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610 results on '"CANNIZZARO G"'

1. SN 2018is: a low-luminosity Type IIP supernova with narrow hydrogen emission lines at early phases

Author

Dastidar, R., Misra, K., Valenti, S., Sand, D. J., Pastorello, A., Reguitti, A., Pignata, G., Benetti, S., Bose, S., Gangopadhyay, A., Singh, M., Tomasella, L., Andrews, J. E., Arcavi, I., Ashall, C., Bilinski, C., Bostroem, K. A., Buckley, D. A. H., Cannizzaro, G., Chomiuk, L., Congiu, E., Dong, S., Dong, Y., Elias-Rosa, N., Fraser, M., Gall, C., Gromadzki, M., Hiramatsu, D., Hosseinzadeh, G., Howell, D. A., Hsiao, E. Y., McCully, C., Smith, N., and Strader, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a comprehensive photometric and spectroscopic study of the Type IIP SN 2018is. The $V$-band luminosity and the expansion velocity at 50 days post-explosion are $-$15.1$\pm$0.2 mag (corrected for A$_V$=1.34 mag) and 1400 km s$^{-1}$, classifying it as a low-luminosity SN II. The recombination phase in the $V$-band is shorter, lasting around 110 days, and exhibits a steeper decline (1.0 mag per 100 days) compared to most other low-luminosity SNe II. Additionally, the optical and near-infrared spectra display hydrogen emission lines that are strikingly narrow, even for this class. The Fe II and Sc II line velocities are at the lower end of the typical range for low-luminosity SNe II. Semi-analytical modelling of the bolometric light curve suggests an ejecta mass of $\sim$8 M$_\odot$, corresponding to a pre-supernova mass of $\sim$9.5 M$_\odot$, and an explosion energy of $\sim$0.40 $\times$ 10$^{51}$ erg. Hydrodynamical modelling further indicates that the progenitor had a zero-age main sequence mass of 9 M$_\odot$, coupled with a low explosion energy of 0.19 $\times$ 10$^{51}$ erg. The nebular spectrum reveals weak [O I] $\lambda\lambda$6300,6364 lines, consistent with a moderate-mass progenitor, while features typical of Fe core-collapse events, such as He I, [C I], and [Fe I], are indiscernible. However, the redder colours and low ratio of Ni to Fe abundance do not support an electron-capture scenario either. As a low-luminosity SN II with an atypically steep decline during the photospheric phase and remarkably narrow emission lines, SN 2018is contributes to the diversity observed within this population., Comment: 25 pages, 21 figures, accepted for publication in A&A

Published
2025

4. The fall of CSS100217: a tidal disruption-induced low state in an apparently hostless active galactic nucleus

Author

Cannizzaro, G., Levan, A. J., van Velzen, S., and Brown, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

CSS100217 was a nuclear, rapid and luminous flare in a Narrow-Line Seyfert 1 galaxy, whose initial interpretation as a supernova is now debated between variability of the active galactic nucleus (AGN) or a tidal disruption event (TDE). In this paper, we present and discuss new evidence in favour of a TDE or extreme flaring episode scenario. After the decay of the flare, the galaxy entered a long-term low luminosity state, 0.4 magnitudes lower than the pre-outburst emission in the V band. We attribute this to the creation of a cavity in the accretion disk after the tidal disruption of a star in a retrograde orbit with respect to the accretion disk rotation, making a TDE our favoured interpretation of the flare. We also show how the host galaxy shows a point-like, compact profile, no evidence for an extended component and a relatively low mass, unlike what expected from an AGN host galaxy at z=0.147. A compact host galaxy may result in an increased TDE rate, strengthening our interpretation of the event., Comment: 11 pages, 4 figures, accepted for publication on MNRAS

Published
2022
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5. The nuclear transient AT 2017gge: a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH

Author

Onori, F., Cannizzaro, G., Jonker, P. G., Kim, M., Nicholl, M., Mattila, S., Reynolds, T. M., Fraser, M., Wevers, T., Brocato, E., Anderson, J. P., Carini, R., Charalampopoulos, P., Clark, P., Gromadzki, M., Gutiérrez, C. P., Ihanec, N., Inserra, C., Lawrence, A., Leloudas, G., Lundqvist, P., Müller-Bravo, T. E., Piranomonte, S., Pursiainen, M., Rybicki, K. A., Somero, A., Young, D. R., Chambers, K. C., Gao, H., de Boer, T. J. L., and Magnier, E. A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results from a dense multi-wavelength (optical/UV, near-infrared (IR), and X-ray) follow-up campaign of the nuclear transient AT2017gge, covering a total of 1698 days from the transient's discovery. The bolometric lightcurve, the black body temperature and radius, the broad H and He I $\lambda$5876 emission lines and their evolution with time, are all consistent with a tidal disruption event (TDE) nature. A soft X-ray flare is detected with a delay of $\sim$200 days with respect to the optical/UV peak and it is rapidly followed by the emergence of a broad He II $\lambda$4686 and by a number of long-lasting high ionization coronal emission lines. This indicate a clear connection between a TDE flare and the appearance of extreme coronal line emission (ECLEs). An IR echo, resulting from dust re-radiation of the optical/UV TDE light is observed after the X-ray flare and the associated near-IR spectra show a transient broad feature in correspondence of the He I $\lambda$10830 and, for the first time in a TDE, a transient high-ionization coronal NIR line (the [Fe XIII] $\lambda$10798) is also detected. The data are well explained by a scenario in which a TDE occurs in a gas and dust rich environment and its optical/UV, soft X-ray, and IR emission have different origins and locations. The optical emission may be produced by stellar debris stream collisions prior to the accretion disk formation, which is instead responsible for the soft X-ray flare, emitted after the end of the circularization process., Comment: Accepted for publication in MNRAS

Published
2022
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6. Probing for the host galaxies of the fast X-ray transients XRT 000519 and XRT 110103

Author

Eappachen, D., Jonker, P. G., Fraser, M., Torres, M. A. P., Dhillon, V. S., Marsh, T., Littlefair, S. P., Quirola-Vasquez, J., Maguire, K., Sanchez, D. Mata, Cannizzaro, G., Kostrzewa-Rutkowska, Z., Wevers, T., Onori, F., Inkenhaag, Anne, and Brennan, S. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

Over the past few years, $\sim$30 extragalactic fast X-ray transients (FXRTs) have been discovered, mainly in Chandra and XMM-Newton data. Their nature remains unclear, with proposed origins including a double neutron star merger, a tidal disruption event involving an intermediate-mass black hole and a white dwarf, or a supernova shock breakout. A decisive differentiation between these three promising mechanisms for their origin requires an understanding of the FXRT energetics, environments, and/or host properties. We present optical observations obtained with the Very Large Telescope for the FXRTs XRT 000519 and XRT 110103 and Gran Telescopio Canarias observations for XRT 000519 designed to search for host galaxies of these FXRTs. In the $g_s$, $r_s$ and $R$-band images, we detect an extended source on the North-West side of the $\sim$ $1^{\prime\prime}$ (68% confidence) error circle of the X-ray position of XRT 000519 with a Kron magnitude of $g_s=$26.29$\pm$0.09 (AB magnitude). We discuss the XRT 000519 association with the probable host candidate for various possible distances, and we conclude that if XRT 000519 is associated with the host candidate a supernova shock breakout scenario is likely excluded. No host galaxy is found near XRT 110103 down to a limiting magnitude of $R>25.8$., Comment: 11 pages, 11 figures, submitted to MNRAS

Published
2022
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7. An elliptical accretion disk following the tidal disruption event AT 2020zso

Author

Wevers, T., Nicholl, M., Guolo, M., Charalampopoulos, P., Gromadzki, M., Reynolds, T. M., Kankare, E., Leloudas, G., Anderson, J. P., Arcavi, I., Cannizzaro, G., Chen, T. W., Ihanec, N., Inserra, C., Gutiérrez, C. P., Jonker, P. G., Lawrence, A., Magee, M. R., Müller-Bravo, T. E., Onori, F., Ridley, E., Schulze, S., Short, P., Hiramatsu, D., Newsome, M., Terwel, J. H., Yang, S., and Young, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

[Abridged] We classify AT 2020zso as a TDE based on the blackbody evolution inferred from UV/optical photometric observations, and spectral line content and evolution. We identify transient, double-peaked Bowen (N III), He I, He II and Halpha emission lines. We model medium resolution optical spectroscopy of the He II (after careful deblending of the N III contribution) and Halpha lines during the rise, peak and early decline of the light curve using relativistic, elliptical accretion disk models. We find that the spectral evolution before peak can be explained by optical depth effects consistent with an outflowing, optically thick Eddington envelope. Around peak the envelope reaches its maximum extent (approximately 10^15 or 3000-6000 gravitational radii for an inferred black hole mass of 5-10 10^5) and becomes optically thin. The Halpha and He II emission lines at and after peak can be reproduced with a highly inclined (i=85+-5 degrees), highly elliptical (e=0.97+-0.01) and relatively compact (Rin = several 100 Rg and Rout = several 1000 Rg ) accretion disk. Overall, the line profiles suggest a highly elliptical geometry for the new accretion flow, consistent with theoretical expectations of newly formed TDE disks. We quantitatively confirm, for the first time, the high inclination nature of a Bowen (and X-ray dim) TDE, consistent with the unification picture of TDEs where the inclination largely determines the observational appearance. Rapid line profile variations rule out the binary SMBH hypothesis as the origin of the eccentricity; these results thus provide a direct link between a TDE in an AGN and the eccentric accretion disk. We illustrate for the first time how optical spectroscopy can be used to constrain the black hole spin, through (the lack of) disk precession signatures (changes in inferred inclination) - and rule out high black hole spin values (a < 0.8)., Comment: 20 pages, 15 figures and 5 tables. Accepted for publication in A&A. The spectra will be made publicly available through WISErep

Published
2022
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8. How low can you go? SN 2018zd as a low-mass Fe core-collapse supernova

