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Detection and Observable Behaviours of High Redshift Superluminous Supernovae

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Detection and Observable Behaviours of High Redshift Superluminous Supernovae Detection and Observable Behaviours of High Redshift Superluminous Supernovae Christopher M. Curtin Presented in fulfillment of the requirements of the degree of Doctor of Philosophy August 28, 2019 Faculty of Science and Engineering Technology Swinburne University i Abstract We apply Lyman Break Galaxy (LBG) Selection and Monitoring to photometry from the ongoing Dark Energy Survey (DES), Survey Using DECam for Superluminous Super- novae (SUDSS) and Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) to more efficiently identify high redshift (z & 2) superluminous supernovae (SLSNe) and enable spectroscopic follow-up near peak. SLSNe are a luminosity class of supernovae ∼10–100× more luminous than an average type-Ia supernova. We construct deep griz stacks with cadenced data from DES and the SUDSS, as well as uncadenced DECam archival data. Deep image stacks are required for effective selection of LBGs. We achieve gri(z) depths of ∼27.5 (27) mag on the two DES deep fields (6 deg2) and ∼26.5 (26) mag on two SUDSS fields (6 deg2). These stacks can be used to select LBGs at z ∼ 4 with no additional photometry. We initiated u0SUDSS, the DECam u0-band extension to SUDSS, to provide u0-band deep stack photometry (∼26.2 mag) on select fields. Deep u-band (3000–4000Å) photome- try extends LBG selection to lower redshifts (z ∼ 2 and z ∼ 3) and increases selection sizes by up to a factor of 30. We construct deep u0-band stacks from proprietary and archival photometry on three DES/SUDSS fields (9 deg2) with a fourth field under way. This depth is sufficient to increase the LBG sample size by a factor of ∼15. We develop LBG colour selection criteria for DECam using composite LBG spectra and synthetic colours of model star-forming galaxy spectral templates measured from 0 < z < 6. We then refine the criteria with spectroscopic redshift confirmations of ∼100 sources observed with the Keck Low Resolution Imaging Spectrometer (LRIS) and several hundred archival spectroscopic redshifts. Efficiency estimates of the refined criteria range from 70–85% and completeness estimates range from 40–50%. The most developed catalogue on the DES C3 deep field (3 deg2) includes ∼150,000 sources. Extensive z ∼ 2 LBG selections (∼60,000 sources) are catalogued on two other fields (6 deg2) with deep u0-band photometry. We monitor LBGs in the DES C3 field for transient activity during the fourth and fifth years of the survey using the DES transient catalogue. We inspect the light curve behaviour of each event to rule out active galactic nuclei (AGN) and low redshift SNe- Ia. We identify 25 photometric candidates of interest over both seasons. High redshift SLSN candidates are considered for spectroscopic follow-up based on their confidence and brightness. Additional targets are provided by the Subaru HIgh-Z sUpernovae CAmpaign (SHIZUCA). ii We perform four spectroscopic follow-up campaigns using Keck LRIS. Poor observing conditions and light cirrus during each campaign restricted the selection and number of targets and reduced the quality of collected spectra, with one campaign being completely weathered out. Spectra of three DES targets are successfully collected and reduced. Of these two events are considered to be likely low redshift supernovae and one is an AGN at z = 1:697. Spectra of five SHIZUCA photometric candidates are also collected and reduced. Two are low redshift supernovae and three are determined to be SLSNe at z = 1.851, 1.965 and 2.399, the latter being the highest redshift supernova observed spectroscopically near peak to date. The spectroscopic subtype of each event is indeterminate. With this thesis we demonstrate that deep follow-up spectroscopy of z ∼ 2–4 SLSNe near peak is achievable with modern surveys and 8m-class telescopes, even when classically scheduled. The three spectra of z ∼ 2 supernovae near maximum light obtained during this work nearly double the number of such spectra collected to date, and there are many more photometric candidates than are able to be targeted with the follow-up time awarded. Accumulating more spectra of SLSNe at redshifts of z ∼ 2–6 is crucial for recognizing and understanding their far-UV behaviours. This is a pre-requisite for identifying SLSNe at z ∼ 6–20 as future large telescopes and JWST will only have access to the restframe far-UV at these redshifts. Future work includes analysing all photometric SLSN candidates and obtaining spectroscopic redshifts of their hosts to constrain rates, identify general far-UV light curve behaviours and optimise the efficiency of LBG S&M for future surveys. iii iv Acknowledgements I’d like to express my deepest gratitude to my advisory team, Professors Jeff Cooke, Emma Ryan-Weber and Jeremy Mould, for their steady support and guidance throughout my project. Thanks to Australia, Swinburne and CAS