424 results on '"Benetti, Stefano"'
Search Results
102. Photometric and spectroscopic evolution of the peculiar Type IIn SN 2012ab
- Author
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Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Istituto Nazionale di Fisica Nucleare, Gangopadhyay, Anjansha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, Pandey, Shashi Bhushan, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Istituto Nazionale di Fisica Nucleare, Gangopadhyay, Anjansha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, and Pandey, Shashi Bhushan
- Abstract
We present an extensive (∼1200 d) photometric and spectroscopic monitoring of the Type IIn supernova (SN) 2012ab. After a rapid initial rise leading to a bright maximum (MR = −19.39 mag), the light curves show a plateau lasting about 2 months followed by a steep decline up to about 100 d. Only in the U band, the decline is constant in the same interval. At later phases, the light curves remain flatter than the 56Co decline, suggesting the increasing contribution of the interaction between SN ejecta with circumstellar material (CSM). Although heavily contaminated by emission lines of the host galaxy, the early spectral sequence (until 32 d) shows persistent narrow emissions, indicative of slow unshocked CSM, and the emergence of broad Balmer lines of hydrogen with P-Cygni profiles over a blue continuum, arising from a fast expanding SN ejecta. From about 2 months to ∼1200 d, the P-Cygni profiles are overcome by intermediate width emissions [full width at half-maximum (FWHM) ∼6000 km s−1], produced in the shocked region due to interaction. On the red wing, a red bump appears after 76 d, likely a signature of the onset of interaction of the receding ejecta with the CSM. The presence of fast material both approaching and then receding is suggestive that we are observing the SN along the axis of a jet-like ejection in a cavity devoid of or uninterrupted by CSM in the innermost regions.
- Published
- 2020
103. CLOSING GAPS TO OUR ORIGINS THE UV WINDOW INTO THE UNIVERSE
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Castro, Ana I. Gomez de, Barstow, Martin A., Baudin, Fréderic, Benetti, Stefano, Bouret, Jean Claude, Brosch, Noah, Martino, Domitilla de, Zanna, Giulio del, Evans, Chris, García, Miriam, Gaensicke, Boris, Kehrig, Carolina, Lapington, Jon, Etangs, Alain Lecavelier des, Naletto, Giampiero, Nazé, Yael, Neiner, Coralie, Nichols, Jonathan, Orio, Marina, Pagano, Isabella, Rauw, Gregor, Shore, Steven, Tovmasian, Gagik, ud-Doula, Asif, France, Kevin, Hillenbrand, Lynne, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Space Astronomy Research Group – Universidad Complutense de Madrid, and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,[SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] - Published
- 2019
104. The ultraviolet researcher to investigate the emergence of life: a mission proposal to ESA's F-call
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den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Gómez de Castro, Ana I., de Isidro-Gómez, Ana I., de Leyva, Diego, Bachiotti, Francesca, León, Julia, Ribes, Pol, Casalta, Joan Manel, Miravet, Carlos, Vallejo, Juan C., Sachkov, Mikhail, Canet, Ada, Shustov, Boris, de la Fuente, Raúl, France, Kevin, Patty, Lucas, Benetti, Stefano, and ud-Doula, Asif
- Published
- 2022
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105. Photometric and spectroscopic evolution of the peculiar Type IIn SN 2012ab
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Gangopadhyay, Anjasha, primary, Turatto, Massimo, additional, Benetti, Stefano, additional, Misra, Kuntal, additional, Kumar, Brajesh, additional, Cappellaro, Enrico, additional, Pastorello, Andrea, additional, Tomasella, Lina, additional, Vanni, Sabrina, additional, Fiore, Achille, additional, Morales-Garoffolo, A, additional, Elias-Rosa, Nancy, additional, Singh, Mridweeka, additional, Dastidar, Raya, additional, Ochner, Paolo, additional, Tartaglia, Leonardo, additional, Kumar, Brijesh, additional, and Pandey, Shashi Bhushan, additional
- Published
- 2020
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106. Observations of the low-luminosity Type Iax supernova 2019gsc: a fainter clone of SN 2008ha?
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Tomasella, Lina, primary, Stritzinger, Maximilian, primary, Benetti, Stefano, primary, Elias-Rosa, Nancy, primary, Cappellaro, Enrico, primary, Kankare, Erkki, primary, Lundqvist, Peter, primary, Magee, Mark, primary, Maguire, Kate, primary, Pastorello, Andrea, primary, Prentice, Simon, primary, and Reguitti, Andrea, primary
- Published
- 2020
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107. Evidence for Type Ia Supernova Diversity from Ultraviolet Observations with the Hubble Space Telescope
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Wang, Xiaofeng, Wang, Lifan, Filippenko, Alexei, Baron, Eddie, Kromer, Markus, Jack, Dennis, Zhang, Tianmeng, Aldering, Greg, Antilogus, Pierre, Arnett, W. David, Baade, Dietrich, Barris, Brian J, Benetti, Stefano, Bouchet, Patrice, Burrows, Adam S, Canal, Ramon, Cappellaro, Enrico, Carlberg, Raymond, di Carlo, Elisa, Challis, Peter, Crotts, Arlin, Danziger, John I, Della Valle, Massimo, and Holland, Stephen T
- Subjects
Astronomy - Abstract
We present ultraviolet (UV) spectroscopy and photometry of four Type Ia supernovae (SNe 2004dt, 2004ef, 2005M, and 2005cf) obtained with the UV prism of the Advanced Camera for Surveys on the Hubble Space Telescope, This dataset provides unique spectral time series down to 2000 A. Significant diversity is seen in the near-maximum-light spectra (approx.2000-3500 A) for this small sample. The corresponding photometric data, together with archival data from Swift Ultraviolet/Optical Telescope observations, provide further evidence of increased dispersion in the UV emission with respect to the optical. The peak luminosities measured in the uvw lIF250W filter are found to correlate with the B-band light-curve shape parameter .(Delta)m15(B), but with much larger scatter relative to the correlation in the broad-band B band (e.g., approx. 0.4 mag versus approx. 0.2 mag for those with 0.8 <.(Delta)m15(B) < 1.7 mag). SN 2004dt is found as an outlier of this correlation (at> 3(sigma), being brighter than normal SNe Ia such as SN 2005cf by approx. 0,9 mag and approx. 2.0 mag in the uvwl1F250W and uvm2/F220W filters, respectively. We show that different progenitor metallicity or line-expansion velocities alone cannot explain such a large discrepancy. Viewing-angle effects, such as due to an asymmetric explosion, may have a significant influence on the flux emitted in the UV region. Detailed modeling is needed to disentangle and quantify the above effects
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- 2012
108. Closing gaps to our origins. The UV window into the Universe
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Gomez de Castro, Ana I., Barstow, Martin A., Baudin, Fréderic, BENETTI, Stefano, Bouret, Jean Claude, Brosch, Noah, DE MARTINO, Domitilla, del Zanna, Giulio, Evans, Chris, García, Miriam, Gaensicke, Boris, Kehrig, Carolina, Lapington, Jon, Lecavelier des Etangs, Alain, Naletto, Giampiero, Nazé, Yael, Neiner, Coralie, Nichols, Jonathan, ORIO, Marina, PAGANO, Isabella, Rauw, Gregor, Shore, Steven, Tovmasian, Gagik, ud-Doula, Asif, France, Kevin, Hillenbrand, Lynne, and ESP
- Abstract
The investigation of the emergence of life is a major endeavour of science. Astronomy is contributing to it in three fundamental manners: (1) by measuring the chemical enrichment of the Universe, (2) by investigating planet formation and searching for exoplanets with signatures of life and, (3) by determining the abundance of aminoacids and the chemical routes to aminoacid and protein growth in astronomical bodies. This proposal deals with the first two. In the Voyage to 2050, the world-wide scientific community is getting equipped with large facilities for the investigation of the emergence of life in the Universe (i.e. VLT, JWST, ELT, GMT, TMT, ALMA, FAST, VLA, ATHENA, SKA) including the ESA's CHEOPS, PLATO and ARIEL missions. This white paper is a community effort to call for the development of a large ultraviolet optical observatory to gather fundamental data for this investigation that will not be accessible through other ranges of the electromagnetic spectrum. A versatile space observatory with UV sensitivity a factor of 50-100 greater than existing facilities will revolutionize our understanding of the pathway to life in the Universe.
