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1. DESI-253.2534+26.8843: A New Einstein Cross Spectroscopically Confirmed with VLT/MUSE and Modeled with GIGA-Lens

Author: Cikota, Aleksandar, Bertolla, Ivonne Toro, Huang, Xiaosheng, Baltasar, Saul, Ratier-Werbin, Nicolas, Sheu, William, Storfer, Christopher, Suzuki, Nao, Schlegel, David J., Cartier, Regis, Torres, Simon, Cikota, Stefan, and Jullo, Eric
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Gravitational lensing provides unique insights into astrophysics and cosmology, including the determination of galaxy mass profiles and constraining cosmological parameters. We present spectroscopic confirmation and lens modeling of the strong lensing system DESI-253.2534+26.8843, discovered in the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys data. This system consists of a massive elliptical galaxy surrounded by four blue images forming an Einstein Cross pattern. We obtained spectroscopic observations of this system using the Multi Unit Spectroscopic Explorer (MUSE) on ESO's Very Large Telescope (VLT) and confirmed its lensing nature. The main lens, which is the elliptical galaxy, has a redshift of $z_{L1} = 0.636\pm 0.001$, while the spectra of the background source images are typical of a starburst galaxy and have a redshift of $z_s = 2.597 \pm 0.001$. Additionally, we identified a faint galaxy foreground of one of the lensed images, with a redshift of $z_{L2} = 0.386$. We employed the GIGA-Lens modeling code to characterize this system and determined the Einstein radius of the main lens to be $\theta_{E} =2.520{''}_{-0.031}^{+0.032}$, which corresponds to a velocity dispersion of $\sigma$ = 379 $\pm$ 2 km s$^{-1}$. Our study contributes to a growing catalog of this rare kind of strong lensing systems and demonstrates the effectiveness of spectroscopic integral field unit observations and advanced modeling techniques in understanding the properties of these systems., Comment: Accepted for publication in ApJL
Published: 2023
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2. An independent determination of the distance to supernova SN 1987A by means of the light echo AT 2019xis

Author: Cikota, Aleksandar, Ding, Jiachen, Wang, Lifan, Baade, Dietrich, Cikota, Stefan, Höflich, Peter, Maund, Justyn, and Yang, Ping
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Accurate distance determination to astrophysical objects is essential for the understanding of their intrinsic brightness and size. The distance to SN 1987A has been previously measured by the expanding photosphere method, and by using the angular size of the circumstellar rings with absolute sizes derived from light curves of narrow UV emission lines, with reported distances ranging from 46.77 kpc to 55 kpc. In this study, we independently determined the distance to SN 1987A using photometry and imaging polarimetry observations of AT 2019xis, a light echo of SN 1987A, by adopting a radiative transfer model of the light echo developed in Ding et al. (2021). We obtained distances to SN 1987A in the range from 49.09 $\pm$ 2.16 kpc to 59.39 $\pm$ 3.27 kpc, depending on the interstellar polarization and extinction corrections, which are consistent with the literature values. This study demonstrates the potential of using light echoes as a tool for distance determination to astrophysical objects in the Milky Way, up to kiloparsec level scales., Comment: Accepted for publication in ApJL
Published: 2023
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3. MARCOT Pathfinder at Calar Alto Progress Report

Author: Roth, Martin M., Aceituno, Jesús, Ortiz, José L., Madhav, Kalaga, Cikota, Stefan, Davenport, John, Amado, Pedro, Pozuelos, Fran, Luque, Rafael, and Morales, Nicolas
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: MARCOT Pathfinder is a precursor for MARCOT (Multi Array of Combined Telescopes) at Calar Alto Observatory (CAHA) in Spain. MARCOT is intended to provide CARMENES, currently fiber-fed from the CAHA 3.5m Telescope, with a 5-15m light collecting area from a battery of several tens of small telescopes that are incoherently fed into the final joint single fiber feed of the spectrograph. The modular concept, based on commercially available telescopes, results in cost estimates that are a fraction of the ones for extremely large telescopes (ELT). As a novel approach, MARCOT will employ Multi-Mode Photonic Lanterns (MM-PL) that are being developed as a variant of classical photonic lanterns, to combine the light from the individual telescopes to a single fiber feed to the instrument. This progress report presents the overall concept of MARCOT, the pathfinder telescope and enclosure that is being commissioned at CAHA, the concept of MM-PL, and the next step of installing the Potsdam Multiplex Raman Spectrograph (MRS). MARCOT Pathfinder will be used to validate the conceptual design and predicted performance of MM-PL on sky with a 7 unit telescope prototype., Comment: 10 pages, 7 figures, submitted to SPIE
Published: 2022

4. Linear spectropolarimetry of 35 Type Ia Supernovae with VLT/FORS: An analysis of the Si II line polarization

Author: Cikota, Aleksandar, Patat, Ferdinando, Wang, Lifan, Wheeler, J. Craig, Bulla, Mattia, Baade, Dietrich, Höflich, Peter, Cikota, Stefan, Clocchiatti, Alejandro, Maund, Justyn R., Stevance, Heloise F., and Yang, Yi
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Spectropolarimetry enables us to measure the geometry and chemical structure of the ejecta in supernova explosions, which is fundamental for the understanding of their explosion mechanism(s) and progenitor systems. We collected archival data of 35 Type Ia Supernovae (SNe Ia), observed with FORS on the Very Large Telescope at 127 epochs in total. We examined the polarization of the Si II $\lambda$6355 $\AA$ line (p$_{\rm Si II}$) as a function of time which is seen to peak at a range of various polarization degrees and epochs relative to maximum brightness. We reproduced the $\Delta$m$_{15}$-p$_{\rm Si II}$ relationship identified in a previous study, and show that subluminous and transitional objects display polarization values below the $\Delta$m$_{15}$-p$_{\rm Si II}$ relationship for normal SNe Ia. We found a statistically significant linear relationship between the polarization of the Si II $\lambda$6355 $\AA$ line before maximum brightness and the Si II line velocity and suggest that this, along with the $\Delta$m$_{15}$-p$_{\rm Si II}$ relationship, may be explained in the context of a delayed-detonation model. In contrast, we compared our observations to numerical predictions in the $\Delta$m$_{15}$-v$_{\rm Si II}$ plane and found a dichotomy in the polarization properties between Chandrasekhar and sub-Chandrasekhar mass explosions, which supports the possibility of two distinct explosion mechanisms. A subsample of SNe display evolution of loops in the $q$-$u$ plane that suggests a more complex Si structure with depth. This insight, which could not be gleaned from total flux spectra, presents a new constraint on explosion models. Finally, we compared our statistical sample of the Si II polarization to quantitative predictions of the polarization levels for the double-detonation, delayed-detonation, and violent-merger models., Comment: 22 pages, accepted for publication in MNRAS
Published: 2019
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5. Pointing System for the Large Size Telescopes Prototype of the Cherenkov Telescope Array

Author: Zarić, Darko, Cikota, Stefan, Fiasson, Armand, Godinović, Nikola, Noda, Koji, Wagner, Robert, Will, Martin, and Piel, Quentin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The pointing system of the prototype of the Large Size Telescope (LST-1) for the Cherenkov Telescope Array observatory, should ensure mapping of the gamma-ray image of a point-like source in the Cherenkov camera to the sky coordinates with a precision better than 14 arcseconds. Detailed studies of the telescope deformations are performed in order to disentangle different deformations and quantify their contributions to the miss-pointing, to learn how to correct for them, and finally how to design the system for offline and online pointing corrections. The LST-1 pointing precision system consist of several devices mounted at the center of the dish: Starguider Camera (SG), Camera Displacement Monitor (CDM), two inclinometers, four distance meters, and an Optical Axis Reference Laser (OARL), working together with the LEDs mounted in a circle around the Cherenkov camera. The online pointing corrections are based on a bending model as currently done by existing IACTs. The offline corrections will be performed combining measurements done by the SG and CDM cameras. SG will provide the position of the Cherenkov camera center with respect to the sky coordinates with a precision of 5 arcseconds, while CDM will provide the deviation of the telescope optical axis defined by the OARL spots with respect to the Cherenkov camera center with a precision better than 5 arcseconds. Laboratory measurements on dedicated test benches showed that the required pointing precision can be achieved for SG, CDM and inclinometer.
Published: 2019

