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|Title:||The host galaxy and late-time evolution of the superluminous supernova PTF12dam||Authors:||Chen, T. -W.
Smartt, S. J.
ELIAS DE LA ROSA, NANCY DEL CARMEN
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||452||Issue:||2||First Page:||1567||Abstract:||Superluminous supernovae (SLSNe) of Type Ic have a tendency to occur in faint host galaxies which are likely to have low mass and low metallicity. PTF12dam is one of the closest and best-studied superluminous explosions that has a broad and slowly fading light curve similar to SN 2007bi. Here we present new photometry and spectroscopy for PTF12dam from 200-500 d (rest frame) after peak and a detailed analysis of the host galaxy (SDSS J142446.21+461348.6 at z = 0.107). Using deep templates and image subtraction we show that the light curve can be fit with a magnetar model if escape of high-energy gamma rays is taken into account. The full bolometric light curve from -53 to +399 d (with respect to peak) cannot be fit satisfactorily with the pair-instability models. An alternative model of interaction with a dense circumstellar material (CSM) produces a good fit to the data although this requires a very large mass (̃13 M<SUB>☉</SUB>) of hydrogen-free CSM. The host galaxy is a compact dwarf (physical size ̃1.9 kpc) and with M<SUB>g</SUB> = -19.33 ± 0.10, it is the brightest nearby SLSN Ic host discovered so far. The host is a low-mass system (2.8 × 10<SUP>8</SUP> M<SUB>☉</SUB>) with a star formation rate (5.0 M<SUB>☉</SUB> yr<SUP>-1</SUP>), which implies a very high specific star formation rate (17.9 Gyr<SUP>-1</SUP>). The remarkably strong nebular emission provide detections of the [O III] λ4363 and [O II] λλ7320, 7330auroral lines and an accurate oxygen abundance of 12 + log (O/H) = 8.05 ± 0.09. We show here that they are at the extreme end of the metallicity distribution of dwarf galaxies and propose that low metallicity is a requirement to produce these rare and peculiar SNe.||Acknowledgments:||The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no.  (PI: S. J. Smartt). T-WC thanks Daniel Kasen for the PISN models, and expresses appreciation for Yen-Chen Pan, Kai-Lung Sun, Meng-Chun Tsai, Chorng-Yuan Hwang, Max Pettini, Mark Sullivan, Gary J. Ferland, Edward Schlafly and David R. Young for their useful advice. After the submission to the archive, this article has benefited greatly from the helpful feedback from the referee and Giorgos Leloudas, Avishay Gal-Yam, Alan Fitzsimmons, Michel Dennefeld and Paul Vreeswijk. RPK and FB acknowledge support by the National Science Foundation under grant AST-100878798. NE-R acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 Astronomy Fellowships in Italy (AstroFIt). MF is supported by the European Union FP7 programme through ERC grant no. 320360. This work is based on observations collected at the WHT, operated on the island of La Palma by the Isaac Newton Group of Telescope; the LT, which is operated by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council; the GTC, installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma; the NOT, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias.||URI:||http://hdl.handle.net/20.500.12386/24146||URL:||https://academic.oup.com/mnras/article/452/2/1567/1060927||ISSN:||0035-8711||DOI:||10.1093/mnras/stv1360||Bibcode ADS:||2015MNRAS.452.1567C||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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