@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:32944850, title = {SN 2019va: a Type IIP Supernova with Large Influence of Nickel-56 Decay on the Plateau-phase Light Curve}, url = {https://m2.mtmt.hu/api/publication/32944850}, author = {Zhang, Xinghan and Wang, Xiaofeng and Sai, Hanna and Mo, Jun and Nagy, Andrea and Zhang, Jicheng and Cai, Yongzhi and Lin, Han and Zhang, Jujia and Baron, Eddie and DerKacy, James M. and Zhang, Tianmeng and Li, Zhitong and Graham, Melissa and Huang, Fang}, doi = {10.1093/mnras/stac1166}, journal-iso = {MON NOT R ASTRON SOC}, journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}, volume = {513}, unique-id = {32944850}, issn = {0035-8711}, abstract = {We present multiband photometric and spectroscopic observations of the type II supernova, (SN) 2019va, which shows an unusually flat plateau-phase evolution in its V-band light curve. Its pseudo-bolometric light curve even shows a weak brightening towards the end of the plateau phase. These uncommon features are related to the influence of Ni-56 decay on the light curve during the plateau phase, when the SN emission is usually dominated by cooling of the envelope. The inferred Ni-56 mass of SN 2019va is 0.088 +/- 0.018 M-circle dot, which is significantly larger than most SNe II. To estimate the influence of Ni-56 decay on the plateau-phase light curve, we calculate the ratio (dubbed as eta(Ni)) between the integrated time-weighted energy from Ni-56 decay and that from envelope cooling within the plateau phase, obtaining a value of 0.8 for SN 2019va, which is the second largest value among SNe II that has been measured. After removing the influence of Ni-56 decay on the plateau-phase light curve, we found that the progenitor/explosion parameters derived for SN 2019va are more reasonable. In addition, SN 2019va is found to have weaker metal lines in its spectra compared to other SNe IIP at similar epochs, implying a low-metallicity progenitor, which is consistent with the metal-poor environment inferred from the host-galaxy spectrum. We further discuss the possible reasons that might lead to SN 2019va-like events.}, keywords = {supernovae: general; supernovae: individual (SN 2019va); galaxies: individual (UGC 08577)}, year = {2022}, eissn = {1365-2966}, pages = {4556-4572} } @article{MTMT:32541555, title = {Rescued from oblivion: detailed analysis of archival Spitzer data of SN 1993J}, url = {https://m2.mtmt.hu/api/publication/32541555}, author = {Zsíros, Szanna and Nagy, Andrea and Szalai, Tamás}, doi = {10.1093/mnras/stab3075}, journal-iso = {MON NOT R ASTRON SOC}, journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}, volume = {509}, unique-id = {32541555}, issn = {0035-8711}, abstract = {We present an extensive analysis of the late-time mid-infrared (mid-IR) evolution of the Type IIb SN 1993J from 10-26 yr post-explosion based on archival - mostly previously unpublished - photometric data from the Spitzer Space Telescope in conjunction with an archival InfraRed Spectrograph spectrum. SN 1993J is one of the best-studied supernovae (SNe) with an extensive decade-long multiwavelength data set published in various papers; however, its detailed late-time mid-IR analysis is still missing from the literature. Mid-IR data follow not just the continuously cooling SN ejecta but also late-time dust-formation and circumstellar-interaction processes. We provide evidence that the observed late-time mid-IR excess of SN 1993J can be described by the presence of two-component local dust with a dust mass of ~(3.5-6.0) × 10-3 M⊙ in the case of a partly silicate-based dust composition. The source of these components could be either newly formed dust grains or heating of pre-existing dust via ongoing circumstellar matter interaction also detected at other wavelengths. If it is newly formed, the dust is assumed to be located both in the unshocked inner ejecta and in the outer cold dense shell, just as in the Cassiopeia A remnant and also assumed in other dust-forming SNe a few years after explosion.}, keywords = {Astrophysics - Solar and Stellar Astrophysics; circumstellar matter; infrared: stars; supernovae: general; Astrophysics - High Energy Astrophysical Phenomena; supernovae: individual: SN 1993J}, year = {2022}, eissn = {1365-2966}, pages = {3235-3246} } @article{MTMT:31395641, title = {A low-luminosity core-collapse supernova very similar to SN 2005cs}, url = {https://m2.mtmt.hu/api/publication/31395641}, author = {Jäger, Zoltán and Vinkó, József and Bíró, Imre Barna and Hegedüs, Tibor and Borkovits, Tamás and Jäger, Zoltán Sr. and Nagy, Andrea and Molnár, László and Kriskovics, Levente}, doi = {10.1093/mnras/staa1743}, journal-iso = {MON NOT R ASTRON SOC}, journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}, volume = {496}, unique-id = {31395641}, issn = {0035-8711}, keywords = {methods: data analysis; methods: numerical; Astrophysics - Solar and Stellar Astrophysics; techniques: photometric; Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - High Energy Astrophysical Phenomena; instrumentation: photometers; 2012aw; supernovae: individual: PSN J17292918+7542390; 1997D; 1999em; 2004et; 2009md; 2005cs}, year = {2020}, eissn = {1365-2966}, pages = {3725-3740}, orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Borkovits, Tamás/0000-0002-8806-496X} } @article{MTMT:30682388, title = {The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase}, url = {https://m2.mtmt.hu/api/publication/30682388}, author = {Szalai, Tamás and Vinkó, József and Könyves-Tóth, Réka and Nagy, Andrea and Bostroem, K. Azalee and Sárneczky, Krisztián and Brown, Peter J. and Pejcha, Ondrej and Bódi, Attila and Cseh, Borbála and Csörnyei, Géza and Dencs, Zoltán and Hanyecz, Ottó and Ignácz, Bernadett and Kalup, Csilla and Kriskovics, Levente and Ordasi, András and Pál, András and Seli, Bálint and Sódor, Ádám and Szakáts, Róbert and Vida, Krisztián and Zsidi, Gabriella and Konkoly, team and Arcavi, Iair and Ashall, Chris and Burke, Jamison and Galbany, Lluís and Hiramatsu, Daichi and Hosseinzadeh, Griffin and Hsiao, Eric Y. and Howell, D. Andrew and McCully, Curtis and Moran, Shane and Rho, Jeonghee and Sand, David J. and Shahbandeh, Melissa and Valenti, Stefano and Wang, Xiaofeng and Wheeler, J. Craig and Supernova, Project Global}, doi = {10.3847/1538-4357/ab12d0}, journal-iso = {ASTROPHYS J}, journal = {ASTROPHYSICAL JOURNAL}, volume = {876}, unique-id = {30682388}, issn = {1538-4357}, abstract = {The nearby SN 2017eaw is a Type II-P (“plateau”) supernova (SN) showing early-time, moderate CSM interaction. We present a comprehensive study of this SN, including the analysis of high-quality optical photometry and spectroscopy covering the very early epochs up to the nebular phase, as well as near-ultraviolet and near-infrared spectra and early-time X-ray and radio data. The combined data of SNe 2017eaw and 2004et allow us to get an improved distance to the host galaxy, NGC 6946, of D ∼ 6.85 ± 0.63 Mpc; this fits into recent independent results on the distance of the host and disfavors the previously derived (30% shorter) distances based on SN 2004et. From modeling the nebular spectra and the quasi-bolometric light curve, we estimate the progenitor mass and some basic physical parameters for the explosion and ejecta. Our results agree well with previous reports on a red supergiant progenitor star with a mass of ∼15–16 M ⊙. Our estimation of the pre-explosion mass-loss rate (\\dot{M}∼ 3× {10}-7{--}1× {10}-6{M}ȯ yr‑1) agrees well with previous results based on the opacity of the dust shell enshrouding the progenitor, but it is orders of magnitude lower than previous estimates based on general light-curve modeling of Type II-P SNe. Combining late-time optical and mid-infrared data, a clear excess at 4.5 μm can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw.}, keywords = {supernovae: general; supernovae: individual: SN 2017eaw}, year = {2019}, eissn = {0004-637X}, orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Bódi, Attila/0000-0002-8585-4544} } @inbook{MTMT:30605340, title = {Az SN 1987A harminc éve, avagy a jó, a rossz és csúf szupernóva}, url = {https://m2.mtmt.hu/api/publication/30605340}, author = {Nagy, Andrea}, booktitle = {Meteor Csillagászati Évkönyv 2018.}, unique-id = {30605340}, year = {2018}, pages = {235} } @article{MTMT:3400842, title = {Average Opacity Calculation for Core-collapse Supernovae}, url = {https://m2.mtmt.hu/api/publication/3400842}, author = {Nagy, Andrea}, doi = {10.3847/1538-4357/aace56}, journal-iso = {ASTROPHYS J}, journal = {ASTROPHYSICAL JOURNAL}, volume = {862}, unique-id = {3400842}, issn = {1538-4357}, abstract = {Supernovae (SNe) are among the most intensely studied objects of modern astrophysics, but due to their complex physical nature, theoretical models are essential to better understand these exploding stars, as well as the properties of the variation of the emitted radiation. One possibility for modeling SNe light curves (LCs) is the construction of a simplified semianalytic model, which can be used for getting order-of magnitude estimates of the SN properties. One of the strongest simplifications in most of these LC models is the assumption of the constant Thomson-scattering opacity that can be determined as the average opacity of the ejecta. Here we present a systematic analysis for estimating the average opacity in different types of core-collapse supernovae that can be used as the constant opacity of the ejecta in simplified semianalytic models. To use these average opacities self-consistently during LC fit, we estimate their values from hydrodynamic simulations. In this analysis, we first generate MESA stellar models with different physical parameters (initial mass, metallicity, and rotation), which determine the mass-loss history of the model star. Then we synthesize SN LCs from these models with the SNEC hydrodynamic code and calculate the Rosseland mean opacity in every mass element. Finally, we compute the average opacities by integrating these Rosseland mean opacities. As a result, we find that the average opacities from our calculations show adequate agreement with the opacities generally used in previous studies.