6. Testing the magnetar scenario for superluminous supernovae with circular polarimetry

Author: Cikota, Aleksandar, Leloudas, Giorgos, Bulla, Mattia, Inserra, Cosimo, Chen, Ting-Wan, Spyromilio, Jason, Patat, Ferdinando, Cano, Zach, Cikota, Stefan, Coughlin, Michael W., Kankare, Erkki, Lowe, Thomas B., Maund, Justyn R., Rest, Armin, Smartt, Stephen J., Smith, Ken W., Wainscoat, Richard J., and Young, David R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Superluminous supernovae (SLSNe) are at least $\sim$5 times more luminous than common supernovae (SNe). Especially hydrogen-poor SLSN-I are difficult to explain with conventional powering mechanisms. One possible scenario that might explain such luminosities is that SLSNe-I are powered by an internal engine, such as a magnetar or an accreting black hole. Strong magnetic fields or collimated jets can circularly polarize light. In this work, we measured circular polarization of two SLSNe-I with the FOcal Reducer and low dispersion Spectrograph (FORS2) mounted at the ESO's Very Large Telescope (VLT). PS17bek, a fast evolving SLSN-I, was observed around peak, while OGLE16dmu, a slowly evolving SLSN-I, was observed 100 days after maximum. Neither SLSN shows evidence of circularly polarized light, however, these non-detections do not rule out the magnetar scenario as the powering engine for SLSNe-I. We calculate the strength of the magnetic field and the expected circular polarization as a function of distance from the magnetar, which decreases very fast. Additionally, we observed no significant linear polarization for PS17bek at four epochs, suggesting that the photosphere near peak is close to spherical symmetry., Comment: accepted for publication in MNRAS
Published: 2018
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7. Spectropolarimetry of Galactic stars with anomalous extinction sightlines

Author: Cikota, Aleksandar, Hoang, Thiem, Taubenberger, Stefan, Patat, Ferdinando, Mazzei, Paola, Cox, Nick L. J., Zelaya, Paula, Cikota, Stefan, Tomasella, Lina, Benetti, Stefano, and Rodeghiero, Gabriele
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Highly reddened type Ia Supernovae (SNe Ia) with low total-to-selective visual extinction ratio values, $R_V$, also show peculiar linear polarization wavelength dependencies with peak polarizations at short wavelengths ($\lambda_{max} \lesssim 0.4 \mu m$). It is not clear why sightlines to SNe Ia display such different continuum polarization profiles from interstellar sightlines in the Milky Way with similar $R_V$ values. We investigate polarization profiles of a sample of Galactic stars with low $R_V$ values, along anomalous extinction sightlines, with the aim to find similarities to the polarization profiles that we observe in SN Ia sightlines. We undertook spectropolarimetry of 14 stars, and used archival data for three additional stars, and run dust extinction and polarization simulations to infer a simple dust model that can reproduce the observed extinction and polarization curves. Our sample of Galactic stars with low $R_V$ values and anomalous extinction sightlines displays normal polarization profiles with an average $\lambda_{max} \sim 0.53 {\mu m}$, and is consistent within 3$\sigma$ to a larger coherent sample of Galactic stars from literature. Despite the low $R_V$ values of dust towards the stars in our sample, the polarization curves do not show any similarity to the continuum polarization curves observed towards SNe Ia with low $R_V$ values. There is a correlation between the best-fit Serkowski parameters $K$ and $\lambda_{max}$, but we did not find any significant correlation between $R_V$ and $\lambda_{max}$. Our simulations show that the $K-\lambda_{max}$ relationship is an intrinsic property of polarization. Furthermore, we have shown that in order to reproduce polarization curves with normal $\lambda_{max}$ and low $R_V$ values, a population of large (a $\geq 0.1 \mu m$) interstellar silicate grains must be contained in the dust's composition., Comment: accepted for publication in A&A
Published: 2018
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8. Activity of (2060) Chiron possibly caused by impacts?

Author: Cikota, Stefan, Fernández-Valenzuela, Estela, Ortiz, Jose Luis, Morales, Nicolás, Duffard, René, Aceituno, Jesus, Cikota, Aleksandar, and Santos-Sanz, Pablo
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The centaur 95P/(2060) Chiron is showing comet-like activity since its discovery, but the mass-loss mechanisms triggering its activity remained unexplained. Although the collision rates in the centaur region are expected to be very low, and impacts are thought not to be responsible for the mass-loss, since the recent indications that Chiron might possess a ring similar to Chariklo's, and assuming that there is debris orbiting around, the impact triggered mass-loss mechanism should not be excluded as a possible cause of its activity. From time series observations collected on Calar Alto Observatory in Spain between 2014 and 2016, we found that the photometric scatter in Chiron's data is larger than a control star's scatter, indicating a possible microactivity, possibly caused by debris falling back to Chiron's surface and lifting small clouds of material. We also present rotational light curves, and measurements of Chiron's absolute magnitudes, that are consistent with the models supporting the presumption that Chiron possesses rings. By co-adding the images acquired in 2015, we have detected a $ \sim $5 arcsec long tail, showing a surface brightness of 25.3 mag(V)/arcsec$^{2}$., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS) on 2017 December 28
Published: 2018
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9. Common continuum polarization properties: a possible link between proto-planetary nebulae and Type Ia Supernovae progenitors

Author: Cikota, Aleksandar, Patat, Ferdinando, Cikota, Stefan, Spyromilio, Jason, and Rau, Gioia
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The lines-of-sight to highly reddened SNe Ia show peculiar continuum polarization curves, growing toward blue wavelengths and peaking at $\lambda_{max} \lesssim 0.4 \mu m$, like no other sight line to any normal Galactic star. We examined continuum polarization measurements of a sample of asymptotic giant branch (AGB) and post-AGB stars from the literature, finding that some PPNe have polarization curves similar to those observed along SNe Ia sight lines. Those polarization curves are produced by scattering on circumstellar dust. We discuss the similarity and the possibility that at least some SNe Ia might explode during the post-AGB phase of their binary companion. Furthermore, we speculate that the peculiar SNe Ia polarization curves might provide observational support to the core-degenerate progenitor model., Comment: 6 pages, 2 figures. Accepted for publication in MNRAS
Published: 2017
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10. Spatially resolved analysis of Superluminous Supernovae PTF~11hrq and PTF~12dam host galaxies

Author: Cikota, Aleksandar, De Cia, Annalisa, Schulze, Steve, Vreeswijk, Paul M., Leloudas, Giorgos, Gal-Yam, Avishay, Perley, Daniel A., Cikota, Stefan, Kim, Sam, Patat, Ferdinando, Lunnan, Ragnhild, Quimby, Robert, Yaron, Ofer, Yan, Lin, and Mazzali, Paolo A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: Superluminous supernovae (SLSNe) are the most luminous supernovae in the universe. They are found in extreme star-forming galaxies and are probably connected with the death of massive stars. One hallmark of very massive progenitors would be a tendency to explode in very dense, UV-bright, and blue regions. In this paper we investigate the resolved host galaxy properties of two nearby hydrogen-poor SLSNe, PTF~11hrq and PTF~12dam. For both galaxies \textit{Hubble Space Telescope} multi-filter images were obtained. Additionally, we performe integral field spectroscopy of the host galaxy of PTF~11hrq using the Very Large Telescope Multi Unit Spectroscopic Explorer (VLT/MUSE), and investigate the line strength, metallicity and kinematics. Neither PTF~11hrq nor PTF~12dam occurred in the bluest part of their host galaxies, although both galaxies have overall blue UV-to-optical colors. The MUSE data reveal a bright starbursting region in the host of PTF~11hrq, although far from the SN location. The SN exploded close to a region with disturbed kinematics, bluer color, stronger [OIII], and lower metallicity. The host galaxy is likely interacting with a companion. PTF~12dam occurred in one of the brightest pixels, in a starbursting galaxy with a complex morphology and a tidal tail, where interaction is also very likely. We speculate that SLSN explosions may originate from stars generated during star-formation episodes triggered by interaction. High resolution imaging and integral field spectroscopy are fundamental for a better understanding of SLSNe explosion sites and how star formation varies across their host galaxies., Comment: Accepted for publication in MNRAS
Published: 2017
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11. Linear spectropolarimetry of polarimetric standard stars with VLT/FORS2