- Published
- 2019
109. Spectroscopic observation of AT 2019azh by NUTS (NOT Un-biased Transient Survey)
- Author
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Heikkila, Teppo, Reynolds, Tom, Kankare, Erkki, Mattila, Seppo, Arcavi, Iair, French, K. Decker, Zabludoff, Ann, Gromadzki, Mariusz, Lundqvist, Peter, Benetti, Stefano, Viuho, Joonas, Jimenez, Rosa Clavero, Heikkila, Teppo, Reynolds, Tom, Kankare, Erkki, Mattila, Seppo, Arcavi, Iair, French, K. Decker, Zabludoff, Ann, Gromadzki, Mariusz, Lundqvist, Peter, Benetti, Stefano, Viuho, Joonas, and Jimenez, Rosa Clavero
- Abstract
The Nordic Optical Telescope (NOT) Unbiased Transient Survey (NUTS; ATel #8992) reports the spectroscopic observation of the nuclear transient ZTF17aaazdba / ASASSN-19dj in the host galaxy KUG 0810+227.
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- 2019
110. Strongly Bipolar Inner Ejecta of the Normal Type IIP Supernova ASASSN-16at
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Bose, Subhash, Dong, Subo, Elias-Rosa, N., Shappee, B. J., Bersier, David, Benetti, Stefano, Stritzinger, M. D., Grupe, D., Kochanek, C. S., Prieto, J. L., Chen, Ping, Kuncarayakti, H., Mattila, Seppo, Morales-Garoffolo, Antonia, Morrell, Nidia, Onori, F., Reynolds, Thomas M., Siviero, A., Somero, Auni, Stanek, K. Z., Terreran, Giacomo, Thompson, Todd A., Tomasella, L., Ashall, C., Gall, Christa, Gromadzki, M., Holoien, T. W-S, Bose, Subhash, Dong, Subo, Elias-Rosa, N., Shappee, B. J., Bersier, David, Benetti, Stefano, Stritzinger, M. D., Grupe, D., Kochanek, C. S., Prieto, J. L., Chen, Ping, Kuncarayakti, H., Mattila, Seppo, Morales-Garoffolo, Antonia, Morrell, Nidia, Onori, F., Reynolds, Thomas M., Siviero, A., Somero, Auni, Stanek, K. Z., Terreran, Giacomo, Thompson, Todd A., Tomasella, L., Ashall, C., Gall, Christa, Gromadzki, M., and Holoien, T. W-S
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- 2019
111. Sudare: The Supernova Search With Omegacam@Vst
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Cappellaro, Enrico, Botticella, Maria Teresa, Greggio, Laura, Pignata, Giuliano, Della Valle, Massimo, Grado, Aniello, Limatola, Luca, Baruffolo, Andrea, Benetti, Stefano, Bufano, F., Capaccioli, Massimo, Cascone, Enrico, Covone, Giovanni, De Cicco, Demetra, Falocco, S., Haeussler, B., Harutyunyan, V., Jarvis, M., Marchetti, L., Napolitano, Nicola, Paolillo, Maurizio, Pastorello, A., Radovich, Mario, Schipani, Pietro, Tomasella, L., Turatto, Massimo, and Vaccari, Mattia
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
SUDARE is a project intended to study the evolution of the supernova rate with cosmic time. A major component of the project is a supernova search conducted with the VST+Omegacam on two selected sky fields (COSMOS and CDFS). We present the result of this project, the lesson learned and the current lines of research.
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- 2018
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112. Gaia17biu/SN 2017egm in NGC 3191:the closest hydrogen-poor superluminous supernova to date is in a 'normal', massive, metal-rich spiral galaxy
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Bose, Subhash, Dong, Subo, Pastorello, A., Filippenko, Alexei V., Kochanek, C. S., Mauerhan, Jon, Romero-Canizales, C., Brink, Thomas, Chen, Ping, Prieto, J. L., Post, R., Ashall, Christopher, Grupe, Dirk, Tomasella, L., Benetti, Stefano, Shappee, B. J., Stanek, K. Z., Cai, Zheng, Falco, E., Lundqvist, Peter, Mattila, Seppo, Mutel, Robert, Ochner, Paolo, Pooley, David, Stritzinger, M. D., Villanueva, S., Zheng, Weikang, Beswick, R. J., Brown, Peter J., Cappellaro, E., Davis, Scott, Jaeger, Thomas, Elias-Rosa, N., Christa Gall, Gaudi, B. Scott, Herczeg, Gregory J., Hestenes, Julia, Holoien, T. W. -S, Hosseinzadeh, Griffin, Hsiao, E. Y., Hu, Shaoming, Jaejin, Shin, Jeffers, Ben, Koff, R. A., Kumar, Sahana, Kurtenkov, Alexander, Lau, Marie Wingyee, Prentice, Simon, Rudy, Richard J., Shahbandeh, Melissa, Somero, Auni, Stassun, Keivan G., Thompson, T. A., Valenti, Stefano, Woo, Jong-Hak, and Yunus, Sameen
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astro-ph.HE ,astro-ph.SR ,astro-ph.GA ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The rare hydrogen-poor superluminous supernovae (SLSNe-I) have been predominantly found in low-metallicity, star-forming dwarf galaxies. Here we identify Gaia17biu/SN 2017egm as an SLSN-I occurring in a "normal" spiral galaxy (NGC 3191) in terms of stellar mass (several times 10^10 M_sun) and metallicity (roughly solar). At redshift z=0.031, Gaia17biu is also the lowest redshift SLSN-I to date, and the absence of a larger population of SLSNe-I in dwarf galaxies of similar redshift suggests that metallicity is likely less important to the production of SLSNe-I than previously believed. With the smallest distance and highest apparent brightness for a SLSN-I, we are able to study Gaia17biu in unprecedented detail. Its pre-peak NUV to optical color is similar to that of Gaia16apd and among the bluest observed for a SLSN-I, while its peak luminosity (M_g = -21) is at the low end of the SLSN-I luminosity function. The pre-peak spectra resemble those of some fast-declining SLSNe-I while the post-peak spectra are similar to those of slow-declining SLSNe-I, suggesting that the post-peak decline rate is probably not a useful indicator for describing the spectral diversity of SLSNe-I. Thanks to the high SNRs of our spectra, we identify several new spectroscopic features that may help to probe the properties of these enigmatic explosions. We also detect polarization at the ~0.5% level that is not strongly dependent on wavelength, suggesting a modest, global departure from spherical symmetry for the source. In addition, we put the tightest upper limit yet on the radio luminosity of an SLSN-I at
- Published
- 2018
113. Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System
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Li, Wenxiong, primary, Wang, Xiaofeng, additional, Hu, Maokai, additional, Yang, Yi, additional, Zhang, Jujia, additional, Mo, Jun, additional, Chen, Zhihao, additional, Zhang, Tianmeng, additional, Benetti, Stefano, additional, Cappellaro, Enrico, additional, Elias-Rosa, Nancy, additional, Isern, Jordi, additional, Morales-Garoffolo, Antonia, additional, Huang, Fang, additional, Ochner, Paolo, additional, Pastorello, Andrea, additional, Reguitti, Andrea, additional, Tartaglia, Leonardo, additional, Terreran, Giacomo, additional, Tomasella, Lina, additional, and Wang, Lifan, additional
- Published
- 2019
- Full Text
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114. Strongly Bipolar Inner Ejecta of the Normal Type IIP Supernova ASASSN-16at
- Author
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Bose, Subhash, primary, Dong, Subo, additional, Elias-Rosa, N., additional, Shappee, B. J., additional, Bersier, David, additional, Benetti, Stefano, additional, Stritzinger, M. D., additional, Grupe, D., additional, Kochanek, C. S., additional, Prieto, J. L., additional, Chen, Ping, additional, Kuncarayakti, H., additional, Mattila, Seppo, additional, Morales-Garoffolo, Antonia, additional, Morrell, Nidia, additional, Onori, F., additional, Reynolds, Thomas M, additional, Siviero, A., additional, Somero, Auni, additional, Stanek, K. Z., additional, Terreran, Giacomo, additional, Thompson, Todd A., additional, Tomasella, L., additional, Ashall, C., additional, Gall, Christa, additional, Gromadzki, M., additional, and Holoien, T. W.-S., additional
- Published
- 2019
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115. Observations of a Fast-expanding and UV-bright Type Ia Supernova SN 2013gs