}, year = {2018}, eissn = {0004-637X} } @article{MTMT:3366737, title = {Absolute Distances to Nearby Type Ia Supernovae via Light Curve Fitting Methods}, url = {https://m2.mtmt.hu/api/publication/3366737}, author = {Vinkó, József and Ordasi, A and Szalai, Tamás and Sarneczky, K and Banyai, E and Bíró, Imre Barna and Borkovits, Tamás and Hegedus, T and Hodosan, G and Kelemen, J and Klagyivik, Péter and Kriskovics, Levente and Kun, Emma and Marion, GH and Marschalkó, Gábor and Molnar, L and Nagy, Andrea and Pal, A and Silverman, JM and Szakáts, Róbert and Szegedi-Elek, E and Székely, Péter and Szing, A and Vida, K and Wheeler, JC}, doi = {10.1088/1538-3873/aab258}, journal-iso = {PUBL ASTRON SOC PAC}, journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC}, volume = {130}, unique-id = {3366737}, issn = {0004-6280}, abstract = {We present a comparative study of absolute distances to a sample of very nearby, bright Type Ia supernovae (SNe) derived from high cadence, high signal-to-noise, multi-band photometric data. Our sample consists of four SNe: 2012cg, 2012ht, 2013dy and 2014J. We present new homogeneous, high-cadence photometric data in Johnson-Cousins BVRI and Sloan g' r' i' z' bands taken from two sites (Piszkesteto and Baja, Hungary), and the light curves are analyzed with publicly available light curve fitters (MLCS2k2, SNooPy2 and SALT2.4). When comparing the best-fit parameters provided by the different codes, it is found that the distance moduli of moderately reddened SNe Ia agree within less than or similar to 0.2 mag, and the agreement is even better (less than or similar to 0.1 mag) for the highest signal-to-noise BVRI data. For the highly reddened SN 2014J the dispersion of the inferred distance moduli is slightly higher. These SN-based distances are in good agreement with the Cepheid distances to their host galaxies. We conclude that the current state-of-the-art light curve fitters for Type Ia SNe can provide consistent absolute distance moduli having less than similar to 0.1-0.2 mag uncertainty for nearby SNe. Still, there is room for future improvements to reach the desired similar to 0.05 mag accuracy in the absolute distance modulus.}, keywords = {photometry; CONSTRAINTS; extinction; ULTRAVIOLET; DUST; MAGNITUDES; DARK ENERGY; HUBBLE-SPACE-TELESCOPE; CONSTANT; HOST GALAXIES; Distances and redshifts; supernovae: individual (SN 2012cg, SN 2012ht, SN 2013dy, SN 2014J)}, year = {2018}, eissn = {1538-3873}, orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Borkovits, Tamás/0000-0002-8806-496X; Kun, Emma/0000-0003-2769-3591; Marschalkó, Gábor/0000-0002-7989-2704} } @article{MTMT:3414249, title = {Calculating the average opacity for core-collapse supernovae}, url = {https://m2.mtmt.hu/api/publication/3414249}, author = {Nagy, Andrea}, journal-iso = {MEMOR SOC ASTRONOM ITAL}, journal = {MEMORIE DELLA SOCIETA ASTRONOMICA ITALIANA - JOURNAL OF THE ITALIAN ASTRONOMICAL SOCIETY}, volume = {88}, unique-id = {3414249}, issn = {0037-8720}, year = {2017}, eissn = {1824-016X}, pages = {274-277} } @article{MTMT:3330281, title = {A new supernova light curve modeling program}, url = {https://m2.mtmt.hu/api/publication/3330281}, author = {Jäger, Zoltán and Nagy, Andrea and Bíró, Imre Barna and Vinkó, József}, journal-iso = {ROMANIAN ASTRONOM J}, journal = {ROMANIAN ASTRONOMICAL JOURNAL}, volume = {27}, unique-id = {3330281}, issn = {1220-5168}, abstract = {Supernovae are extremely energetic explosions that highlight the violent deaths of various types of stars. Studying such cosmic explosions may be important because of several reasons. Supernovae play a key role in cosmic nucleosynthesis processes, and they are also the anchors of methods of measuring extragalactic distances. Several exotic physical processes take place in the expanding ejecta produced by the explosion. We have developed a fast and simple semi-analytical code to model the the light curve of core collapse supernovae. This allows the determination of their most important basic physical parameters, like the the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others.}, keywords = {methods: data analysis; Supernovae; light curve modeling; Extragalactic astronomy}, year = {2017}, eissn = {2285-3758}, pages = {203-210}, orcid-numbers = {Vinkó, József/0000-0001-8764-7832} }