Author: Cikota, Aleksandar, Patat, Ferdinando, Cikota, Stefan, and Faran, Tamar
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We reduced ESO's archival linear spectropolarimetry data (4000-9000\AA) of 6 highly polarized and 8 unpolarized standard stars observed between 2010 and 2016, for a total of 70 epochs, with the FOcal Reducer and low dispersion Spectrograph (FORS2) mounted at the Very Large Telescope. We provide very accurate standard stars polarization measurements as a function of wavelength, and test the performance of the spectropolarimetric mode (PMOS) of FORS2. We used the unpolarized stars to test the time stability of the PMOS mode, and found a small ($\leq$0.1%), but statistically significant, on-axis instrumental polarization wavelength dependency, possibly caused by the tilted surfaces of the dispersive element. The polarization degree and angle are found to be stable at the level of $\leq$0.1% and $\leq$0.2 degrees, respectively. We derived the polarization wavelength dependence of the polarized standard stars and found that, in general, the results are consistent with those reported in the literature, e.g. Fossati et al. (2007) who performed a similar analysis using FORS1 data. The re-calibrated data provide a very accurate set of standards that can be very reliably used for technical and scientific purposes. The analysis of the Serkowski parameters revealed a systematic deviation from the width parameter $K$ reported by Whittet et al. (1992). This is most likely explained by incorrect effective wavelengths adopted in that study for the R and I bands., Comment: 12 pages, 10 figures, accepted for publication in MNRAS
Published: 2016
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12. DESI-253.2534+26.8843: A New Einstein Cross Spectroscopically Confirmed with Very Large Telescope/MUSE and Modeled with GIGA-Lens

Author: Cikota, Aleksandar, primary, Bertolla, Ivonne Toro, additional, Huang, Xiaosheng, additional, Baltasar, Saul, additional, Ratier-Werbin, Nicolas, additional, Sheu, William, additional, Storfer, Christopher, additional, Suzuki, Nao, additional, Schlegel, David J., additional, Cartier, Regis, additional, Torres, Simon, additional, Cikota, Stefan, additional, and Jullo, Eric, additional
Published: 2023
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13. An Independent Determination of the Distance to Supernova SN 1987A by Means of the Light Echo AT 2019xis

Author: Cikota, Aleksandar, primary, Ding, Jiachen, additional, Wang, Lifan, additional, Baade, Dietrich, additional, Cikota, Stefan, additional, Höflich, Peter, additional, Maund, Justyn, additional, and Yang, Ping, additional
Published: 2023
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14. MARCOT Pathfinder at Calar Alto progress report

Author: Roth, Martin M., primary, Aceituno, Jesus, additional, Ortiz, Jose L., additional, Madhav, Kalaga, additional, Cikota, Stefan, additional, Davenport, John, additional, Fechner, Thomas, additional, Amado, Pedro J., additional, Pozuelos, Fran J., additional, Luque, Rafael, additional, and Morales, Nicolas, additional
Published: 2022
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15. MARCOT Pathfinder at Calar Alto progress report

Author: Ministerio de Ciencia, Innovación y Universidades (España), Junta de Andalucía, Roth, Martin M., Aceituno, Jesús, Ortiz, José Luis, Madhav, Kalaga, Cikota, Stefan, Davenport, John, Fechner, Thomas, Amado, Pedro J., Pozuelos, Francisco José, Luque, Alejandro, Morales, Nicolás, Ministerio de Ciencia, Innovación y Universidades (España), Junta de Andalucía, Roth, Martin M., Aceituno, Jesús, Ortiz, José Luis, Madhav, Kalaga, Cikota, Stefan, Davenport, John, Fechner, Thomas, Amado, Pedro J., Pozuelos, Francisco José, Luque, Alejandro, and Morales, Nicolás
Abstract: MARCOT Pathfinder is a precursor for MARCOT (Multi Array of Combined Telescopes) at Calar Alto Observatory (CAHA) in Spain. MARCOT is intended to provide CARMENES, currently fiber-fed from the CAHA 3.5m Telescope, with a 5-15m light collecting area from a battery of several tens of small telescopes that are incoherently fed into the final joint single fiber feed of the spectrograph. The modular concept, based on commercially available telescopes, results in cost estimates that are a fraction of the ones for extremely large telescopes (ELT). As a novel approach, MARCOT will employ Multi-Mode Photonic Lanterns (MM-PL) that are being developed as a variant of classical photonic lanterns, to combine the light from the individual telescopes to a single fiber feed to the instrument. This progress report presents the overall concept of MARCOT, the pathfinder telescope and enclosure that is being commissioned at CAHA, the concept of MM-PL, and the next step of installing the Potsdam Multiplex Raman Spectrograph (MRS). MARCOT Pathfinder will be used to validate the conceptual design and predicted performance of MM-PL on sky with a 7-unit telescope prototype. © 2022 SPIE.
Published: 2022

