Hintze Centre for Astrophysical Surveys

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KiDSlens: Gotta Catch’em All

VST in the Era of the Large Sky Surveys (2018) 13-13

Authors:

Chiara Spiniello, Nicola Napolitano, Fedor Getman, Marilena Spavone, MA Raj, Giuseppe D’Ago, Massimo Capaccioli, Adriano Agnello, A Sergeyev, Crescenzo Tortora, E Petrillo, Elena Bannikova, KIDS Collaboration
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Radio-loudness in black hole transients: evidence for an inclination effect

(2018)

Authors:

SE Motta, P Casella, R Fender
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Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations

(2018)

Authors:

Michael W Coughlin, Tim Dietrich, Zoheyr Doctor, Daniel Kasen, Scott Coughlin, Anders Jerkstrand, Giorgos Leloudas, Owen McBrien, Brian D Metzger, Richard O'Shaughnessy, Stephen J Smartt
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HST grism confirmation of 16 structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) survey

Astrophysical Journal Institute of Physics 859:1 (2018) 38

Authors:

G Noirot, D Stern, S Mei, D Wylezalek, EA Cooke, C De Breuck, A Galametz, NA Hatch, J Vernet, M Brodwin, P Eisenhardt, AH Gonzalez, Matthew Jarvis, A Rettura, N Seymour

Abstract:

We report spectroscopic results from our 40-orbit Hubble Space Telescope slitless grism spectroscopy program observing the 20 densest Clusters Around Radio-Loud AGN (CARLA) candidate galaxy clusters at 1.4 1.4.
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SN 2015as: a low-luminosity Type IIb supernova without an early light-curve peak

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 476:3 (2018) 3611-3630

Authors:

Anjasha Gangopadhyay, Kuntal Misra, A Pastorello, DK Sahu, L Tomasella, L Tartaglia, Mridweeka Singh, Raya Dastidar, S Srivastav, P Ochner, Peter J Brown, GC Anupama, S Benetti, E Cappellaro, Brajesh Kumar, Brijesh Kumar, SB Pandey

Abstract:

AbstractWe present results of the photometric (from 3 to 509 d post-explosion) and spectroscopic (up to 230 d post-explosion) monitoring campaign of the He-rich Type IIb supernova (SN) 2015as. The (B − V) colour evolution of SN 2015as closely resemble those of SN 2008ax, suggesting that SN 2015as belongs to the SN IIb subgroup that does not show the early, short-duration photometric peak. The light curve of SN 2015as reaches the B-band maximum about 22 d after the explosion, at an absolute magnitude of −16.82 ± 0.18 mag. At ∼75 d after the explosion, its spectrum transitions from that of a SN II to a SN Ib. P Cygni features due to He i lines appear at around 30 d after explosion, indicating that the progenitor of SN 2015as was partially stripped. For SN 2015as, we estimate a 56Ni mass of ∼0.08 M⊙ and ejecta mass of 1.1–2.2 M⊙, which are similar to the values inferred for SN 2008ax. The quasi-bolometric analytical light-curve modelling suggests that the progenitor of SN 2015as has a modest mass (∼0.1 M⊙), a nearly compact (∼0.05 × 1013 cm) H envelope on top of a dense, compact (∼2 × 1011 cm) and a more massive (∼1.2 M⊙) He core. The analysis of the nebular phase spectra indicates that ∼0.44 M⊙ of O is ejected in the explosion. The intensity ratio of the [Ca ii]/[O i] nebular lines favours either a main-sequence progenitor mass of ∼15 M⊙ or a Wolf–Rayet star of 20 M⊙.
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