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Zhang, Tianmeng, primary, Wang, Xiaofeng, additional, Zhao, Xulin, additional, Xu, Dong, additional, Reguitti, Andrea, additional, Zhang, Jujia, additional, Pastorello, Andrea, additional, Tomasella, Lina, additional, Ochner, Paolo, additional, Tartaglia, Leonardo, additional, Benetti, Stefano, additional, Turatto, Massimo, additional, Harutyunyan, Avet, additional, Elias-Rosa, Nancy, additional, Huang, Fang, additional, Zhang, Kaicheng, additional, Chen, Juncheng, additional, Jiang, Zhaoji, additional, Ma, Jun, additional, Nie, Jundan, additional, Peng, Xiyan, additional, Zhou, Xu, additional, Zhou, Zhimin, additional, and Zou, Hu, additional
- Published
- 2019
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116. SN 2017dio : A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium
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Kuncarayakti, Hanindyo, Maeda, Keiichi, Ashall, Christopher J., Prentice, Simon J., Mattila, Seppo, Kankare, Erkki, Fransson, Claes, Lundqvist, Peter, Pastorello, Andrea, Leloudas, Giorgos, Anderson, Joseph P., Benetti, Stefano, Bersten, Melina C., Cappellaro, Enrico, Cartier, Regis, Denneau, Larry, Della Valle, Massimo, Elias-Rosa, Nancy, Folatelli, Gaston, Fraser, Morgan, Galbany, Lluis, Gall, Christa, Gal-Yam, Avishay, Gutierrez, Claudia P., Hamanowicz, Aleksandra, Heinze, Ari, Inserra, Cosimo, Kangas, Tuomas, Mazzali, Paolo, Melandri, Andrea, Pignata, Giuliano, Rest, Armin, Reynolds, Thomas, Roy, Rupak, Smartt, Stephen J., Smith, Ken W., Sollerman, Jesper, Somero, Auni, Stalder, Brian, Stritzinger, Maximilian, Taddia, Francesco, Tomasella, Lina, Tonry, John, Weiland, Henry, Young, David R., Kuncarayakti, Hanindyo, Maeda, Keiichi, Ashall, Christopher J., Prentice, Simon J., Mattila, Seppo, Kankare, Erkki, Fransson, Claes, Lundqvist, Peter, Pastorello, Andrea, Leloudas, Giorgos, Anderson, Joseph P., Benetti, Stefano, Bersten, Melina C., Cappellaro, Enrico, Cartier, Regis, Denneau, Larry, Della Valle, Massimo, Elias-Rosa, Nancy, Folatelli, Gaston, Fraser, Morgan, Galbany, Lluis, Gall, Christa, Gal-Yam, Avishay, Gutierrez, Claudia P., Hamanowicz, Aleksandra, Heinze, Ari, Inserra, Cosimo, Kangas, Tuomas, Mazzali, Paolo, Melandri, Andrea, Pignata, Giuliano, Rest, Armin, Reynolds, Thomas, Roy, Rupak, Smartt, Stephen J., Smith, Ken W., Sollerman, Jesper, Somero, Auni, Stalder, Brian, Stritzinger, Maximilian, Taddia, Francesco, Tomasella, Lina, Tonry, John, Weiland, Henry, and Young, David R.
- Abstract
SN 2017dio shows both spectral characteristics of a type-Ic supernova (SN) and signs of a hydrogen-rich circumstellar medium (CSM). Prominent, narrow emission lines of H and He are superposed on the continuum. Subsequent evolution revealed that the SN ejecta are interacting with the CSM. The initial SN Ic identification was confirmed by removing the CSM interaction component from the spectrum and comparing with known SNe Ic and, reversely, adding a CSM interaction component to the spectra of known SNe Ic and comparing them to SN 2017dio. Excellent agreement was obtained with both procedures, reinforcing the SN Ic classification. The light curve constrains the pre-interaction SN Ic peak absolute magnitude to be around M-g = -17.6 mag. No evidence of significant extinction is found, ruling out a brighter luminosity required by an SN Ia classification. These pieces of evidence support the view that SN 2017dio is an SN Ic, and therefore the first firm case of an SN Ic with signatures of hydrogen-rich CSM in the early spectrum. The CSM is unlikely to have been shaped by steady-state stellar winds. The mass loss of the progenitor star must have been intense, M similar to 0.02 (epsilon(H alpha)/0.01)(-1) (nu(wind)/500 km s(-1)) (nu(shock)/10,000 km s(-1))M--3(circle dot) yr(-1), peaking at a few decades before the SN. Such a high mass-loss rate might have been experienced by the progenitor through eruptions or binary stripping.
- Published
- 2018
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117. Gaia17biu/SN 2017egm in NGC 3191 : The Closest Hydrogen-poor Superluminous Supernova to Date Is in a Normal, Massive, Metal-rich Spiral Galaxy
- Author
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Bose, Subhash, Dong, Subo, Pastorello, A., Filippenko, Alexei V., Kochanek, C. S., Mauerhan, Jon, Romero-Canizales, C., Brink, Thomas G., Chen, Ping, Prieto, J. L., Post, R., Ashall, Christopher, Grupe, Dirk, Tomasella, L., Benetti, Stefano, Shappee, B. J., Stanek, K. Z., Cai, Zheng, Falco, E., Lundqvist, Peter, Mattila, Seppo, Mutel, Robert, Ochner, Paolo, Pooley, David, Stritzinger, M. D., Villanueva, S., Zheng, WeiKang, Beswick, R. J., Brown, Peter J., Cappellaro, E., Davis, Scott, Fraser, Morgan, de Jaeger, Thomas, Elias-Rosa, N., Gall, C., Gaudi, B. Scott, Herczeg, Gregory J., Hestenes, Julia, Holoien, T. W. -S., Hosseinzadeh, Griffin, Hsiao, E. Y., Hu, Shaoming, Jaejin, Shin, Jeffers, Ben, Koff, R. A., Kumar, Sahana, Kurtenkov, Alexander, Lau, Marie Wingyee, Prentice, Simon, Reynolds, T., Rudy, Richard J., Shahbandeh, Melissa, Somero, Auni, Stassun, Keivan G., Thompson, Todd A., Valenti, Stefano, Woo, Jong-Hak, Yunus, Sameen, Bose, Subhash, Dong, Subo, Pastorello, A., Filippenko, Alexei V., Kochanek, C. S., Mauerhan, Jon, Romero-Canizales, C., Brink, Thomas G., Chen, Ping, Prieto, J. L., Post, R., Ashall, Christopher, Grupe, Dirk, Tomasella, L., Benetti, Stefano, Shappee, B. J., Stanek, K. Z., Cai, Zheng, Falco, E., Lundqvist, Peter, Mattila, Seppo, Mutel, Robert, Ochner, Paolo, Pooley, David, Stritzinger, M. D., Villanueva, S., Zheng, WeiKang, Beswick, R. J., Brown, Peter J., Cappellaro, E., Davis, Scott, Fraser, Morgan, de Jaeger, Thomas, Elias-Rosa, N., Gall, C., Gaudi, B. Scott, Herczeg, Gregory J., Hestenes, Julia, Holoien, T. W. -S., Hosseinzadeh, Griffin, Hsiao, E. Y., Hu, Shaoming, Jaejin, Shin, Jeffers, Ben, Koff, R. A., Kumar, Sahana, Kurtenkov, Alexander, Lau, Marie Wingyee, Prentice, Simon, Reynolds, T., Rudy, Richard J., Shahbandeh, Melissa, Somero, Auni, Stassun, Keivan G., Thompson, Todd A., Valenti, Stefano, Woo, Jong-Hak, and Yunus, Sameen
- Abstract
Hydrogen-poor superluminous supernovae (SLSNe-I) have been predominantly found in low-metallicity, star-forming dwarf galaxies. Here we identify Gaia17biu/SN 2017egm as an SLSN-I occurring in a normal spiral galaxy (NGC 3191) in terms of stellar mass (several times 10(10) M-circle dot) and metallicity (roughly solar). At redshift z = 0.031, Gaia17biu is also the lowest-redshift SLSN-I to date, and the absence of a larger population of SLSNe-I in dwarf galaxies of similar redshift suggests that metallicity is likely less important to the production of SLSNe-I than previously believed. With the smallest distance and highest apparent brightness for an SLSN-I, we are able to study Gaia17biu in unprecedented detail. Its pre-peak near-ultraviolet to optical color is similar to that of Gaia16apd and among the bluest observed for an SLSN-I, while its peak luminosity (M-g = -21 mag) is substantially lower than that of Gaia16apd. Thanks to the high signal-to-noise ratios of our spectra, we identify several new spectroscopic features that may help to probe the properties of these enigmatic explosions. We detect polarization at the similar to 0.5% level that is not strongly dependent on wavelength, suggesting a modest, global departure from spherical symmetry. In addition, we put the tightest upper limit yet on the radio luminosity of an SLSN-I with < 5.4 x 10(26) erg s(-1) Hz(-1) at 10 GHz, which is almost a factor of 40 better than previous upper limits and one of the few measured at an early stage in the evolution of an SLSN-I. This limit largely rules out an association of this SLSN-I with known populations of gamma-ray-burst-like central engines.