16. Activities on small Solar System bodies and modern methods of determining their physical characteristics

Author: Cikota, Stefan, Babić, Ana, and Ortiz Moreno, José Luis
Subjects: activities, Physics, aktivnosti, observational [methods], individual: (2060) Chiron [asteroids], dwarf planet (136108) Haumea, mala tijela Sunčevog sustava, NATURAL SCIENCES. Physics, small bodies of the solar system, opažačke [metode], in general [comets], rings [planets and natural satellites], PRIRODNE ZNANOSTI. Fizika, stellar astrophysics, općenito [kometi], instrumentacija i metode u astrofizici, prstenovi [planeti i prirodni sateliti], zvjezdana astrofizika, udc:53(043.3), pojedino: (2060) Chiron [asteroidi], Fizika, patuljasti planet (136108) Haumea, instrumentation and methods in astrophysics
Abstract: U Sunčevom sustavu, osim Sunca i planeta, do danas je otkriveno gotovo milijun malih tijela Sunčevog sustava. Zbog njihovih malih dimenzija, oni spadaju u objekte čije istraživanje često zahtijeva teleskope velikih promjera ili primjenu suvremenih opažačkih metoda. Jedna od suvremenih opažačkih metoda određivanja fizikalnih karakteristika malih tijela Sunčevog sustava, koja dozvoljava razlučivosti veće od bilo koje druge zemaljske metode, jest metoda zvjezdanih okultacija. Mala tijela po sastavu i orbitalnim parametrima možemo klasificirati u asteroide i komete. Međutim, među asteroidima se pojavljuje malobrojna skupina objekata koji pokazuju aktivnosti slične kometskim. U doktorskom radu istražena je mikroaktivnost malog tijela 95P/(2060) Chiron. Zbog nedavne indikacije da bi Chiron mogao posjedovati prstenove, njegov mehanizam gubitka mase može biti objašnjen udarima krhotina iz Chironove orbite koje padaju na njegovu površinu. Opažanja su prikupljana na Španjolskoj zvjezdarnici Calar Alto, a za analizu su uglavnom korištene fotometrijske metode. Određivanjem Chironove rotacijske krivulje sjaja i njegove apsolutne zvjezdane veličine, potvrđena je pretpostavka da Chiron posjeduje prstenove. Kao primjer primjene metode zvjezdanih okultacija u svrhu istraživanja fizičkih karakteristika malih tijela Sunčevog sustava, opisano je određivanje veličine, oblika, albeda i gustoće patuljastog planeta Haumea, gornje granice Haumeine atmosfere, te otkriće i karakterizacija prstenova oko glavnog tijela Haumee. U svrhu poboljšanja vremenske razlučivosti opažanja zvjezdanih okultacija s malim tijelima, istražena je i opisana mogućnost primjene atmosferskih Čerenkovljevih teleskopa MAGIC. Njihovi veliki promjeri i osjetljivi fotomultiplikatorski detektori s visokim frekvencijama uzorkovanja, osim za unapređenje razlučivosti u određivanju fizičkih karakteristika malih tijela Sunčevog sustava, mogu biti korišteni za izravna mjerenja promjera zvijezda. U doktorskom radu opisana je metoda određivanja zvjezdanih promjera pomoću detekcije Fresnelovih difrakcijskih uzoraka, koji se mogu opaziti tijekom zvjezdanih okultacija. Detaljno je modeliran signal kakav bi bio opažen teleskopima MAGIC, uzevši u obzir karakteristike teleskopa i osjetljivost detektora. Kroz opažačke prijedloge ostvareno je teleskopsko vrijeme za opažanje zvjezdanih okultacija s MAGIC teleskopima. Extended abstract - Besides the Sun and the planets, our Solar System contains nearly 1 million discovered small Solar System bodies. Due to their small size, they belong to objects whose research often requires large-sized telescopes or the application of modern observation methods. One of today’s modern observational methods used for determining the physical characteristics of the small Solar System bodies, allowing several orders of magnitude better resolutions than any other Earth-based method, is the stellar occultations method. By composition and orbital parameters, small Solar System bodies can be classified into asteroids and comets. Nevertheless, there is a group of asteroid-like objects that show cometlike activities. This doctoral thesis consists of 3 parts. In part one, the observed micro activity of the small Solar System body 95P/(2060) Chiron was investigated. In part two, as an extensive example of the application of the stellar occultation method to investigate the physical characteristics of small Solar System bodies, the determination of the dwarf planet’s Haumea size, shape, albedo, and density was described. In part three, in order to improve the temporal resolution of observations of stellar occultations with small bodies, the potential of using the atmospheric Cherenkov telescopes MAGIC for observing stellar occultations was investigated. Activity of 95P/(2060) Chiron The minor planet 95P/(2060) Chiron belongs to the asteroid group of centaurs, which according to dynamic parameters belongs to asteroids. Chiron has an orbit far away from the Sun, in which sublimation of water ice is not considered as a possible cause for triggering mass loss mechanisms. The expected rate of collisions among small bodies in the region of centaurs is not expected to be high. Regardless of that, since its discovery, Chiron has repeatedly shown indications of cometary activity (Kowal et al. 1979; Tholen et al. 1988; Meech Belton 1990). In 2015, Ortiz et al. (2015) found indications that (2060) Chiron possesses rings. Motivated by these findings, additional observations and interpretations of the cause of its activity were made and described in this doctoral thesis (and published in Cikota et al., 2018). Observations were carried out in three different observation campaigns between 2014 and 2016, using three different instruments located at the Calar Alto Observatory (CAHA) in Almeria, Spain - 3.5 m MOSCA, 1.23 m DLR-MKIII and 2.2 m CAFOS. From the collected observations, amplitudes of Chiron’s rotational light curves and measurements of Chiron’s absolute magnitudes were determined. The measured amplitudes are consistent with the model proposed by Ortiz et al. (2015) which is taking into account both, Chiron’s triangular ellipsoid-like shape and the light contribution of rings around Chiron. Although the frequency of collisions among small bodies in the centaur region is very low, iv due to the recent indication that Chiron possesses rings, and assuming that there is debris orbiting around Chiron, it is well possible that some of this debris may be continually falling and impacting on its surface, producing outbursts and forming a bound or quasi-bound coma. Consequently, a dust release mechanism triggered by impacts should not be excluded as a possible cause for its activity. To study this hypothesis, the scatter in Chiron’s photometric data was compared to the scatter of comparison stars of similar brightness as Chiron. The scatter of Chiron’s photometric measurements for the observations carried out on July 23 and 24, 2014, with the DLR-MKIII 1.23 m CAHA telescope was found to be 0.027 mag, while the comparison star’s scatter is 0.014 mag. During the photometric campaign in 2015, containing data collected with CAFOS 2.2 m CAHA telescope on September 11 and September 13, the scatter of Chiron’s photometric measurements was determined to be 0.029 mag, while the comparison star’s scatter values were 0.018 mag. The noticeable difference between the comparison star’s and Chiron’s photometric scatter supports our hypothesis of continuous micro activity on Chiron. That mechanism could also be a plausible explanation for impulsive brightening on a timescale of hours that have been observed by Luu Jewitt (1990). We hypothesize that some activity outbursts on regular comets could also be triggered by collisions, either with debris orbiting them or with meteoroids. Additionally, the data collected with the CAFOS 2.2 m CAHA telescope over 3 nights between September 11 and September 14, 2015, was used to search for comet-like activity signs like coma or tail. The data was combined to a false-color image of Chiron that contains 95 integrations of 300 s each, resulting in a total integration time of 28500 s (475 min). The combined image of Chiron shows that the coma itself is not detectable, but a very faint asymmetric shape with a measured position angle of ∼ 87◦ was observed. The feature can be explained by a ∼5 arcsec long comet-like tail, of a determined surface brightness of 25.3 mag(R)/arcsec2. Determination of the dwarf planet Haumea’s physical characteristics - Five dwarf planets are currently known in our Solar system. (1) Ceres is the closest dwarf planet to us, and the only dwarf planet orbiting in the inner part of the Solar system, within the main belt of asteroids. Four dwarf planets - (134340) Pluto, (136199) Eris, (136108) Haumea, and (136472) Makemake, are members of the Kuiper belt, located in the outer part of the Solar system beyond Neptune’s orbit. Due to the large distances of dwarf planets in the outer Solar system, indirect observation methods are necessary to accurately determine their physical characteristics. Among trans-Neptunian objects, the dwarf planet Haumea stands out in its elongated shape and extremely short rotation period (Brown et al. 2005; Rabinowitz et al. 2006; Brown et al. 2007). Unlike other dwarf planets (Sicardy et al. 2011; Ortiz et al. 2012; Stern et al. v 2015), Haumea’s physical characteristics were not precisely determined. In this doctoral thesis, the determination of Haumea’s size, shape, albedo, and density was described, as well as the discovery and characterization of its rings (published in Ortiz et al. 2017). On January 21, 2017, a stellar occultation of the dwarf planet Haumea was observed. The occulted star URAT1 533-182543 with its apparent brightness of 𝑚𝑅 = 17.6 mag made it observable already for small- and mid-sized telescopes. Therefore, the occultation event was observed from many locations and resulted in 12 positive detections from 10 different sites across Europe. From the collected sequences of CCD images, photometric measurements of the synthetic aperture were performed. In the case of data collected from the Črni Vrh Observatory by the drift method, a special procedure of photometric analysis was applied to the stellar trail. By fitting a square well model to the collected photometric measurements, the times of the star’s disappearance and reappearance were determined, and occultation chords were generated for each observation location. To the chords in the projected plane, an elliptical limb was fitted by minimizing a 𝜒2 function. By that, the apparent edge of the shape of the ellipse, which represents the outline of Haumea’s shadow, was determined. The determined parameters of the major and minor axis of the ellipse are 1 704 ± 4 km and 1 138 ± 26 km respectively. The position angle of the minor axis is -76.3◦ ± 1.2◦. A search for an atmosphere was performed and the upper value of Haumea’s atmospheric pressure was determined by using the best available data set collected by the Asiago Observatory. From Haumea’s mass, and assuming that the body is in hydrostatic equilibrium, an average surface gravity of 0.39 ms−2 was determined. By comparing a modelled occultation light curve with the observed light curve, the upper value of Haumea’s pure isothermal global atmosphere of 𝑁2 in thermal equilibrium can be determined. Assuming a surface temperature of 40 K, we find a 1 𝜎 upper limit for 𝑝surface(𝑁2) = 3 nbar, and a 3 𝜎 upper limit for 𝑝surface(𝑁2) = 15 nbar. In addition to the main occultation, there are brief dimmings prior to and after the main event. These dips are consistently explained by a narrow and dense ring around Haumea that absorbed about 50% of the incoming stellar flux. A distinct cross-sectional profile of the rings collected in an observation with the 1 m telescope of the Konkoly Observatory reveals a radial ring width of 𝑊ring ≈ 74 km at the occultation ingress and 𝑊ring ≈ 44 km at the occultation egress, with corresponding apparent transparency of p’ = 0.55 and p’ = 0.56. The locations of twelve detected secondary events, projected in the sky plane, allow the retrieval of the full ring orbit, assuming an apparent elliptical shape, and using the same approach as used for fitting Haumea’s limb. The parameters of the elliptical fit to the rings are 𝑎0 ring = 2287+75 −45 km for the apparent semimajor axis, and 𝑏0 ring = 541 ± 23 km for a semiminor axis. The position angle of the minor vi axis is 𝑃ring = -74.3◦ ± 1.3◦. Assuming the rings are circular, it implies a radius of the ring of 𝑟ring = 2287+75 −45 km and an inclination angle of 𝐵ring = 13,8◦ ± 0.5◦. The circular ring assumption is supported by the fact that the center of the ring ellipse coincides with the order of uncertainty with the center of the limb of Haumea’s main body. The position angle of the ring minor axis 𝑃ring = -74.3◦ ±1.3◦ coincides with that of the limb minor axis 𝑃limb = -76.3◦ ± 1.2◦, which is another strong argument that we are observing a ring that settled into Haumea’s equatorial plane. Furthermore, it was found that the radius of the rings coincides with the area where 3:1 spin-orbit resonances are expected. From the determined parameters of Haumea’s limb, a three-dimensional shape and density of Haumea were determined. The obtained parameters of the triaxial ellipsoid a × b × c are (1 161 ± 30) km × (852 ± 2) km × (513 ± 16) km. The mean value of the Haumea density, determined through the parameters of the triangular ellipsoid, and the mass determined by the orbital period of the Hi’iake satellite, is 1 885 ± 80 kg m−3. The geometric albedo of Haumea determined by our observations is 0.51, which is significantly smaller than the value of 0.804, as available in the most recent literature (Fornasier et al. 2013). Application of the atmospheric Cherenkov telescopes MAGIC for observing stellar occultations - In order to accurately determine the physical characteristics of small bodies by using the occultation method, a high temporal resolution of the detector is required. In order to improve the observational methods of stellar occultations, the use of the MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes was considered. With its sensitive central pixel, the MAGIC-II telescope has shown to be an excellent instrument for detecting millisecond flashes in the visible spectra. Compared to any other optical telescope used for observing stellar occultations, its central pixel with a temporal resolution of 10 kHz, combined with a large 17 m aperture, the MAGIC-II telescope enables reaching two orders higher resolutions. However, some of its limiting characteristics are the inability to control the sampling frequency, sensitivity only in the visible spectrum between 300 and 400 nm, and a low angular resolution (due to physically large pixels) responsible for a limitation in the apparent brightness of m = 13.5 ± 0.6 mag. In addition to determining the physical characteristics of small bodies, using the stellar occultation method enables us to determine the angular sizes of the occulted stars. Since stars are not point sources (they have a finite angular diameter), during the occultation of a stellar disk, its light curve does not show a sharp brightness drop but describes a Fresnel interference pattern whose details depend on the angular diameter of the occulted star. High sampling rates make it possible to record these interference patterns. Therefore, the high temporal resolution vii of the detector is the key for direct measurements of stellar radii. In this doctoral thesis, the method of determining stellar radii by observing Fresnel diffraction patterns that can be detected during stellar occultations is described. Models of the expected signal were performed, taking into account the characteristics of the MAGIC telescopes and the sensitivity of its detectors. Through observational proposals, telescope time was granted and first observations of stellar occultations with the MAGIC telescopes were acquired. Additionally, the effects of limb darkening of stellar disks were investigated. It was found that diffraction patterns formed by occultations of large disks with angular diameters of 0.7 mas and high limb darkening factors of u = 1.0 deviate in intensity up to approximately 5% from diffraction patterns of homogeneously illuminated stellar disks (u = 0.0). For stellar disks of smaller diameters or smaller limb darkening factors, the intensity deviations are smaller. These deviations in the intensity of diffraction patterns are reflected in the determination of the angular diameters of stellar disks. It was found that the angular radius of a homogeneously illuminated stellar disk, compared to a disk with a limb darkening factor of u = 1.0 taken into account, deviates by approximately 12.4%. Taking the limb darkening factors into account contributes to the accuracy of measurements of the angular diameters of stellar disks, but to achieve this accuracy, photometric measurements with uncertainties below 5% are required. Historically, almost all measurements of the stellar radii smaller than ∼1 arc millisecond have been performed by interferometric measurements. Measurements of stellar radii by observing occultations with asteroids allow reaching angular resolutions up to 0.1 milliarcseconds, which is at least a factor of two larger than the one available through interferometric measurements, and a factor of 10 larger than what can be achieved by observing lunar occultations. Therefore, the asteroid occultation method is extremely useful for measuring the angular diameters of stars below 1 milliarcsecond. In the period from December 2017 to February 2020, a total of 6 occultation observations with the MAGIC-II telescope were scheduled. Four observations were not successfully acquired due to bad weather or technical reasons. Two occultation events, those by the small bodies (83) Beatrix and (28) Bellona, were successfully acquired but resulted in a negative detection. Although the occultation events of (83) Beatrix and (28) Bellona occurred over sufficiently bright sources, and their probability of observation was estimated at 99%, the negative detections can be explained by a too small brightness drops, ∼1.5 mag for the (83) Beatrix event (2.5 𝜎), and ∼0.9 mag for the (28) Bellona event (1.5 𝜎). Based on the analysis presented in this thesis, we expect that any event with a brightness drop larger than 1.8-3.0 mag (3-5 𝜎 above background noise) should be detected. Therefore, the observation campaign of occultations on MAGIC telescopes will be continued in the future.
Published: 2022