Author

Callis, E., Fraser, M., Pastorello, A., Dong, Subo, Brennan, S. J., Chen, P., Bose, S., Reynolds, T., Salmon, L., Jonker, P., Benetti, S., Berton, M., Cannizzaro, G., Cappellaro, E., Congiu, E., Dyrbye, S., Eappachen, D., Elias-Rosa, N., Gromadzki, M., Gutiérrez, C. P., Holmbo, S., Holoien, T. W. S., Itagaki, K., Kankare, E., Mattila, S., Mutel, R., Ochner, P., Post, R. S., Prieto, J., Reguitti, A., Roth, T., Ryon, J., Sagués-Carracedo, A., Shappee, B. J., Siviero, A., Stassun, K. G., Stritzinger, M., Tomasella, L., Villanueva Jr., S., Wevers, T., and Wiggins, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present spectroscopy and photometry of SN 2018zd, a Type IIP core-collapse supernova with signatures of interaction with circumstantial material in its earliest spectra. High ionization lines, the earmark of shock breakout, are not seen in the earliest spectral epoch, and are only seen in a single spectrum at 4.9 d after explosion. The strength and brevity of these features imply a confined circumstellar material shell in the immediate vicinity of the progenitor. Once the narrow emission lines disappear, SN 2018zd evolves similarly to a Type IIP SN, although the blue colour and enhanced plateau magnitude of SN 2018zd suggests an additional source of luminosity throughout the plateau phase. While SN 2018zd has previously been proposed as an electron-capture SN, we suggest that it is an Fe core-collapse from a low mass red supergiant progenitor. Differences in interpretation for SN 2018zd arise in part due to the large uncertainty on the distance to the host-galaxy NGC 2146, which we re-derive here to be $15.6^{+6.1}_{-3.0}$ Mpc. We find the ejected $^{56}$Ni mass for SN 2018zd to be 0.017 M$_{\odot}$, significantly higher than models of ECSNe predict. We also find the Ni/Fe ratio in SN 2018zd to be much lower that would be expected for an ECSN.

Published
2021

9. A detailed spectroscopic study of Tidal Disruption Events

Author

Charalampopoulos, P., Leloudas, G., Malesani, D. B., Wevers, T., Arcavi, I., Nicholl, M., Pursiainen, M., Lawrence, A., Anderson, J. P., Benetti, S., Cannizzaro, G., Chen, T. -W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Jonker, P. G., Müller-Bravo, T. E., Onori, F., Short, P., Sollerman, J., and Young, D. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Spectroscopically, TDEs are characterized by broad ( 10$^{4}$ km/s) emission lines and show large diversity as well as different line profiles. After carefully and consistently performing a series of data reduction tasks including host galaxy light subtraction, we present here the first detailed, spectroscopic population study of 16 optical/UV TDEs. We report a time lag between the peaks of the optical light-curves and the peak luminosity of H$\alpha$ spanning between 7 - 45 days. If interpreted as light-echoes, these lags correspond to distances of 2 - 12 x 10$^{16}$ cm, one to two orders of magnitudes larger than the estimated blackbody radii (R$_{\rm BB}$) of the same TDEs and we discuss the possible origin of this surprisingly large discrepancy. We also report time lags for the peak luminosity of He I $\lambda$5876 line; smaller than the ones of H$\alpha$ for H TDEs and similar or larger for N III Bowen TDEs. We report that N III Bowen TDEs have lower H$\alpha$ velocity widths compared to the rest of the TDEs in our sample and we also find that a strong X-ray to optical ratio might imply weakening of the line widths. Furthermore, we study the evolution of line luminosities and ratios with respect to their radii (R$_{\rm BB}$) and temperatures (T$_{\rm BB}$). We find a linear relationship between H$\alpha$ luminosity and the R$_{\rm BB}$ and potentially an inverse power-law relation with T$_{\rm BB}$ leading to weaker H$\alpha$ emission for T$_{\rm BB}$ $\geq$ 25000 K. The He II/He I ratio becomes large at the same temperatures possibly pointing to an ionization effect. The He II/H$\alpha$ ratio becomes larger as the photospheric radius recedes, implying a stratified photosphere where Helium lies deeper than Hydrogen. We suggest that the large diversity of the spectroscopic features seen in TDEs along with their X-ray properties, can potentially be attributed to viewing angle effects., Comment: Published in A&A (part of 2022 A&A Highlights). 31 pages (10 of the Appendix), 21 Figures

Published
2021
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10. Intermediate-luminosity red transients: Spectrophotometric properties and connection to electron-capture supernova explosions

Author

Cai, Y. -Z., Pastorello, A., Fraser, M., Botticella, M. T., Elias-Rosa, N., Wang, L. -Z., Kotak, R., Benetti, S., Cappellaro, E., Turatto, M., Reguitti, A., Mattila, S., Smartt, S. J., Ashall, C., Benitez, S., Chen, T. -W., Harutyunyan, A., Kankare, E., Lundqvist, P., Mazzali, P. A., Morales-Garoffolo, A., Ochner, P., Pignata, G., Prentice, S. J., Reynolds, T. M., Shu, X. -W., Stritzinger, M. D., Tartaglia, L., Terreran, G., Tomasella, L., Valenti, S., Valerin, G., Wang, G. -J., Wang, X. -F., Borsato, L., Callis, E., Cannizzaro, G., Chen, S., Congiu, E., Ergon, M., Galbany, L., Gal-Yam, A., Gao, X., Gromadzki, M., Holmbo, S., Huang, F., Inserra, C., Itagaki, K., Kostrzewa-Rutkowska, Z., Maguire, K., Margheim, S., Moran, S., Onori, F., Carracedo, A. Sagués, Smith, K. W., Sollerman, J., Somero, A., Wang, B., and Young, D. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the spectroscopic and photometric study of five intermediate-luminosity red transients (ILRTs), namely AT 2010dn, AT 2012jc, AT 2013la, AT 2013lb, and AT 2018aes. They share common observational properties and belong to a family of objects similar to the prototypical ILRT SN~2008S. These events have a rise time that is less than 15 days and absolute peak magnitudes of between $-11.5$ and $-14.5$ mag. Their pseudo-bolometric light curves peak in the range $0.5$ - $9.0 \times10^{40}~\mathrm{erg~s}^{-1}$ and their total radiated energies are on the order of (0.3 - 3) $\times$~10$^{47}$~erg. After maximum brightness, the light curves show a monotonic decline or a plateau, resembling those of faint supernovae IIL or IIP, respectively. At late phases, the light curves flatten, roughly following the slope of the $^{56}$Co decay. If the late-time power source is indeed radioactive decay, these transients produce $^{56}$Ni masses on the order of $10^{-4}$ to $10^{-3}$~\msun. The spectral energy distribution of our ILRT sample, extending from the optical to the mid-infrared (MIR) domain, reveals a clear IR excess soon after explosion and non-negligible MIR emission at very late phases. The spectra show prominent H lines in emission with a typical velocity of a few hundred km~s$^{-1}$, along with Ca~II features. In particular, the [Ca~II] $\lambda$7291,7324 doublet is visible at all times, which is a characteristic feature for this family of transients. The identified progenitor of SN~2008S, which is luminous in archival Spitzer MIR images, suggests an intermediate-mass precursor star embedded in a dusty cocoon. We propose the explosion of a super-asymptotic giant branch star forming an electron-capture supernova as a plausible explanation for these events., Comment: 31 pages, 17 figures; accepted for publication in Astronomy and Astrophysics

Published
2021
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11. The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study

Author

Álvarez-Hernández, A., Torres, M. A. P., Rodríguez-Gil, P., Shahbaz, T., Anupama, G. C., Gazeas, K. D., Pavana, M., Raj, A., Hakala, P., Stone, G., Gomez, S., Jonker, P. G., Ren, J. -J., Cannizzaro, G., Pastor-Marazuela, I., Goff, W., Corral-Santana, J. M., and Sabo, R.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present a complete dynamical study of the intermediate polar and dwarf nova cataclysmic variable GK Per (Nova Persei 1901) based on a multi-site optical spectroscopy and $R$-band photometry campaign. The radial velocity curve of the evolved donor star has a semi-amplitude $K_2=126.4 \pm 0.9 \, \mathrm{km}\,\mathrm{s}^{-1}$ and an orbital period $P=1.996872 \pm 0.000009 \, \mathrm{d}$. We refine the projected rotational velocity of the donor star to $v_\mathrm{rot} \sin i = 52 \pm 2 \, \mathrm{km}\,\mathrm{s}^{-1}$ which, together with $K_2$, provides a donor star to white dwarf mass ratio $q=M_2/M_1=0.38 \pm 0.03$. We also determine the orbital inclination of the system by modelling the phase-folded ellipsoidal light curve and obtain $i=67^{\circ} \pm 5^{\circ}$. The resulting dynamical masses are $M_{1}=1.03^{+0.16}_{-0.11} \, \mathrm{M}_{\odot}$ and $M_2 = 0.39^{+0.07}_{-0.06} \, \mathrm{M}_{\odot}$ at $68$ per cent confidence level. The white dwarf dynamical mass is compared with estimates obtained by modelling the decline light curve of the $1901$ nova event and X-ray spectroscopy. The best matching mass estimates come from the nova light curve models and an X-ray data analysis that uses the ratio between the Alfv\'en radius in quiescence and during dwarf nova outburst., Comment: 15 pages, 6 figures, 8 tables, accepted for publication in MNRAS

Published
2021
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13. Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg

Author

Cannizzaro, G., Wevers, T., Jonker, P. G., Pérez-Torres, M. A., Moldon, J., Mata-Sánchez, D., Leloudas, G., Pasham, D. R., Mattila, S., Arcavi, I., French, K. Decker, Onori, F., Inserra, C., Nicholl, M., Gromadzki, M., Chen, T. -W., Müller-Bravo, T. E., Short, P., Anderson, J. P., Young, D. R., Gendreau, K. C., Arzoumanian, Z., Löwenstein, M., Remillard, R., Roy, R., and Hiramatsu, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the results of a large multi-wavelength follow-up campaign of the Tidal Disruption Event (TDE) \dsg, focusing on low to high resolution optical spectroscopy, X-ray, and radio observations. The galaxy hosts a super massive black hole of mass $\rm (5.4\pm3.2)\times10^6\,M_\odot$ and careful analysis finds no evidence for the presence of an Active Galactic Nucleus, instead the TDE host galaxy shows narrow optical emission lines that likely arise from star formation activity. The transient is luminous in the X-rays, radio, UV and optical. The X-ray emission becomes undetected after $\sim$125 days, and the radio luminosity density starts to decay at frequencies above 5.4 GHz by $\sim$180 days. Optical emission line signatures of the TDE are present up to $\sim$250 days after the discovery of the transient. The medium to high resolution spectra show traces of absorption lines that we propose originate in the self-gravitating debris streams. At late times, after $\sim$200 days, narrow Fe lines appear in the spectra. The TDE was previously classified as N-strong, but after careful subtraction of the host galaxy's stellar contribution, we find no evidence for these N lines in the TDE spectrum, even though O Bowen lines are detected. The observed properties of the X-ray emission are fully consistent with the detection of the inner regions of a cooling accretion disc. The optical and radio properties are consistent with this central engine seen at a low inclination (i.e., seen from the poles)., Comment: Submitted to MNRAS, October 2020; 25 pages, 21 figures

Published
2020
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14. An outflow powers the optical rise of the nearby, fast-evolving tidal disruption event AT2019qiz

Author

Nicholl, M., Wevers, T., Oates, S. R., Alexander, K. D., Leloudas, G., Onori, F., Jerkstrand, A., Gomez, S., Campana, S., Arcavi, I., Charalampopoulos, P., Gromadzki, M., Ihanec, N., Jonker, P. G., Lawrence, A., Mandel, I., Schulze, S., Short, P., Burke, J., McCully, C., Hiramatsu, D., Howell, D. A., Pellegrino, C., Abbot, H., Anderson, J. P., Berger, E., Blanchard, P. K., Cannizzaro, G., Chen, T. -W., Dennefeld, M., Galbany, L., Gonzalez-Gaitan, S., Hosseinzadeh, G., Inserra, C., Irani, I., Kuin, P., Muller-Bravo, T., Pineda, J., Ross, N. P., Roy, R., Smartt, S. J., Smith, K. W., Tucker, B., Wyrzykowski, L., and Young, D. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

At 66 Mpc, AT2019qiz is the closest optical tidal disruption event (TDE) to date, with a luminosity intermediate between the bulk of the population and iPTF16fnl. Its proximity allowed a very early detection and triggering of multiwavelength and spectroscopic follow-up well before maximum light. The velocity dispersion of the host galaxy and fits to the TDE light curve indicate a black hole mass $\approx 10^6$ M$_\odot$, disrupting a star of $\approx 1$ M$_\odot$. Comprehensive UV, optical and X-ray data shows that the early optical emission is dominated by an outflow, with a luminosity evolution $L \propto t^2$, consistent with a photosphere expanding at constant velocity ($\gtrsim 2000$ km s$^{-1}$), and a line-forming region producing initially blueshifted H and He II profiles with $v=3000-10000$ km s$^{-1}$. The fastest optical ejecta approach the velocity inferred from radio detections (modelled in a forthcoming companion paper from K.~D.~Alexander et al.), thus the same outflow may be responsible for both the fast optical rise and the radio emission -- the first time this connection has been observed in a TDE. The light curve rise begins $29 \pm 2$ days before maximum light, peaking when the photosphere reaches the radius where optical photons can escape. The photosphere then undergoes a sudden transition, first cooling at constant radius then contracting at constant temperature. At the same time, the blueshifts disappear from the spectrum and Bowen fluorescence lines (N III) become prominent, implying a source of far-UV photons, while the X-ray light curve peaks at $\approx 10^{41}$ erg s$^{-1}$. Assuming that these X-rays are from prompt accretion, the size and mass of the outflow are consistent with the reprocessing layer needed to explain the large optical to X-ray ratio in this and other optical TDEs, possibly favouring accretion-powered over collision-powered outflow models., Comment: Accepted for publication in MNRAS

Published
2020
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15. AT 2017gbl: a dust obscured TDE candidate in a luminous infrared galaxy

Author

Kool, E. C., Reynolds, T. M., Mattila, S., Kankare, E., Perez-Torres, M. A., Efstathiou, A., Ryder, S., Romero-Canizales, C., Lu, W., Heikkila, T., Anderson, G. E., Berton, M., Bright, J., Cannizzaro, G., Eappachen, D., Fraser, M., Gromadzki, M., Jonker, P. G., Kuncarayakti, H., Lundqvist, P., Maeda, K., McDermid, R. M., Medling, A. M., Moran, S., Reguitti, A., Shahbandeh, M., Tsygankov, S., U, V., and Wevers, T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the discovery with Keck of the extremely infrared (IR) luminous transient AT 2017gbl, coincident with the Northern nucleus of the luminous infrared galaxy (LIRG) IRAS 23436+5257. Our extensive multi-wavelength follow-up spans ~900 days, including photometry and spectroscopy in the optical and IR, and (very long baseline interferometry) radio and X-ray observations. Radiative transfer modelling of the host galaxy spectral energy distribution and long-term pre-outburst variability in the mid-IR indicate the presence of a hitherto undetected dust obscured active galactic nucleus (AGN). The optical and near-IR spectra show broad 2000 km/s hydrogen, He I and O I emission features that decrease in flux over time. Radio imaging shows a fast evolving compact source of synchrotron emission spatially coincident with AT 2017gbl. We infer a lower limit for the radiated energy of 7.3 x 10^50 erg from the IR photometry. An extremely energetic supernova would satisfy this budget, but is ruled out by the radio counterpart evolution. Instead, we propose AT 2017gbl is related to an accretion event by the central supermassive black hole, where the spectral signatures originate in the AGN broad line region and the IR photometry is consistent with re-radiation by polar dust. Given the fast evolution of AT 2017gbl, we deem a tidal disruption event (TDE) of a star a more plausible scenario than a dramatic change in the AGN accretion rate. This makes AT 2017gbl the third TDE candidate to be hosted by a LIRG, in contrast to the so far considered TDE population discovered at optical wavelengths and hosted preferably by post-starburst galaxies., Comment: Accepted for publication by MNRAS. 32 pages, 22 figures

Published
2020
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16. Extreme variability in an active galactic nucleus: Gaia16aax

Author

Cannizzaro, G., Fraser, M., Jonker, P. G., Pringle, J. E., Mattila, S., Hewett, P. C., Wevers, T., Kankare, E., Kostrzewa-Rutkowska, Z., Wyrzykowski, Ł., Onori, F., Harmanen, J., Ford, K. E. S., McKernan, B., and Nixon, C. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results of a multi-wavelength follow up campaign for the luminous nuclear transient Gaia16aax, which was first identified in January 2016. The transient is spatially consistent with the nucleus of an active galaxy at z=0.25, hosting a black hole of mass $\rm \sim6\times10^8M_\odot$. The nucleus brightened by more than 1 magnitude in the Gaia G-band over a timescale of less than one year, before fading back to its pre-outburst state over the following three years. The optical spectra of the source show broad Balmer lines similar to the ones present in a pre-outburst spectrum. During the outburst, the $\rm H\alpha$ and $\rm H\beta$ emission lines develop a secondary peak. We also report on the discovery of two transients with similar light curve evolution and spectra: Gaia16aka and Gaia16ajq. We consider possible scenarios to explain the observed outbursts. We exclude that the transient event could be caused by a microlensing event, variable dust absorption or a tidal encounter between a neutron star and a stellar mass black hole in the accretion disk. We consider variability in the accretion flow in the inner part of the disk, or a tidal disruption event of a star $\geq 1 M_{\odot}$ by a rapidly spinning supermassive black hole as the most plausible scenarios. We note that the similarity between the light curves of the three Gaia transients may be a function of the Gaia alerts selection criteria., Comment: 21 pages, 17 figure - accepted for publication in MNRAS main journal

Published
2020
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17. The transitional gap transient AT 2018hso: new insights on the luminous red nova phenomenon

Author

Cai, Y-Z., Pastorello, A., Fraser, M., Prentice, S. J., Reynolds, T. M., Cappellaro, E., Benetti, S., Morales-Garoffolo, A., Reguitti, A., Elias-Rosa, N., Brennan, S., Callis, E., Cannizzaro, G., Fiore, A., Gromadzki, M., Galindo-Guil, F. J., Gall, C., Heikkilä, T., Mason, E., Moran, S., Onori, F., Carracedo, A. Sagués, and Valerin, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims: AT 2018hso is a new transient showing transitional properties between those of LRNe and the class of intermediate luminosity red transients (ILRTs) similar to SN 2008S. Through the detailed analysis of the observed parameters, our study support that it actually belongs to the LRN class, and was likely produced by the coalescence of two massive stars. Methods: We obtained ten months of optical and near-infrared photometric monitoring, and eleven epochs of low-resolution optical spectroscopy of AT~2018hso. We compared its observed properties with those of other ILRTs and LRNe. We also inspected the archival Hubble Space Telescope (HST) images obtained about 15 years ago to constrain the progenitor's properties. Results: The light curves of AT 2018hso show a first sharp peak (Mr = -13.93 mag), followed by a broader and shallower second peak, that resembles a plateau in the optical bands. The spectra dramatically change with time. Early time spectra show prominent Balmer emission lines and a weak Ca II] doublet, which is usually observed in ILRTs. However, the major decrease in the continuum temperature, the appearance of narrow metal absorption lines, the major change in the H$\alpha$ strength and profile, and the emergence of molecular bands support a LRN classification. The possible detection of an I ~ -8 mag source at the position of AT 2018hso in HST archive images is consistent with expectations for a pre-merger massive binary, similar to the precursor of the 2015 LRN in M101. Conclusions: We provide reasonable arguments to support a LRN classification for AT~2018hso. This study reveals growing heterogeneity in the observables of LRNe than thought in the past, making sometimes tricky the discrimination between LRNe and ILRTs. This suggests the need of monitoring the entire evolution of gap transients to avoid misclassifications., Comment: 10 pages, 6 figures, 3 tables. Submitted to A&A Letter

Published
2019
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18. Optical follow-up of the tidal disruption event iPTF16fnl: new insights from X-shooter observations

