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172 results on '"Tartaglia, L"'

1. A magnetar giant flare in the nearby starburst galaxy M82

Author: Mereghetti, S, Rigoselli, M, Salvaterra, R, Pacholski, D, Craig Rodi, J, Gotz, D, Arrigoni, E, D’Avanzo, P, Adami, C, Bazzano, A, Bozzo, E, Brivio, R, Campana, S, Cappellaro, E, Chenevez, J, De Luise, F, Ducci, L, Esposito, P, Ferrigno, C, Ferro, M, Luca Israel, G, Le Floc’h, E, Martin-Carrillo, A, Onori, F, Rea, N, Reguitti, A, Savchenko, V, Souami, D, Tartaglia, L, Thuillot, W, Tiengo, A, Tomasella, L, Topinka, M, Turpin, D, Ubertini, P, Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Dominik Patryk Pacholski, James Craig Rodi, Diego Gotz, Edoardo Arrigoni, Paolo D’Avanzo, Christophe Adami, Angela Bazzano, Enrico Bozzo, Riccardo Brivio, Sergio Campana, Enrico Cappellaro, Jerome Chenevez, Fiore De Luise, Lorenzo Ducci, Paolo Esposito, Carlo Ferrigno, Matteo Ferro, Gian Luca Israel, Emeric Le Floc’h, Antonio Martin-Carrillo, Francesca Onori, Nanda Rea, Andrea Reguitti, Volodymyr Savchenko, Damya Souami, Leonardo Tartaglia, William Thuillot, Andrea Tiengo, Lina Tomasella, Martin Topinka, Damien Turpin, Pietro Ubertini, Mereghetti, S, Rigoselli, M, Salvaterra, R, Pacholski, D, Craig Rodi, J, Gotz, D, Arrigoni, E, D’Avanzo, P, Adami, C, Bazzano, A, Bozzo, E, Brivio, R, Campana, S, Cappellaro, E, Chenevez, J, De Luise, F, Ducci, L, Esposito, P, Ferrigno, C, Ferro, M, Luca Israel, G, Le Floc’h, E, Martin-Carrillo, A, Onori, F, Rea, N, Reguitti, A, Savchenko, V, Souami, D, Tartaglia, L, Thuillot, W, Tiengo, A, Tomasella, L, Topinka, M, Turpin, D, Ubertini, P, Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Dominik Patryk Pacholski, James Craig Rodi, Diego Gotz, Edoardo Arrigoni, Paolo D’Avanzo, Christophe Adami, Angela Bazzano, Enrico Bozzo, Riccardo Brivio, Sergio Campana, Enrico Cappellaro, Jerome Chenevez, Fiore De Luise, Lorenzo Ducci, Paolo Esposito, Carlo Ferrigno, Matteo Ferro, Gian Luca Israel, Emeric Le Floc’h, Antonio Martin-Carrillo, Francesca Onori, Nanda Rea, Andrea Reguitti, Volodymyr Savchenko, Damya Souami, Leonardo Tartaglia, William Thuillot, Andrea Tiengo, Lina Tomasella, Martin Topinka, Damien Turpin, and Pietro Ubertini
Abstract: Magnetar giant flares are rare explosive events releasing up to 1047 erg in gamma rays in less than 1 second from young neutron stars with magnetic fields up to 1015−16 G (refs. 1,2). Only three such flares have been seen from magnetars in our Galaxy3,4 and in the Large Magellanic Cloud5 in roughly 50 years. This small sample can be enlarged by the discovery of extragalactic events, as for a fraction of a second giant flares reach luminosities above 1046 erg s−1, which makes them visible up to a few tens of megaparsecs. However, at these distances they are difficult to distinguish from short gamma-ray bursts (GRBs); much more distant and energetic (1050−53 erg) events, originating in compact binary mergers6. A few short GRBs have been proposed7–11, with different amounts of confidence, as candidate giant magnetar flares in nearby galaxies. Here we report observations of GRB 231115A, positionally coincident with the starburst galaxy M82 (ref. 12). Its spectral properties, along with the length of the burst, the limits on its X-ray and optical counterparts obtained within a few hours, and the lack of a gravitational wave signal, unambiguously qualify this burst as a giant flare from a magnetar in M82.
Published: 2024

2. Reducing agalsidase beta infusion time in Fabry patients: low incidence of antibody formation and infusion-associated reactions in an Italian multicenter study

Author: Mignani, R, Americo, C, Aucella, F, Battaglia, Y, Cianci, V, Sapuppo, A, Lanzillo, C, Pennacchiotti, F, Tartaglia, L, Marchi, G, Pieruzzi, F, Mignani, Renzo, Americo, Claudio, Aucella, Filippo, Battaglia, Yuri, Cianci, Vittoria, Sapuppo, Annamaria, Lanzillo, Chiara, Pennacchiotti, Fabio, Tartaglia, Luciano, Marchi, Giacomo, Pieruzzi, Federico, Mignani, R, Americo, C, Aucella, F, Battaglia, Y, Cianci, V, Sapuppo, A, Lanzillo, C, Pennacchiotti, F, Tartaglia, L, Marchi, G, Pieruzzi, F, Mignani, Renzo, Americo, Claudio, Aucella, Filippo, Battaglia, Yuri, Cianci, Vittoria, Sapuppo, Annamaria, Lanzillo, Chiara, Pennacchiotti, Fabio, Tartaglia, Luciano, Marchi, Giacomo, and Pieruzzi, Federico
Abstract: Background Fabry disease is a rare progressive X-linked lysosomal storage disease caused by mutations in the GLA gene that encodes alpha-galactosidase A. Agalsidase beta is a recombinant enzyme replacement therapy authorized in Europe at a standard dose of 1.0 mg/kg intravenously every other week at an initial infusion rate of <= 0.25 mg/min until patient tolerance is established, after which the infusion rate may be increased gradually. However, specific practical guidance regarding the progressive reduction in infusion time is lacking. This study investigated a new and specific protocol for reducing agalsidase beta infusion time in which a stable dosage of 15 mg/h is infused for the first four months, and the infusion rate is increased progressively from 15 to 35 mg/h for the subsequent four infusions. The shortest infusion time is reached after six months and maintained thereafter. The incidence of infusion-associated reactions (IARs) and the development of anti-drug antibodies were analyzed, and the disease burden and the clinical evolution of the disease at 12 months were evaluated. Results Twenty-five of the 31 patients were naive to enzyme or chaperone treatment at baseline and six patients had been switched from agalsidase alfa. The reduced infusion time protocol was well tolerated. Only one patient exhibited an IAR, with mild symptoms that resolved with low-dose steroids. Six patients globally seroconverted during treatment (4 with a classic phenotype and 2 with late-onset disease). All but three patients were seronegative at month 12. All patients were stable at the study's end (FAbry STabilization indEX value < 20%); reducing infusion time did not negatively impact clinical outcomes in any patient. The perceived medical assessment showed that the quality of life of all patients improved. Conclusions The study demonstrates that reducing agalsidase beta infusion time is possible and safe from both an immunogenic and clinical point of view. The use of
Published: 2024

3. SN 2023emq : A Flash-ionized Ibn Supernova with Possible C iii Emission

Author: Pursiainen, M., Leloudas, G., Schulze, Steve, Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., Young, D. R., Pursiainen, M., Leloudas, G., Schulze, Steve, Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., and Young, D. R.
Abstract: SN 2023emq is a fast-evolving transient initially classified as a rare Type Icn supernova (SN), interacting with a H- and He-free circumstellar medium (CSM) around maximum light. Subsequent spectroscopy revealed the unambiguous emergence of narrow He lines, confidently placing SN 2023emq in the more common Type Ibn class. Photometrically, SN 2023emq has several uncommon properties regardless of its class, including its extreme initial decay (faster than >90% of Type Ibn/Icn SNe) and sharp transition in the decline rate from 0.20 to 0.07 mag day−1 at +20 days. The bolometric light curve can be modeled as CSM interaction with 0.32M⊙ of ejecta and 0.12M⊙ of CSM, with 0.006M⊙ of nickel, as expected of fast, interacting SNe. Furthermore, broadband polarimetry at +8.7 days (P = 0.55% ± 0.30%) is consistent with spherical symmetry. A discovery of a transitional Type Icn/Ibn SN would be unprecedented and would give valuable insights into the nature of mass loss suffered by the progenitor just before death, but we favor an interpretation that SN 2023emq is a Type Ibn SN that exhibited flash-ionized features in the earliest spectrum, as the features are not an exact match with other Type Icn SNe to date. However, the feature at 5700 Å, in the region of C iii and N ii emission, is significantly stronger in SN 2023emq than in the few other flash-ionized Type Ibn SNe, and if it is related to C iii, it possibly implies a continuum of properties between the two classes.
Published: 2023
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4. Hidden shock powering the peak of SN 2020faa

Author: Salmaso, I., Cappellaro, E., Tartaglia, L., Benetti, S., Botticella, M. T., Elias-Rosa, N., Pastorello, A., Patat, F., Reguitti, A., Tomasella, L., Valerin, G., Yang, Sheng, Salmaso, I., Cappellaro, E., Tartaglia, L., Benetti, S., Botticella, M. T., Elias-Rosa, N., Pastorello, A., Patat, F., Reguitti, A., Tomasella, L., Valerin, G., and Yang, Sheng
Abstract: Context. The link between the fate of the most massive stars and the resulting supernova (SN) explosion is still a matter of debate, in major part because of the ambiguity among light-curve powering mechanisms. When stars explode as SNe, the light-curve luminosity is typically sustained by a central engine (radioactive decay, magnetar spin-down, or fallback accretion). However, since massive stars eject considerable amounts of material during their evolution, there may be a significant contribution coming from interactions with the previously ejected circumstellar medium (CSM). Reconstructing the progenitor configuration at the time of explosion requires a detailed analysis of the long-term photometric and spectroscopic evolution of the related transient. Aims. In this paper, we present the results of our follow-up campaign of SN 2020faa. Given the high luminosity and peculiar slow light curve, it is purported to have a massive progenitor. We present the spectro-photometric dataset and investigate di fferent options to explain the unusual observed properties that support this assumption. Methods. We computed the bolometric luminosity of the supernova and the evolution of its temperature, radius, and expansion velocity. We also fit the observed light curve with a multi-component model to infer information on the progenitor and the explosion mechanism. Results. Reasonable parameters are inferred for SN 2020faa with a magnetar of energy, Ep = 1.5(-0.2)(+0.5) x 10(50) erg, and spin-down time, t(spin) = 15 +/- 1 d, a shell mass, M-shell = 2.4(-0.4)(+0.5) M-circle dot, and kinetic energy, E-kin(shell) = 0.9(-0.3)(+0.5) x10(51) erg, and a core with M-core = 21.5(-0.7)(+1.4) M-circle dot and E(kin()core) = 3.9(-0.4)(+0.1) x 10(51) erg. In addition, we need an extra source to power the luminosity of the second peak. We find that a hidden interaction with either a CSM disc or several delayed and choked jets is a viable mechanism for supplying the required energy to achieve th
Published: 2023
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5. A long life of excess : The interacting transient SN 2017hcc

Author: Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, Ting-Wan, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Müller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., Young, D. R., Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, Ting-Wan, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Müller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., and Young, D. R.
Abstract: In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 ± 2 days, ATLAS o band) and high luminosity (peaking at −20.78 ± 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 d. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs ≳+800 d.
Published: 2023
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6. SN 2023emq: A Flash-ionized Ibn Supernova with Possible C iii Emission

Author: Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., Young, D. R., Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., and Young, D. R.
Abstract: SN 2023emq is a fast-evolving transient initially classified as a rare Type Icn supernova (SN), interacting with a H- and He-free circumstellar medium (CSM) around maximum light. Subsequent spectroscopy revealed the unambiguous emergence of narrow He lines, confidently placing SN 2023emq in the more common Type Ibn class. Photometrically, SN 2023emq has several uncommon properties regardless of its class, including its extreme initial decay (faster than >90% of Type Ibn/Icn SNe) and sharp transition in the decline rate from 0.20 to 0.07 mag day−1 at +20 days. The bolometric light curve can be modeled as CSM interaction with 0.32M⊙ of ejecta and 0.12M⊙ of CSM, with 0.006M⊙ of nickel, as expected of fast, interacting SNe. Furthermore, broadband polarimetry at +8.7 days (P = 0.55% ± 0.30%) is consistent with spherical symmetry. A discovery of a transitional Type Icn/Ibn SN would be unprecedented and would give valuable insights into the nature of mass loss suffered by the progenitor just before death, but we favor an interpretation that SN 2023emq is a Type Ibn SN that exhibited flash-ionized features in the earliest spectrum, as the features are not an exact match with other Type Icn SNe to date. However, the feature at 5700 Å, in the region of C iii and N ii emission, is significantly stronger in SN 2023emq than in the few other flash-ionized Type Ibn SNe, and if it is related to C iii, it possibly implies a continuum of properties between the two classes.
Published: 2023