- Published
- 2018
- Full Text
- View/download PDF
118. The Type IIn Supernova SN 2010bt : The Explosion of a Star in Outburst
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Elias-Rosa, Nancy, Van Dyk, Schuyler D., Benetti, Stefano, Cappellaro, Enrico, Smith, Nathan, Kotak, Rubina, Turatto, Massimo, Filippenko, Alexei V., Pignata, Giuliano, Fox, Ori D., Galbany, Lluis, González-Gaitán, Santiago, Miluzio, Matteo, Monard, L. A. G., Ergon, Mattias, Elias-Rosa, Nancy, Van Dyk, Schuyler D., Benetti, Stefano, Cappellaro, Enrico, Smith, Nathan, Kotak, Rubina, Turatto, Massimo, Filippenko, Alexei V., Pignata, Giuliano, Fox, Ori D., Galbany, Lluis, González-Gaitán, Santiago, Miluzio, Matteo, Monard, L. A. G., and Ergon, Mattias
- Abstract
It is well known that massive stars (M > 8M(circle dot)) evolve up to the collapse of the stellar core, resulting in most cases in a supernova (SN) explosion. Their heterogeneity is related mainly to different configurations of the progenitor star at the moment of the explosion and to their immediate environments. We present photometry and spectroscopy of SN. 2010bt, which was classified as a Type. IIn. SN from a spectrum obtained soon after discovery and was observed extensively for about 2 months. After the seasonal interruption owing to its proximity to the Sun, the SN was below the detection threshold, indicative of a rapid luminosity decline. We can identify the likely progenitor with a very luminous star (log L/L-circle dot approximate to 7) through comparison of Hubble Space Telescope images of the host galaxy prior to explosion with those of the SN obtained after maximum light. Such a luminosity is not expected for a quiescent star, but rather for a massive star in an active phase. This progenitor candidate was later confirmed via images taken in 2015 (similar to 5 yr post-discovery), in which no bright point source was detected at the SN position. Given these results and the SN behavior, we conclude that SN. 2010bt was likely a Type IIn SN and that its progenitor was a massive star that experienced an outburst shortly before the final explosion, leading to a dense H-rich circumstellar environment around the SN progenitor.
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- 2018
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119. SN 2017dio:A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium
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Kuncarayakti, Hanindyo, Maeda, Keiichi, Ashall, Christopher J., Prentice, Simon J., Mattila, Seppo, Kankare, Erkki, Fransson, Claes, Lundqvist, Peter, Pastorello, Andrea, Leloudas, Giorgos, Anderson, Joseph P., Benetti, Stefano, Bersten, Melina C., Cappellaro, Enrico, Cartier, Regis, Denneau, Larry, Della Valle, Massimo, Elias-Rosa, Nancy, Folatelli, Gaston, Fraser, Morgan, Galbany, Lluis, Gall, Christa, Gal-Yam, Avishay, Gutierrez, Claudia P., Hamanowicz, Aleksandra, Heinze, Ari, Inserra, Cosimo, Kangas, Tuomas, Mazzali, Paolo, Melandri, Andrea, Pignata, Giuliano, Rest, Armin, Reynolds, Thomas, Roy, Rupak, Smartt, Stephen J., Smith, Ken W., Sollerman, Jesper, Somero, Auni, Stalder, Brian, Stritzinger, Maximilian, Taddia, Francesco, Tomasella, Lina, Tonry, John, Weiland, Henry, Young, David R., Kuncarayakti, Hanindyo, Maeda, Keiichi, Ashall, Christopher J., Prentice, Simon J., Mattila, Seppo, Kankare, Erkki, Fransson, Claes, Lundqvist, Peter, Pastorello, Andrea, Leloudas, Giorgos, Anderson, Joseph P., Benetti, Stefano, Bersten, Melina C., Cappellaro, Enrico, Cartier, Regis, Denneau, Larry, Della Valle, Massimo, Elias-Rosa, Nancy, Folatelli, Gaston, Fraser, Morgan, Galbany, Lluis, Gall, Christa, Gal-Yam, Avishay, Gutierrez, Claudia P., Hamanowicz, Aleksandra, Heinze, Ari, Inserra, Cosimo, Kangas, Tuomas, Mazzali, Paolo, Melandri, Andrea, Pignata, Giuliano, Rest, Armin, Reynolds, Thomas, Roy, Rupak, Smartt, Stephen J., Smith, Ken W., Sollerman, Jesper, Somero, Auni, Stalder, Brian, Stritzinger, Maximilian, Taddia, Francesco, Tomasella, Lina, Tonry, John, Weiland, Henry, and Young, David R.
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- 2018
120. The 1.82m Copernico telescope - User Manual
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TOMASELLA, Lina, BENETTI, Stefano, CHIOMENTO, Venerio, FRIGO, Aldo, MARTORANA, Giorgio, Rebeschini, Mauro, TRAVERSO, Luciano, and Fiaschi, Marco
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- 2017
121. The Ekar Schmidt 67/91 telescope - User Manual
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OCHNER, PAOLO, TOMASELLA, Lina, BENETTI, Stefano, CHIOMENTO, Venerio, FRIGO, Aldo, MARTORANA, Giorgio, Rebeschini, Mauro, TRAVERSO, Luciano, and Fiaschi, Marco
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- 2017
122. Analysis of the photospheric epoch spectra of type 1a supernovae SN 1990N and SN 1991T
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Jeffery, David J, Leibundgut, Bruno, Kirshner, Robert P, Benetti, Stefano, Branch, David, and Sonneborn, George
- Subjects
Astrophysics - Abstract
This paper presents an LTE analysis of the photospheric epoch optical and IUE UV spectra of the recent Type Ia supernovae SN 1990N and SN 1991T. It is found that SN 1990N has matter moving as fast as 40,000 km/s, while SN 1991T has matter moving as fast as 20,000 km/s. The exponential density profile with e-folding velocity of 3160 km/s suggested by deflation and delayed/late-detonation explosion models is adequate for calculating fits to the observed spectra. Findings on the iron peak elements suggest that in both SNe some nuclear burning continues into the outer ejecta or the newly synthesized elements are mixed into the outer ejecta. The observed spectra of SN 1990N are consistent with a composition of the inner envelope like that of model W7. Intermediate-mass elements with abundances higher than solar are probably in the outer ejecta of both SNe, while silicon, sulfur, and calcium are underabundance in SN 1991T relative to SN 1990N by factors of order 3, 3, and 120, respectively.