Author

Onori, F., Cannizzaro, G., Jonker, P. G., Fraser, M., Kostrzewa-Rutkowska, Z., Martin-Carrillo, A., Benetti, S., Elias-Rosa, N., Gromadzki, M., Harmanen, J., Mattila, S., Strizinger, M. D., Terreran, G., and Wevers, T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results from Nordic Optical Telescope and X-shooter follow-up campaigns of the tidal disruption event (TDE) iPTF16fnl, covering the first $\sim$100 days after the transient discovery. We followed the source photometrically until the TDE emission was no longer detected above the host galaxy light. The bolometric luminosity evolution of the TDE is consistent with an exponential decay with e-folding constant t$_{0}$=17.6$\pm$0.2 days. The early time spectra of the transient are dominated by broad He II $\lambda$4686, H$\beta$, H$\alpha$ and N III $\lambda$4100 emission lines. The latter is known to be produced together with the N III $\lambda$4640 in the Bowen fluorescence mechanism. Thanks to the medium resolution X-shooter spectra we have been able to separate the Bowen blend contribution from the broad He II emission line. The detection of the Bowen fluorescence lines in iPTF16fnl place this transient among the N-rich TDE subset. In the late-time X-shooter spectra, narrow emission lines of [O III] and [N II] originating from the host galaxy are detected, suggesting that the host galaxy harbours a weak AGN in its core. The properties of all broad emission lines evolve with time. The equivalent widths follow an exponential decay compatible with the bolometric luminosity evolution. The full-width a half maximum of the broad lines decline with time and the line profiles develop a narrow core at later epochs. Overall, the optical emission of iPTF16fnl can be explained by being produced in an optically thick region in which high densities favour the Bowen fluorescence mechanism and where multiple electron scatterings are responsible for the line broadening., Comment: 20 pages, 15 figures. Accepted for publication in MNRAS

Published
2019
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19. 2D Anisotropic KPZ at stationarity: scaling, tightness and non triviality

Author

Cannizzaro, G., Erhard, D., and Schönbauer, P.

Subjects
Mathematics - Probability, 60H15
Abstract

In this work we focus on the two-dimensional anisotropic KPZ (aKPZ) equation, which is formally given by \begin{equation*}\partial_t h =\frac{\nu}{2}\Delta h + \lambda((\partial_1 h)^2 - (\partial_2 h)^2) + \nu^\frac{1}{2}\xi,\end{equation*} where $\xi$ denotes a noise which is white in both space and time, and $\lambda$ and $\nu$ are positive constants. Due to the wild oscillations of the noise and the quadratic nonlinearity, the previous equation is classically ill-posed. It is not possible to linearise it via the Cole-Hopf transformation and the pathwise techniques for singular SPDEs (the theory of Regularity Structures by M. Hairer or the paracontrolled distributions approach of M. Gubinelli, P. Imkeller, N. Perkowski) are not applicable. In the present work, we consider a regularised version of aKPZ which preserves its invariant measure. We show that in order to have subsequential limits once the regularisation is removed, it is necessary to suitably renormalise $\lambda$ and $\nu$. Moreover, we prove that, in the regime suggested by the (non-rigorous) renormalisation group computations of [D.E. Wolf, "Kinetic roughening of vicinal surfaces'', Phys. Rev. Lett., 1991], i.e. $\nu$ constant and the coupling constant $\lambda$ converging to $0$ as the inverse of the square root logarithm, any limit differs from the solution to the linear equation obtained by simply dropping the nonlinearity in aKPZ.

Published
2019

20. The Evolution of Luminous Red Nova AT 2017jfs in NGC 4470

Author

Pastorello, A., Chen, T. -W., Cai, Y. -Z., Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, Ping, Dong, Subo, Dyrbye, S., Elias-Rosa, N., Floers, A., Fraser, M., Geier, S., Goranskij, V. P., Kann, D. A., Kuncarayakti, H., Onori, F., Reguitti, A., Reynolds, T., Losada, I. R., Carracedo, A. Sagues, Schweyer, T., Smartt, S. J., Tatarnikov, A. M., Valeev, A. F., Vogl, C., Wevers, T., Postigo, A. de Ugarte, Izzo, L., Inserra, C., Kankare, E., Maguire, K., Smith, K. W., Stalder, B., Tartaglia, L., Thoene, C. C., Valerin, G., and Young, D. R.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg=-15.46+-0.15 mag and a bolometric luminosity of 5.5x10^41 erg/s. Its light curve has the double-peak shape typical of Luminous Red Novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappeared in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC4490-2011OT1., Comment: 7 pages, 4 figures, 2 Tables (incl. one on-line). Published in A&A Letters

Published
2019
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21. Gaia Data Release 2: Observational Hertzsprung-Russell diagrams

Author

Gaia Collaboration, Babusiaux, C., van Leeuwen, F., Barstow, M. A., Jordi, C., Vallenari, A., Bossini, D., Bressan, A., Cantat-Gaudin, T., van Leeuwen, M., Brown, A. G. A., Prusti, T., de Bruijne, J. H. J., Bailer-Jones, C. A. L., Biermann, M., Evans, D. W., Eyer, L., Jansen, F., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., Walton, N. A., Arenou, F., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Lattanzi, M. G., Bakker, J., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., DeAngeli, F., Fabricius, C., Guerra, R., Holl, B., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Panuzzo, P., Portell, J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Teyssier, D., Altmann, M., Andrae, R., Audard, M., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Burgess, P., Busso, G., Carry, B., Cellino, A., Clementini, G., Clotet, M., Creevey, O., Davidson, M., DeRidder, J., Delchambre, L., Dell'Oro, A., Ducourant, C., Fernández-Hernández, J., Fouesneau, M., Frémat, Y., Galluccio, L., García-Torres, M., González-Núñez, J., González-Vidal, J. J., Gosset, E., Guy, L. P., Halbwachs, J. -L., Hambly, N. C., Harrison, D. L., Hernández, J., Hestroffer, D., Hodgkin, S. T., Hutton, A., Jasniewicz, G., Jean-Antoine-Piccolo, A., Jordan, S., Korn, A. J., Krone-Martins, A., Lanzafame, A. C., Lebzelter, T., Löffler, W., Manteiga, M., Marrese, P. M., Martín-Fleitas, J. M., Moitinho, A., Mora, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J. -M., Recio-Blanco, A., Richards, P. J., Rimoldini, L., Robin, A. C., Sarro, L. M., Siopis, C., Smith, M., Sozzetti, A., Süveges, M., Torra, J., vanReeven, W., Abbas, U., Aramburu, A. Abreu, Accart, S., Aerts, C., Altavilla, G., Álvarez, M. A., Alvarez, R., Alves, J., Anderson, R. I., Andrei, A. H., Varela, E. Anglada, Antiche, E., Antoja, T., Arcay, B., Astraatmadja, T. L., Bach, N., Baker, S. G., Balaguer-Núñez, L., Balm, P., Barache, C., Barata, C., Barbato, D., Barblan, F., Barklem, P. S., Barrado, D., Barros, M., Muñoz, S. Bartholomé, Bassilana, J. -L., Becciani, U., Bellazzini, M., Berihuete, A., Bertone, S., Bianchi, L., Bienaymé, O., Blanco-Cuaresma, S., Boch, T., Boeche, C., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bragaglia, A., Bramante, L., Breddels, M. A., Brouillet, N., Brüsemeister, T., Brugaletta, E., Bucciarelli, B., Burlacu, A., Busonero, D., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzaro, G., Carballo, R., Carlucci, T., Carrasco, J. M., Casamiquela, L., Castellani, M., Castro-Ginard, A., Charlot, P., Chemin, L., Chiavassa, A., Cocozza, G., Costigan, G., Cowell, S., Crifo, F., Crosta, M., Crowley, C., Cuypers, J., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., deLaverny, P., DeLuise, F., DeMarch, R., deMartino, D., deSouza, R., deTorres, A., Debosscher, J., delPozo, E., Delbo, M., Delgado, A., Delgado, H. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Drazinos, P., Durán, J., Edvardsson, B., Enke, H., Eriksson, K., Esquej, P., Bontemps, G. Eynard, Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Casas, M. Farràs, Federici, L., Fedorets, G., Fernique, P., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fraile, E., Fraser, M., Frézouls, B., Gai, M., Galleti, S., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavel, A., Gavras, P., Gerssen, J., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Glass, F., Gomes, M., Granvik, M., Gueguen, A., Guerrier, A., Guiraud, J., Gutiérrez-Sánchez, R., Haigron, R., Hatzidimitriou, D., Hauser, M., Haywood, M., Heiter, U., Helmi, A., Heu, J., Hilger, T., Hobbs, D., Hofmann, W., Holland, G., Huckle, H. E., Hypki, A., Icardi, V., Janßen, K., JevardatdeFombelle, G., Jonker, P. G., Juhász, Á. L., Julbe, F., Karampelas, A., Kewley, A., Klar, J., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, M., Kontizas, E., Koposov, S. E., Kordopatis, G., Kostrzewa-Rutkowska, Z., Koubsky, P., Lambert, S., Lanza, A. F., Lasne, Y., Lavigne, J. -B., LeFustec, Y., LePoncin-Lafitte, C., Lebreton, Y., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., López, M., Managau, S., Mann, R. G., Mantelet, G., Marchal, O., Marchant, J. M., Marconi, M., Marinoni, S., Marschalkó, G., Marshall, D. J., Martino, M., Marton, G., Mary, N., Massari, D., Matijevič, G., Mazeh, T., McMillan, P. J., Messina, S., Michalik, D., Millar, N. R., Molina, D., Molinaro, R., Molnár, L., Montegriffo, P., Mor, R., Morbidelli, R., Morel, T., Morris, D., Mulone, A. F., Muraveva, T., Musella, I., Nelemans, G., Nicastro, L., Noval, L., O'Mullane, W., Ordénovic, C., Ordóñez-Blanco, D., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Panahi, A., Pawlak, M., Piersimoni, A. M., Pineau, F. -X., Plachy, E., Plum, G., Poggio, E., Poujoulet, E., Prša, A., Pulone, L., Racero, E., Ragaini, S., Rambaux, N., Ramos-Lerate, M., Regibo, S., Reylé, C., Riclet, F., Ripepi, V., Riva, A., Rivard, A., Rixon, G., Roegiers, T., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sellés, T. Sagristà, Sahlmann, J., Salgado, J., Salguero, E., Sanna, N., Santana-Ros, T., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Ségransan, D., Shih, I-C., Siltala, L., Silva, A. F., Smart, R. L., Smith, K. W., Solano, E., Solitro, F., Sordo, R., SoriaNieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Surdej, J., Szabados, L., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Teyssandier, P., Thuillot, W., Titarenko, A., TorraClotet, F., Turon, C., Ulla, A., Utrilla, E., Uzzi, S., Vaillant, M., Valentini, G., Valette, V., vanElteren, A., Van Hemelryck, E., Vaschetto, M., Vecchiato, A., Veljanoski, J., Viala, Y., Vicente, D., Vogt, S., vonEssen, C., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Wertz, O., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Ziaeepour, H., Zorec, J., Zschocke, S., Zucker, S., Zurbach, C., and Zwitter, T.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies., Comment: Published in the A&A Gaia Data Release 2 special issue. Tables 2 and A.4 corrected. Tables available at http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A10

