Hintze Centre for Astrophysical Surveys

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MIGHTEE: are giant radio galaxies more common than we thought?

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 501:3 (2021) 3833-3845

Authors:

J Delhaize, I Heywood, M Prescott, Mj Jarvis, I Delvecchio, Ih Whittam, Sv White, Mj Hardcastle, Cl Hale, J Afonso, Y Ao, M Brienza, M Brueggen, Jd Collier, E Daddi, M Glowacki, N Maddox, Lk Morabito, I Prandoni, Z Randriamanakoto, S Sekhar, Fangxia An, Nj Adams, S Blyth, Raa Bowler, L Leeuw, L Marchetti, Sm Randriamampandry, K Thorat, N Seymour, O Smirnov, Ar Taylor, C Tasse, M Vaccari
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The Fast-evolving Type Ib Supernova SN 2015dj in NGC 7371

The Astrophysical Journal American Astronomical Society 909:2 (2021) 100-100

Authors:

Mridweeka Singh, Kuntal Misra, Stefano Valenti, Griffin Hosseinzadeh, Andrea Pastorello, Shubham Srivastav, Anjasha Gangopadhyay, Raya Dastidar, Lina Tomasella, Iair Arcavi, Stefano Benetti, Emma Callis, Enrico Cappellaro, Nancy Elias-Rosa, D Andrew Howell, Sang Chul Kim, Curtis McCully, Leonardo Tartaglia, Giacomo Terreran, Massimo Turatto

Abstract:

Abstract We present the detailed optical evolution of a Type Ib SN 2015dj in NGC 7371, using data spanning up to ∼170 days after discovery. SN 2015dj shares similarity in light-curve shape with SN 2007gr and peaks at M V = −17.37 ± 0.02 mag. Analytical modeling of the quasi bolometric light curve yields 0.06 ± 0.01 M ⊙ of 56Ni, ejecta mass M ⊙, and kinetic energy erg. The spectral features show a fast evolution and resemble those of spherically symmetric ejecta. The analysis of nebular phase spectral lines indicates a progenitor mass between 13–20 M ⊙, suggesting a binary scenario.
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Forbidden hugs in pandemic times

Astronomy & Astrophysics EDP Sciences 647 (2021) a93

Authors:

A Pastorello, G Valerin, M Fraser, N Elias-Rosa, S Valenti, A Reguitti, PA Mazzali, RC Amaro, JE Andrews, Y Dong, J Jencson, M Lundquist, DE Reichart, DJ Sand, S Wyatt, SJ Smartt, KW Smith, S Srivastav, Y-Z Cai, E Cappellaro, S Holmbo, A Fiore, D Jones, E Kankare, E Karamehmetoglu, P Lundqvist, A Morales-Garoffolo, TM Reynolds, MD Stritzinger, SC Williams, KC Chambers, TJL de Boer, ME Huber, A Rest, R Wainscoat
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The Fornax3D project: Assembly histories of lenticular galaxies from a combined dynamical and population orbital analysis

Astronomy & Astrophysics EDP Sciences 647 (2021) a145

Authors:

A Poci, RM McDermid, M Lyubenova, L Zhu, G van de Ven, E Iodice, L Coccato, F Pinna, EM Corsini, J Falcón-Barroso, DA Gadotti, RJJ Grand, K Fahrion, I Martín-Navarro, M Sarzi, S Viaene, PT de Zeeuw
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GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3-2.2 mu m extragalactic background light

Monthly Notices of the Royal Astronomical Society Royal Astronomical Society 503:2 (2021) 2033-2052

Authors:

Soheil Koushan, Simon P Driver, Sabine Bellstedt, Luke J Davies, Aaron SG Robotham, Claudia del P Lagos, Abdolhosein Hashemizadeh, Danail Obreschkow, Jessica E Thorne, Malcolm Bremer, Bw Holwerda, Matt J Jarvis, Andrew M Hopkins, Malgorzata Siudek, Rogier A Windhorst

Abstract:

We present a revised measurement of the optical extragalactic background light (EBL), based on the contribution of resolved galaxies to the integrated galaxy light (IGL). The cosmic optical background radiation (COB), encodes the light generated by star formation, and provides a wealth of information about the cosmic star formation history (CSFH). We combine wide and deep galaxy number counts from the Galaxy And Mass Assembly survey (GAMA) and Deep Extragalactic VIsible Legacy Survey (DEVILS), along with the Hubble Space Telescope (HST) archive and other deep survey data sets, in nine multiwavelength filters to measure the COB in the range from 0.35  μm to 2.2  μm. We derive the luminosity density in each band independently and show good agreement with recent and complementary estimates of the optical-EBL from very high-energy (VHE) experiments. Our error analysis suggests that the IGL and γ-ray measurements are now fully consistent to within ∼10 per cent⁠, suggesting little need for any additional source of diffuse light beyond the known galaxy population. We use our revised IGL measurements to constrain the CSFH, and place amplitude constraints on a number of recent estimates. As a consistency check, we can now demonstrate convincingly, that the CSFH, stellar mass growth, and the optical-EBL provide a fully consistent picture of galaxy evolution. We conclude that the peak of star formation rate lies in the range 0.066–0.076 M⊙ yr−1 Mpc−3 at a lookback time of 9.1 to 10.9 Gyr.
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