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- 1992
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123. ASASSN-15nx: A Luminous Type II Supernova with a “Perfect” Linear Decline
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Bose, Subhash, primary, Dong, Subo, additional, Kochanek, C. S., additional, Pastorello, Andrea, additional, Katz, Boaz, additional, Bersier, David, additional, Andrews, Jennifer E., additional, Prieto, J. L., additional, Stanek, K. Z., additional, Shappee, B. J., additional, Smith, Nathan, additional, Kollmeier, Juna, additional, Benetti, Stefano, additional, Cappellaro, E., additional, Chen, Ping, additional, Elias-Rosa, N., additional, Milne, Peter, additional, Morales-Garoffolo, Antonia, additional, Tartaglia, Leonardo, additional, Tomasella, L., additional, Bilinski, Christopher, additional, Brimacombe, Joseph, additional, Frank, Stephan, additional, Holoien, T. W.-S., additional, Kilpatrick, Charles D., additional, Kiyota, Seiichiro, additional, Madore, Barry F., additional, and Rich, Jeffrey A., additional
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- 2018
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124. The Copernico Telescope testing facility for AO on-sky demonstrations
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Chinellato, Simonetta, primary, Ragazzoni, Roberto, primary, Farinato, Jacopo, primary, Biondi, Federico, primary, Greggio, Davide, primary, Dima, Marco, primary, Bergomi, Maria, primary, Carolo, Elena, primary, Magrin, Demetrio, primary, Marafatto, Luca, primary, Portaluri, Elisa, primary, Umbriaco, Gabriele, primary, Vassallo, Daniele, primary, Viotto, Valentina, primary, Benetti, Stefano, primary, Chiomento, Venerio, primary, Frigo, Aldo, primary, Martorana, Giorgio, primary, Tomasella, Lina, primary, Traverso, Luciano, primary, Fiaschi, M., primary, and Lessio, Luigi, primary
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- 2018
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125. Spectropolarimetry of Galactic stars with anomalous extinction sightlines
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Cikota, Aleksandar, primary, Hoang, Thiem, additional, Taubenberger, Stefan, additional, Patat, Ferdinando, additional, Mazzei, Paola, additional, Cox, Nick L.J., additional, Zelaya, Paula, additional, Cikota, Stefan, additional, Tomasella, Lina, additional, Benetti, Stefano, additional, and Rodeghiero, Gabriele, additional
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- 2018
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126. The Type IIn Supernova SN 2010bt: The Explosion of a Star in Outburst
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Elias-Rosa, Nancy, primary, Van Dyk, Schuyler D., additional, Benetti, Stefano, additional, Cappellaro, Enrico, additional, Smith, Nathan, additional, Kotak, Rubina, additional, Turatto, Massimo, additional, Filippenko, Alexei V., additional, Pignata, Giuliano, additional, Fox, Ori D., additional, Galbany, Lluis, additional, González-Gaitán, Santiago, additional, Miluzio, Matteo, additional, Monard, L. A. G., additional, and Ergon, Mattias, additional
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- 2018
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127. SN 2017dio: A Type-Ic Supernova Exploding in a Hydrogen-rich Circumstellar Medium
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Kuncarayakti, Hanindyo, primary, Maeda, Keiichi, additional, Ashall, Christopher J., additional, Prentice, Simon J., additional, Mattila, Seppo, additional, Kankare, Erkki, additional, Fransson, Claes, additional, Lundqvist, Peter, additional, Pastorello, Andrea, additional, Leloudas, Giorgos, additional, Anderson, Joseph P., additional, Benetti, Stefano, additional, Bersten, Melina C., additional, Cappellaro, Enrico, additional, Cartier, Régis, additional, Denneau, Larry, additional, Della Valle, Massimo, additional, Elias-Rosa, Nancy, additional, Folatelli, Gastón, additional, Fraser, Morgan, additional, Galbany, Lluís, additional, Gall, Christa, additional, Gal-Yam, Avishay, additional, Gutiérrez, Claudia P., additional, Hamanowicz, Aleksandra, additional, Heinze, Ari, additional, Inserra, Cosimo, additional, Kangas, Tuomas, additional, Mazzali, Paolo, additional, Melandri, Andrea, additional, Pignata, Giuliano, additional, Rest, Armin, additional, Reynolds, Thomas, additional, Roy, Rupak, additional, Smartt, Stephen J., additional, Smith, Ken W., additional, Sollerman, Jesper, additional, Somero, Auni, additional, Stalder, Brian, additional, Stritzinger, Maximilian, additional, Taddia, Francesco, additional, Tomasella, Lina, additional, Tonry, John, additional, Weiland, Henry, additional, and Young, David R., additional
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- 2018
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128. Gaia17biu/SN 2017egm in NGC 3191: The Closest Hydrogen-poor Superluminous Supernova to Date Is in a “Normal,” Massive, Metal-rich Spiral Galaxy
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Bose, Subhash, primary, Dong, Subo, additional, Pastorello, A., additional, Filippenko, Alexei V., additional, Kochanek, C. S., additional, Mauerhan, Jon, additional, Romero-Cañizales, C., additional, Brink, Thomas G., additional, Chen, Ping, additional, Prieto, J. L., additional, Post, R., additional, Ashall, Christopher, additional, Grupe, Dirk, additional, Tomasella, L., additional, Benetti, Stefano, additional, Shappee, B. J., additional, Stanek, K. Z., additional, Cai, Zheng, additional, Falco, E., additional, Lundqvist, Peter, additional, Mattila, Seppo, additional, Mutel, Robert, additional, Ochner, Paolo, additional, Pooley, David, additional, Stritzinger, M. D., additional, Villanueva, S., additional, Zheng, WeiKang, additional, Beswick, R. J., additional, Brown, Peter J., additional, Cappellaro, E., additional, Davis, Scott, additional, Fraser, Morgan, additional, Jaeger, Thomas de, additional, Elias-Rosa, N., additional, Gall, C., additional, Gaudi, B. Scott, additional, Herczeg, Gregory J., additional, Hestenes, Julia, additional, Holoien, T. W.-S., additional, Hosseinzadeh, Griffin, additional, Hsiao, E. Y., additional, Hu, Shaoming, additional, Jaejin, Shin, additional, Jeffers, Ben, additional, Koff, R. A., additional, Kumar, Sahana, additional, Kurtenkov, Alexander, additional, Lau, Marie Wingyee, additional, Prentice, Simon, additional, Reynolds, T., additional, Rudy, Richard J., additional, Shahbandeh, Melissa, additional, Somero, Auni, additional, Stassun, Keivan G., additional, Thompson, Todd A., additional, Valenti, Stefano, additional, Woo, Jong-Hak, additional, and Yunus, Sameen, additional
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- 2018
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129. Type Ibn Supernovae Show Photometric Homogeneity and Spectral Diversity at Maximum Light
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Hosseinzadeh, Griffin, Arcavi, Iair, Valenti, Stefano, McCully, Curtis, Howell, D. Andrew, Johansson, Joel, Sollerman, Jesper, Pastorello, Andrea, Benetti, Stefano, Cao, Yi, Cenko, S. Bradley, Clubb, Kelsey I., Corsi, Alessandra, Duggan, Gina, Elias-Rosa, Nancy, Filippenko, Alexei V., Fox, Ori D., Fremling, Christoffer, Horesh, Assaf, Karamehmetoglu, Emir, Kasliwal, Mansi, Marion, G. H., Ofek, Eran, Sand, David, Taddia, Francesco, Zheng, WeiKang, Fraser, Morgan, Gal-Yam, Avishay, Inserra, Cosimo, Laher, Russ, Masci, Frank, Rebbapragada, Umaa, Smartt, Stephen, Smith, Ken W., Sullivan, Mark, Surace, Jason, Woźniak, Przemek, Hosseinzadeh, Griffin, Arcavi, Iair, Valenti, Stefano, McCully, Curtis, Howell, D. Andrew, Johansson, Joel, Sollerman, Jesper, Pastorello, Andrea, Benetti, Stefano, Cao, Yi, Cenko, S. Bradley, Clubb, Kelsey I., Corsi, Alessandra, Duggan, Gina, Elias-Rosa, Nancy, Filippenko, Alexei V., Fox, Ori D., Fremling, Christoffer, Horesh, Assaf, Karamehmetoglu, Emir, Kasliwal, Mansi, Marion, G. H., Ofek, Eran, Sand, David, Taddia, Francesco, Zheng, WeiKang, Fraser, Morgan, Gal-Yam, Avishay, Inserra, Cosimo, Laher, Russ, Masci, Frank, Rebbapragada, Umaa, Smartt, Stephen, Smith, Ken W., Sullivan, Mark, Surace, Jason, and Woźniak, Przemek
- Abstract
Type Ibn supernovae (SNe) are a small yet intriguing class of explosions whose spectra are characterized by low-velocity helium emission lines with little to no evidence for hydrogen. The prevailing theory has been that these are the core-collapse explosions of very massive stars embedded in helium-rich circumstellar material (CSM). We report optical observations of six new SNe Ibn: PTF11rfh, PTF12ldy, iPTF14aki, iPTF15ul, SN 2015G, and iPTF15akq. This brings the sample size of such objects in the literature to 22. We also report new data, including a near-infrared spectrum, on the Type Ibn SN 2015U. In order to characterize the class as a whole, we analyze the photometric and spectroscopic properties of the full Type Ibn sample. We find that, despite the expectation that CSM interaction would generate a heterogeneous set of light curves, as seen in SNe IIn, most Type Ibn light curves are quite similar in shape, declining at rates around 0.1 mag day(-1) during the first month after maximum light, with a few significant exceptions. Early spectra of SNe Ibn come in at least two varieties, one that shows narrow P Cygni lines and another dominated by broader emission lines, both around maximum light, which may be an indication of differences in the state of the progenitor system at the time of explosion. Alternatively, the spectral diversity could arise from viewing-angle effects or merely from a lack of early spectroscopic coverage. Together, the relative light curve homogeneity and narrow spectral features suggest that the CSM consists of a spatially confined shell of helium surrounded by a less dense extended wind.