Published
2018
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22. The Spectral Evolution of at 2018dyb and the Presence of Metal Lines in Tidal Disruption Events

Author

Leloudas, G, Dai, L, Arcavi, I, Vreeswijk, PM, Mockler, B, Roy, R, Malesani, DB, Schulze, S, Wevers, T, Fraser, M, Ramirez-Ruiz, E, Auchettl, K, Burke, J, Cannizzaro, G, Charalampopoulos, P, Chen, TW, Cikota, A, Della Valle, M, Galbany, L, Gromadzki, M, Heintz, KE, Hiramatsu, D, Jonker, PG, Kostrzewa-Rutkowska, Z, Maguire, K, Mandel, I, Nicholl, M, Onori, F, Roth, N, Smartt, SJ, Wyrzykowski, L, and Young, DR

Subjects
astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present light curves and spectra of the tidal disruption event (TDE) ASASSN-18pg/AT 2018dyb spanning a period of one year. The event shows a plethora of strong emission lines, including the Balmer series, He ii, He i, and metal lines of O iii λ3760 and N iii λλ4100, 4640 (blended with He ii). The latter lines are consistent with originating from the Bowen fluorescence mechanism. By analyzing literature spectra of past events, we conclude that these lines are common in TDEs. The spectral diversity of optical TDEs is thus larger than previously thought and includes N-rich events besides H- and He-rich events. We study how the spectral lines evolve with time, by means of their width, relative strength, and velocity offsets. The velocity width of the lines starts at ∼13,000 km s-1 and decreases with time. The ratio of He ii to N iii increases with time. The same is true for ASASSN-14li, which has a very similar spectrum to AT 2018dyb but its lines are narrower by a factor of >2. We estimate a black hole mass of M BH = 3.3-2.0+5.0 × 106 Mo˙ by using the M-σ relation. This is consistent with the black hole mass derived using the MOSFiT transient fitting code. The detection of strong Bowen lines in the optical spectrum is an indirect proof for extreme ultraviolet and (reprocessed) X-ray radiation and favors an accretion origin for the TDE optical luminosity. A model where photons escape after multiple scatterings through a super-Eddington thick disk and its optically thick wind, viewed at an angle close to the disk plane, is consistent with the observations.

Published
2019

23. A kilonova as the electromagnetic counterpart to a gravitational-wave source

Author

Smartt, S. J., Chen, T. -W., Jerkstrand, A., Coughlin, M., Kankare, E., Sim, S. A., Fraser, M., Inserra, C., Maguire, K., Chambers, K. C., Huber, M. E., Kruhler, T., Leloudas, G., Magee, M., Shingles, L. J., Smith, K. W., Young, D. R., Tonry, J., Kotak, R., Gal-Yam, A., Lyman, J. D., Homan, D. S., Agliozzo, C., Anderson, J. P., Ashall, C. R. Angus C., Barbarino, C., Bauer, F. E., Berton, M., Botticella, M. T., Bulla, M., Bulger, J., Cannizzaro, G., Cano, Z., Cartier, R., Cikota, A., Clark, P., De Cia, A., Della Valle, M., Denneau, L., Dennefeld, M., Dessart, L., Dimitriadis, G., Elias-Rosa, N., Firth, R. E., Flewelling, H., Flors, A., Franckowiak, A., Frohmaier, C., Galbany, L., Gonzalez-Gaitan, S., Greiner, J., Gromadzki, M., Guelbenzu, A. Nicuesa, Gutierrez, C. P., Hamanowicz, A., Hanlon, L., Harmanen, J., Heintz, K. E., Heinze, A., Hernandez, M. -S., Hodgkin, S. T., Hook, I. M., Izzo, L., James, P. A., Jonker, P. G., Kerzendorf, W. E., Klose, S., Kostrzewa-Rutkowska, Z., Kowalski, M., Kromer, M., Kuncarayakti, H., Lawrence, A., Lowe, T. B., Magnier, E. A., Manulis, I., Martin-Carrillo, A., Mattila, S., McBrien, O., Muller, A., Nordin, J., O'Neill, D., Onori, F., Palmerio, J. T., Pastorello, A., Patat, F., Pignata, G., Podsiadlowski, Ph., Pumo, M. L., Prentice, S. J., Rau, A., Razza, A., Rest, A., Reynolds, T., Roy, R., Ruiter, A. J., Rybicki, K. A., Salmon, L., Schady, P., Schultz, A. S. B., Schweyer, T., Seitenzahl, I. R., Smith, M., Sollerman, J., Stalder, B., Stubbs, C. W., Sullivan, M., Szegedi, H., Taddia, F., Taubenberger, S., Terreran, G., van Soelen, B., Vos, J., Wainscoat, R. J., Walton, N. A., Waters, C., Weiland, H., Willman, M., Wiseman, P., Wright, D. E., Wyrzykowski, L., and Yaron, O.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Gravitational waves were discovered with the detection of binary black hole mergers and they should also be detectable from lower mass neutron star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal called a kilonova. The gravitational wave source GW170817 arose from a binary neutron star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC4993, which is spatially coincident with GW170817 and a weak short gamma-ray burst. The transient has physical parameters broadly matching the theoretical predictions of blue kilonovae from neutron star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 Msol, with an opacity of kappa <= 0.5 cm2/gm at a velocity of 0.2 +/- 0.1c. The power source is constrained to have a power law slope of beta = -1.2 +/- 0.3, consistent with radioactive powering from r-process nuclides. We identify line features in the spectra that are consistent with light r-process elements (90 < A < 140). As it fades, the transient rapidly becomes red, and emission may have contribution by a higher opacity, lanthanide-rich ejecta component. This indicates that neutron star mergers produce gravitational waves, radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements., Comment: Nature, in press, DOI 10.1038/nature24303. Data files will be made available at http://www.pessto.org

Published
2017
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27. The mass of the white dwarf in GK Per

Author

Álvarez-Hernández, A., Torres, M. A. P., Rodríguez-Gil, P., Shahbaz, T., Anupama, G. C., Gazeas, K. D., Pavana, M., Raj, A., Hakala, P., Stone, G., Gomez, S., Jonker, P. G., Ren, J.-J., Cannizzaro, G., Pastor-Marazuela, I., Goff, W., Corral-Santana, J. M., and Sabo, R.

Subjects
binary stars, cataclysmic variable, X-ray, intermediate polar, white dwarf, dynamical study
Abstract

Poster contribution to the XV Scientific Meeting of the Sociedad Española de Astronomía (2022). We present a dynamical study of the cataclysmic variable GK Per, comparing our dynamical white dwarf mass with several estimates obtained from indirect methods.

Published
2022
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28. An elliptical accretion disk following the tidal disruption event AT 2020zso

Author

Wevers, T., primary, Nicholl, M., additional, Guolo, M., additional, Charalampopoulos, P., additional, Gromadzki, M., additional, Reynolds, T. M., additional, Kankare, E., additional, Leloudas, G., additional, Anderson, J. P., additional, Arcavi, I., additional, Cannizzaro, G., additional, Chen, T.-W., additional, Ihanec, N., additional, Inserra, C., additional, Gutiérrez, C. P., additional, Jonker, P. G., additional, Lawrence, A., additional, Magee, M. R., additional, Müller-Bravo, T. E., additional, Onori, F., additional, Ridley, E., additional, Schulze, S., additional, Short, P., additional, Hiramatsu, D., additional, Newsome, M., additional, Terwel, J. H., additional, Yang, S., additional, and Young, D., additional

Published
2022
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29. The nuclear transient AT 2017gge: a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH

Author

Onori, F, primary, Cannizzaro, G, additional, Jonker, P G, additional, Kim, M, additional, Nicholl, M, additional, Mattila, S, additional, Reynolds, T M, additional, Fraser, M, additional, Wevers, T, additional, Brocato, E, additional, Anderson, J P, additional, Carini, R, additional, Charalampopoulos, P, additional, Clark, P, additional, Gromadzki, M, additional, Gutiérrez, C P, additional, Ihanec, N, additional, Inserra, C, additional, Lawrence, A, additional, Leloudas, G, additional, Lundqvist, P, additional, Müller-Bravo, T E, additional, Piranomonte, S, additional, Pursiainen, M, additional, Rybicki, K A, additional, Somero, A, additional, Young, D R, additional, Chambers, K C, additional, Gao, H, additional, de Boer, T J L, additional, and Magnier, E A, additional

Published
2022
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34. A detailed spectroscopic study of tidal disruption events

Author

Charalampopoulos, P., Leloudas, G., Malesani, D.B., Wevers, T., Arcavi, I., Nicholl, M., Cannizzaro, G., Jonker, P.G., Onori, F., Sollerman, J., Young, D.R., Charalampopoulos, P., Leloudas, G., Malesani, D.B., Wevers, T., Arcavi, I., Nicholl, M., Cannizzaro, G., Jonker, P.G., Onori, F., Sollerman, J., and Young, D.R.