17. Multiwavelength variability and correlation studies of Mrk421 during historically low X-ray and γ-ray activity in 2015–2016

Author: Banerjee, Biswajit, primary, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Baack, Dominik, additional, Babić, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra González, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Berti, Alessio, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bošnjak, Željka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinović, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jimenez-Martinez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, López-Coto, Rubén, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martínez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Nava, Lara, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Noda, Koji, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel C., additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Temnikov, Petar, additional, Terzić, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, Zarić, Darko, additional, Balbo, Matteo, additional, Bretz, Thomas, additional, Buss, Jens, additional, Eisenberger, Laura, additional, Hildebrand, Dorothee, additional, Iotov, Roman, additional, Kalenski, Adelina, additional, Mitchell, Alison, additional, Neise, Dominik, additional, Noethe, Maximilian, additional, Paravac, Aleksander, additional, Sliusar, Vitalii, additional, Walter, Roland, additional, Valverde, J., additional, Horan, D., additional, Giroletti, M., additional, Perri, M., additional, Verrecchia, F., additional, Leto, C., additional, C. Sadun, A., additional, W. Moody, J., additional, Joner, M., additional, P. Marscher, A., additional, G. Jorstad, S., additional, Lähteenmäki, A., additional, ~Tornikoski, M., additional, Ramakrishnan, V., additional, Järvelä, E., additional, J. C. Vera, R., additional, Righini, S., additional, and Y. Lien, A., additional
Published: 2021
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18. Observation of a relatively low luminosity long duration GRB 201015A by the MAGIC telescopes

Author: Suda, Yusuke, primary, Artero, Manuel, additional, Asano, Katsuaki, additional, Berti, Alessio, additional, Nava, Lara, additional, Noda, Koji, additional, Terauchi, Kenta, additional, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Baack, Dominik, additional, Babic, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra Gonzalez, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bosnjak, Zeljka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinovic, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jiménez Martínez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, Lopez-Coto, Ruben, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martinez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Temnikov, Petar, additional, Terzic, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo Francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, and Zarić, Darko, additional
Published: 2021
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19. MAGIC and H.E.S.S. detect VHE gamma rays from the blazar OT081 for the first time: a deep multiwavelength study

Author: Manganaro, Marina, primary, Seglar-Arroyo, Monica, additional, Becerra-González, Josefa, additional, Sanchez, David, additional, Cerruti, Matteo, additional, Tavecchio, Fabrizio, additional, Fallah-Ramazani, Vandad, additional, Agudo, Ivan, additional, Ciprini, Stefano, additional, Filippenko, Alexei Vladimir, additional, Esteban-Gutierrez, A., additional, Hovatta, Talvikki, additional, Jermak, Helen, additional, Jorstad, Svetlana G., additional, Kopatskaya, Evgenia N., additional, Larionov, Valeri M., additional, Larionova, L. V., additional, Lähteenmäki, Anne, additional, Marscher, Alan, additional, Morozova, D. A., additional, Pahljina, Marko, additional, Tornikoski, Merja, additional, Troitskaya, Yuliya, additional, Troitsky, I., additional, Verrecchia, Francesco, additional, Xiao, H. B., additional, Weaver, Z. R., additional, Zheng, Weikang, additional, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Baack, Dominik, additional, Babic, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra Gonzalez, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Berti, Alessio, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bosnjak, Zeljka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinovic, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jiménez Martínez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, Lopez-Coto, Ruben, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martinez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Nava, Lara, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Noda, Koji, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel C., additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Temnikov, Petar, additional, Terzic, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, and Zarić, Darko, additional
Published: 2021
Full Text: View/download PDF

20. Protons Spectrum from MAGIC Telescopes data

Author: Temnikov, Petar, primary, VERGUILOV, Vassil, additional, Maneva, Galina, additional, Mirzoyan, Razmik, additional, Baack, Dominik, additional, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Babić, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra González, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Berti, Alessio, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bošnjak, Željka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinović, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jiménez Martínez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, López-Coto, Rubén, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martínez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Nava, Lara, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Noda, Koji, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel, additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Terzić, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, Vigorito, Carlo Francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, and Zarić, Darko, additional
Published: 2021
Full Text: View/download PDF

21. MAGIC observations of the nearby short GRB 160821B

Author: Noda, Koji, primary, Nava, Lara, additional, Inoue, Susumu, additional, Fukami, Satoshi, additional, Palatiello, Michele, additional, Berti, Alessio, additional, Longo, Francesco, additional, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Baack, Dominik, additional, Babic, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra Gonzalez, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bosnjak, Zeljka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinovic, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jiménez Martínez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Lopez-Coto, Ruben, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martinez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel, additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Temnikov, Petar, additional, Terzic, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo Francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, and Zarić, Darko, additional
Published: 2021
Full Text: View/download PDF

22. Recent MAGIC results on Galactic binaries

Author: Molina, Edgar, primary, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Baack, Dominik, additional, Babić, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra González, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Berti, Alessio, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bošnjak, Željka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinović, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jimenez-Martinez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, López-Coto, Rubén, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martínez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Nava, Lara, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Noda, Koji, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Satalecka, Konstancja, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel C., additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Temnikov, Petar, additional, Terzić, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, and Zarić, Darko, additional
Published: 2021
Full Text: View/download PDF