7. SN 2023emq: a flash-ionised Ibn supernova with possible CIII emissio

Author: Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T. -W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., Young, D. R., Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T. -W., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-Bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., and Young, D. R.
Abstract: SN 2023emq is a fast-evolving transient initially classified as a rare Type Icn supernova (SN), interacting with a H- and He-free circumstellar medium (CSM) around maximum light. Subsequent spectroscopy revealed the unambiguous emergence of narrow He lines, confidently placing SN 2023emq in the more common Type Ibn class. Photometrically SN 2023emq has several uncommon properties regardless of its class, including its extreme initial decay (faster than > 90% of Ibn/Icn SNe) and sharp transition in the decline rate from 0.20 mag/d to 0.07 mag/d at +20 d. The bolometric light curve can be modelled as CSM interaction with 0.32M_Sun of ejecta and 0.12M_Sun of CSM, with 0.006M_Sun of nickel, as expected of fast interacting SNe. Furthermore, broad-band polarimetry at +8.7 days (P = 0.55 +/- 0.30%) is consistent with spherical symmetry. A discovery of a transitional Icn/Ibn SN would be unprecedented and would give valuable insights into the nature of mass loss suffered by the progenitor just before death, but we favour an interpretation that SN 2023emq is a type Ibn SN that exhibited flash-ionised features in the earliest spectrum, as the features are not an exact match with other SNe Icn to date. However, the feature at 5700{\AA}, in the region of C III and N II emission, is significantly stronger in SN 2023emq than in the few other flash-ionised Type Ibn SNe, and if it is related to C III, it possibly implies a continuum of properties between the two classes., Comment: Accepted to ApJL on 22/11/2023
Published: 2023

8. Hidden shock powering the peak of SN 2020faa

Author: Salmaso, I., Cappellaro, E., Tartaglia, L., Benetti, S., Botticella, M. T., Elias-Rosa, N., Pastorello, A., Patat, F., Reguitti, A., Tomasella, L., Valerin, G., Yang, S., Salmaso, I., Cappellaro, E., Tartaglia, L., Benetti, S., Botticella, M. T., Elias-Rosa, N., Pastorello, A., Patat, F., Reguitti, A., Tomasella, L., Valerin, G., and Yang, S.
Abstract: The link between the fate of the most massive stars and the resulting supernova (SN) explosion is still a matter of debate, in major part because of the ambiguity among light-curve powering mechanisms. When stars explode as SNe, the light-curve luminosity is typically sustained by a central engine (radioactive decay, magnetar spin-down, or fallback accretion). However, since massive stars eject considerable amounts of material during their evolution, there may be a significant contribution coming from interactions with the previously ejected circumstellar medium (CSM). Reconstructing the progenitor configuration at the time of explosion requires a detailed analysis of the long-term photometric and spectroscopic evolution of the related transient. In this paper, we present the results of our follow-up campaign of SN 2020faa. Given the high luminosity and peculiar slow light curve, it is purported to have a massive progenitor. We present the spectro-photometric dataset and investigate different options to explain the unusual observed properties that support this assumption. We computed the bolometric luminosity of the supernova and the evolution of its temperature, radius, and expansion velocity. We also fit the observed light curve with a multi-component model to infer information on the progenitor and the explosion mechanism. Reasonable parameters are inferred for SN 2020faa with a magnetar of energy Ep=1.5(+0.5,-0.2)x10^50 erg and spin-down time t(spin)=15+/-1 d, a shell mass M(shell)=2.4(+0.5,-0.4) Msun and kinetic energy Ekin(shell)=0.9(+0.5,-0.3)x 10^51 erg, and a core with M(core)=21.5(+1.4,-0.7) Msun and Ekin(core)=3.9(+0.1,-0.4)x10^51 erg. In addition, we need an extra source to power the luminosity of the second peak. We find that hidden interaction with either a CSM disc or delayed, choked jets is a viable mechanism for supplying the required energy to achieve this effect., Comment: 14 pages, 14 figures. Accepted to Astronomy & Astrophysics
Published: 2023
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9. A long life of excess:The interacting transient SN 2017hcc

Author: Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutierrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Mueller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., Young, D. R., Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutierrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Mueller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., and Young, D. R.
Abstract: In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 +/- 2 days, ATLAS o band) and high luminosity (peaking at -20.78 +/- 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 d. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs greater than or similar to+800 d.
Published: 2023

10. A long life of excess:The interacting transient SN 2017hcc

Author: Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutierrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Mueller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., Young, D. R., Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutierrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Mueller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., and Young, D. R.
Abstract: In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 +/- 2 days, ATLAS o band) and high luminosity (peaking at -20.78 +/- 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 d. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs greater than or similar to+800 d.
Published: 2023

11. A long life of excess: The interacting transient SN 2017hcc

Author: Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della valle, M., Dennefeld, M., Elias-rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., Young, D. R., Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T-W, Della valle, M., Dennefeld, M., Elias-rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., and Young, D. R.
Abstract: In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 ± 2 days, ATLAS o band) and high luminosity (peaking at −20.78 ± 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 days. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs >∼+800 days.
Published: 2023

12. Forbidden hugs in pandemic times:IV. Panchromatic evolution of three luminous red novae

Author: Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., Magnier, E., Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., and Magnier, E.
Published: 2023

13. SN 2023emq:A Flash-ionized Ibn Supernova with Possible C iii Emission

Author: Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-w., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., Young, D. R., Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-w., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., and Young, D. R.
Published: 2023

14. Forbidden hugs in pandemic times:IV. Panchromatic evolution of three luminous red novae

Author: Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., Magnier, E., Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-rosa, N., Filippenko, A. V., Rojas-bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y.-z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutiérrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z.-t., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., Mccully, C., Misra, K., Morales-garoffolo, A., Moran, S., Morrell, N., Newsome, M., Padilla Gonzalez, E., Pan, Y.-c., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S.-y., Wang, L., Wang, X.-f., Williams, S. C., Wyatt, S., Zhang, T.-m., De Boer, T., Chambers, K., Gao, H., and Magnier, E.
Published: 2023

15. SN 2023emq:A Flash-ionized Ibn Supernova with Possible C iii Emission

Author: Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-w., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., Young, D. R., Pursiainen, M., Leloudas, G., Schulze, S., Charalampopoulos, P., Angus, C. R., Anderson, J. P., Bauer, F., Chen, T.-w., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Inserra, C., Lyman, J., Müller-bravo, T. E., Nicholl, M., Smartt, S. J., Tartaglia, L., Wiseman, P., and Young, D. R.
Published: 2023

16. SN 2018ijp: The explosion of a stripped-envelope star within a dense H-rich shell?

Author: Tartaglia, L, Tartaglia, L, Sollerman, J, Barbarino, C, Taddia, F, Mason, E, Berton, M, Taggart, K, Bellm, EC, De, K, Frederick, S, Fremling, C, Gal-Yam, A, Golkhou, VZ, Graham, M, Ho, AYQ, Hung, T, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Perley, DA, Porter, MD, Reiley, DJ, Riddle, R, Rusholme, B, Soumagnac, MT, Walters, R, Tartaglia, L, Tartaglia, L, Sollerman, J, Barbarino, C, Taddia, F, Mason, E, Berton, M, Taggart, K, Bellm, EC, De, K, Frederick, S, Fremling, C, Gal-Yam, A, Golkhou, VZ, Graham, M, Ho, AYQ, Hung, T, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Perley, DA, Porter, MD, Reiley, DJ, Riddle, R, Rusholme, B, Soumagnac, MT, and Walters, R
Abstract: In this paper, we discuss the outcomes of the follow-up campaign of SN 2018ijp, discovered as part of the Zwicky Transient Facility survey for optical transients. Its first spectrum shows similarities to broad-lined Type Ic supernovae around maximum light, whereas later spectra display strong signatures of interaction between rapidly expanding ejecta and a dense H-rich circumstellar medium, coinciding with a second peak in the photometric evolution of the transient. This evolution, along with the results of modeling of the first light-curve peak, suggests a scenario where a stripped star exploded within a dense circumstellar medium. The two main phases in the evolution of the transient could be interpreted as a first phase dominated by radioactive decays, and a later interaction-dominated phase where the ejecta collide with a pre-existing shell. We therefore discuss SN 2018jp within the context of a massive star depleted of its outer layers exploding within a dense H-rich circumstellar medium.
Published: 2021

17. SN 2018ijp: The explosion of a stripped-envelope star within a dense H-rich shell?

Author: Tartaglia, L, Tartaglia, L, Sollerman, J, Barbarino, C, Taddia, F, Mason, E, Berton, M, Taggart, K, Bellm, EC, De, K, Frederick, S, Fremling, C, Gal-Yam, A, Golkhou, VZ, Graham, M, Ho, AYQ, Hung, T, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Perley, DA, Porter, MD, Reiley, DJ, Riddle, R, Rusholme, B, Soumagnac, MT, Walters, R, Tartaglia, L, Tartaglia, L, Sollerman, J, Barbarino, C, Taddia, F, Mason, E, Berton, M, Taggart, K, Bellm, EC, De, K, Frederick, S, Fremling, C, Gal-Yam, A, Golkhou, VZ, Graham, M, Ho, AYQ, Hung, T, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Perley, DA, Porter, MD, Reiley, DJ, Riddle, R, Rusholme, B, Soumagnac, MT, and Walters, R
Abstract: In this paper, we discuss the outcomes of the follow-up campaign of SN 2018ijp, discovered as part of the Zwicky Transient Facility survey for optical transients. Its first spectrum shows similarities to broad-lined Type Ic supernovae around maximum light, whereas later spectra display strong signatures of interaction between rapidly expanding ejecta and a dense H-rich circumstellar medium, coinciding with a second peak in the photometric evolution of the transient. This evolution, along with the results of modeling of the first light-curve peak, suggests a scenario where a stripped star exploded within a dense circumstellar medium. The two main phases in the evolution of the transient could be interpreted as a first phase dominated by radioactive decays, and a later interaction-dominated phase where the ejecta collide with a pre-existing shell. We therefore discuss SN 2018jp within the context of a massive star depleted of its outer layers exploding within a dense H-rich circumstellar medium.
Published: 2021

18. The Hydrogen-Poor Superluminous Supernovae from the Zwicky Transient Facility Phase-I Survey: I. Data

Author: Chen, Z. H., Yan, Lin, Kangas, T., Lunnan, R., Schulze, S., Sollerman, J., Perley, D. A., Chen, T. -W., Gal-Yam, A., Wang, X. F., Andreoni, I., Bellm, E., Bloom, J. S., Burdge, K., Burgos, A., Cook, D., Dahiwale, A., De, K., Dekany, R., Dugas, A., Frederik, S., Fremling, C., Graham, M., Hankins, M., Ho, A., Jencson, J., Karambelkar, V., Kasliwal, M., Kulkarni, S., Laher, R., Rusholme, B., Sharma, Y., Taddia, F., Taggart, K., Tartaglia, L., Tzanidakis, A., Van Roestel, J., Walter, R., Yang, Y., Yao, Y. H., Yaron, O., Chen, Z. H., Yan, Lin, Kangas, T., Lunnan, R., Schulze, S., Sollerman, J., Perley, D. A., Chen, T. -W., Gal-Yam, A., Wang, X. F., Andreoni, I., Bellm, E., Bloom, J. S., Burdge, K., Burgos, A., Cook, D., Dahiwale, A., De, K., Dekany, R., Dugas, A., Frederik, S., Fremling, C., Graham, M., Hankins, M., Ho, A., Jencson, J., Karambelkar, V., Kasliwal, M., Kulkarni, S., Laher, R., Rusholme, B., Sharma, Y., Taddia, F., Taggart, K., Tartaglia, L., Tzanidakis, A., Van Roestel, J., Walter, R., Yang, Y., Yao, Y. H., and Yaron, O.
Abstract: During the Zwicky Transient Facility (ZTF) Phase-I operation, 78 hydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than three years, making up the largest sample from a single survey. This paper (Paper I) presents the data, including the optical/ultraviolet light curves and classification spectra, while Paper II in this series will focus on the detailed analysis of the light curves and modeling. Our photometry is primarily taken by the ZTF in the $g,r,i$ bands, and with additional data from other ground-based facilities and $\it Swift$. The events of our sample cover a redshift range of $z = 0.06 - 0.67$, with a median and $1\sigma$ error ($16\%$ and $84\%$ percentiles) $z_{med} = 0.265^{+0.143}_{-0.135}$. The peak luminosity covers $-22.9\,{\rm mag} \leq M_{g,peak} \leq -19.9\,$mag, with a median value of $-21.54^{+1.12}_{-0.61}\,$mag. Their light curves evolve slowly with the mean rest-frame rise time of $t_{rise} =42.0\pm17.8\,$days. The luminosity and time scale distributions suggest that low luminosity SLSNe-I with peak luminosity $\sim -20\,$mag or extremely fast rising events ($<10 - 15\,$days) exist but are rare. We confirm previous findings that slowly rising SLSNe-I also tend to fade slowly. The rest-frame color and temperature evolution show large scatters, suggesting that the SLSN-I population may have diverse spectral energy distributions. The peak rest-frame color shows a moderate correlation with the peak absolute magnitude, $\it i.e.$ brighter SLSNe-I tend to have bluer colors. With optical and ultraviolet photometry, we construct bolometric luminosity and derive a bolometric correction relation generally applicable for converting $g,r$-band photometry to bolometric luminosity for SLSNe-I., Comment: 34 pages, 23 figures, Submitted to APJ
Published: 2022