Abstract

Contains fulltext : 247870.pdf (Publisher’s version ) (Open Access)

Published
2022

35. The nuclear transient AT 2017gge:a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH

Author

Onori, F., Cannizzaro, G., Jonker, P. G., Kim, M., Nicholl, M., Mattila, S., Reynolds, T. M., Fraser, M., Wevers, T., Brocato, E., Anderson, J. P., Carini, R., Charalampopoulos, P., Clark, P., Gromadzki, M., Gutierrez, C. P., Ihanec, N., Inserra, C., Lawrence, A., Leloudas, G., Lundqvist, P., Muller-Bravo, T. E., Piranomonte, S., Pursiainen, M., Rybicki, K. A., Somero, A., Young, D. R., Chambers, K. C., Gao, H., de Boer, T. J. L., Magnier, E. A., Onori, F., Cannizzaro, G., Jonker, P. G., Kim, M., Nicholl, M., Mattila, S., Reynolds, T. M., Fraser, M., Wevers, T., Brocato, E., Anderson, J. P., Carini, R., Charalampopoulos, P., Clark, P., Gromadzki, M., Gutierrez, C. P., Ihanec, N., Inserra, C., Lawrence, A., Leloudas, G., Lundqvist, P., Muller-Bravo, T. E., Piranomonte, S., Pursiainen, M., Rybicki, K. A., Somero, A., Young, D. R., Chambers, K. C., Gao, H., de Boer, T. J. L., and Magnier, E. A.

Abstract

We present the results from a dense multwavelength [optical/UV, near-infrared (IR), and X-ray] follow-up campaign of the nuclear transient AT 2017gge, covering a total of 1698 d from the transient's discovery. The bolometric light curve, the blackbody temperature and radius, the broad H and He i lambda 5876 emission lines and their evolution with time, are all consistent with a tidal disruption event (TDE) nature. A soft X-ray flare is detected with a delay of similar to 200 d with respect to the optical/UV peak and it is rapidly followed by the emergence of a broad He ii lambda 4686 and by a number of long-lasting high ionization coronal emission lines. This indicate a clear connection between a TDE flare and the appearance of extreme coronal line emission (ECLEs). An IR echo, resulting from dust re-radiation of the optical/UV TDE light is observed after the X-ray flare and the associated near-IR spectra show a transient broad feature in correspondence of the He i lambda 10830 and, for the first time in a TDE, a transient high-ionization coronal NIR line (the [Fe xiii] lambda 10798) is also detected. The data are well explained by a scenario in which a TDE occurs in a gas-and-dust rich environment and its optical/UV, soft X-ray, and IR emission have different origins and locations. The optical emission may be produced by stellar debris stream collisions prior to the accretion disc formation, which is instead responsible for the soft X-ray flare, emitted after the end of the circularization process.

Published
2022

36. Probing for the host galaxies of the fast X-ray transients XRT 000519 and XRT 110103

Author

Eappachen, D, primary, Jonker, P G, additional, Fraser, M, additional, Torres, M A P, additional, Dhillon, V S, additional, Marsh, T, additional, Littlefair, S P, additional, Quirola-Vásquez, J, additional, Maguire, K, additional, Mata Sánchez, D, additional, Cannizzaro, G, additional, Kostrzewa-Rutkowska, Z, additional, Wevers, T, additional, Onori, F, additional, Inkenhaag, Anne, additional, and Brennan, S J, additional

Published
2022
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37. A detailed spectroscopic study of tidal disruption events

Author

Charalampopoulos, P., primary, Leloudas, G., additional, Malesani, D. B., additional, Wevers, T., additional, Arcavi, I., additional, Nicholl, M., additional, Pursiainen, M., additional, Lawrence, A., additional, Anderson, J. P., additional, Benetti, S., additional, Cannizzaro, G., additional, Chen, T.-W., additional, Galbany, L., additional, Gromadzki, M., additional, Gutiérrez, C. P., additional, Inserra, C., additional, Jonker, P. G., additional, Müller-Bravo, T. E., additional, Onori, F., additional, Short, P., additional, Sollerman, J., additional, and Young, D. R., additional

Published
2022
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38. Intermediate-luminosity red transients: Spectrophotometric properties and connection to electron-capture supernova explosions

Author

Cai, Y.-Z., primary, Pastorello, A., additional, Fraser, M., additional, Botticella, M. T., additional, Elias-Rosa, N., additional, Wang, L.-Z., additional, Kotak, R., additional, Benetti, S., additional, Cappellaro, E., additional, Turatto, M., additional, Reguitti, A., additional, Mattila, S., additional, Smartt, S. J., additional, Ashall, C., additional, Benitez, S., additional, Chen, T.-W., additional, Harutyunyan, A., additional, Kankare, E., additional, Lundqvist, P., additional, Mazzali, P. A., additional, Morales-Garoffolo, A., additional, Ochner, P., additional, Pignata, G., additional, Prentice, S. J., additional, Reynolds, T. M., additional, Shu, X.-W., additional, Stritzinger, M. D., additional, Tartaglia, L., additional, Terreran, G., additional, Tomasella, L., additional, Valenti, S., additional, Valerin, G., additional, Wang, G.-J., additional, Wang, X.-F., additional, Borsato, L., additional, Callis, E., additional, Cannizzaro, G., additional, Chen, S., additional, Congiu, E., additional, Ergon, M., additional, Galbany, L., additional, Gal-Yam, A., additional, Gao, X., additional, Gromadzki, M., additional, Holmbo, S., additional, Huang, F., additional, Inserra, C., additional, Itagaki, K., additional, Kostrzewa-Rutkowska, Z., additional, Maguire, K., additional, Margheim, S., additional, Moran, S., additional, Onori, F., additional, Sagués Carracedo, A., additional, Smith, K. W., additional, Sollerman, J., additional, Somero, A., additional, Wang, B., additional, and Young, D. R., additional

Published
2021
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39. The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study

Author

Álvarez-Hernández, A, primary, Torres, M A P, additional, Rodríguez-Gil, P, additional, Shahbaz, T, additional, Anupama, G C, additional, Gazeas, K D, additional, Pavana, M, additional, Raj, A, additional, Hakala, P, additional, Stone, G, additional, Gomez, S, additional, Jonker, P G, additional, Ren, J-J, additional, Cannizzaro, G, additional, Pastor-Marazuela, I, additional, Goff, W, additional, Corral-Santana, J M, additional, and Sabo, R, additional

Published
2021
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41. The Brownian Web as a random R-tree

Author

Cannizzaro, G, Hairer, M, and Engineering & Physical Science Research Council (E

Subjects
60G, Mathematics::Probability, math.PR
Abstract

Motivated by [G. Cannizzaro, M. Hairer, arXiv:2010.02766], we provide an alternative characterisation of the Brownian Web (see [T\'oth B., Werner W., Probab. Theory Related Fields, '98] and [L. R. G. Fontes, M. Isopi, C. M. Newman, and K. Ravishankar, Ann. Probab., '04]), i.e. a family of coalescing Brownian motions starting from every point in $\mathbb R^2$ simultaneously, and fit it into the wider framework of random (spatial) $\mathbb R$-trees. We determine some of its properties (e.g. its box-counting dimension) and recover some which were determined in earlier works, such as duality, special points and convergence of the graphical representation of coalescing random walks. Along the way, we introduce a modification of the topology of spatial $\mathbb R$-trees in [T. Duquesne, J.-F. Le Gall, Probab. Theory Related Fields, '05] and [M. T. Barlow, D. A. Croydon, T. Kumagai, Ann. Probab. '17] which makes it Polish and could be of independent interest.

Published
2021

42. The Brownian Castle

Author

Cannizzaro, G, Hairer, M, and Engineering & Physical Science Research Council (E

Subjects
60G, Mathematics::Probability, math.PR
Abstract

We introduce a $1+1$-dimensional temperature-dependent model such that the classical ballistic deposition model is recovered as its zero-temperature limit. Its $\infty$-temperature version, which we refer to as the $0$-Ballistic Deposition ($0$-BD) model, is a randomly evolving interface which, surprisingly enough, does {\it not} belong to either the Edwards--Wilkinson (EW) or the Kardar--Parisi--Zhang (KPZ) universality class. We show that $0$-BD has a scaling limit, a new stochastic process that we call {\it Brownian Castle} (BC) which, although it is "free", is distinct from EW and, like any other renormalisation fixed point, is scale-invariant, in this case under the $1:1:2$ scaling (as opposed to $1:2:3$ for KPZ and $1:2:4$ for EW). In the present article, we not only derive its finite-dimensional distributions, but also provide a "global" construction of the Brownian Castle which has the advantage of highlighting the fact that it admits backward characteristics given by the (backward) Brownian Web (see [T\'oth B., Werner W., Probab. Theory Related Fields, '98] and [L. R. G. Fontes, M. Isopi, C. M. Newman, and K. Ravishankar, Ann. Probab., '04]). Among others, this characterisation enables us to establish fine pathwise properties of BC and to relate these to special points of the Web. We prove that the Brownian Castle is a (strong) Markov and Feller process on a suitable space of c\`adl\`ag functions and determine its long-time behaviour. At last, we give a glimpse to its universality by proving the convergence of $0$-BD to BC in a rather strong sense.

Published
2021

43. The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study

Author

Alvarez-Hernandez, A. Torres, M. A. P. Rodriguez-Gil, P. and Shahbaz, T. Anupama, G. C. Gazeas, K. D. Pavana, M. Raj, A. Hakala, P. Stone, G. Gomez, S. Jonker, P. G. Ren, J-J Cannizzaro, G. Pastor-Marazuela, I Goff, W. and Corral-Santana, J. M. Sabo, R.

Abstract

We present a dynamical study of the intermediate polar and dwarf nova cataclysmic variable GK Persei (Nova Persei 1901) based on a multisite optical spectroscopy and R-band photometry campaign. The radial velocity curve of the evolved donor star has a semi-amplitude K-2 = 126.4 +/- 0.9 km s(-1) and an orbital period P = 1.996872 +/- 0.000009 d. We refine the projected rotational velocity of the donor star to v(rot) sin i = 52 +/- 2 km s(-1) that, together with K-2, provides a donor star to white dwarf mass ratio q = M-2/M-1 = 0.38 +/- 0.03. We also determine the orbital inclination of the system by modelling the phase-folded ellipsoidal light curve and obtain i = 67 degrees +/- 5 degrees. The resulting dynamical masses are M-1 = 1.03(-0.11)(+0.16) M-circle dot and M-2 = 0.39(-0.06)(+0.07) M-circle dot at 68 per cent confidence level. The white dwarf dynamical mass is compared with estimates obtained by modelling the decline light curve of the 1901 nova event and X-ray spectroscopy. The best matching mass estimates come from the nova light curve models and an X-ray data analysis that uses the ratio between the Alfven radius in quiescence and during dwarf nova outburst.