23. Multi-epoch monitoring of TXS 0506+056 with MAGIC and MWL partners

Author: Satalecka, Konstancja, primary, Acciari, Victor A., additional, Ansoldi, Stefano, additional, Antonelli, Lucio Angelo, additional, Arbet Engels, Axel, additional, Artero, Manuel, additional, Asano, Katsuaki, additional, Baack, Dominik, additional, Babic, Ana, additional, Baquero, Andrés, additional, Barres de Almeida, Ulisses, additional, Barrio, Juan Abel, additional, Batković, Ivana, additional, Becerra Gonzalez, Josefa, additional, Bednarek, Wlodek, additional, Bellizzi, Lorenzo, additional, Bernardini, Elisa, additional, Bernardos, Maria-Isabel, additional, Berti, Alessio, additional, Besenrieder, Jürgen, additional, Bhattacharyya, Wrijupan, additional, Bigongiari, Ciro, additional, Biland, Adrian, additional, Blanch, Oscar, additional, Bökenkamp, Hendrik, additional, Bonnoli, Giacomo, additional, Bosnjak, Zeljka, additional, Busetto, Giovanni, additional, Carosi, Roberto, additional, Ceribella, Giovanni, additional, Cerruti, Matteo, additional, Chai, Yating, additional, Chilingarian, Ashot Agassi, additional, Cikota, Stefan, additional, Colak, Sidika Merve, additional, Colombo, Eduardo, additional, Contreras, Jose Luis, additional, Cortina, Juan, additional, Covino, Stefano, additional, D'Amico, Giacomo, additional, D'Elia, Valerio, additional, Da Vela, Paolo, additional, Dazzi, Francesco, additional, De Angelis, Alessandro, additional, De Lotto, Barbara, additional, Delfino, Manuel, additional, Delgado, Jordi, additional, Delgado Mendez, Carlos, additional, Depaoli, Davide, additional, Di Pierro, Federico, additional, Di Venere, Leonardo, additional, Do Souto Espiñeira, Elia, additional, Dominis Prester, Dijana, additional, Donini, Alice, additional, Dorner, Daniela, additional, Doro, Michele, additional, Elsaesser, Dominik, additional, Fallah Ramazani, Vandad, additional, Fattorini, Alicia, additional, Fonseca, Maria Victoria, additional, Font, Lluis, additional, Fruck, Christian, additional, Fukami, Satoshi, additional, Fukazawa, Yasushi, additional, García López, Ramon J., additional, Garczarczyk, Markus, additional, Gasparyan, Sargis, additional, Gaug, Markus, additional, Giglietto, Nicola, additional, Giordano, Francesco, additional, Gliwny, Pawel, additional, Godinovic, Nikola, additional, Green, David, additional, Green, Jarred Gershon, additional, Hadasch, Daniela, additional, Hahn, Alexander, additional, Heckmann, Lea, additional, Herrera, Javier, additional, Hoang, John, additional, Hrupec, Dario, additional, Hütten, Moritz, additional, Inada, Tomohiro, additional, Ishio, Kazuma, additional, Iwamura, Yuki, additional, Jiménez Martínez, Irene, additional, Jormanainen, Jenni, additional, Jouvin, Léa, additional, Karjalainen, Marie, additional, Kerszberg, Daniel, additional, Kobayashi, Yukiho, additional, Kubo, Hidetoshi, additional, Kushida, Junko, additional, Lamastra, Alessandra, additional, LELAS, Damir, additional, Leone, Francesco, additional, Lindfors, Elina, additional, Linhoff, Lena, additional, Lombardi, Saverio, additional, Longo, Francesco, additional, Lopez-Coto, Ruben, additional, López-Moya, Marcos, additional, López-Oramas, Alicia, additional, Loporchio, Serena, additional, Machado de Oliveira Fraga, Bernardo, additional, Maggio, Camilla, additional, Majumdar, Pratik, additional, MAKARIEV, Martin, additional, Mallamaci, Manuela, additional, Maneva, Galina, additional, Manganaro, Marina, additional, Mannheim, Karl, additional, Maraschi, Laura, additional, Mariotti, Mosè, additional, Martinez, Manel, additional, Mazin, Daniel, additional, Menchiari, Stefano, additional, Mender, Simone, additional, Mićanović, Saša, additional, Miceli, Davide, additional, Miener, Tjark, additional, Miranda, Jose Miguel, additional, Mirzoyan, Razmik, additional, Molina, Edgar, additional, Moralejo, Abelardo, additional, Morcuende, Daniel, additional, Moreno, Victoria, additional, Moretti, Elena, additional, Nakamori, Takeshi, additional, Nava, Lara, additional, Neustroev, Vitaly, additional, Nigro, Cosimo, additional, Nilsson, Kari, additional, Nishijima, Kyoshi, additional, Noda, Koji, additional, Nozaki, Seiya, additional, Ohtani, Yoshiki, additional, Oka, Tomohiko, additional, Otero-Santos, Jorge, additional, Paiano, Simona, additional, Palatiello, Michele, additional, Paneque, David, additional, Paoletti, Riccardo, additional, Paredes, Josep M., additional, Pavletić, Lovro, additional, Peñil, Pablo, additional, Persic, Massimo, additional, Pihet, Marine, additional, Prada Moroni, Pier Giorgio, additional, Prandini, Elisa, additional, Priyadarshi, Chaitanya, additional, Puljak, Ivica, additional, Rhode, Wolfgang, additional, Ribó, Marc, additional, Rico, Javier, additional, Righi, Chiara, additional, Rugliancich, Andrea, additional, Sahakyan, Narek, additional, Saito, Takayuki, additional, Sakurai, Shunsuke, additional, Saturni, Francesco Gabriele, additional, Schleicher, Bernd, additional, Schmidt, Kevin, additional, Schweizer, Thomas, additional, Sitarek, Julian, additional, Šnidarić, Iva, additional, Sobczyńska, Dorota, additional, Spolon, Alessia, additional, Stamerra, Antonio, additional, Strišković, Jelena, additional, Strom, Derek, additional, Strzys, Marcel, additional, Suda, Yusuke, additional, Surić, Tihomir, additional, Takahashi, Mitsunari, additional, Takeishi, Ryuji, additional, Tavecchio, Fabrizio, additional, Temnikov, Petar, additional, Terzic, Tomislav, additional, Teshima, Masahiro, additional, Tosti, Luca, additional, Truzzi, Stefano, additional, Tutone, Antonio, additional, Ubach, Santiago, additional, van Scherpenberg, Juliane, additional, Vanzo, Gaia, additional, VAZQUEZ ACOSTA, Monica, additional, Ventura, Sofia, additional, VERGUILOV, Vassil, additional, Vigorito, Carlo Francesco, additional, Vitale, Vincenzo, additional, Vovk, Ievgen, additional, Will, Martin, additional, Wunderlich, Carolin, additional, Yamamoto, Tokonatsu, additional, Zarić, Darko, additional, Aniello, Tommaso, additional, D'Ammando, Filippo, additional, Viale, Ilaria, additional, Hovatta, Talvikki, additional, Edwards, Philip G., additional, Kiehlmann, Sebastian, additional, Readhead, Anthony, additional, Kadler, Matthias, additional, Bach, Uwe, additional, Berge, David, additional, Buson, Sara, additional, Eppel, Florian, additional, Giroletti, Marcello, additional, Hervet, Olivier, additional, Gokus, Andrea, additional, Heßdörfer, Jonas, additional, Koyama, Shoko, additional, Kraus, Alex, additional, Krichbaum, Thomas, additional, de Menezes, Raniere, additional, Ojha, Roopesh, additional, Paraschos, Georgios, additional, Pueschel, Elisa, additional, Rösch, Florian, additional, Ros, Eduardo, additional, Sinapius, Jonas, additional, Wilms, Jörn, additional, Zacharias, Michael, additional, and Stevens, Jamie, additional
Published: 2021
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24. MARCOT Pathfinder at Calar Alto progress report

Author: Marshall, Heather K., Spyromilio, Jason, Usuda, Tomonori, Roth, Martin M., Aceituno, Jesús, Ortiz, José L., Madhav, Kalaga, Cikota, Stefan, Davenport, John, Fechner, Thomas, Amado, Pedro, Pozuelos, Fran J., Luque, Rafael, and Morales, Nicolas
Published: 2022
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25. Detection of sub-TeV gamma-ray emission from the flaring blazar TXS 1515-273 with the MAGIC telescopes