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- 2017
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130. Erratum: On the diversity of superluminous supernovae: ejected mass as the dominant factor
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Nicholl, M., Smartt, S. J., Jerkstrand, A., Inserra, C., Sim, S. A., Chen, T. -W., BENETTI, Stefano, Fraser, M., Gal-Yam, A., Kankare, E., Maguire, K., Smith, K., Sullivan, M., Valenti, S., Young, D. R., Baltay, C., Bauer, F. E., Baumont, S., Bersier, D., BOTTICELLA, MARIA TERESA, Childress, M., Dennefeld, M., DELLA VALLE, Massimo, ELIAS DE LA ROSA, NANCY DEL CARMEN, Feindt, U., Galbany, L., Hadjiyska, E., Le Guillou, L., Leloudas, G., Mazzali, P., McKinnon, R., Polshaw, J., Rabinowitz, D., Rostami, S., Scalzo, R., Schmidt, B. P., Schulze, S., Sollerman, J., Taddia, F., and Yuan, F.
- Abstract
This is an erratum to the paper ‘On the diversity of superluminous supernovae: ejected mass as the dominant factor’, published in MNRAS, 2015, 452.\ud\udWe have noticed that some of the supernova peak magnitudes in Table 1 are given in the wrong rows. The error affected the rows ‘PS1-11ap’ to ‘PS1-10ky’, with each magnitude displaced downwards by one cell. The nature of this error is purely typographic. Originally, the objects were grouped into high- and low-redshift bins, rather than by wavelength coverage; the error occurred when moving PS1-11ap from the high-z group into the ‘Gold’ coverage group. This does not affect any of the other tables, figures, or analysis in the paper.
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- 2016
131. Distretto della pesca e filiera ittica: un parallelo con riferimento all’Alto Adriatico
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Benetti, Stefano
- Abstract
The topic of this thesis was inspired by the question “Can the fishing industry in the province of Ferrara become a district?”, asked by Massimo Buriani in an article published in the 2012 edition of the Socioeconomic Annual Report of Ferrara. Considering the importance of the contribution given by fishing economy to the productivity growth of this country, this work’s main objective is to clarify the differences and analogies between the fishing district and the small- and large-sized fishing industry; moreover, to which extent the notion of “district” can be adapted to the economic reality of the High-Adriatic District, particularly considering the case of Ferrara. Finally, the topic deals with important current issues of European interest related to environmental protection zones fish - district considered: the Marine Strategy , the European Fisheries Fund and the Group of Coastal Action ., Argomenti, N° 2 (2015): settembre - dicembre
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- 2015
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132. Type Ibn Supernovae Show Photometric Homogeneity and Spectral Diversity at Maximum Light
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Hosseinzadeh, Griffin, primary, Arcavi, Iair, additional, Valenti, Stefano, additional, McCully, Curtis, additional, Howell, D. Andrew, additional, Johansson, Joel, additional, Sollerman, Jesper, additional, Pastorello, Andrea, additional, Benetti, Stefano, additional, Cao, Yi, additional, Cenko, S. Bradley, additional, Clubb, Kelsey I., additional, Corsi, Alessandra, additional, Duggan, Gina, additional, Elias-Rosa, Nancy, additional, Filippenko, Alexei V., additional, Fox, Ori D., additional, Fremling, Christoffer, additional, Horesh, Assaf, additional, Karamehmetoglu, Emir, additional, Kasliwal, Mansi, additional, Marion, G. H., additional, Ofek, Eran, additional, Sand, David, additional, Taddia, Francesco, additional, Zheng, WeiKang, additional, Fraser, Morgan, additional, Gal-Yam, Avishay, additional, Inserra, Cosimo, additional, Laher, Russ, additional, Masci, Frank, additional, Rebbapragada, Umaa, additional, Smartt, Stephen, additional, Smith, Ken W., additional, Sullivan, Mark, additional, Surace, Jason, additional, and Woźniak, Przemek, additional
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- 2017
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133. A testing facility for AO on-sky demonstrations at the Copernico’s Telescope within the ADONI framework
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Chinellato, Simonetta, primary, Ragazzoni, Roberto, additional, Farinato, Jacopo, additional, Greggio, Davide, additional, Dima, Marco, additional, Biondi, Federico, additional, Benetti, Stefano, additional, Bergomi, Maria, additional, Cappellaro, Enrico, additional, Carolo, Elena, additional, Chiomento, Venerio, additional, Frigo, Aldo, additional, Lessio, Luigi, additional, Magrin, Demetrio, additional, Marafatto, Luca, additional, Martorana, Giorgio, additional, Portaluri, Elisa, additional, Rebeschini, Mauro, additional, Tomasella, Lina, additional, Traverso, Luciano, additional, Turatto, Massimo, additional, Umbriaco, Gabriele, additional, Vassallo, Daniele, additional, and Viotto, Valentina, additional
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- 2017
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134. LIGO/Virgo G194575: INAF-TNG/Asiago Telescope follow-up of iPTF15dld
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TOMASELLA, Lina, CAPPELLARO, Enrico, D'AVANZO, Paolo, PIRANOMONTE, Silvia, Branchesi, M., CAMPANA, Sergio, BENETTI, Stefano, BROCATO, Enzo, ANTONELLI, Lucio Angelo, Astone, P., COVINO, Stefano, D'Elia, V., GETMAN, FEDOR, Giuffrida, G., GRADO, ANIELLO, Greco, G., Limatola, L., Lisi, M., Marinoni, S., MARRESE, Paola Maria, MELANDRI, Andrea, NICASTRO, LUCIANO, PALAZZI, ELIANA, PIAN, Elena, PULONE, Luigi, Ricci, F., Stratta, G., TAGLIAFERRI, Gianpiero, TESTA, Vincenzo, Boschin, W., Carosati, D., and Di Fabrizio, L.
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- 2015
135. The spectacular evolution of Supernova 1996al over 15 years: a low energy explosion of a stripped massive star in a highly structured environment
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Caldwell, N., Tomasella, L., Pignata, G., Neuhäuser, R., Cupani, G., Turatto, M., Pastorello, A., Patat, F., Cappellaro, E., Utrobin, V., Chugai, N., Benetti, S., Tomasella, Lina, Pignata, Giuliano, Caldwell, Nelson, Neuhauser, Ralph, Cupani, Guido, Turatto, Massimo, Pastorello, Andrea, Patat, Ferdinando, Cappellaro, Enrico, Utrobin, Victor, Chugai, Nikolai, and Benetti, Stefano
- Subjects
Physics ,010308 nuclear & particles physics ,Astronomy ,Balmer series ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Spectral line ,Photometry (optics) ,symbols.namesake ,Supernova ,Low energy ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,symbols ,Ejecta ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Spectrophotometry of SN 1996al carried out throughout 15 years is presented. The early photometry suggests that SN 1996al is a Linear type-II supernova, with an absolute peak of Mv ~ -18.2 mag. Early spectra present broad, asymmetric Balmer emissions, with super-imposed narrow lines with P-Cygni profile, and He I features with asymmetric, broad emission components. The analysis of the line profiles shows that the H and He broad components form in the same region of the ejecta. By day +142, the Halpha profile dramatically changes: the narrow P-Cygni profile disappears, and the Halpha is fitted by three emission components, that will be detected over the remaining 15 yrs of the SN monitoring campaign. Instead, the He I emissions become progressively narrower and symmetric. A sudden increase in flux of all He I lines is observed between 300 and 600 days. Models show that the supernova luminosity is sustained by the interaction of low mass (~1.15 Msun) ejecta, expelled in a low kinetic energy (~ 1.6 x 10^50 erg) explosion, with highly asymmetric circumstellar medium. The detection of Halpha emission in pre-explosion archive images suggests that the progenitor was most likely a massive star (~25 Msun ZAMS) that had lost a large fraction of its hydrogen envelope before explosion, and was hence embedded in a H-rich cocoon. The low-mass ejecta and modest kinetic energy of the explosion are explained with massive fallback of material into the compact remnant, a 7-8 Msun black hole., Comment: 27 pages, 23 figures, Accepted for publication in MNRAS
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- 2015
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136. A testing facility at the Asiago Copernico telescope in the framework of the ADaptive Optics National laboratory of Italy: ADONI