19. The Zwicky Transient Facility phase I sample of hydrogen-rich superluminous supernovae without strong narrow emission lines

Author: Kangas, Tuomas, Yan, Lin, Schulze, S., Fransson, C., Sollerman, J., Lunnan, R., Omand, C. M. B., Andreoni, I, Burruss, R., Chen, T-W, Drake, A. J., Fremling, C., Gal-Yam, A., Graham, M. J., Groom, S. L., Lezmy, J., Mahabal, A. A., Masci, F. J., Perley, D., Riddle, R., Tartaglia, L., Yao, Y., Kangas, Tuomas, Yan, Lin, Schulze, S., Fransson, C., Sollerman, J., Lunnan, R., Omand, C. M. B., Andreoni, I, Burruss, R., Chen, T-W, Drake, A. J., Fremling, C., Gal-Yam, A., Graham, M. J., Groom, S. L., Lezmy, J., Mahabal, A. A., Masci, F. J., Perley, D., Riddle, R., Tartaglia, L., and Yao, Y.
Abstract: We present a sample of 14 hydrogen-rich superluminous supernovae (SLSNe II) from the Zwicky Transient Facility (ZTF) between 2018 and 2020. We include all classified SLSNe with peaks M-g < -20 mag with observed broad but not narrow Balmer emission, corresponding to roughly 20 per cent of all hydrogen-rich SLSNe in ZTF phase I. We examine the light curves and spectra of SLSNe II and attempt to constrain their power source using light-curve models. The brightest events are photometrically and spectroscopically similar to the prototypical SN 2008es, while others are found spectroscopically more reminiscent of non-superluminous SNe II, especially SNe II-L. Ni-56 decay as the primary power source is ruled out. Light-curve models generally cannot distinguish between circumstellar interaction (CSI) and a magnetar central engine, but an excess of ultraviolet (UV) emission signifying CSI is seen in most of the SNe with UV data, at a wide range of photometric properties. Simultaneously, the broad H alpha profiles of the brightest SLSNe II can be explained through electron scattering in a symmetric circumstellar medium (CSM). In other SLSNe II without narrow lines, the CSM may be confined and wholly overrun by the ejecta. CSI, possibly involving mass lost in recent eruptions, is implied to be the dominant power source in most SLSNe II, and the diversity in properties is likely the result of different mass loss histories. Based on their radiated energy, an additional power source may be required for the brightest SLSNe II, however - possibly a central engine combined with CSI., QC 20220916
Published: 2022
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20. Forbidden hugs in pandemic times III. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Author: Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., Zhang, X-H, Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., and Zhang, X-H
Abstract: We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from similar to 231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of similar to 1.6 x 10(41) erg s(-1), followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (T-BB approximate to 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a similar to 20 M-circle dot progenitor candidate with log (L/L-circle dot)= 5.0 dex and T-eff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17-24 M(circle dot)( )primary component.
Published: 2022

21. Forbidden hugs in pandemic times III. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Author: Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., Zhang, X-H, Cai, Y-Z, Pastorello, A., Fraser, M., Wang, X-F, Filippenko, A., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W-L, Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu, Li, Z-T, Lin, C-C, Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S-Y, Zhang, J-J, Zhang, T-M, Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H-W, Gutierrez, C. P., Lin, H., Misra, K., Ou, Z-W, Salmaso, Nico, Tartaglia, L., Xiao, L., and Zhang, X-H
Abstract: We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from similar to 231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of similar to 1.6 x 10(41) erg s(-1), followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (T-BB approximate to 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a similar to 20 M-circle dot progenitor candidate with log (L/L-circle dot)= 5.0 dex and T-eff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17-24 M(circle dot)( )primary component.
Published: 2022

22. A long life of excess: The interacting transient SN 2017hcc

Author: Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T. -W., Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Müller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., Young, D. R., Moran, S., Fraser, M., Kotak, R., Pastorello, A., Benetti, S., Brennan, S. J., Gutiérrez, C. P., Kankare, E., Kuncarayakti, H., Mattila, S., Reynolds, T. M., Anderson, J. P., Brown, P. J., Campana, S., Chambers, K. C., Chen, T. -W., Della Valle, M., Dennefeld, M., Elias-Rosa, N., Galbany, L., Galindo-Guil, F. J., Gromadzki, M., Hiramatsu, D., Inserra, C., Leloudas, G., Müller-Bravo, T. E., Nicholl, M., Reguitti, A., Shahbandeh, M., Smartt, S. J., Tartaglia, L., and Young, D. R.
Abstract: In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 $\pm$ 2 days, ATLAS $o$ band) and high luminosity (peaking at $-$20.78 $\pm$ 0.01 mag in the ATLAS $o$ band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 days. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs >$\sim$+800 days., Comment: Accepted to A&A
Published: 2022
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23. Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

Author: Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-Rosa, N., Filippenko, A. V., Rojas-Bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y. -Z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutierrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z. -T., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., McCully, C., Misra, K., Morales-Garoffolo, A., Moran, S., Morrell, N., Newsome, M., Gonzalez, E. Padilla, Pan, Y. -C., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S. -Y., Wang, L., Wang, X. -F., Williams, S. C., Wyatt, S., Zhang, T. -M., de Boer, T., Chambers, K., Gao, H., Magnier, E., Pastorello, A., Valerin, G., Fraser, M., Reguitti, A., Elias-Rosa, N., Filippenko, A. V., Rojas-Bravo, C., Tartaglia, L., Reynolds, T. M., Valenti, S., Andrews, J. E., Ashall, C., Bostroem, K. A., Brink, T. G., Burke, J., Cai, Y. -Z., Cappellaro, E., Coulter, D. A., Dastidar, R., Davis, K. W., Dimitriadis, G., Fiore, A., Foley, R. J., Fugazza, D., Galbany, L., Gangopadhyay, A., Geier, S., Gutierrez, C. P., Haislip, J., Hiramatsu, D., Holmbo, S., Howell, D. A., Hsiao, E. Y., Hung, T., Jha, S. W., Kankare, E., Karamehmetoglu, E., Kilpatrick, C. D., Kotak, R., Kouprianov, V., Kravtsov, T., Kumar, S., Li, Z. -T., Lundquist, M. J., Lundqvist, P., Matilainen, K., Mazzali, P. A., McCully, C., Misra, K., Morales-Garoffolo, A., Moran, S., Morrell, N., Newsome, M., Gonzalez, E. Padilla, Pan, Y. -C., Pellegrino, C., Phillips, M. M., Pignata, G., Piro, A. L., Reichart, D. E., Rest, A., Salmaso, I., Sand, D. J., Siebert, M. R., Smartt, S. J., Smith, K. W., Srivastav, S., Stritzinger, M. D., Taggart, K., Tinyanont, S., Yan, S. -Y., Wang, L., Wang, X. -F., Williams, S. C., Wyatt, S., Zhang, T. -M., de Boer, T., Chambers, K., Gao, H., and Magnier, E.
Abstract: We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT2018bwo, AT2021afy, and AT2021blu. AT2018bwo was discovered in NGC45 (at 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 10^40 erg/s. AT2021afy, hosted by UGC10043 (49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(+-0.6)x10^41 erg/s. For AT2021blu in UGC5829, (8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of AT2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5x10^40 erg/s, which is half of that of AT2021afy. The spectra of AT2021afy and AT2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from 13Mo for AT2018bwo, to 13-18Mo for AT2021blu, and over 40Mo for AT2021afy., Comment: 33 pages, 19 figures, 7 tables (plus 3 available at the CDS). Accepted for publication in A&A
Published: 2022
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24. Early Lightcurves of Type Ia Supernovae are Consistent with Nondegenerate Progenitor Companions

Author: Burke, J., Howell, D. A., Sand, D. J., Amaro, R. C., Brown, P. J., Andrews, J. E., Bostroem, K. A., Dong, Y., Haislip, J., Hiramatsu, D., Hosseinzadeh, G., Kouprianov, V., Lundquist, M. J., McCully, C., Pellegrino, C., Reichart, D., Tartaglia, L., Valenti, S., Yang, S., Burke, J., Howell, D. A., Sand, D. J., Amaro, R. C., Brown, P. J., Andrews, J. E., Bostroem, K. A., Dong, Y., Haislip, J., Hiramatsu, D., Hosseinzadeh, G., Kouprianov, V., Lundquist, M. J., McCully, C., Pellegrino, C., Reichart, D., Tartaglia, L., Valenti, S., and Yang, S.
Abstract: If Type Ia supernovae (SNe~Ia) result from a white dwarf being ignited by Roche lobe overflow from a nondegenerate companion, then as the supernova explosion runs into the companion star its ejecta will be shocked, causing an early blue excess in the lightcurve. A handful of these excesses have been found in single-object studies, but inferences about the population of SNe~Ia as a whole have been limited because of the rarity of multiwavelength followup within days of explosion. Here we present a three-year investigation yielding an unbiased sample of nine nearby ($z<0.01$) SNe~Ia with exemplary early data. The data are truly multiwavelength, covering $UBVgri$ and Swift bandpasses, and also early, with an average first epoch 16.0 days before maximum light. Of the nine objects, three show early blue excesses. We do not find enough statistical evidence to reject the null hypothesis that SNe~Ia predominantly arise from Roche-lobe-overflowing single-degenerate systems ($p=0.94$). When looking at the objects' colors, we find the objects are almost uniformly near-UV-blue, in contrast to earlier literature samples which found that only a third of SNe~Ia are near-UV-blue, and we find a seemingly continuous range of $B-V$ colors in the days after explosion, again in contrast with earlier claims in the literature. This study highlights the importance of early, truly multiwavelength, high-cadence data in determining the progenitor systems of SNe~Ia and in revealing their diverse early behavior., Comment: 28 pages, 10 figures
Published: 2022

25. Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Author: Cai, Y. -Z., Pastorello, A., Fraser, M., Wang, X. -F., Filippenko, A. V., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W. -L., Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu., Li, Z. -T., Lin, C. -C., Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D. V., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N. I., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R. I., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S. -Y., Zhang, J. -J., Zhang, T. -M., Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H. -W., Gutiérrez, C. P., Lin, H., Misra, K., Ou, Z. -W., Salmaso, I., Tartaglia, L., Xiao, L., Zhang, X. -H., Cai, Y. -Z., Pastorello, A., Fraser, M., Wang, X. -F., Filippenko, A. V., Reguitti, A., Patra, K. C., Goranskij, V. P., Barsukova, E. A., Brink, T. G., Elias-Rosa, N., Stevance, H. F., Zheng, W., Yang, Y., Atapin, K. E., Benetti, S., de Boer, T. J. L., Bose, S., Burke, J., Byrne, R., Cappellaro, E., Chambers, K. C., Chen, W. -L., Emami, N., Gao, H., Hiramatsu, D., Howell, D. A., Huber, M. E., Kankare, E., Kelly, P. L., Kotak, R., Kravtsov, T., Lander, V. Yu., Li, Z. -T., Lin, C. -C., Lundqvist, P., Magnier, E. A., Malygin, E. A., Maslennikova, N. A., Matilainen, K., Mazzali, P. A., McCully, C., Mo, J., Moran, S., Newsome, M., Oparin, D. V., Gonzalez, E. Padilla, Reynolds, T. M., Shatsky, N. I., Smartt, S. J., Smith, K. W., Stritzinger, M. D., Tatarnikov, A. M., Terreran, G., Uklein, R. I., Valerin, G., Vallely, P. J., Vozyakova, O. V., Wainscoat, R., Yan, S. -Y., Zhang, J. -J., Zhang, T. -M., Zheltoukhov, S. G., Dastidar, R., Fulton, M., Galbany, L., Gangopadhyay, A., Ge, H. -W., Gutiérrez, C. P., Lin, H., Misra, K., Ou, Z. -W., Salmaso, I., Tartaglia, L., Xiao, L., and Zhang, X. -H.
Abstract: We present an observational study of the luminous red nova (LRN) AT\,2021biy in the nearby galaxy NGC\,4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from $\sim 231$\,days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT\,2021biy shows a short-duration blue peak, with a bolometric luminosity of $\sim 1.6 \times 10^{41}$\,erg\,s$^{-1}$, followed by the longest plateau among LRNe to date, with a duration of 210\,days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT\,2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum ($T_{\mathrm{BB}} \approx 2050$ K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT\,2021biy has local dust properties similar to those of V838\,Mon in the Milky Way Galaxy. Inspection of archival {\it Hubble Space Telescope} data taken on 2003 August 3 reveals a $\sim 20$\,\msun\ progenitor candidate with log\,$(L/{\rm L}_{\odot}) = 5.0$\,dex and $T_{\rm{eff}} = 5900$\,K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17--24\,\msun\ primary component., Comment: 21 pages, 14 figures. Accepted by Astronomy and Astrophysics
Published: 2022
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26. The Hydrogen-Poor Superluminous Supernovae from the Zwicky Transient Facility Phase-I Survey: I. Light Curves and Measurements