Author: Mirzoyan, Razmik, Babić, Ana, Bošnjak, Željka, Cikota, Stefan, Dominis Prester, Dijana, Godinović, Nikola, Hrupec, Dario, Lelas, Damir, Manganaro, Marina, Mićanović, Saša, Puljak, Ivica, Surić, Tihomir, Šnidarić, Iva, Terzić, Tomislav, and Zarić, Darko
Subjects: Gamma Ray, GeV%22">>GeV, TeV, VHE, AGN, Blazar
Abstract: The MAGIC collaboration reports the first detection of very-high-energy (VHE ; E>100 GeV) gamma-ray emission from the flaring blazar TXS1515-273 (RA=15 18 03.610, Dec= -27 31 31.40, J2000.0). The object was observed with the MAGIC telescopes for 1.9 hours on 2019/02/28 under moderate moonlight in the zenith distance range 55 - 60 deg. The preliminary real-time analysis of this data shows a detection of TXS1515-273 with a statistical significance more than 5 standard deviations. The MAGIC observations were triggered by the flaring activity reported by Fermi-LAT from 2019/02/24 to 2019/02/25 (ATel#12532). Few hours before that ATel, a communication from Dave Thompson from the Fermi team alerted the MAGIC collaboration about this source. The redshift of this source is uncertain, with an upper limit z
Published: 2019

26. First time detection of a GRB at sub-TeV energies ; MAGIC detects the GRB 190114C

Author: Mirzoyan, Razmik, Babić, Ana, Bošnjak, Željka, Cikota, Stefan, Dominis Prester, Dijana, Godinović, Nikola, Hrupec, Dario, Lelas, Damir, Manganaro, Marina, Mićanović, Saša, Puljak, Ivica, Surić, Tihomir, Šnidarić, Iva, Terzić, Tomislav, Zarić, Darko, and (the MAGIC Collaboration)
Subjects: Gamma Ray, GeV%22">>GeV, TeV, VHE, Request for Observations, Gamma-Ray Burst
Abstract: The MAGIC telescopes performed a rapid follow-up observation of GRB 190114C (Gropp et al., GCN 23688 ; Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN 23693, Selsing et al. GCN 23695). This observation was triggered by the Swift-BAT alert ; we started observing at about 50s after Swift T0: 20:57:03.19. The MAGIC real-time analysis shows a significance >20 sigma in the first 20 min of observations (starting at T0+50s) for energies >300GeV. The relatively high detection threshold is due to the large zenith angle of observations (>60 degrees) and the presence of partial Moon. Given the brightness of the event, MAGIC will continue the observation of GRB 190114C until it is observable tonight and also in the next days. We strongly encourage follow-up observations by other instruments. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and K. Noda (nodak@icrr.u-tokyo.ac.jp). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
Published: 2019

27. MAGIC detection of an increased activity from BL Lacertae at very-high-energy gamma rays

Author: Mirzoyan, Razmik, Babić, Ana, Bošnjak, Željka, Cikota, Stefan, Dominis Prester, Dijana, Godinović, Nikola, Hrupec, Dario, Lelas, Damir, Manganaro, Marina, Mićanović, Saša, Puljak, Ivica, Surić, Tihomir, Šnidarić, Iva, Terzić, Tomislav, and Zarić, Darko.
Subjects: Gamma Ray, GeV%22">>GeV, TeV, VHE, Request for Observations, AGN, Blazar, Quasar
Abstract: The MAGIC telescopes have observed an increase in the very-high-energy (VHE ; >100 GeV) gamma-ray flux from a position compatible with the blazar BL Lacertae (RA=22h02m43.3s Dec=+42d16m40s, J2000.0, z=0.07). The preliminary analysis of 0.76 hours of MAGIC data taken on 2019/05/03 (MJD 58606.18 to 58606.20) under zenith angle range from 46 to 53 deg and dark time conditions with the atmospheric transmission of 0.85, indicates a flux larger than 0.1 of the flux from the Crab nebula above 200 GeV, and detection significance over 6 sigma. The MAGIC observations were triggered by the flaring activity at HE gamma-rays reported by Fermi-LAT (ATel #12718), and optical observations by Astronomical Observatory of the University of Siena (ATel #12722). MAGIC observations on BL Lacertae will continue during the next days and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and D. Dominis Prester (dijana@phy.uniri.hr) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
Published: 2019

28. MAGIC detects an unprecedented activity from the blazar 1ES 1218+304 at very high energy gamma rays

Author: Mirzoyan, Razmik, Babić, Ana, Bošnjak, Željka, Cikota, Stefan, Dominis Prester, Dijana, Godinović, Nikola, Hrupec, Dario, Lelas, Damir, Manganaro, Marina, Mićanović, Saša, Puljak, Ivica, Surić, Tihomir, Šnidarić, Iva, Terzić, Tomislav, Zarić, Darko, and (the MAGIC Collaboration)
Subjects: Gamma Ray, GeV%22">>GeV, TeV, VHE, AGN, Blazar
Abstract: The MAGIC telescopes have observed an unprecedented level of very-high-energy (VHE ; >100 GeV) gamma-ray flux from 1ES 1218+304 (12h21m21.941s, +30d10m37.11s, J2000.0). The preliminary analysis of the data from 2018/12/31 to 2019/01/02 indicates a VHE gamma-ray flux reaching the level of ~25 % of the flux from the Crab nebula above 100 GeV. Compared to the quiescent state reported by VERITAS, this implies an increase by a factor of ~4. The previous record of VHE gamma-ray flux of this source was ~20% of the flux from the Crab nebula above 100 GeV. It was measured by VERITAS on the night of 30 January 2009 (2010ApJ, 709L, 163A). 1ES 1218+304 is a high-synchrotron-peaked BL Lac object located at redshift z=0.182. It was first recognized as a VHE gamma-ray emitter by the MAGIC Collaboration in 2005 (Albert, J., 2006, ApJ, 642L, 119A). The MAGIC observations were triggered by the flaring activity in the optical R-band, measured by the KVA telescope from 2018/12/24 to 2019/01/02. The KVA data showed a flux of 2.35+/-0.05 mJy on 2019/01/02, which is the highest optical flux measurement from this source in a time span of 15 years (http://users.utu.fi/kani/1m/1ES_1218+304_jy.html). MAGIC observations on 1ES 1218+304 will continue during the next weeks and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), V. Fallah Ramazani (vafara@utu.fi) and M. Cerruti (matteo.cerruti@icc.ub.edu). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
Published: 2019

29. MAGIC detects enhanced flux of VHE gamma rays from TXS 0506+056

Author: Mirzoyan, Razmik, Babić, Ana, Cikota, Stefan, Dominis Prester, Dijana, Godinović, Nikola, Hrupec, Dario, Lelas, Damir, Manganaro, Marina, Mićanović, Saša, Puljak, Ivica, Surić, Tihomir, Šnidarić, Iva, Terzić, Tomislav, Zarić, Darko, and (the MAGIC Collaboration)
Subjects: Gamma Ray, GeV%22">>GeV, TeV, VHE, AGN, Blazar
Abstract: We report an enhanced emission of VHE gamma-rays from the direction of the blazar TXS 0506+056 (05 09 25.96370, +05 41 35.3279 (J2000), [Lani et al., Astron. J., 139, 1695-1712 (2010)]), located 6 arcmin from the estimated direction of the high energy IceCube neutrino event IceCube-170922A (ATel #10791). On Dec 3rd 2018 the MAGIC telescopes observed this source for about 2 hours under good weather conditions. The source was detected at VHE gamma-rays above 90 GeV with a significance larger than 5 sigma. The preliminary analysis yields an estimate of the VHE gamma-ray flux above 90 GeV of ~10-15% of the flux from the Crab Nebula above the same energy threshold, and a spectral index of ~4. This flux is consistent with the emission level integrated between September 28th 2017 to October 3rd 2017, when the source was discovered at VHE gamma-rays (ATel #10817). The MAGIC telescopes will continue monitoring the VHE gamma-ray emission of TXS 0506+056. Soft-X-rays and ultraviolet ToO observations with the Neil Gehrels Swift Observatory have been approved for the next three nights (PI: Cerruti, on behalf of MAGIC), to occur within the time-window 00:00 to 04:00 UTC. NuSTAR ToO observations have also been approved (PI: Satalecka). Multi-wavelength observations (quasi)-simultaneous with MAGIC in this time-window are strongly encouraged.
Published: 2018

30. Linear spectropolarimetry of 35 Type Ia supernovae with VLT/FORS: an analysis of the Si ii line polarization

Author: Cikota, Aleksandar, primary, Patat, Ferdinando, additional, Wang, Lifan, additional, Wheeler, J Craig, additional, Bulla, Mattia, additional, Baade, Dietrich, additional, Höflich, Peter, additional, Cikota, Stefan, additional, Clocchiatti, Alejandro, additional, Maund, Justyn R, additional, Stevance, Heloise F, additional, and Yang, Yi, additional
Published: 2019
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31. Spectropolarimetry of Galactic stars with anomalous extinction sightlines