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Chinellato, Simonetta, additional, Ragazzoni, Roberto, additional, Farinato, Jacopo, additional, Greggio, Davide, additional, Benetti, Stefano, additional, Bergomi, Maria, additional, Biondi, Federico, additional, Cappellaro, Enrico, additional, Carolo, Elena, additional, Chiomento, Venerio, additional, Dima, Marco, additional, Frigo, Aldo, additional, Gullieuszik, Marco, additional, Lessio, Luigi, additional, Magrin, Demetrio, additional, Marafatto, Luca, additional, Martorana, Giorgio, additional, Portaluri, Elisa, additional, Rebeschini, Mauro, additional, Tomasella, Lina, additional, Traverso, Luciano, additional, Turatto, Massimo, additional, Vassallo, Daniele, additional, and Viotto, Valentina, additional
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- 2016
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137. SN 2012ec: Mass of the progenitor from PESSTO follow-up of the photospheric phase
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Barbarino, C, Dall'Ora, Massimo, Botticella, M T, Della Valle, M, Zampieri, L, Maund, J. R., Pumo, M.L., Jerkstrand, Anders, Benetti, Stefano, Elias-Rosa (Elias de la Rosa), Nancy, Fraser, M, Gal-Yam, Avishay, Hamuy, M., Inserra, Cosimo, Knapic, C., LaCluyze, A. P., Molinaro, M., Ochner, P., Pastorello, A., Pignata, G., Reichart, D E, Ries, C., Riffeser, A, Schmidt, M., Smareglia, R., Smartt, Stephen J., Smith, K, Sollerman, J., Sullivan, M, Tomasella, L, Turatto, Massimo, Valenti, S, Yaron, Ofer, Young , D, Barbarino, C, Dall'Ora, Massimo, Botticella, M T, Della Valle, M, Zampieri, L, Maund, J. R., Pumo, M.L., Jerkstrand, Anders, Benetti, Stefano, Elias-Rosa (Elias de la Rosa), Nancy, Fraser, M, Gal-Yam, Avishay, Hamuy, M., Inserra, Cosimo, Knapic, C., LaCluyze, A. P., Molinaro, M., Ochner, P., Pastorello, A., Pignata, G., Reichart, D E, Ries, C., Riffeser, A, Schmidt, M., Smareglia, R., Smartt, Stephen J., Smith, K, Sollerman, J., Sullivan, M, Tomasella, L, Turatto, Massimo, Valenti, S, Yaron, Ofer, and Young , D
- Abstract
We present the results of a photometric and spectroscopic monitoring campaign of SN 2012ec, which exploded in the spiral galaxy NGC 1084, during the photospheric phase. The photometric light curve exhibits a plateau with luminosity L = 0.9 × 1042 erg s−1 and duration ∼90 d, which is somewhat shorter than standard Type II-P supernovae (SNe). We estimate the nickel mass M(56Ni) = 0.040 ± 0.015 M from the luminosity at the beginning of the radioactive tail of the light curve. The explosion parameters of SN 2012ec were estimated from the comparison of the bolometric light curve and the observed temperature and velocity evolution of the ejecta with predictions from hydrodynamical models. We derived an envelope mass of 12.6 M, an initial progenitor radius of 1.6 × 1013 cm and an explosion energy of 1.2 foe. These estimates agree with an independent study of the progenitor star identified in pre-explosion images, for which an initial mass of M = 14−22 M was determined. We have applied the same analysis to two other Type II-P SNe (SNe 2012aw and 2012A), and carried out a comparison with the properties of SN 2012ec derived in this paper. We find a reasonable agreement between the masses of the progenitors obtained from pre-explosion images and masses derived from hydrodynamical models. We estimate the distance to SN 2012ec with the standardized candle method (SCM) and compare it with other estimates based on other primary and secondary indicators. SNe 2012A, 2012aw and 2012ec all follow the standard relations for the SCM for the use of Type II-P SNe as distance indicators.
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- 2015
138. SN 2009ip �� la PESSTO: No evidence for core-collapse yet
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Fraser, Morgan, Inserra, Cosimo, Jerkstrand, Anders, Kotak, Rubina, Pignata, Giuliano, Benetti, Stefano, Botticella, Maria-Teresa, Bufano, Filomena, Childress, Michael, Mattila, Seppo, Pastorello, Andrea, Smartt, Stephen J., Turatto, Massimo, Yuan, Fang, Anderson, Joe P., Bayliss, Daniel D. R., Bauer, Franz Erik, Chen, Ting-Wan, Bur��n, Francisco F��rster, Gal-Yam, Avishay, Haislip, Joshua B., Knapic, Cristina, Guillou, Laurent Le, Marchi, Sebasti��n, Mazzali, Paolo, Molinaro, Marco, Moore, Justin P., Reichart, Daniel, Smareglia, Riccardo, Smith, Ken W., Sternberg, Assaf, Sullivan, Mark, Tak��ts, Katalin, Tucker, Brad E., Valenti, Stefano, Yaron, Ofer, Young, David R., and Zhou, George
- Subjects
FOS: Physical sciences ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We present observations of the interacting transient SN 2009ip, from the start of the outburst in October 2012 until the end of the 2012 observing season. The transient reached a peak of $M_V$=-17.7 mag before fading rapidly, with a total integrated luminosity of 1.9$\times10^{49}$ erg over the period of August-December 2012. The optical and near infrared spectra are dominated by narrow emission lines, signaling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities between 0.5-1.2$\times10^4$ km s$^{-1}$\. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudo-nebular spectra. We set a limit of $, 28 pages, submitted to MNRAS. Abstract abridged for arXiv
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- 2013
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139. Effects of the explosion asymmetry and viewing angle on the type ia supernova colour and luminosity calibration
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Maeda, Keiichi, Leloudas, Giorgos, Taubenberger, Stefan, Stritzinger, Maximilian, Sollerman, Jesper, Elias-Rosa, Nancy, Benetti, Stefano, Hamuy-Wackenhut, Mario, Folatelli, Gaston, and Mazzali, Paolo A.
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- 2011
140. SN 2009ip at late times – an interacting transient at +2 years
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Fraser, Morgan, primary, Kotak, Rubina, additional, Pastorello, Andrea, additional, Jerkstrand, Anders, additional, Smartt, Stephen J., additional, Chen, Ting-Wan, additional, Childress, Michael, additional, Gilmore, Gerard, additional, Inserra, Cosimo, additional, Kankare, Erkki, additional, Margheim, Steve, additional, Mattila, Seppo, additional, Valenti, Stefano, additional, Ashall, Christopher, additional, Benetti, Stefano, additional, Botticella, Maria Teresa, additional, Bauer, Franz Erik, additional, Campbell, Heather, additional, Elias-Rosa, Nancy, additional, Fleury, Mathilde, additional, Gal-Yam, Avishay, additional, Hachinger, Stephan, additional, Howell, D. Andrew, additional, Le Guillou, Laurent, additional, Léget, Pierre-François, additional, Morales-Garoffolo, Antonia, additional, Polshaw, Joe, additional, Spiro, Susanna, additional, Sullivan, Mark, additional, Taubenberger, Stefan, additional, Turatto, Massimo, additional, Walker, Emma S., additional, Young, David R., additional, and Zhang, Bonnie, additional
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- 2015
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141. High-density circumstellar interaction in the luminous type IIn SN 2010jl : The first 1100 days
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Fransson, Claes, Ergon, Mattias, Challis, Peter J., Chevalier, Roger A., France, Kevin, Kirshner, Robert P., Marion, G. H., Milisavljevic, Dan, Smith, Nathan, Bufano, Filomena, Friedman, Andrew S., Kangas, Tuomas, Larsson, Josefin, Mattila, Seppo, Benetti, Stefano, Chornock, Ryan, Czekala, Ian, Soderberg, Alicia, Sollerman, Jesper, Fransson, Claes, Ergon, Mattias, Challis, Peter J., Chevalier, Roger A., France, Kevin, Kirshner, Robert P., Marion, G. H., Milisavljevic, Dan, Smith, Nathan, Bufano, Filomena, Friedman, Andrew S., Kangas, Tuomas, Larsson, Josefin, Mattila, Seppo, Benetti, Stefano, Chornock, Ryan, Czekala, Ian, Soderberg, Alicia, and Sollerman, Jesper
- Abstract
