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|a (TOE)ost1614732
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|a E 1.99:fermilab-pub-20-016-ae
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|a E 1.99:fermilab-pub-20-016-ae
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|a fermilab-pub-20-016-ae
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|a Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey
|h [electronic resource]
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|a Batavia, Ill. :
|b Fermi National Accelerator Laboratory ;
|a Oak Ridge, Tenn. :
|b Distributed by the Office of Scientific and Technical Information, U.S. Department of Energy,
|c 2020.
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|a Medium: ED :
|b digital, PDF file.
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|a text
|b txt
|2 rdacontent.
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|a computer
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|2 rdamedia.
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|a online resource
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|a Published through Scitech Connect.
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|a 02/18/2020.
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|a "fermilab-pub-20-016-ae"
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|a "Other: oai:inspirehep.net:1790666"
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|a de Jaeger, T. ;
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|a USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
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|a Despite vast improvements in the measurement of the cosmological parameters, thenature of dark energy and an accurate value of the Hubble constant (H0) in theHubble-Lemâtre law remain unknown. To break the current impasse, it is necessaryto develop as many independent techniques as possible, such as the use of Type IIsupernovae (SNe II). Here, we present a sample from the Dark Energy Survey Super-nova Program (DES-SN) consisting of 15 SNe II with photometric and spectroscopicinformation spanning a redshift range up to 0.35. Combining our DES SNe with pub-licly available samples, and using the standard candle method (SCM), we constructthe largest available Hubble diagram with SNe II in the Hubble ow (70 SNe II) and nd an observed dispersion of 0.28 mag. We demonstrate that adding a colour term tothe SN II standardisation does not reduce the scatter in the Hubble diagram. As thenext generation of surveys will discover a large number of SNe without spectroscopicfollow-up observations, we use a purely photometric method to derive extragalacticdistances. Nevertheless, we show that both methods are viable for using SNe II as dis-tance indicators, and this work addresses important issues for improving their utilityas independent extragalactic beacons: nd new correlations, de ne a more standardsubclass of SNe II, construct new SN II templates, and dedicate more observing timeto high-redshift SNe II. Finally, for the rst time, we perform simulations to estimatethe redshift-dependent distance modulus bias due to selection e ects.
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|b AC02-07CH11359.
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|a 79 astronomy and astrophysics
|2 local.
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|a Fermi National Accelerator Laboratory.
|4 res
|4 spn.
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|a United States.
|b Department of Energy.
|b Office of Scientific and Technical Information
|4 dst.
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|u http://www.osti.gov/servlets/purl/1614732
|z Full Text (via OSTI)
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|a .b110064136
|b 11-30-21
|c 05-11-20
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|a web
|b 05-11-20
|c f
|d m
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|f eng
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|s 301c39f8-836a-5d4d-9525-5994a9dbb484
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|p Can circulate
|a University of Colorado Boulder
|b Online
|c Online
|d Online
|e E 1.99:fermilab-pub-20-016-ae
|h Superintendent of Documents classification
|i web
|n 1
|