for the opportunity and resources to conduct my research and write my thesis. To my fellow team members, Igor, Uros, Garry, Trooper, Sara, Stephi, it was a pleasure working with you and thanks for all your help. To the science fiction book club, Colin, Rob, Stefan, our wildly speculative conversa- tions were both a scientific motivation and a much needed distraction for me near the end. Thanks for the ride. To those who wouldn’t leave me alone near the end, Yeshe, Rossana, Wael, and to those who kept tabs, of whom there are too many to list, I truly appreciate it. You held me accountable, as good friends do. To my family, you know yourselves, thanks for making me know that I was loved and believed in at every step along the way here. I love you, too. To the next gen, David Isaac, Samantha, Dain, Topher, you can do anything you put your mind to. And know that whatever that is, I’ll be cheering you on. A special thanks to the counsellors at Swinhealth who kept me sane at no charge. And I thank my God, for everything, always. v vi Declaration The work presented in this thesis has been carried out in the Centre for Astrophysics & Supercomputing at Swinburne University of Technology between 2014 and 2019. This thesis contains no material that has been accepted for the award of any other degree or diploma. To the best of my knowledge, this thesis contains no material previously published or written by another author, except where due reference is made in the text of the thesis. The content of the chapters listed below has appeared in refereed journals. Minor alterations have been made to the published papers in order to maintain argument continuity and consistency of spelling and style. • Chapter 5 has been published as “First Release of High-redshift Superluminous Super- novae from the Subaru HIgh-Z sUpernova CAmpaign (SHIZUCA). II. Spectroscopic Properties” in The Astrophysical Journal Supplement Series, Volume 241, Issue 2, article id. 17, 14 pp. (2019). My contribution to this paper was the collection of the spectra, data reduction and analysis, and the writing of the text. My co-authors contributed in discussions about and revisions to early manuscript drafts, and certain specialised software tools used in the analysis of the reduced data. Christopher M. Curtin Melbourne, Victoria, Australia August 28, 2019 vii viii Dedicated to the memory of my dear Aunt Martha, 1951–2019, who loved me to pieces. See you among your stars Mart. 0.1. SURVEYS ix Acronymus, Abbreviations and Conventions 0.1 Surveys • ASAS-SN: All-Sky Automated Survey for Supernovae • CRTS: Catalina Real-time Transient Survey • CFHTLS: Canada-France-Hawaii Telescope Legacy Survey • DES: Dark Energy Survey • GOODS: Great Observatories Origins Deep Survey • HSC-SSP: Hyper-SuprimeCam Subaru Strategic Program • HZT: High-Z Supernova Search Team • PS1: Panoramic Survey Telescope And Rapid Response System 1 • PTF: Palomar Transient Factory • SCP: Supernova Cosmology Project • SDSS: Sloan Digital Sky Survey • SHIZUCA: Subaru HIgh-Z sUpernovae CAmpaign • SNLS: Supernova Legacy Survey • SUDSS: Survey Using DECam for Superluminous Supernovae • TSS: Texas Supernova Search • USNO-B1: United States Naval Observatory B1.0 Catalogue • u0SUDSS: The DECam u0-band SUDSS Extension • VIDEO: VISTA Deep Extragalactic Observations Survey • ZFOURGE: FourStar Galaxy Evolution Survey • ZTF: Zwicky Transient Facility x 0.2 Observatories and Instruments • AAO: Australian Astronomical Observatory • ACS: Advanced Camera for Surveys • CFHT: Canada-France-Hawaii Telescope • COS: Cosmic Origin Spectrograph • CTIO: Cerro Tololo Inter-american Observatory • DECam: Dark Energy Camera • HSC: Hyper-SuprimeCam • HST: Hubble Space Telescope • JWST: James Webb Space Telescope • KDUST: Kunlun Dark Universe Survey Telescope • LRIS: Low Resolution Imaging Spectrometer • LSST: Large Synoptic Survey Telescope • NOAO: National Optical Astronomical Observatories • STIS: Space Telescope Imaging Spectrograph • TAO: University of Tokyo Atacama Observatory • VIRCAM: VISTA InfraRed CAMera • VISTA: Visible and Infrared Survey Telescope for Astronomy • VLT: Very Large Telescope Contents Abstract i Acknowledgements iii Declaration v 0.1 Surveys . ix 0.2 Observatories and Instruments . x Acronymus, Abbreviations and Conventions ix List of Figures xiii List of Tables xvii 1 Introduction 1 1.1 Background . 1 1.2 SLSN Subtypes and Mechanics . 3 1.2.1 SLSNe-I . 4 1.2.2 SLSNe-II . 6 1.2.3 PISNe . 9 1.2.4 P-PISN . 11 1.3 SLSNe at High Redshift . 12 1.4 Lyman Break Galaxy Selection & Monitoring . 15 1.5 Surveys and Fields . 16 1.6 Purpose of the Thesis . 20 2 Deep Stacking 21 2.1 Introduction . 21 2.2 Maximizing Depth . 23 2.3 Image Sets . 24 2.4 Software . 26 2.5 Astrometrics . 26 2.6 Image Set Calibration . 27 2.7 Image Stacking and Source Extraction . 30 2.8 Photometric Calibration . 33 2.8.1 Zeropoints . 36 xi xii CONTENTS 2.8.2 u0-band Rectification . 37 2.8.3 Photometric Uncertainties . 39 2.9 Filter Crossmatching . 39 2.10 Depth Estimates and Conclusion .
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