Hubble Space Telescope and ground-based observations of the Type IIn supernova (SN) 2010jl are analyzed, including photometry and spectroscopy in the ultraviolet, optical, and near-IR bands, 26-1128 days after first detection. At maximum, the bolometric luminosity was similar to 3 x 10(43) erg s(-1) and even at 850 days exceeds 10(42) erg s(-1). A near-IR excess, dominating after 400 days, probably originates in dust in the circumstellar medium (CSM). The total radiated energy is greater than or similar to 6.5x10(50) erg, excluding the dust component. The spectral lines can be separated into one broad component that is due to electron scattering and one narrow with expansion velocity similar to 100 km s(-1) from the CSM. The broad component is initially symmetric around zero velocity but becomes blueshifted after similar to 50 days, while remaining symmetric about a shifted centroid velocity. Dust absorption in the ejecta is unlikely to explain the line shifts, and we attribute the shift instead to acceleration by the SN radiation. From the optical lines and the X-ray and dust properties, there is strong evidence for large-scale asymmetries in the CSM. The ultraviolet lines indicate CNO processing in the progenitor, while the optical shows a number of narrow coronal lines excited by the X-rays. The bolometric light curve is consistent with a radiative shock in an r(-2) CSM with a mass-loss rate of M similar to 0.1 M(circle dot)yr(-1). The total mass lost is greater than or similar to 3 M-circle dot. These properties are consistent with the SN expanding into a CSM characteristic of a luminous blue variable progenitor with a bipolar geometry. The apparent absence of nuclear processing is attributed to a CSM that is still opaque to electron scattering., QC 20150304
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- 2014
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142. Abundance stratification in Type Ia Supernovae - IV: the luminous, peculiar SN 1991T
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Sasdelli, Michele, Mazzali, Paolo A., Pian, Elena, Nomoto, Ken'ichi, Hachinger, Stephan, Cappellaro, Enrico, Benetti, Stefano, Sasdelli, Michele, Mazzali, Paolo A., Pian, Elena, Nomoto, Ken'ichi, Hachinger, Stephan, Cappellaro, Enrico, and Benetti, Stefano
- Abstract
The abundance distribution of the elements in the ejecta of the peculiar, luminous Type Ia supernova (SN Ia) 1991T is obtained modelling spectra from before maximum light until a year after the explosion, with the method of "Abundance Tomography". SN 1991T is different from other slowly declining SNe Ia (e.g. SN 1999ee) in having a weaker Si II 6355 line and strong features of iron group elements before maximum. The distance to the SN is investigated along with the abundances and the density profile. The ionization transition that happens around maximum sets a strict upper limit on the luminosity. Both W7 and the WDD3 delayed detonation model are tested. WDD3 is found to provide marginally better fits. In this model the core of the ejecta is dominated by stable Fe with a mass of about 0.15 solar masses, as in most SNe Ia. The layer above is mainly 56Ni up to v~10000 km/s (~0.78 solar masses). A significant amount of 56Ni (~3 %) is located in the outer layers. A narrow layer between 10000 km/s and ~12000 km/s is dominated by intermediate mass elements (IME), ~0.18 solar masses. This is small for a SN Ia. The high luminosity and the consequently high ionization, and the high 56Ni abundance at high velocities explain the peculiar early-time spectra of SN 1991T. The outer part is mainly of oxygen, ~0.3 solar masses. Carbon lines are never detected, yielding an upper limit of 0.01 solar masses for C. The abundances obtained with the W7 density model are qualitatively similar to those of the WDD3 model. Different elements are stratified with moderate mixing, resembling a delayed detonation., Comment: 19 pages, 9 figures, 4 tables, accepted for publication in MNRAS
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- 2014
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143. PESSTO monitoring of SN 2012hn: Further heterogeneity among faint type I supernovae
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Valenti, S, Yuan, Fang, Taubenberger, Stefano, Maguire, K., Pastorello, A, Benetti, Stefano, Smartt, Stephen J., Cappellaro, Enrico, Howell, D. A., Bildsten, Lars, Scalzo, Richard, Moore, K., Benitez-Herrera, S, Valenti, S, Yuan, Fang, Taubenberger, Stefano, Maguire, K., Pastorello, A, Benetti, Stefano, Smartt, Stephen J., Cappellaro, Enrico, Howell, D. A., Bildsten, Lars, Scalzo, Richard, Moore, K., and Benitez-Herrera, S
- Abstract
We present optical and infrared monitoring data of SN2012hn collected by the Public European Southern Observatory Spectroscopic Survey for Transient Objects. We show that SN 2012hn has a faint peak magnitude (MR ~ -15.65) and shows no hydrogen and no clea
- Published
- 2014
144. SN2012ca: A stripped envelope core-collapse SN interacting with dense circumstellar medium
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Inserra, Cosimo, Smartt, Stephen J., Scalzo, Richard, Fraser, Morgan, Pastorello, A, Childress, Michael, Pignata, G., Jerkstrand, Anders, Kotak, Rubina, Benetti, Stefano, Della Valle, M, Gal-Yam, Avishay, Mazzali, Paolo A, Smith, K, Sullivan, M, Valenti, S, Yaron, Ofer, Young , D, Reichart, D E, Inserra, Cosimo, Smartt, Stephen J., Scalzo, Richard, Fraser, Morgan, Pastorello, A, Childress, Michael, Pignata, G., Jerkstrand, Anders, Kotak, Rubina, Benetti, Stefano, Della Valle, M, Gal-Yam, Avishay, Mazzali, Paolo A, Smith, K, Sullivan, M, Valenti, S, Yaron, Ofer, Young , D, and Reichart, D E
- Abstract
We report optical and near-infrared observations of SN2012ca with the Public ESO Spectroscopy Survey of Transient Objects (PESSTO), spread over one year since discovery. The supernova (SN) bears many similarities to SN1997cy and to other events classified
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- 2014
145. On the progenitor of the type IIP SN 2013ej in M74
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Fraser, Morgan, Maund, Justyn, Smartt, Stephen J., Kotak, Rubina, Lawrence, Andy, Bruce, Alistair, Valenti, Stefano, Yuan, Fang, Benetti, Stefano, Chen, Ting-Wan, Gal-Yam, Avishay, Inserra, Cosimo, Young , D, Fraser, Morgan, Maund, Justyn, Smartt, Stephen J., Kotak, Rubina, Lawrence, Andy, Bruce, Alistair, Valenti, Stefano, Yuan, Fang, Benetti, Stefano, Chen, Ting-Wan, Gal-Yam, Avishay, Inserra, Cosimo, and Young , D
- Abstract
We use natural seeing imaging of SN 2013ej in M74 to identify a progenitor candidate in archival Hubble Space Telescope (HST) + Advanced Camera for Survey images. We find a source coincident with the supernova (SN) in the F814W filter within the total 75
- Published
- 2014
146. HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS
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Fransson, Claes, primary, Ergon, Mattias, additional, Challis, Peter J., additional, Chevalier, Roger A., additional, France, Kevin, additional, Kirshner, Robert P., additional, Marion, G. H., additional, Milisavljevic, Dan, additional, Smith, Nathan, additional, Bufano, Filomena, additional, Friedman, Andrew S., additional, Kangas, Tuomas, additional, Larsson, Josefin, additional, Mattila, Seppo, additional, Benetti, Stefano, additional, Chornock, Ryan, additional, Czekala, Ian, additional, Soderberg, Alicia, additional, and Sollerman, Jesper, additional
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- 2014
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147. Peculiar, Low Luminosity Type II Supernovae: Site of Black Hole Formation?
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Zampieri, Luca, primary, Pastorello, Andrea, additional, Turatto, Massimo, additional, Cappellaro, Enrico, additional, Benetti, Stefano, additional, Altavilla, Giuseppe, additional, Mazzali, Paolo, additional, and Hamuy, Mario, additional
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148. Variety in Supernovae
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Turatto, Massimo, primary, Benetti, Stefano, additional, and Cappellaro, Enrico, additional
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149. Faint Core-Collapse Supernovae
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Pastorello, Andrea, primary, Baron, Eddie, additional, Benetti, Stefano, additional, Branch, David, additional, Cappellaro, Enrico, additional, Patat, Ferdinando, additional, Turatto, Massimo, additional, Zampieri, Luca, additional, Hamuy, Mario, additional, Armstrong, Mark, additional, and Meikle, Peter, additional
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150. An Intermediate Redshift Supernova Search at ESO: Reduction Tools and Efficiency Tests
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Riello, Marco, primary, Altavilla, Giuseppe, additional, Cappellaro, Enrico, additional, Benetti, Stefano, additional, Pastorello, Andrea, additional, Patat, Ferdinando, additional, Prevedello, Marco, additional, Turatto, Massimo, additional, and Zampieri, Luca, additional
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