Published
2021

45. Tidal Disruption Events and Hypervariable Active Galactic Nuclei

Author

Cannizzaro, G., Jonker, P.G., Fraser, M., and Radboud University Nijmegen

Subjects
Astronomy
Abstract

Contains fulltext : 233925.pdf (Publisher’s version ) (Open Access) Radboud University, 24 juni 2021 Promotor : Jonker, P.G. Co-promotor : Fraser, M. iii, 188 p.

Published
2021

46. nuclear transient AT 2017gge: a tidal disruption event in a dusty and gas-rich environment and the awakening of a dormant SMBH.

Author

Onori, F, Cannizzaro, G, Jonker, P G, Kim, M, Nicholl, M, Mattila, S, Reynolds, T M, Fraser, M, Wevers, T, Brocato, E, Anderson, J P, Carini, R, Charalampopoulos, P, Clark, P, Gromadzki, M, Gutiérrez, C P, Ihanec, N, Inserra, C, Lawrence, A, and Leloudas, G

Subjects
SOFT X rays, LIGHT curves, ACCRETION disks, SOLAR flares, ACTIVE galaxies, X-rays
Abstract

We present the results from a dense multwavelength [optical/UV, near-infrared (IR), and X-ray] follow-up campaign of the nuclear transient AT 2017gge, covering a total of 1698 d from the transient's discovery. The bolometric light curve, the blackbody temperature and radius, the broad H and He  i λ5876 emission lines and their evolution with time, are all consistent with a tidal disruption event (TDE) nature. A soft X-ray flare is detected with a delay of ∼200 d with respect to the optical/UV peak and it is rapidly followed by the emergence of a broad He  ii λ4686 and by a number of long-lasting high ionization coronal emission lines. This indicate a clear connection between a TDE flare and the appearance of extreme coronal line emission (ECLEs). An IR echo, resulting from dust re-radiation of the optical/UV TDE light is observed after the X-ray flare and the associated near-IR spectra show a transient broad feature in correspondence of the He  i λ10830 and, for the first time in a TDE, a transient high-ionization coronal NIR line (the [Fe  xiii ] λ10798) is also detected. The data are well explained by a scenario in which a TDE occurs in a gas-and-dust rich environment and its optical/UV, soft X-ray, and IR emission have different origins and locations. The optical emission may be produced by stellar debris stream collisions prior to the accretion disc formation, which is instead responsible for the soft X-ray flare, emitted after the end of the circularization process. [ABSTRACT FROM AUTHOR]

Published
2022
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47. Observational Hertzsprung-Russell diagrams