Author: Chen, Z. H., Yan, Lin, Kangas, T., Lunnan, R., Schulze, S., Sollerman, J., Perley, D. A., Chen, T. -W., Taggart, K., Hinds, K. R., Gal-Yam, A., Wang, X. F., Andreoni, I., Bellm, E., Bloom, J. S., Burdge, K., Burgos, A., Cook, D., Dahiwale, A., De, K., Dekany, R., Dugas, A., Frederik, S., Fremling, C., Graham, M., Hankins, M., Ho, A., Jencson, J., Karambelkar, V., Kasliwal, M., Kulkarni, S., Laher, R., Rusholme, B., Sharma, Y., Taddia, F., Tartaglia, L., Thomas, B. P., Tzanidakis, A., Van Roestel, J., Walter, R., Yang, Y., Yao, Y. H., Yaron, O., Chen, Z. H., Yan, Lin, Kangas, T., Lunnan, R., Schulze, S., Sollerman, J., Perley, D. A., Chen, T. -W., Taggart, K., Hinds, K. R., Gal-Yam, A., Wang, X. F., Andreoni, I., Bellm, E., Bloom, J. S., Burdge, K., Burgos, A., Cook, D., Dahiwale, A., De, K., Dekany, R., Dugas, A., Frederik, S., Fremling, C., Graham, M., Hankins, M., Ho, A., Jencson, J., Karambelkar, V., Kasliwal, M., Kulkarni, S., Laher, R., Rusholme, B., Sharma, Y., Taddia, F., Tartaglia, L., Thomas, B. P., Tzanidakis, A., Van Roestel, J., Walter, R., Yang, Y., Yao, Y. H., and Yaron, O.
Abstract: During the Zwicky Transient Facility (ZTF) Phase-I operation, 78 hydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than three years, making up the largest sample from a single survey. This paper (Paper I) presents the data, including the optical/ultraviolet light curves and classification spectra, while Paper II in this series will focus on the detailed analysis of the light curves and modeling. Our photometry is primarily taken by the ZTF in the $g,r,i$ bands, and with additional data from other ground-based facilities and Swift. The events of our sample cover a redshift range of $z = 0.06 - 0.67$, with a median and $1\sigma$ error (16\% and 84\% percentiles) $z_{\rm med} = 0.265^{+0.143}_{-0.135}$. The peak luminosity covers $-22.8\,{\rm mag} \leq M_{g,\rm peak} \leq -19.8$\,mag, with a median value of $-21.48^{+1.13}_{-0.61}$\,mag. Their light curves evolve slowly with the mean rest-frame rise time of $t_{\rm rise} = 41.9\pm17.8$\,days. The luminosity and time scale distributions suggest that low luminosity SLSNe-I with peak luminosity $\sim -20$\,mag or extremely fast rising events ($<10$\,days) exist but are rare. We confirm previous findings that slowly rising SLSNe-I also tend to fade slowly. The rest-frame color and temperature evolution show large scatters, suggesting that the SLSN-I population may have diverse spectral energy distributions. The peak rest-frame color shows a moderate correlation with the peak absolute magnitude, i.e. brighter SLSNe-I tend to have bluer colors. With optical and ultraviolet photometry, we construct bolometric luminosity and derive a bolometric correction relation generally applicable for converting $g,r$-band photometry to bolometric luminosity for SLSNe-I., Comment: 38 pages, 25 figures, Accepted by APJ
Published: 2022
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27. Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Author: Abbott, B, Abbott, R, Abbott, T, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M, Altin, P, Amato, A, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Antier, S, Appert, S, Arai, K, Araya, M, Areeda, J, Arene, M, Arnaud, N, Aronson, S, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baird, J, Baker, P, Baldaccini, F, Ballardin, G, Ballmer, S, Bals, A, Banagiri, S, Barayoga, J, Barbieri, C, Barclay, S, Barish, B, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I, Bell, A, Beniwal, D, Benjamin, M, Bergmann, G, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, I, Bilgili, S, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Bitossi, M, Bizouard, M, Blackburn, J, Blackman, J, Blair, C, Blair, D, Blair, R, Bloemen, S, Bobba, F, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, S, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Buy, C, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callister, T, Calloni, E, Camp, J, Campbell, W, Canepa, M, Cannon, K, Cao, H, Cao, J, Carapella, G, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Cheeseboro, B, Chen, H, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chiadini, F, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Cieslar, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Cleva, F, Coccia, E, Cohadon, P, Cohen, D, Colleoni, M, Collette, C, Collins, C, Colpi, M, Cominsky, L, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cullen, T, Cumming, A, Cunningham, L, Cuoco, E, Canton, T, Dalya, G, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davier, M, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L, Demos, N, Dent, T, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Varona, O, Dhurandhar, S, Diaz, M, Dietrich, T, Di Fiore, L, Difronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Ducoin, J, Dupej, P, Durante, O, Dwyer, S, Easter, P, Eddolls, G, Edo, T, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Fafone, V, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Fidecaro, F, Fiori, I, Fiorucci, D, Fishbach, M, Fisher, R, Fishner, J, Fittipaldi, R, Fitz-Axen, M, Fiumara, V, Flaminio, R, Fletcher, M, Floden, E, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Vivanco, F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fritschel, P, Frolov, V, Fronze, G, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gammaitoni, L, Gaonkar, S, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Gibson, D, Gill, K, Glover, L, Gniesmer, J, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Castro, J, Gopakumar, A, Gossan, S, Gosselin, M, Gouaty, R, Grace, B, Grado, A, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Grimaldi, A, Grimm, S, Groot, P, Grote, H, Grunewald, S, Gruning, P, Guidi, G, Gulati, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, B, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hasskew, R, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heitmann, H, Hellman, F, Hello, P, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heurs, M, Hild, S, Hinderer, T, Hochheim, S, Hofman, D, Holgado, A, Holland, N, Holt, K, Holz, D, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Huang, Y, Hubner, M, Huerta, E, Huet, D, Hughey, B, Hui, V, Husa, S, Huttner, S, Huynh-Dinh, T, Idzkowski, B, Iess, A, Inchauspe, H, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H, Isac, J, Isi, M, Iyer, B, Jacqmin, T, Jadhav, S, Jani, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jenkins, A, Jiang, J, Johnson, D, Jones, A, Jones, D, Jones, J, Jones, R, 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E., Sanchis-Gual N., Sanders J. R., Santiago K. A., Santos E., Sarin N., Sassolas B., Sauter O., Savage R. L., Schale P., Scheel M., Scheuer J., Schmidt P., Schnabel R., Schofield R. M. S., Schonbeck A., Schreiber E., Schulte B. W., Schutz B. F., Scott J., Scott S. M., Seidel E., Sellers D., Sengupta A. S., Sennett N., Sentenac D., Sequino V., Sergeev A., Setyawati Y., Shaddock D. A., Shaffer T., Shahriar M. S., Shaner M. B., Sharma A., Sharma P., Shawhan P., Shen H., Shink R., Shoemaker D. H., Shoemaker D. M., Shukla K., Shyamsundar S., Siellez K., Sieniawska M., Sigg D., Singer L. P., Singh D., Singh N., Singhal A., Sintes A. M., Sitmukhambetov S., Skliris V., Slagmolen B. J. J., Slaven-Blair T. J., Smith J. R., Smith R. J. E., Somala S., Son E. J., Soni S., Sorazu B., Sorrentino F., Souradeep T., Sowell E., Spencer A. P., Spera M., Srivastava A. K., Srivastava V., Staats K., Stachie C., Standke M., Steer D. A., Steinke M., Steinlechner J., Steinlechner S., Steinmeyer D., Stevenson S. P., Stocks D., Stone R., Stops D. J., Strain K. A., Stratta G., Strigin S. E., Strunk A., Sturani R., Stuver A. L., Sudhir V., Summerscales T. Z., Sun L., Sunil S., Sur A., Suresh J., Sutton P. J., Swinkels B. L., Szczepanczyk M. J., Tacca M., Tait S. C., Talbot C., Tanner D. B., Tao D., Tapai M., Tapia A., Tasson J. D., Taylor R., Tenorio R., Terkowski L., Thomas M., Thomas P., Thondapu S. R., Thorne K. A., Thrane E., Tiwari S., Tiwari V., Toland K., Tonelli M., Tornasi Z., Torres-Forne A., Torrie C. I., Toyra D., Travasso F., Traylor G., Tringali M. C., Tripathee A., Trovato A., Trozzo L., Tsang K. W., Tse M., Tso R., Tsukada L., Tsuna D., Tsutsui T., Tuyenbayev D., Ueno K., Ugolini D., Unnikrishnan C. S., Urban A. L., Usman S. A., Vahlbruch H., Vajente G., Valdes G., Valentini M., Van Bakel N., Van Beuzekom M., Van Den Brand J. F. J., Van Den Broeck C., Vander-Hyde D. C., Van Der Schaaf L., Vanheijningen J. V., Van Veggel A. A., Vardaro M., Varma V., Vass S., Vasuth M., Vecchio A., Vedovato G., Veitch J., Veitch P. J., Venkateswara K., Venugopalan G., Verkindt D., Vetrano F., Vicere A., Viets A. D., Vinciguerra S., Vine D. J., Vinet J. -Y., Vitale S., Vo T., Vocca H., Vorvick C., Vyatchanin S. P., Wade A. R., Wade L. E., Wade M., Walet R., Walker M., Wallace L., Walsh S., Wang H., Wang J. Z., Wang S., Wang W. H., Wang Y. F., Ward R. L., Warden Z. A., Warner J., Was M., Watchi J., Weaver B., Wei L. -W., Weinert M., Weinstein A. J., Weiss R., Wellmann F., Wen L., Wessel E. K., Wessels P., Westhouse J. W., Wette K., Whelan J. T., Whiting B. F., Whittle C., Wilken D. M., Williams D., Williamson A. R., Willis J. L., Willke B., Winkler W., Wipf C. C., Wittel H., Woan G., Woehler J., Wofford J. K., Wright J. L., Wu D. S., Wysocki D. M., Xiao S., Xu R., Yamamoto H., Yancey C. C., Yang L., Yang Y., Yang Z., Yap M. J., Yazback M., Yeeles D. W., Yu H., Yuen S. H. R., Zadrozny A. K., Zadrozny A., Zanolin M., Zelenova T., Zendri J. -P., Zevin M., Zhang J., Zhang L., Zhang T., Zhao C., Zhao G., Zhou M., Zhou Z., Zhu X. J., Zucker M. E., Zweizig J., Holoien T. W. -S., Kochanek C. S., Prieto J. L., Shappee B. J., Stanek K. Z., Haislip J., Kouprianov V., Reichart D. E., Sand D. J., Tartaglia L., Valenti S., Wyatt S., Yang S., and Salemi F.
Abstract: We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. The sources with neutrino-driven explosions are detectable at the distances approaching 5 kpc, and for magnetorotationally driven explosions the distances are up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes, we constrained the gravitational-wave energy emitted during core collapse at the levels of 4.27×10-4 M·c2 and 1.28×10-1 M·c2 for emissions at 235 and 1304 Hz, respectively. These constraints are 2 orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo, and GEO 600 data.
Published: 2020

