713},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:32558149,
	title = {SN 2018agk: A Prototypical Type Ia Supernova with a Smooth Power-law Rise in Kepler (K2)},
	url = {https://m2.mtmt.hu/api/publication/32558149},
	author = {Wang, Qinan and Rest, Armin and Zenati, Yossef and Ridden-Harper, Ryan and Dimitriadis, Georgios and Narayan, Gautham and Villar, V. Ashley and Magee, Mark R. and Foley, Ryan J. and Shaya, Edward J. and Garnavich, Peter and Wang, Lifan and Hu, Lei and Bódi, Attila and Armstrong, Patrick and Auchettl, Katie and Barclay, Thomas and Barentsen, Geert and Sódorné Bognár, Zsófia and Brimacombe, Joseph and Bulger, Joanna and Burke, Jamison and Challis, Peter and Chambers, Kenneth and Coulter, David A. and Csörnyei, Géza and Cseh, Borbála and Deckers, Maxime and Dotson, Jessie L. and Galbany, Lluís and González-Gaitán, Santiago and Gromadzki, Mariusz and Gully-Santiago, Michael and Hanyecz, Ottó and Hedges, Christina and Hiramatsu, Daichi and Hosseinzadeh, Griffin and Howell, D. Andrew and Howell, Steve B. and Huber, Mark E. and Jha, Saurabh W. and Jones, David O. and Könyves-Tóth, Réka and Kalup, Csilla and Kilpatrick, Charles D. and Kriskovics, Levente and Li, Wenxiong and Lowe, Thomas B and Margheim, Steven and McCully, Curtis and Mitra, Ayan and Muñoz, Jose A. and Nicholl, Matt and Nordin, Jakob and Pál, András and Pan, Yen-Chen and Piro, Anthony L. and Rest, Sofia and Rino-Silvestre, João and Rojas-Bravo, César and Sárneczky, Krisztián and Siebert, Matthew R. and Smartt, Stephen J. and Smith, Ken and Sódor, Ádám and Stritzinger, Maximilian D. and Szabó, Róbert and Szakáts, Róbert and Tucker, Brad E. and Vinkó, József and Wang, Xiaofeng and Wheeler, J. Craig and Young, David R. and Zenteno, Alfredo and Zhang, KaiCheng and Zsidi, Gabriella},
	doi = {10.3847/1538-4357/ac2c84},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {923},
	unique-id = {32558149},
	issn = {1538-4357},
	year = {2021},
	eissn = {0004-637X},
	orcid-numbers = {Wang, Qinan/0000-0001-5233-6989; Rest, Armin/0000-0002-4410-5387; Ridden-Harper, Ryan/0000-0003-1724-2885; Dimitriadis, Georgios/0000-0001-9494-179X; Narayan, Gautham/0000-0001-6022-0484; Villar, V. Ashley/0000-0002-5814-4061; Magee, Mark R./0000-0002-0629-8931; Foley, Ryan J./0000-0002-2445-5275; Shaya, Edward J./0000-0002-3234-8699; Garnavich, Peter/0000-0003-4069-2817; Wang, Lifan/0000-0001-7092-9374; Hu, Lei/0000-0001-7201-1938; Bódi, Attila/0000-0002-8585-4544; Armstrong, Patrick/0000-0003-1997-3649; Auchettl, Katie/0000-0002-4449-9152; Barclay, Thomas/0000-0001-7139-2724; Barentsen, Geert/0000-0002-3306-3484; Burke, Jamison/0000-0003-0035-6659; Chambers, Kenneth/0000-0001-6965-7789; Coulter, David A./0000-0003-4263-2228; Deckers, Maxime/0000-0001-8857-9843; Dotson, Jessie L./0000-0003-4206-5649; Galbany, Lluís/0000-0002-1296-6887; González-Gaitán, Santiago/0000-0002-4020-3457; Gromadzki, Mariusz/0000-0002-1650-1518; Gully-Santiago, Michael/0000-0002-4020-3457; Hanyecz, Ottó/0000-0002-9415-5219; Hedges, Christina/0000-0002-3385-8391; Hiramatsu, Daichi/0000-0002-1125-9187; Hosseinzadeh, Griffin/0000-0002-0832-2974; Howell, D. Andrew/0000-0003-4253-656X; Howell, Steve B./0000-0002-2532-2853; Huber, Mark E./0000-0003-1059-9603; Jha, Saurabh W./0000-0001-8738-6011; Jones, David O./0000-0002-6230-0151; Lowe, Thomas B/0000-0002-9438-3617; Margheim, Steven/0000-0001-8205-9441; McCully, Curtis/0000-0001-5807-7893; Mitra, Ayan/0000-0002-9436-8871; Muñoz, Jose A./0000-0001-9833-2959; Nicholl, Matt/0000-0002-2555-3192; Nordin, Jakob/0000-0001-8342-6274; Pan, Yen-Chen/0000-0001-8415-6720; Piro, Anthony L./0000-0001-6806-0673; Rest, Sofia/0000-0002-3825-0553; Rino-Silvestre, João/0000-0003-0793-3287; Rojas-Bravo, César/0000-0002-7559-315X; Siebert, Matthew R./0000-0003-2445-3891; Smartt, Stephen J./0000-0002-8229-1731; Smith, Ken/0000-0001-9535-3199; Stritzinger, Maximilian D./0000-0002-5571-1833; Szabó, Róbert/0000-0002-3258-1909; Tucker, Brad E./0000-0002-4283-5159; Vinkó, József/0000-0001-8764-7832; Wang, Xiaofeng/0000-0002-7334-2357; Wheeler, J. Craig/0000-0003-1349-6538; Young, David R./0000-0002-1229-2499}
}