Author: Cikota, Aleksandar, primary, Hoang, Thiem, additional, Taubenberger, Stefan, additional, Patat, Ferdinando, additional, Mazzei, Paola, additional, Cox, Nick L.J., additional, Zelaya, Paula, additional, Cikota, Stefan, additional, Tomasella, Lina, additional, Benetti, Stefano, additional, and Rodeghiero, Gabriele, additional
Published: 2018
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32. Withdrawn as Duplicate: Testing the magnetar scenario for superluminous supernovae with circular polarimetry

Author: Cikota, Aleksandar, primary, Leloudas, Giorgos, additional, Bulla, Mattia, additional, Inserra, Cosimo, additional, Chen, Ting-Wan, additional, Spyromilio, Jason, additional, Patat, Ferdinando, additional, Cano, Zach, additional, Cikota, Stefan, additional, Coughlin, Michael W, additional, Kankare, Erkki, additional, Lowe, Thomas B, additional, Maund, Justyn R, additional, Rest, Armin, additional, Smartt, Stephen J, additional, Smith, Ken W, additional, Wainscoat, Richard J, additional, and Young, David R, additional
Published: 2018
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33. Testing the magnetar scenario for superluminous supernovae with circular polarimetry

Author: Cikota, Aleksandar, primary, Leloudas, Giorgos, additional, Bulla, Mattia, additional, Inserra, Cosimo, additional, Chen, Ting-Wan, additional, Spyromilio, Jason, additional, Patat, Ferdinando, additional, Cano, Zach, additional, Cikota, Stefan, additional, Coughlin, Michael W, additional, Kankare, Erkki, additional, Lowe, Thomas B, additional, Maund, Justyn R, additional, Rest, Armin, additional, Smartt, Stephen J, additional, Smith, Ken W, additional, Wainscoat, Richard J, additional, and Young, David R, additional
Published: 2018
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34. Activity of (2060) Chiron possibly caused by impacts?

Author: Cikota, Stefan, primary, Fernández-Valenzuela, Estela, primary, Ortiz, Jose Luis, primary, Morales, Nicolás, primary, Duffard, René, primary, Aceituno, Jesus, primary, Cikota, Aleksandar, primary, and Santos-Sanz, Pablo, primary
Published: 2018
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35. Spatially resolved analysis of superluminous supernovae PTF 11hrq and PTF 12dam host galaxies

Author: Cikota, Aleksandar, De Cia, Annalisa, Schulze, Steve, Vreeswijk, Paul M., Leloudas, Giorgos, Gal-Yam, Avishay, Perley, Daniel A., Cikota, Stefan, Kim, Sam, Patat, Ferdinando, Lunnan, Ragnhild, Quimby, Robert, Yaron, Ofer, Yan, Lin, Mazzali, Paolo A., Cikota, Aleksandar, De Cia, Annalisa, Schulze, Steve, Vreeswijk, Paul M., Leloudas, Giorgos, Gal-Yam, Avishay, Perley, Daniel A., Cikota, Stefan, Kim, Sam, Patat, Ferdinando, Lunnan, Ragnhild, Quimby, Robert, Yaron, Ofer, Yan, Lin, and Mazzali, Paolo A.
Published: 2017

36. Common continuum polarization properties: a possible link between proto-planetary nebulae and Type Ia Supernova progenitors

Author: Cikota, Aleksandar, primary, Patat, Ferdinando, primary, Cikota, Stefan, primary, Spyromilio, Jason, primary, and Rau, Gioia, primary
Published: 2017
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37. Spatially resolved analysis of superluminous supernovae PTF 11hrq and PTF 12dam host galaxies

Author: Cikota, Aleksandar, primary, De Cia, Annalisa, additional, Schulze, Steve, additional, Vreeswijk, Paul M., additional, Leloudas, Giorgos, additional, Gal-Yam, Avishay, additional, Perley, Daniel A., additional, Cikota, Stefan, additional, Kim, Sam, additional, Patat, Ferdinando, additional, Lunnan, Ragnhild, additional, Quimby, Robert, additional, Yaron, Ofer, additional, Yan, Lin, additional, and Mazzali, Paolo A., additional
Published: 2017
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38. Linear spectropolarimetry of polarimetric standard stars with VLT/FORS2

Author: Cikota, Aleksandar, primary, Patat, Ferdinando, additional, Cikota, Stefan, additional, and Faran, Tamar, additional
Published: 2016
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39. Linear spectropolarimetry of polarimetric standard stars with VLT/FORS2.

Author: Cikota, Aleksandar, Patat, Ferdinando, Cikota, Stefan, and Faran, Tamar
Subjects: ASTROPHYSICAL spectropolarimetry, ASTRONOMICAL observations, SPECTROGRAPHS, VERY large telescopes, WAVELENGTHS
Abstract: We reduced European Southern Observatory's archival linear spectropolarimetry data (4000-9000 Å) of six highly polarized and eight unpolarized standard stars observed between 2010 and 2016, for a total of 70 epochs, with the FOcal Reducer and low dispersion Spectrograph (FORS2) mounted at the Very Large Telescope. We provide very accurate standard stars polarization measurements as a function of wavelength, and test the performance of the spectropolarimetric mode (PMOS) of FORS2.We used the unpolarized stars to test the time stability of the PMOS mode, and found a small (≤0.1 per cent), but statistically significant, on-axis instrumental polarization wavelength dependence, possibly caused by the tilted surfaces of the dispersive element. The polarization degree and angle are found to be stable at the level of ≤0.1 per cent and ≤0.2 degrees, respectively. We derived the polarization wavelength dependence of the polarized standard stars and found that, in general, the results are consistent with those reported in the literature, e.g. Fossati et al., who performed a similar analysis using FORS1 data. The re-calibrated data provide a very accurate set of standards, which can be very reliably used for technical and scientific purposes. The analysis of the Serkowski parameters revealed a systematic deviation from the width parameter K reported by Whittet et al. This is most likely explained by incorrect effective wavelengths adopted in that study for the R and I bands. [ABSTRACT FROM AUTHOR]
Published: 2017
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40. Withdrawn as Duplicate: Testing the magnetar scenario for superluminous supernovae with circular polarimetry.

Author: Cikota, Aleksandar, Leloudas, Giorgos, Bulla, Mattia, Inserra, Cosimo, Chen, Ting-Wan, Spyromilio, Jason, Patat, Ferdinando, Cano, Zach, Cikota, Stefan, Coughlin, Michael W, Kankare, Erkki, Lowe, Thomas B, Maund, Justyn R, Rest, Armin, Smartt, Stephen J, Smith, Ken W, Wainscoat, Richard J, and Young, David R
Subjects: POLARIMETRY, SUPERNOVAE, MAGNETARS
Published: 2019
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41. Photosynthesis

Author: Fulgosi, Hrvoje, Bosanac, Slobodan D., Cikota, Aleksandar, and Cikota, Stefan
Subjects: oxygenic photosnthesis, plants, cyanobacteria
Abstract: For us humans, photosynthesis is arguably the most important biochemical process on Earth. Plants, algae, and photosynthetic bacteria carry out the fundamental processes of photosynthetic energy conversion, transforming sunlight into chemical energy necessary to sustain autotrophic life. Evidence exist that basic forms of (anoxygenic) photosynthesis emerged on Earth already 3.6 billion years ago, followed by more elaborate oxygenic photosynthesis. Oxygenic photosynthesis has changed the Earth and life on it fundamentally. Photosynthetic apparatus of vascular plants is a mosaic structure consisting of elements that have evolved separately and have come up together in the process of endosymbiosis. I will present theories of how light harvesting antenna complexes evolved, how water-splitting reaction centres were formed, and how some photosynthetic molecular pathways are build further, with each step fulfilling more efficient function.
Published: 2014

42. Quantum chemical study of bis(L-threoninato)copper(II) and bis(L-allo-threoninato)copper(II) as isolated complexes

Author: Marković, Marijana, Ramek, Michael, Sabolović, Jasmina, Bosanac, Slobodan Danko, Cikota, Aleksandar, and Cikota, Stefan
Subjects: copper, L-threonine, L-allo-threonine, conformational analysis, isolated molecules, QM, DFT/B3LYP
Abstract: Visible absorption and circular dichroism measurements of the title compounds, conducted in aqueous solution at neutral pH, showed that both ligands maintained their “glycine-like” configuration, i.e. they were bonded to Cu(II) via the amino nitrogen and carboxylato oxygen atoms, and formed bis-complexes.[1] This coordination mode is stable in the pH range 7
Published: 2014

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