28. Bright, Months-long stellar outbursts announce the explosion of interaction-powered supernovae

Author: Strotjohann, NL, Strotjohann, NL, Ofek, EO, Gal-Yam, A, Bruch, R, Schulze, S, Shaviv, N, Sollerman, J, Filippenko, AV, Yaron, O, Fremling, C, Nordin, J, Kool, EC, Perley, DA, Ho, AYQ, Yang, Y, Yao, Y, Soumagnac, MT, Graham, ML, Barbarino, C, Tartaglia, L, De, K, Goldstein, DA, Cook, DO, Brink, TG, Taggart, K, Yan, L, Lunnan, R, Kasliwal, M, Kulkarni, SR, Nugent, PE, Masci, FJ, Rosnet, P, Adams, SM, Andreoni, I, Bagdasaryan, A, Bellm, EC, Burdge, K, Duev, DA, Dugas, A, Frederick, S, Goldwasser, S, Hankins, M, Irani, I, Karambelkar, V, Kupfer, T, Liang, J, Neill, JD, Porter, M, Riddle, RL, Sharma, Y, Short, P, Taddia, F, Tzanidakis, A, Van Roestel, J, Walters, R, Zhuang, Z, Strotjohann, NL, Strotjohann, NL, Ofek, EO, Gal-Yam, A, Bruch, R, Schulze, S, Shaviv, N, Sollerman, J, Filippenko, AV, Yaron, O, Fremling, C, Nordin, J, Kool, EC, Perley, DA, Ho, AYQ, Yang, Y, Yao, Y, Soumagnac, MT, Graham, ML, Barbarino, C, Tartaglia, L, De, K, Goldstein, DA, Cook, DO, Brink, TG, Taggart, K, Yan, L, Lunnan, R, Kasliwal, M, Kulkarni, SR, Nugent, PE, Masci, FJ, Rosnet, P, Adams, SM, Andreoni, I, Bagdasaryan, A, Bellm, EC, Burdge, K, Duev, DA, Dugas, A, Frederick, S, Goldwasser, S, Hankins, M, Irani, I, Karambelkar, V, Kupfer, T, Liang, J, Neill, JD, Porter, M, Riddle, RL, Sharma, Y, Short, P, Taddia, F, Tzanidakis, A, Van Roestel, J, Walters, R, and Zhuang, Z
Abstract: Interaction-powered supernovae (SNe) explode within an optically thick circumstellar medium (CSM) that could be ejected during eruptive events. To identify and characterize such pre-explosion outbursts, we produce forcedphotometry light curves for 196 interacting SNe, mostly of Type IIn, detected by the Zwicky Transient Facility between early 2018 and 2020 June. Extensive tests demonstrate that we only expect a few false detections among the 70,000 analyzed pre-explosion images after applying quality cuts and bias corrections. We detect precursor eruptions prior to 18 Type IIn SNe and prior to the Type Ibn SN 2019uo. Precursors become brighter and more frequent in the last months before the SN and month-long outbursts brighter than magnitude -13 occur prior to 25% (5-69%, 95% confidence range) of all Type IIn SNe within the final three months before the explosion. With radiative energies of up to 1049erg, precursors could eject ~1M⊙of material. Nevertheless, SNe with detected precursors are not significantly more luminous than other SNe IIn, and the characteristic narrow hydrogen lines in their spectra typically originate from earlier, undetected mass-loss events. The long precursor durations require ongoing energy injection, and they could, for example, be powered by interaction or by a continuum-driven wind. Instabilities during the neon- and oxygen-burning phases are predicted to launch precursors in the final years to months before the explosion; however, the brightest precursor is 100 times more energetic than anticipated.
Published: 2021

29. SN 2018bsz: significant dust formation in a nearby superluminous supernova

Author: Chen, T. -W., Brennan, S. J., Wesson, R., Fraser, M., Schweyer, T., Inserra, C., Schulze, S., Nicholl, M., Anderson, J. P., Hsiao, E. Y., Jerkstrand, A., Kankare, E., Kool, E. C., Kravtsov, T., Kuncarayakti, H., Leloudas, G., Li, C. -J., Matsuura, M., Pursiainen, M., Roy, R., Ruiter, A. J., Schady, P., Seitenzahl, I., Sollerman, J., Tartaglia, L., Wang, L., Yates, R. M., Yang, S., Baade, D., Carini, R., Gal-Yam, A., Galbany, L., Gonzalez-Gaitan, S., Gromadzki, M., Gutierrez, C. P., Kotak, R., Maguire, K., Mazzali, P. A., Mueller-Bravo, T. E., Paraskeva, E., Pessi, P. J., Pignata, G., Rau, A., Young, D. R., Chen, T. -W., Brennan, S. J., Wesson, R., Fraser, M., Schweyer, T., Inserra, C., Schulze, S., Nicholl, M., Anderson, J. P., Hsiao, E. Y., Jerkstrand, A., Kankare, E., Kool, E. C., Kravtsov, T., Kuncarayakti, H., Leloudas, G., Li, C. -J., Matsuura, M., Pursiainen, M., Roy, R., Ruiter, A. J., Schady, P., Seitenzahl, I., Sollerman, J., Tartaglia, L., Wang, L., Yates, R. M., Yang, S., Baade, D., Carini, R., Gal-Yam, A., Galbany, L., Gonzalez-Gaitan, S., Gromadzki, M., Gutierrez, C. P., Kotak, R., Maguire, K., Mazzali, P. A., Mueller-Bravo, T. E., Paraskeva, E., Pessi, P. J., Pignata, G., Rau, A., and Young, D. R.
Abstract: We investigate the thermal emission and extinction from dust associated with the nearby superluminous supernova (SLSN) 2018bsz. Our dataset has daily cadence and simultaneous optical and near-infrared coverage up to ~ 100 days, together with late time (+ 1.7 yr) MIR observations. At 230 days after light curve peak the SN is not detected in the optical, but shows a surprisingly strong near-infrared excess, with r - J > 3 mag and r - Ks > 5 mag. The time evolution of the infrared light curve enables us to investigate if the mid-infrared emission is from newly formed dust inside the SN ejecta, from a pre-existing circumstellar envelope, or interstellar material heated by the radiation from the SN. We find the latter two scenarios can be ruled out, and a scenario where new dust is forming in the SN ejecta at epochs > 200 days can self-consistently reproduce the evolution of the SN flux. We can fit the spectral energy distribution well at +230 d with 5 x 10^-4 solar mass of carbon dust, increasing over the following several hundred days to 10^-2 solar mass by +535 d. SN 2018bsz is the first SLSN showing evidence for dust formation within the SN ejecta, and appears to form ten times more dust than normal core-collapse SNe at similar epochs. Together with their preference for low mass, low metallicity host galaxies, we suggest that SLSNe may be a significant contributor to dust formation in the early Universe., Comment: 14 pages and 7 figures in main text, 12 pages and 6 figures in appendix. The observational data will be updated once the paper is accepted
Published: 2021

30. 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., Young, D. R., 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.
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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31. A new photometric and dynamical study of the eclipsing binary star HW Virginis

Author: Brown-Sevilla, S. B., Nascimbeni, V., Borsato, L., Tartaglia, L., Nardiello, D., Granata, V., Libralato, M., Damasso, M., Piotto, G., Pollacco, D., West, R. G., Colombo, L. S., Cunial, A., Piazza, G., Scaggiante, F., Brown-Sevilla, S. B., Nascimbeni, V., Borsato, L., Tartaglia, L., Nardiello, D., Granata, V., Libralato, M., Damasso, M., Piotto, G., Pollacco, D., West, R. G., Colombo, L. S., Cunial, A., Piazza, G., and Scaggiante, F.
Abstract: A growing number of eclipsing binary systems of the "HW Vir" kind (i. e., composed by a subdwarf-B/O primary star and an M dwarf secondary) show variations in their orbital period, also called Eclipse Time Variations (ETVs). Their physical origin is not yet known with certainty: while some ETVs have been claimed to arise from dynamical perturbations due to the presence of circumbinary planetary companions, other authors suggest that the Applegate effect or other unknown stellar mechanisms could be responsible for them. In this work, we present twenty-eight unpublished high-precision light curves of one of the most controversial of these systems, the prototype HW Virginis. We homogeneously analysed the new eclipse timings together with historical data obtained between 1983 and 2012, demonstrating that the planetary models previously claimed do not fit the new photometric data, besides being dynamically unstable. In an effort to find a new model able to fit all the available data, we developed a new approach based on a global-search genetic algorithm and eventually found two new distinct families of solutions that fit the observed timings very well, yet dynamically unstable at the 10^5-year time scale. This serves as a cautionary tale on the existence of formal solutions that apparently explain ETVs but are not physically meaningful, and on the need of carefully testing their stability. On the other hand, our data confirm the presence of an ETV on HW Vir that known stellar mechanisms are unable to explain, pushing towards further observing and modelling efforts., Comment: 14 pages, 7 figures, 7 tables in the main text and 1 table in the appendix. Accepted for publication in MNRAS
Published: 2021
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32. Evidence for multiple origins of fast declining Type II supernovae from spectropolarimetry of SN 2013ej and SN 2017ahn

Author: Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, M., Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., Reichart, D. E., Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, M., Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., and Reichart, D. E.
Abstract: The origin of the diverse light-curve shapes of Type II supernovae (SNe), and whether they come from similar or distinct progenitors, has been actively discussed for decades. Here we report spectropolarimetry of two fast declining Type II (Type IIL) SNe: SN 2013ej and SN 2017ahn. SN 2013ej exhibited high continuum polarization from very soon after the explosion to the radioactive tail phase with time-variable polarization angles. The origin of this polarimetric behavior can be interpreted as the combination of two different aspherical structures, namely an aspherical interaction of the SN ejecta with circumstellar matter (CSM) and an inherently aspherical explosion. Aspherical explosions are a common feature of slowly declining Type II (Type IIP) SNe. By contrast, SN 2017ahn showed low polarization not only in the photospheric phase but also in the radioactive tail phase. This low polarization in the tail phase, which has never before been observed in other Type IIP/L SNe, suggests that the explosion of SN 2017ahn was nearly spherical. These observations imply that Type IIL SNe have, at least, two different origins: they result from stars that have different explosion properties and/or different mass-loss processes. This fact might indicate that 13ej-like Type IIL SNe originate from a similar progenitor to those of Type IIP SNe accompanied by an aspherical CSM interaction, while 17ahn-like Type IIL SNe come from a more massive progenitor with less hydrogen in its envelope., Comment: 19 pages, 14 figures; accepted for publication in MNRAS
Published: 2021
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33. SN 2020bqj: A Type Ibn supernova with a long-lasting peak plateau

Author: Kool, EC, Kool, EC, Karamehmetoglu, E, Sollerman, J, Schulze, S, Lunnan, R, Reynolds, TM, Barbarino, C, Bellm, EC, De, K, Duev, DA, Fremling, C, Golkhou, VZ, Graham, ML, Green, DA, Horesh, A, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Nordin, J, Perley, DA, Phinney, ES, Porter, M, Reiley, D, Rodriguez, H, Van Roestel, J, Rusholme, B, Sharma, Y, Sfaradi, I, Soumagnac, MT, Taggart, K, Tartaglia, L, Williams, DRA, Yan, L, Kool, EC, Kool, EC, Karamehmetoglu, E, Sollerman, J, Schulze, S, Lunnan, R, Reynolds, TM, Barbarino, C, Bellm, EC, De, K, Duev, DA, Fremling, C, Golkhou, VZ, Graham, ML, Green, DA, Horesh, A, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Nordin, J, Perley, DA, Phinney, ES, Porter, M, Reiley, D, Rodriguez, H, Van Roestel, J, Rusholme, B, Sharma, Y, Sfaradi, I, Soumagnac, MT, Taggart, K, Tartaglia, L, Williams, DRA, and Yan, L
Abstract: Context. Type Ibn supernovae (SNe Ibn) are a rare class of stripped envelope supernovae interacting with a helium-rich circumstellar medium (CSM). The majority of the SNe Ibn reported in the literature display a surprising homogeneity in their fast-evolving lightcurves and are typically found in actively starforming spiral galaxies. Aims. We present the discovery and the study of SN 2020bqj (ZTF20aalrqbu), a SN Ibn with a long-duration peak plateau lasting 40 days and hosted by a faint low-mass galaxy. We aim to explain its peculiar properties using an extensive photometric and spectroscopic data set. Methods. We compare the photometric and spectral evolution of SN 2020bqj with regular SNe Ibn from the literature, as well as with other outliers in the SN Ibn subclass. We fit the bolometric and multi-band lightcurves with powering mechanism models such as radioactive decay and CSM interaction. We also model the host galaxy of SN 2020bqj. Results. The risetime, peak magnitude and spectral features of SN 2020bqj are consistent with those of most SNe Ibn, but the SN is a clear outlier in the subclass based on its bright, long-lasting peak plateau and the low mass of its faint host galaxy. We show through modeling that the lightcurve of SN 2020bqj can be powered predominantly by shock heating from the interaction of the SN ejecta and a dense CSM, combined with radioactive decay. The peculiar Type Ibn SN 2011hw is a close analog to SN 2020bqj in terms of lightcurve and spectral evolution, suggesting a similar progenitor and CSM scenario. In this scenario a very massive progenitor star in the transitional phase between a luminous blue variable and a compact Wolf-Rayet star undergoes core-collapse, embedded in a dense helium-rich CSM with an elevated opacity compared to normal SNe Ibn, due to the presence of residual hydrogen. This scenario is consistent with the observed properties of SN 2020bqj and the modeling results. Conclusions. SN 2020bqj is a compelling example of a
Published: 2021