Author

Eyer, L., Rimoldini, L., Audard, M., Anderson, R. I., Nienartowicz, K., Glass, F., Marchal, O., Grenon, M., Mowlavi, N., Holl, B., Clementini, G., Aerts, C., Mazeh, T., Evans, D. W., Szabados, L., Brown, A. G. A., Vallenari, A., Prusti, T., de Bruijne, J. H. J., Babusiaux, C., Bailer-Jones, C. A. L., Biermann, M., Jansen, F., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., van Leeuwen, F., Walton, N. A., Arenou, F., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Lattanzi, M. G., Bakker, J., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., De Angeli, F., Fabricius, C., Guerra, R., Masana, E., Messineo, R., Panuzzo, P., Portell, J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Teyssier, D., Altmann, M., Andrae, R., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Burgess, P., Busso, G., Carry, B., Cellino, A., Clotet, M., Creevey, O., Davidson, M., De Ridder, J., Delchambre, L., Dell’Oro, A., Ducourant, C., Fernández-Hernández, J., Fouesneau, M., Frémat, Y., Galluccio, L., García-Torres, M., González-Núñez, J., González-Vidal, J. J., Gosset, E., Guy, L. P., Halbwachs, J.-L., Hambly, N. C., Harrison, D. L., Hernández, J., Hestroffer, D., Hodgkin, S. T., Hutton, A., Jasniewicz, G., Jean-Antoine-Piccolo, A., Jordan, S., Korn, A. J., Krone-Martins, A., Lanzafame, A. C., Lebzelter, T., Löffler, W., Manteiga, M., Marrese, P. M., Martín-Fleitas, J. M., Moitinho, A., Mora, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J.-M., Recio-Blanco, A., Richards, P. J., Robin, A. C., Sarro, L. M., Siopis, C., Smith, M., Sozzetti, A., Süveges, M., Torra, J., van Reeven, W., Abbas, U., Abreu Aramburu, A., Accart, S., Altavilla, G., Álvarez, M. A., Alvarez, R., Alves, J., Andrei, A. H., Anglada Varela, E., Antiche, E., Antoja, T., Arcay, B., Astraatmadja, T. L., Bach, N., Baker, S. G., Balaguer-Núñez, L., Balm, P., Barache, C., Barata, C., Barbato, D., Barblan, F., Barklem, P. S., Barrado, D., Barros, M., Barstow, M. A., Bartholomé Muñoz, S., Bassilana, J.-L., Becciani, U., Bellazzini, M., Berihuete, A., Bertone, S., Bianchi, L., Bienaymé, O., Blanco-Cuaresma, S., Boch, T., Boeche, C., Bombrun, A., Borrachero, R., Bossini, D., Bouquillon, S., Bourda, G., Bragaglia, A., Bramante, L., Breddels, M. A., Bressan, A., Brouillet, N., Brüsemeister, T., Brugaletta, E., Bucciarelli, B., Burlacu, A., Busonero, D., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzaro, G., Cantat-Gaudin, T., Carballo, R., Carlucci, T., Carrasco, J. M., Casamiquela, L., Castellani, M., Castro-Ginard, A., Charlot, P., Chemin, L., Chiavassa, A., Cocozza, G., Costigan, G., Cowell, S., Crifo, F., Crosta, M., Crowley, C., Cuypers, J., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., de Laverny, P., De Luise, F., De March, R., de Martino, D., de Souza, R., de Torres, A., Debosscher, J., del Pozo, E., Delbo, M., Delgado, A., Delgado, H. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Drazinos, P., Durán, J., Edvardsson, B., Enke, H., Eriksson, K., Esquej, P., Eynard Bontemps, G., Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Farràs Casas, M., Federici, L., Fedorets, G., Fernique, P., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fraile, E., Fraser, M., Frézouls, B., Gai, M., Galleti, S., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavel, A., Gavras, P., Gerssen, J., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomes, M., Granvik, M., Gueguen, A., Guerrier, A., Guiraud, J., Gutiérrez-Sánchez, R., Haigron, R., Hatzidimitriou, D., Hauser, M., Haywood, M., Heiter, U., Helmi, A., Heu, J., Hilger, T., Hobbs, D., Hofmann, W., Holland, G., Huckle, H. E., Hypki, A., Icardi, V., Janßen, K., Jevardat de Fombelle, G., Jonker, P. G., Juhász, Á. L., Julbe, F., Karampelas, A., Kewley, A., Klar, J., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, M., Kontizas, E., Koposov, S. E., Kordopatis, G., Kostrzewa-Rutkowska, Z., Koubsky, P., Lambert, S., Lanza, A. F., Lasne, Y., Lavigne, J.-B., Le Fustec, Y., Le Poncin-Lafitte, C., Lebreton, Y., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., López, M., Lorenz, D., Managau, S., Mann, R. G., Mantelet, G., Marchant, J. M., Marconi, M., Marinoni, S., Marschalkó, G., Marshall, D. J., Martino, M., Marton, G., Mary, N., Massari, D., Matijevič, G., McMillan, P. J., Messina, S., Michalik, D., Millar, N. R., Molina, D., Molinaro, R., Molnár, L., Montegriffo, P., Mor, R., Morbidelli, R., Morel, T., Morgenthaler, S., Morris, D., Mulone, A. F., Muraveva, T., Musella, I., Nelemans, G., Nicastro, L., Noval, L., O’Mullane, W., Ordénovic, C., Ordóñez-Blanco, D., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Panahi, A., Pawlak, M., Piersimoni, A. M., Pineau, F.-X., Plachy, E., Plum, G., Poggio, E., Poujoulet, E., Prša, A., Pulone, L., Racero, E., Ragaini, S., Rambaux, N., Ramos-Lerate, M., Regibo, S., Reylé, C., Riclet, F., Ripepi, V., Riva, A., Rivard, A., Rixon, G., Roegiers, T., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sagristà Sellés, T., Sahlmann, J., Salgado, J., Salguero, E., Sanna, N., Santana-Ros, T., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Ségransan, D., Shih, I.-C., Siltala, L., Silva, A. F., Smart, R. L., Smith, K. W., Solano, E., Solitro, F., Sordo, R., Soria Nieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Surdej, J., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Teyssandier, P., Thuillot, W., Titarenko, A., Torra Clotet, F., Turon, C., Ulla, A., Utrilla, E., Uzzi, S., Vaillant, M., Valentini, G., Valette, V., van Elteren, A., Van Hemelryck, E., van Leeuwen, M., Vaschetto, M., Vecchiato, A., Veljanoski, J., Viala, Y., Vicente, D., Vogt, S., von Essen, C., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Wertz, O., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Ziaeepour, H., Zorec, J., Zschocke, S., Zucker, S., Zurbach, C., Zwitter, T., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Systèmes de Référence Temps Espace (SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Geneva Observatory, University of Geneva [Switzerland], ISDC Data Centre for Astrophysics, Probabilités, statistique, physique mathématique (PSPM), Institut Camille Jordan [Villeurbanne] (ICJ), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Lyon (ECL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Heckscher-Klinikum, Università di Bologna [Bologna] (UNIBO), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Epicentre [Paris] [Médecins Sans Frontières], Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Agence Spatiale Européenne (ESA), European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Universität Greifswald - University of Greifswald, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Lund Observatory, Lund University [Lund], Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Université Libre de Bruxelles [Bruxelles] (ULB), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Royal Greenwich Observatory (RGO), Zentrum für astronomie, Universität Heidelberg [Heidelberg], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, Department of Intensive Care, Erasmus Medical Centre, Department of Biomedical Sciences, Università degli Studi di Modena e Reggio Emilia (UNIMORE), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Laboratorio de Inmunologıa y Virologıa, Facultad de Ciencias Biológicas, Universidad Autónoma de Nuevo León, San Nicolas de los Garza, University of Barcelona, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Professions, institutions, temporalités (PRINTEMPS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Royal Observatory of Belgium [Brussels], INAF - Osservatorio Astrofisico di Torino (OATo), M2A 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Department of Astronomy and Space Physics [Uppsala], Uppsala University, Instituto de Astronomia, Geofisica e Ciencias Atmosfericas [Sao Paulo] (IAG), Universidade de São Paulo (USP), INAF - Osservatorio Astrofisico di Catania (OACT), European Space Astronomy Centre (ESAC), SIM/IDL Faculdade de Ciências da Universidade de Lisboa (FCUL), University of Lisboa, Universidad de Granada (UGR), Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Osservatorio Astronomico di Bologna (OABO), Universidad Nacional de Educación a Distancia (UNED), AUTRES, Département de Physique Nucléaire (ex SPhN) (DPHN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), IDAEA-CSIC, Department of Physics and Astronomy [Uppsala], Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Physics and Astronomy [Leicester], University of Leicester, University of Cadiz, CEA Le Ripault (CEA Le Ripault), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Université Grenoble Alpes - UFR Langage, lettres et arts du spectacle, information et communication - Dpt Lettres et arts du spectacle (UGA UFR LLASIC LAS), Université Grenoble Alpes (UGA), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), INAF - Osservatorio Astronomico di Bologna (OABO), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], FORMATION STELLAIRE 2019, Geologists, Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département de Physique [Montréal], Université de Montréal [Montréal], Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma Tor Vergata [Roma], Institute of Astronomy [Leuven], Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Service de médecine interne diabète et maladies métaboliqe, Hôpital civil Strasbourg, Institut de recherches sur la catalyse (IRC), Centre National de la Recherche Scientifique (CNRS), Institut de Physique et Chimie des Matériaux de Strasbourg (IPCMS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Matériaux et nanosciences d'Alsace, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Department of Plant Ecology, Technische Universität Dresden (TUD), Mitsubishi Electric ITE-TCL, Sciences Pour l'Oenologie (SPO), Université Montpellier 1 (UM1)-Institut de Recherche pour le Développement (IRD [Nouvelle-Calédonie])-Institut National de la Recherche Agronomique (INRA)-Université de Montpellier (UM)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Foundation for Research and Technology-Hellas, Foundation for Research and Technology - Hellas (FORTH), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Virulence bactérienne et maladies infectieuses (VBMI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Laboratoire d'Electrochimie des Matériaux, UMR CNRS 7555, Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Helmholtz zentrum für Schwerionenforschung GmbH (GSI), Atmel Corporation (ATMEL), ATMEL, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), NSF Center for EUV Science and Technology, NSF, L3 group, Dipartemento di Fisica, Lecce, TKK Helsinki University of Technology (TKK), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Association EURATOM-CEA (CEA/DSM/DRFC), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciènces del Cosmos (ICC), Centre Atlantique de Philosophie (CAPHI), PRES Université Nantes Angers Le Mans (UNAM), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département Réseaux, Information, Multimédia (RIM-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre G2I, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemical and Chemical Engineering, Technische Universität Dortmund [Dortmund] (TU), Inst. Ciencia Molecular, Universitat de València (UV), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Université Panthéon-Sorbonne - UFR d'Économie (UP1 UFR02), Université Panthéon-Sorbonne (UP1), Department of Computer Science, Università degli Studi di Verona, Thales Services, THALES, Departement d'Astrophysique Stellaire et Galactique (DASGAL), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL), Center for health studies, Dipartimento di Fisica, Politecnico di Milano [Milan] (POLIMI), Astrometry, Istituto Nazionale di Astrofisica (INAF)-Istituto Nazionale di Astrofisica (INAF), Karl-Franzens-Universität Graz, Institute of Hydrology, Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Astronomical Observatory of the University of Warsaw, University of Warsaw (UW), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lohrmann Observatory, University of Ljubljana, Department of nuclear medicine, Haukeland University Hospital, University of Bergen (UIB)-University of Bergen (UIB), Human Cancer Genetics Program, Comprehensive Cancer Center-College of Medicine and Public Health [Colombus], Departament de Geodinamica i Geofısica, Facultat de Geologia, M2A 2012, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Solvay Silica, Solvay (France), Instituto Dom Luiz, Universidade de Lisboa (ULISBOA), Department of Medicine, Icahn School of Medicine at Mount Sinai [New York] (MSSM), Department of Environmental Chemistry, IDAEA-CSIC, Spanish National Research Council (CSIC), FORMATION STELLAIRE 2012, CICEnergigune, INAF - Osservatorio Astronomico di Roma (OAR), Centre d'Immunologie et de Maladies Infectieuses (CIMI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' [Rome], Aberystwyth University, Department of Food & Nutritional Sciences, University of Reading (UOR), Institut de Chimie de Clermont-Ferrand (ICCF), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Sigma CLERMONT (Sigma CLERMONT)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche de l'European Business School (IREBS), European Business School Paris (EBS Paris), LEI, Wageningen University and Research Centre [Wageningen] (WUR), National University of Ireland [Galway] (NUI Galway), Centre Hospitalier Régional Universitaire de Nîmes (CHRU Nîmes), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences [Budapest], Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Centre National d'Etudes Spatiales (CNES), M2A 2015, Department of Biomedical, Metabolic and Neural Sciences [Modena], Università degli Studi di Modena e Reggio Emilia [Reggio Emilia] (UNIMORE), Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Université de Las Palmas de Gran Canaria [Espagne] (ULPGC), Astrophysique Interprétation Modélisation (AIM - UMR 7158 - UMR E 9005), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Université Grenoble Alpes (UGA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Université Côte d'Azur (UCA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Chaim Sheba Medical Center [Ramat Gan, Israel], University of Catania, Groupement de Recherche et d'Etudes en Gestion à HEC (GREGH), Ecole des Hautes Etudes Commerciales (HEC Paris)-Centre National de la Recherche Scientifique (CNRS), Helsinki Observatory, University of Helsinki [Helsinki], Chimie Et Interdisciplinarité : Synthèse, Analyse, Modélisation (CEISAM), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), R&D Tonnellerie Radoux, Tonnellerie Radoux, Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), M2A 2013, Institut de Chimie Moléculaire de Reims - UMR 7312 (ICMR), SFR Condorcet, Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS)-SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Department of Mathematics [Philadelphia], University of Pennsylvania [Philadelphia], M2A 2014, Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Universidad de Alicante, Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Lille, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Physics Department, University of Crete (UOC), DEE, Budapest University of Technology and Economics [Budapest] (BME), European Space Astronomy Centre, KELLER Fondations spéciales, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ingienerie des Polymères pour les Hautes Technologies (LIPHT), Ecole européenne de chimie, polymères et matériaux [Strasbourg]-Centre National de la Recherche Scientifique (CNRS), Helsinki University of Techology, Centre for Integrative Physiology, University of Edinburgh, Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Neurologie [Paris], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-IFR70-CHU Pitié-Salpêtrière [APHP], Fondation Universitaire Notre Dame de la Paix (FUNDP), Facultés Universitaires Notre-Dame de la Paix, Institut Mines-Télécom [Paris]-Institut Mines-Télécom [Paris]-Centre G2I, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Etudes Spatiales (CNES), Laboratoire Hubert Curien [Saint Etienne] (LHC), Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), Instituto de Plasmas e Fusão Nuclear [Lisboa] (IPFN), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), EURATOM CIEMAT (CIEMAT), Centro de Investigaciones Energéticas Medioambientales y Tecnológicas [Madrid] (CIEMAT), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Politecnico di Milano [Milan], Equipe EES, Ecologie et biologie des interactions (EBI), Université de Poitiers-Centre National de la Recherche Scientifique (CNRS)-Université de Poitiers-Centre National de la Recherche Scientifique (CNRS), University of Freiburg [Freiburg], Ben-Gurion University of the Negev (BGU), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2020
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48. Tidal Disruption Events and Hypervariable Active Galactic Nuclei

Author

Jonker, P.G., Fraser, M., Cannizzaro, G., Jonker, P.G., Fraser, M., and Cannizzaro, G.

Abstract

Radboud University, 24 juni 2021, Promotor : Jonker, P.G. Co-promotor : Fraser, M., Contains fulltext : 233925.pdf (Publisher’s version ) (Open Access)

Published
2021

50. Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg

Author

Cannizzaro, G., Wevers, T., Jonker, P.G., Pérez-Torres, M.A., Moldon, J., Mata-Sánchez, D., Leloudas, G., Pasham, D.R., Mattila, S., Arcavi, I., Decker French, K., Onori, F., Inserra, C., Nicholl, M., Gromadzki, M., Chen, T.W., Müller-Bravo, T.E., Short, P., Anderson, J.P., Young, D.R., Gendreau, K.C., Arzoumanian, Z., Löwenstein, M., Remillard, R., Roy, R. van, Hiramatsu, D., Cannizzaro, G., Wevers, T., Jonker, P.G., Pérez-Torres, M.A., Moldon, J., Mata-Sánchez, D., Leloudas, G., Pasham, D.R., Mattila, S., Arcavi, I., Decker French, K., Onori, F., Inserra, C., Nicholl, M., Gromadzki, M., Chen, T.W., Müller-Bravo, T.E., Short, P., Anderson, J.P., Young, D.R., Gendreau, K.C., Arzoumanian, Z., Löwenstein, M., Remillard, R., Roy, R. van, and Hiramatsu, D.

Abstract

Contains fulltext : 234233.pdf (Publisher’s version ) (Open Access)

Published
2021

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