34. SN 2018ijp:the explosion of a stripped-envelope star within a dense H-rich shell?

Author: Tartaglia, L., Sollerman, J., Barbarino, C., Taddia, F., Mason, E., Berton, M., Taggart, Kirsty, Bellm, Eric C., De, K., Frederick, S., Fremling, Christoffer U., Gal-Yam, A., Golkhou, V. Z., Graham, M., Ho, Anna Y. Q., Hung, T., Kaye, S., Kim, Young-Lo, Laher, Russ R., Masci, F. J., Perley, Daniel A., Porter, M. D., Reiley, D. J., Riddle, Reed L., Rusholme, B., Soumagnac, Maayane T., Walters, R., Tartaglia, L., Sollerman, J., Barbarino, C., Taddia, F., Mason, E., Berton, M., Taggart, Kirsty, Bellm, Eric C., De, K., Frederick, S., Fremling, Christoffer U., Gal-Yam, A., Golkhou, V. Z., Graham, M., Ho, Anna Y. Q., Hung, T., Kaye, S., Kim, Young-Lo, Laher, Russ R., Masci, F. J., Perley, Daniel A., Porter, M. D., Reiley, D. J., Riddle, Reed L., Rusholme, B., Soumagnac, Maayane T., and Walters, R.
Abstract: In this paper, we discuss the outcomes of the follow-up campaign of SN 2018ijp, discovered as part of the Zwicky Transient Facility survey for optical transients. Its first spectrum shows similarities to broad-lined Type Ic supernovae around maximum light, whereas later spectra display strong signatures of interaction between rapidly expanding ejecta and a dense H-rich circumstellar medium, coinciding with a second peak in the photometric evolution of the transient. This evolution, along with the results of modeling of the first light-curve peak, suggests a scenario where a stripped star exploded within a dense circumstellar medium. The two main phases in the evolution of the transient could be interpreted as a first phase dominated by radioactive decays, and a later interaction-dominated phase where the ejecta collide with a pre-existing shell. We therefore discuss SN 2018jp within the context of a massive star depleted of its outer layers exploding within a dense H-rich circumstellar medium.
Published: 2021

35. Bright, Months-long stellar outbursts announce the explosion of interaction-powered supernovae

Author: Strotjohann, NL, Strotjohann, NL, Ofek, EO, Gal-Yam, A, Bruch, R, Schulze, S, Shaviv, N, Sollerman, J, Filippenko, AV, Yaron, O, Fremling, C, Nordin, J, Kool, EC, Perley, DA, Ho, AYQ, Yang, Y, Yao, Y, Soumagnac, MT, Graham, ML, Barbarino, C, Tartaglia, L, De, K, Goldstein, DA, Cook, DO, Brink, TG, Taggart, K, Yan, L, Lunnan, R, Kasliwal, M, Kulkarni, SR, Nugent, PE, Masci, FJ, Rosnet, P, Adams, SM, Andreoni, I, Bagdasaryan, A, Bellm, EC, Burdge, K, Duev, DA, Dugas, A, Frederick, S, Goldwasser, S, Hankins, M, Irani, I, Karambelkar, V, Kupfer, T, Liang, J, Neill, JD, Porter, M, Riddle, RL, Sharma, Y, Short, P, Taddia, F, Tzanidakis, A, Van Roestel, J, Walters, R, Zhuang, Z, Strotjohann, NL, Strotjohann, NL, Ofek, EO, Gal-Yam, A, Bruch, R, Schulze, S, Shaviv, N, Sollerman, J, Filippenko, AV, Yaron, O, Fremling, C, Nordin, J, Kool, EC, Perley, DA, Ho, AYQ, Yang, Y, Yao, Y, Soumagnac, MT, Graham, ML, Barbarino, C, Tartaglia, L, De, K, Goldstein, DA, Cook, DO, Brink, TG, Taggart, K, Yan, L, Lunnan, R, Kasliwal, M, Kulkarni, SR, Nugent, PE, Masci, FJ, Rosnet, P, Adams, SM, Andreoni, I, Bagdasaryan, A, Bellm, EC, Burdge, K, Duev, DA, Dugas, A, Frederick, S, Goldwasser, S, Hankins, M, Irani, I, Karambelkar, V, Kupfer, T, Liang, J, Neill, JD, Porter, M, Riddle, RL, Sharma, Y, Short, P, Taddia, F, Tzanidakis, A, Van Roestel, J, Walters, R, and Zhuang, Z
Abstract: Interaction-powered supernovae (SNe) explode within an optically thick circumstellar medium (CSM) that could be ejected during eruptive events. To identify and characterize such pre-explosion outbursts, we produce forcedphotometry light curves for 196 interacting SNe, mostly of Type IIn, detected by the Zwicky Transient Facility between early 2018 and 2020 June. Extensive tests demonstrate that we only expect a few false detections among the 70,000 analyzed pre-explosion images after applying quality cuts and bias corrections. We detect precursor eruptions prior to 18 Type IIn SNe and prior to the Type Ibn SN 2019uo. Precursors become brighter and more frequent in the last months before the SN and month-long outbursts brighter than magnitude -13 occur prior to 25% (5-69%, 95% confidence range) of all Type IIn SNe within the final three months before the explosion. With radiative energies of up to 1049erg, precursors could eject ~1M⊙of material. Nevertheless, SNe with detected precursors are not significantly more luminous than other SNe IIn, and the characteristic narrow hydrogen lines in their spectra typically originate from earlier, undetected mass-loss events. The long precursor durations require ongoing energy injection, and they could, for example, be powered by interaction or by a continuum-driven wind. Instabilities during the neon- and oxygen-burning phases are predicted to launch precursors in the final years to months before the explosion; however, the brightest precursor is 100 times more energetic than anticipated.
Published: 2021

36. SN 2020bqj: A Type Ibn supernova with a long-lasting peak plateau

Author: Kool, EC, Kool, EC, Karamehmetoglu, E, Sollerman, J, Schulze, S, Lunnan, R, Reynolds, TM, Barbarino, C, Bellm, EC, De, K, Duev, DA, Fremling, C, Golkhou, VZ, Graham, ML, Green, DA, Horesh, A, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Nordin, J, Perley, DA, Phinney, ES, Porter, M, Reiley, D, Rodriguez, H, Van Roestel, J, Rusholme, B, Sharma, Y, Sfaradi, I, Soumagnac, MT, Taggart, K, Tartaglia, L, Williams, DRA, Yan, L, Kool, EC, Kool, EC, Karamehmetoglu, E, Sollerman, J, Schulze, S, Lunnan, R, Reynolds, TM, Barbarino, C, Bellm, EC, De, K, Duev, DA, Fremling, C, Golkhou, VZ, Graham, ML, Green, DA, Horesh, A, Kaye, S, Kim, YL, Laher, RR, Masci, FJ, Nordin, J, Perley, DA, Phinney, ES, Porter, M, Reiley, D, Rodriguez, H, Van Roestel, J, Rusholme, B, Sharma, Y, Sfaradi, I, Soumagnac, MT, Taggart, K, Tartaglia, L, Williams, DRA, and Yan, L
Abstract: Context. Type Ibn supernovae (SNe Ibn) are a rare class of stripped envelope supernovae interacting with a helium-rich circumstellar medium (CSM). The majority of the SNe Ibn reported in the literature display a surprising homogeneity in their fast-evolving lightcurves and are typically found in actively starforming spiral galaxies. Aims. We present the discovery and the study of SN 2020bqj (ZTF20aalrqbu), a SN Ibn with a long-duration peak plateau lasting 40 days and hosted by a faint low-mass galaxy. We aim to explain its peculiar properties using an extensive photometric and spectroscopic data set. Methods. We compare the photometric and spectral evolution of SN 2020bqj with regular SNe Ibn from the literature, as well as with other outliers in the SN Ibn subclass. We fit the bolometric and multi-band lightcurves with powering mechanism models such as radioactive decay and CSM interaction. We also model the host galaxy of SN 2020bqj. Results. The risetime, peak magnitude and spectral features of SN 2020bqj are consistent with those of most SNe Ibn, but the SN is a clear outlier in the subclass based on its bright, long-lasting peak plateau and the low mass of its faint host galaxy. We show through modeling that the lightcurve of SN 2020bqj can be powered predominantly by shock heating from the interaction of the SN ejecta and a dense CSM, combined with radioactive decay. The peculiar Type Ibn SN 2011hw is a close analog to SN 2020bqj in terms of lightcurve and spectral evolution, suggesting a similar progenitor and CSM scenario. In this scenario a very massive progenitor star in the transitional phase between a luminous blue variable and a compact Wolf-Rayet star undergoes core-collapse, embedded in a dense helium-rich CSM with an elevated opacity compared to normal SNe Ibn, due to the presence of residual hydrogen. This scenario is consistent with the observed properties of SN 2020bqj and the modeling results. Conclusions. SN 2020bqj is a compelling example of a
Published: 2021

37. Evidence for multiple origins of fast declining Type II supernovae from spectropolarimetry of SN 2013ej and SN 2017ahn

Author: Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, Mattia, Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., Reichart, D. E., Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, Mattia, Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., and Reichart, D. E.
Abstract: The origin of the diverse light-curve shapes of Type II supernovae (SNe), and whether they come from similar or distinct progenitors, has been actively discussed for decades. Here, we report spectropolarimetry of two fast declining Type II (Type IIL) SNe: SN 2013ej and SN 2017ahn. SN 2013ej exhibited high continuum polarization from very soon after the explosion to the radioactive tail phase with time-variable polarization angles. The origin of this polarimetric behaviour can be interpreted as the combination of two different aspherical structures, namely an aspherical interaction of the SN ejecta with circumstellar matter (CSM) and an inherently aspherical explosion. Aspherical explosions are a common feature of slowly declining Type II (Type IIP) SNe. By contrast, SN 2017ahn showed low polarization not only in the photospheric phase but also in the radioactive tail phase. This low polarization in the tail phase, which has never before been observed in other Type IIP/L SNe, suggests that the explosion of SN 2017ahn was nearly spherical. These observations imply that Type IIL SNe have, at least, two different origins: they result from stars that have different explosion properties and/or different mass-loss processes. This fact might indicate that 13ej-like Type IIL SNe originate from a similar progenitor to those of Type IIP SNe accompanied by an aspherical CSM interaction, while 17ahn-like Type IIL SNe come from a more massive progenitor with less hydrogen in its envelope.
Published: 2021
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38. SN 2018ijp : the explosion of a stripped-envelope star within a dense H-rich shell?

Author: Tartaglia, L., Sollerman, J., Barbarino, C., Taddia, F., Mason, E., Berton, M., Taggart, Kirsty, Bellm, Eric C., De, K., Frederick, S., Fremling, Christoffer U., Gal-Yam, A., Golkhou, V. Z., Graham, M., Ho, Anna Y. Q., Hung, T., Kaye, S., Kim, Young-Lo, Laher, Russ R., Masci, F. J., Perley, Daniel A., Porter, M. D., Reiley, D. J., Riddle, Reed L., Rusholme, B., Soumagnac, Maayane T., Walters, R., Tartaglia, L., Sollerman, J., Barbarino, C., Taddia, F., Mason, E., Berton, M., Taggart, Kirsty, Bellm, Eric C., De, K., Frederick, S., Fremling, Christoffer U., Gal-Yam, A., Golkhou, V. Z., Graham, M., Ho, Anna Y. Q., Hung, T., Kaye, S., Kim, Young-Lo, Laher, Russ R., Masci, F. J., Perley, Daniel A., Porter, M. D., Reiley, D. J., Riddle, Reed L., Rusholme, B., Soumagnac, Maayane T., and Walters, R.
Abstract: In this paper, we discuss the outcomes of the follow-up campaign of SN 2018ijp, discovered as part of the Zwicky Transient Facility survey for optical transients. Its first spectrum shows similarities to broad-lined Type Ic supernovae around maximum light, whereas later spectra display strong signatures of interaction between rapidly expanding ejecta and a dense H-rich circumstellar medium, coinciding with a second peak in the photometric evolution of the transient. This evolution, along with the results of modeling of the first light-curve peak, suggests a scenario where a stripped star exploded within a dense circumstellar medium. The two main phases in the evolution of the transient could be interpreted as a first phase dominated by radioactive decays, and a later interaction-dominated phase where the ejecta collide with a pre-existing shell. We therefore discuss SN 2018jp within the context of a massive star depleted of its outer layers exploding within a dense H-rich circumstellar medium.
Published: 2021

39. SN 2018bsz: significant dust formation in a nearby superluminous supernova

Author: Chen, T. -W., Brennan, S. J., Wesson, R., Fraser, M., Schweyer, T., Inserra, C., Schulze, S., Nicholl, M., Anderson, J. P., Hsiao, E. Y., Jerkstrand, A., Kankare, E., Kool, E. C., Kravtsov, T., Kuncarayakti, H., Leloudas, G., Li, C. -J., Matsuura, M., Pursiainen, M., Roy, R., Ruiter, A. J., Schady, P., Seitenzahl, I., Sollerman, J., Tartaglia, L., Wang, L., Yates, R. M., Yang, S., Baade, D., Carini, R., Gal-Yam, A., Galbany, L., Gonzalez-Gaitan, S., Gromadzki, M., Gutierrez, C. P., Kotak, R., Maguire, K., Mazzali, P. A., Mueller-Bravo, T. E., Paraskeva, E., Pessi, P. J., Pignata, G., Rau, A., Young, D. R., Chen, T. -W., Brennan, S. J., Wesson, R., Fraser, M., Schweyer, T., Inserra, C., Schulze, S., Nicholl, M., Anderson, J. P., Hsiao, E. Y., Jerkstrand, A., Kankare, E., Kool, E. C., Kravtsov, T., Kuncarayakti, H., Leloudas, G., Li, C. -J., Matsuura, M., Pursiainen, M., Roy, R., Ruiter, A. J., Schady, P., Seitenzahl, I., Sollerman, J., Tartaglia, L., Wang, L., Yates, R. M., Yang, S., Baade, D., Carini, R., Gal-Yam, A., Galbany, L., Gonzalez-Gaitan, S., Gromadzki, M., Gutierrez, C. P., Kotak, R., Maguire, K., Mazzali, P. A., Mueller-Bravo, T. E., Paraskeva, E., Pessi, P. J., Pignata, G., Rau, A., and Young, D. R.
Abstract: We investigate the thermal emission and extinction from dust associated with the nearby superluminous supernova (SLSN) 2018bsz. Our dataset has daily cadence and simultaneous optical and near-infrared coverage up to ~ 100 days, together with late time (+ 1.7 yr) MIR observations. At 230 days after light curve peak the SN is not detected in the optical, but shows a surprisingly strong near-infrared excess, with r - J > 3 mag and r - Ks > 5 mag. The time evolution of the infrared light curve enables us to investigate if the mid-infrared emission is from newly formed dust inside the SN ejecta, from a pre-existing circumstellar envelope, or interstellar material heated by the radiation from the SN. We find the latter two scenarios can be ruled out, and a scenario where new dust is forming in the SN ejecta at epochs > 200 days can self-consistently reproduce the evolution of the SN flux. We can fit the spectral energy distribution well at +230 d with 5 x 10^-4 solar mass of carbon dust, increasing over the following several hundred days to 10^-2 solar mass by +535 d. SN 2018bsz is the first SLSN showing evidence for dust formation within the SN ejecta, and appears to form ten times more dust than normal core-collapse SNe at similar epochs. Together with their preference for low mass, low metallicity host galaxies, we suggest that SLSNe may be a significant contributor to dust formation in the early Universe., Comment: 14 pages and 7 figures in main text, 12 pages and 6 figures in appendix. The observational data will be updated once the paper is accepted
Published: 2021

40. 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., Young, D. R., 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.
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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41. A new photometric and dynamical study of the eclipsing binary star HW Virginis

Author: Brown-Sevilla, S. B., Nascimbeni, V., Borsato, L., Tartaglia, L., Nardiello, D., Granata, V., Libralato, M., Damasso, M., Piotto, G., Pollacco, D., West, R. G., Colombo, L. S., Cunial, A., Piazza, G., Scaggiante, F., Brown-Sevilla, S. B., Nascimbeni, V., Borsato, L., Tartaglia, L., Nardiello, D., Granata, V., Libralato, M., Damasso, M., Piotto, G., Pollacco, D., West, R. G., Colombo, L. S., Cunial, A., Piazza, G., and Scaggiante, F.
Abstract: A growing number of eclipsing binary systems of the "HW Vir" kind (i. e., composed by a subdwarf-B/O primary star and an M dwarf secondary) show variations in their orbital period, also called Eclipse Time Variations (ETVs). Their physical origin is not yet known with certainty: while some ETVs have been claimed to arise from dynamical perturbations due to the presence of circumbinary planetary companions, other authors suggest that the Applegate effect or other unknown stellar mechanisms could be responsible for them. In this work, we present twenty-eight unpublished high-precision light curves of one of the most controversial of these systems, the prototype HW Virginis. We homogeneously analysed the new eclipse timings together with historical data obtained between 1983 and 2012, demonstrating that the planetary models previously claimed do not fit the new photometric data, besides being dynamically unstable. In an effort to find a new model able to fit all the available data, we developed a new approach based on a global-search genetic algorithm and eventually found two new distinct families of solutions that fit the observed timings very well, yet dynamically unstable at the 10^5-year time scale. This serves as a cautionary tale on the existence of formal solutions that apparently explain ETVs but are not physically meaningful, and on the need of carefully testing their stability. On the other hand, our data confirm the presence of an ETV on HW Vir that known stellar mechanisms are unable to explain, pushing towards further observing and modelling efforts., Comment: 14 pages, 7 figures, 7 tables in the main text and 1 table in the appendix. Accepted for publication in MNRAS
Published: 2021
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42. Evidence for multiple origins of fast declining Type II supernovae from spectropolarimetry of SN 2013ej and SN 2017ahn

Author: Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, M., Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., Reichart, D. E., Nagao, T., Patat, F., Taubenberger, S., Baade, D., Faran, T., Cikota, A., Sand, D. J., Bulla, M., Kuncarayakti, H., Maund, J. R., Tartaglia, L., Valenti, S., and Reichart, D. E.
Abstract: The origin of the diverse light-curve shapes of Type II supernovae (SNe), and whether they come from similar or distinct progenitors, has been actively discussed for decades. Here we report spectropolarimetry of two fast declining Type II (Type IIL) SNe: SN 2013ej and SN 2017ahn. SN 2013ej exhibited high continuum polarization from very soon after the explosion to the radioactive tail phase with time-variable polarization angles. The origin of this polarimetric behavior can be interpreted as the combination of two different aspherical structures, namely an aspherical interaction of the SN ejecta with circumstellar matter (CSM) and an inherently aspherical explosion. Aspherical explosions are a common feature of slowly declining Type II (Type IIP) SNe. By contrast, SN 2017ahn showed low polarization not only in the photospheric phase but also in the radioactive tail phase. This low polarization in the tail phase, which has never before been observed in other Type IIP/L SNe, suggests that the explosion of SN 2017ahn was nearly spherical. These observations imply that Type IIL SNe have, at least, two different origins: they result from stars that have different explosion properties and/or different mass-loss processes. This fact might indicate that 13ej-like Type IIL SNe originate from a similar progenitor to those of Type IIP SNe accompanied by an aspherical CSM interaction, while 17ahn-like Type IIL SNe come from a more massive progenitor with less hydrogen in its envelope., Comment: 19 pages, 14 figures; accepted for publication in MNRAS
Published: 2021
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43. The optical properties of three type II supernovae: 2014cx, 2014cy and 2015cz

Author: Dastidar, R., Misra, K., Singh, M., Pastorello, A., Sahu, D. K., Wang, X., Gangopadhyay, A., Tomasella, L., Zhang, J., Bose, S., Mo, J., Elias-Rosa, N., Tartaglia, L., Yan, S., Kumar, B., Anupama, G. C., Pandey, S. B., Rui, L., Zhang, T., Terreran, G., Ochner, P., Huang, F., Dastidar, R., Misra, K., Singh, M., Pastorello, A., Sahu, D. K., Wang, X., Gangopadhyay, A., Tomasella, L., Zhang, J., Bose, S., Mo, J., Elias-Rosa, N., Tartaglia, L., Yan, S., Kumar, B., Anupama, G. C., Pandey, S. B., Rui, L., Zhang, T., Terreran, G., Ochner, P., and Huang, F.
Abstract: We present the photometric and spectroscopic analysis of three Type II SNe: 2014cx, 2014cy and 2015cz. SN 2014cx is a conventional Type IIP with a shallow slope (0.2 mag/50d) and an atypical short plateau ($\sim$86 d). SNe 2014cy and 2015cz show relatively large decline rates (0.88 and 1.64 mag/50d, respectively) at early times before settling to the plateau phase, unlike the canonical Type IIP/L SN light curves. All of them are normal luminosity SN II with an absolute magnitude at mid-plateau of M$_{V,14cx}^{50}$=$-$16.6$\pm$0.4$\,\rm{mag}$, M$_{V,14cy}^{50}$=$-$16.5$\,\pm\,$0.2$\,\rm{mag}$ and M$_{V,15cz}^{50}$=$-$17.4$\,\pm\,$0.3$\,\rm{mag}$. A relatively broad range of $^{56}$Ni masses is ejected in these explosions (0.027-0.070 M$_\odot$). The spectra show the classical evolution of Type II SNe, dominated by a blue continuum with broad H lines at early phases and narrower metal lines with P Cygni profiles during the plateau. High-velocity H I features are identified in the plateau spectra of SN 2014cx at 11600 km s$^{-1}$, possibly a sign of ejecta-circumstellar interaction. The spectra of SN 2014cy exhibit strong absorption profile of H I similar to normal luminosity events whereas strong metal lines akin to sub-luminous SNe. The analytical modelling of the bolometric light curve of the three events yields similar radii for the three objects within errors (478, 507 and 608 R$_\odot$ for SNe 2014cx, 2014cy and 2015cz, respectively) and a range of ejecta masses (15.0, 22.2 and 18.7 M$_\odot$ for SNe 2014cx, 2014cy and 2015cz), and a modest range of explosion energies (3.3 - 6.0 foe where 1 foe = 10$^{51}$ erg)., Comment: 20 pages, 23 Figures, 3 figures in appendix, accepted for publication in MNRAS
Published: 2021
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44. Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Author: Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Nyholm, A., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., van Soelen, B., Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Nyholm, A., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., and van Soelen, B.
Abstract: We present the results from a high cadence, multi-wavelength observation campaign of AT 2016jbu (aka Gaia16cfr), an interacting transient. This dataset complements the current literature by adding higher cadence as well as extended coverage of the lightcurve evolution and late-time spectroscopic evolution. Photometric coverage reveals that AT 2016jbu underwent significant photometric variability followed by two luminous events, the latter of which reached an absolute magnitude of M$_V\sim$-18.5 mag. This is similar to the transient SN 2009ip whose nature is still debated. Spectra are dominated by narrow emission lines and show a blue continuum during the peak of the second event. AT 2016jbu shows signatures of a complex, non-homogeneous circumstellar material (CSM). We see slowly evolving asymmetric hydrogen line profiles, with velocities of 500km$s^{-1}$ seen in narrow emission features from a slow moving CSM, and up to 10,000km$s^{-1}$ seen in broad absorption from some high velocity material. Late-time spectra ($\sim$+1 year) show a lack of forbidden emission lines expected from a core-collapse supernova and are dominated by strong emission from H, He i and Ca ii. Strong asymmetric emission features, a bumpy lightcurve, and continually evolving spectra suggest an inhibit nebular phase. We compare the evolution of H$\alpha$ among SN 2009ip-like transients and find possible evidence for orientation angle effects. The light-curve evolution of AT 2016jbu suggests similar, but not identical, circumstellar environments to other SN 2009ip-like transients., Comment: 27 pages, 21 figures, accepted for publication in MNRAS
Published: 2021
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45. Progenitor, environment, and modelling of the interacting transient, AT 2016jbu (Gaia16cfr)

Author: Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., van Soelen, B., Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., and van Soelen, B.
Abstract: We present the bolometric lightcurve, identification and analysis of the progenitor candidate, and preliminary modelling of AT2016jbu (Gaia16cfr). We find a progenitor consistent with a $\sim$22--25~$M_{\odot}$ yellow hypergiant surrounded by a dusty circumstellar shell, in agreement with what has been previously reported. We see evidence for significant photometric variability in the progenitor, as well as strong H$\alpha$ emission consistent with pre-existing circumstellar material. The age of the environment as well as the resolved stellar population surrounding AT2016jbu, support a progenitor age of $>$10 Myr, consistent with a progenitor mass of $\sim$22~$M_{\odot}$. A joint analysis of the velocity evolution of AT2016jbu, and the photospheric radius inferred from the bolometric lightcurve shows the transient is consistent with two successive outbursts/explosions. The first outburst ejected material with velocity $\sim$650$kms^{-1}$, while the second, more energetic event, ejected material at $\sim$4500$kms^{-1}$. Whether the latter is the core-collapse of the progenitor remains uncertain. We place a limit on the ejected $^{56}$Ni mass of $<$0.016$M_{\odot}$. Using the BPASS code, we explore a wide range of possible progenitor systems, and find that the majority of these are in binaries, some of which are undergoing mass transfer or common envelope evolution immediately prior to explosion. Finally, we use the SNEC code to demonstrate that the low-energy explosion within some of these binary systems, together with sufficient CSM, can reproduce the overall morphology of the lightcurve of AT2016jbu., Comment: 23 pages, 15 figures, accepted for publication in MNRAS
Published: 2021
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46. AT 2019avd: A novel addition to the diverse population of nuclear transients

Author: Malyali, A., Rau, A., Merloni, A., Nandra, K., Buchner, J., Liu, Z., Gezari, S., Sollerman, J., Shappee, B., Trakhtenbrot, B., Arcavi, I., Ricci, C., van Velzen, S., Goobar, A., Frederick, S., Kawka, A., Tartaglia, L., Burke, J., Hiramatsu, D., Schramm, M., van der Boom, D., Anderson, G., Miller-Jones, J. C. A., Bellm, E., Drake, A., Duev, D., Fremling, C., Graham, M., Masci, F., Rusholme, B., Soumagnac, M., Walters, R., Malyali, A., Rau, A., Merloni, A., Nandra, K., Buchner, J., Liu, Z., Gezari, S., Sollerman, J., Shappee, B., Trakhtenbrot, B., Arcavi, I., Ricci, C., van Velzen, S., Goobar, A., Frederick, S., Kawka, A., Tartaglia, L., Burke, J., Hiramatsu, D., Schramm, M., van der Boom, D., Anderson, G., Miller-Jones, J. C. A., Bellm, E., Drake, A., Duev, D., Fremling, C., Graham, M., Masci, F., Rusholme, B., Soumagnac, M., and Walters, R.
Abstract: We report on SRG/eROSITA, ZTF, ASAS-SN, Las Cumbres, NEOWISE-R, and Swift XRT/UVOT observations of the unique ongoing event AT 2019avd, located in the nucleus of a previously inactive galaxy at $z=0.029$. eROSITA first observed AT 2019avd on 2020-04-28 during its first all sky survey, when it was detected as an ultra-soft X-ray source ($kT\sim 85$ eV) that was $\gtrsim 90$ times brighter in the $0.2-2$ keV band than a previous 3$\sigma$ upper flux detection limit (with no archival X-ray detection at this position). The ZTF optical light curve in the $\sim 450$ days preceding the eROSITA detection is double peaked, and the eROSITA detection coincides with the rise of the second peak. Follow-up optical spectroscopy shows the emergence of a Bowen fluorescence feature and high-ionisation coronal lines ([\ion{Fe}{X}] 6375 {\AA}, [\ion{Fe}{XIV}] 5303 {\AA}), along with persistent broad Balmer emission lines (FWHM$\sim 1400$ km s$^{-1}$). Whilst the X-ray properties make AT 2019avd a promising tidal disruption event (TDE) candidate, the optical properties are atypical for optically selected TDEs. We discuss potential alternative origins that could explain the observed properties of AT 2019avd, such as a stellar binary TDE candidate, or a TDE involving a super massive black hole binary., Comment: A&A accepted 18/12/2020. 19 pages, 14 figures, 8 tables. Forthcoming article in A&A special issue: 'First science highlights from SRG/eROSITA'
Published: 2021
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47. Early Ultraviolet Observations of Type IIn Supernovae Constrain the Asphericity of Their Circumstellar Material

Author: Soumagnac, MT, Soumagnac, MT, Ofek, EO, Liang, J, Gal-Yam, A, Nugent, P, Yang, Y, Cenko, SB, Sollerman, J, Perley, DA, Andreoni, I, Barbarino, C, Burdge, KB, Bruch, RJ, De, K, Dugas, A, Fremling, C, Graham, ML, Hankins, MJ, Strotjohann, NL, Moran, S, Neill, JD, Schulze, S, Shupe, DL, Sipőcz, BM, Taggart, K, Tartaglia, L, Walters, R, Yan, L, Yao, Y, Yaron, O, Bellm, EC, Cannella, C, Dekany, R, Duev, DA, Feeney, M, Frederick, S, Graham, MJ, Laher, RR, Masci, FJ, Kasliwal, MM, Kowalski, M, Kupfer, T, Miller, AA, Rigault, M, Rusholme, B, Soumagnac, MT, Soumagnac, MT, Ofek, EO, Liang, J, Gal-Yam, A, Nugent, P, Yang, Y, Cenko, SB, Sollerman, J, Perley, DA, Andreoni, I, Barbarino, C, Burdge, KB, Bruch, RJ, De, K, Dugas, A, Fremling, C, Graham, ML, Hankins, MJ, Strotjohann, NL, Moran, S, Neill, JD, Schulze, S, Shupe, DL, Sipőcz, BM, Taggart, K, Tartaglia, L, Walters, R, Yan, L, Yao, Y, Yaron, O, Bellm, EC, Cannella, C, Dekany, R, Duev, DA, Feeney, M, Frederick, S, Graham, MJ, Laher, RR, Masci, FJ, Kasliwal, MM, Kowalski, M, Kupfer, T, Miller, AA, Rigault, M, and Rusholme, B
Abstract: © 2020. The American Astronomical Society. All rights reserved.. We present a survey of the early evolution of 12 Type IIn supernovae (SNe IIn) at ultraviolet and visible light wavelengths. We use this survey to constrain the geometry of the circumstellar material (CSM) surrounding SN IIn explosions, which may shed light on their progenitor diversity. In order to distinguish between aspherical and spherical CSM, we estimate the blackbody radius temporal evolution of the SNe IIn of our sample, following the method introduced by Soumagnac et al. We find that higher-luminosity objects tend to show evidence for aspherical CSM. Depending on whether this correlation is due to physical reasons or to some selection bias, we derive a lower limit between 35% and 66% for the fraction of SNe IIn showing evidence for aspherical CSM. This result suggests that asphericity of the CSM surrounding SNe IIn is common - consistent with data from resolved images of stars undergoing considerable mass loss. It should be taken into account for more realistic modeling of these events.
Published: 2020

48. Type IIn supernova light-curve properties measured from an untargeted survey sample

Author: Nyholm, A., Sollerman, J., Tartaglia, L., Taddia, F., Fremling, C., Blagorodnova, N., Filippenko, A.V., Gal-Yam, A., Howell, D.A., Karamehmetoglu, E., Kulkarni, S.R., Laher, R., Leloudas, G., Masci, F., Kasliwal, M.M., Morå, K., Moriya, T.J., Ofek, E.O., Papadogiannakis, S., Quimby, R., Rebbapragada, U., Schulze, S., Nyholm, A., Sollerman, J., Tartaglia, L., Taddia, F., Fremling, C., Blagorodnova, N., Filippenko, A.V., Gal-Yam, A., Howell, D.A., Karamehmetoglu, E., Kulkarni, S.R., Laher, R., Leloudas, G., Masci, F., Kasliwal, M.M., Morå, K., Moriya, T.J., Ofek, E.O., Papadogiannakis, S., Quimby, R., Rebbapragada, U., and Schulze, S.
Abstract: Contains fulltext : 219306.pdf (publisher's version ) (Open Access)
Published: 2020

49. SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Author: Ho, AYQ, Ho, AYQ, Kulkarni, SR, Perley, DA, Cenko, SB, Corsi, A, Schulze, S, Lunnan, R, Sollerman, J, Gal-Yam, A, Anand, S, Barbarino, C, Bellm, EC, Bruch, RJ, Burns, E, De, K, Dekany, R, Delacroix, A, Duev, DA, Frederiks, DD, Fremling, C, Goldstein, DA, Golkhou, VZ, Graham, MJ, Hale, D, Kasliwal, MM, Kupfer, T, Laher, RR, Martikainen, J, Masci, FJ, Neill, JD, Ridnaia, A, Rusholme, B, Savchenko, V, Shupe, DL, Soumagnac, MT, Strotjohann, NL, Svinkin, DS, Taggart, K, Tartaglia, L, Yan, L, Zolkower, J, Ho, AYQ, Ho, AYQ, Kulkarni, SR, Perley, DA, Cenko, SB, Corsi, A, Schulze, S, Lunnan, R, Sollerman, J, Gal-Yam, A, Anand, S, Barbarino, C, Bellm, EC, Bruch, RJ, Burns, E, De, K, Dekany, R, Delacroix, A, Duev, DA, Frederiks, DD, Fremling, C, Goldstein, DA, Golkhou, VZ, Graham, MJ, Hale, D, Kasliwal, MM, Kupfer, T, Laher, RR, Martikainen, J, Masci, FJ, Neill, JD, Ridnaia, A, Rusholme, B, Savchenko, V, Shupe, DL, Soumagnac, MT, Strotjohann, NL, Svinkin, DS, Taggart, K, Tartaglia, L, Yan, L, and Zolkower, J
Abstract: We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio luminosity is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB 980425). We model our VLA observations (spanning 13-43 days) as synchrotron emission from a mildly relativistic (v 0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L X 1041 erg that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6× night-1) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z ≲ 0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts 1 day and reaches a peak luminosity M -18. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission.
Published: 2020

50. Helium-rich Superluminous Supernovae From the Zwicky Transient Facility

Author: Yan, Lin, Perley, D., Schulze, S., Lunnan, R., Sollerman, J., De, K., Chen, Z., Fremling, C., Gal-Yam, A., Taggart, K., Chen, T. W., Andreoni, I., Bellm, E. C., Cunningham, V., Dekany, R., Duev, D., Fransson, C., Laher, R., Hankins, M., Ho, A., Jencson, J., Kaye, S., Kulkarni, S., Kasliwal, M., Golkhou, V., Graham, M., Masci, F., Miller, A., Neill, J., Ofek, E., Porter, M., Mróz, P., Reiley, D., Riddle, R., Rigault, M, Rusholme, B., Shupe, D., Soumagnac, M., Smith, R., Tartaglia, L., Yao, Y., Yaron, O., Yan, Lin, Perley, D., Schulze, S., Lunnan, R., Sollerman, J., De, K., Chen, Z., Fremling, C., Gal-Yam, A., Taggart, K., Chen, T. W., Andreoni, I., Bellm, E. C., Cunningham, V., Dekany, R., Duev, D., Fransson, C., Laher, R., Hankins, M., Ho, A., Jencson, J., Kaye, S., Kulkarni, S., Kasliwal, M., Golkhou, V., Graham, M., Masci, F., Miller, A., Neill, J., Ofek, E., Porter, M., Mróz, P., Reiley, D., Riddle, R., Rigault, M, Rusholme, B., Shupe, D., Soumagnac, M., Smith, R., Tartaglia, L., Yao, Y., and Yaron, O.
Abstract: Helium is expected to be present in the ejecta of some hydrogen-poor superluminous supernovae (SLSN-I). However, so far only one event, PTF10hgi has been identified with He features in its photospheric spectra (Quimby et al. 2018). We present the discovery of a new He-rich SLSN-I, ZTF19aawfbtg (SN2019hge) at $z=0.0866$. This event has more than 10 optical spectra at phases from $-41$ to $+103$\,days relative to the peak, most of which match well with that of PTF10hgi. Confirmation comes from a near-IR spectrum taken at $+34$ days, revealing He I features with P-Cygni profiles at 1.083 and 2.058$\mu$m. Using the optical spectra of PTF10hgi and SN2019hge as templates, we examine 70 SLSN-I discovered by ZTF in the first two years of operation and found additional five SLSN-I with distinct He-features. The excitation of He\,I atoms in normal core collapse supernovae requires non-thermal radiation, as proposed by previous studies. These He-rich events can not be explained by traditional $^{56}$Ni mixing model because of their blue spectra, high peak luminosity and slow rising time scales. Magnetar models offer a possible solution since pulsar winds naturally generate high energy particles as sources of non-thermal excitation. An alternative model is ejecta interaction with H-poor CSM which may be supported by the observed light curve undulations. These six SLSN-Ib appear to have relatively low-peak luminosities (rest-frame $M_g = -20.06\pm0.16$ mag)., Comment: 12 pages, 6 figures, Accepted for publication in ApJL. Matched with the published version
Published: 2020
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