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|a (TOE)ost1606223
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|a E 1.99: des-2018-0402
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|a E 1.99:arxiv:2001.11294
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|a E 1.99: fermilab-pub-20-003-ae
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|a E 1.99: des-2018-0402
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|a arxiv:2001.11294
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|a fermilab-pub-20-003-ae
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|a des-2018-0402
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|a First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey
|h [electronic resource] :
|b The Effect of Host Galaxy Properties on Supernova Luminosity.
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| 260 |
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|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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| 336 |
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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
|b cr
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|a Published through Scitech Connect.
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|a 01/30/2020.
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|a "arxiv:2001.11294"
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|a " fermilab-pub-20-003-ae"
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|a " des-2018-0402"
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|a "Other: oai:inspirehep.net:1777962"
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|a Smith, M.; et al.;
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| 500 |
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|a SLAC National Accelerator Lab., Menlo Park, CA (United States)
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| 500 |
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|a USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
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| 520 |
3 |
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|a We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. Fitting spectral energy distributions to the $griz$ photometric measurements of the DES-SN host galaxies, we derive stellar masses and star-formation rates. For the DES-SN sample, when considering a 5D ($z$, $x_1$, $c$, $\alpha$, $\beta$) bias correction, we find evidence of a Hubble residual ̀mass step', where SNe Ia in high mass galaxies ($>10̂ \textrm{M}_{\odot}$) are intrinsically more luminous (after correction) than their low mass counterparts by $\gamma=0.040\pm0.019$mag. This value is larger by $0.031$mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\gamma=0.066\pm0.020$mag. The 1D-5D $\gamma$ difference for DES-SN is $0.026\pm0.009$mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the $x_1$ component of the 5D distance-bias correction. To better understand this effect, we include an intrinsic correlation between light-curve width and stellar mass in simulated SN Ia samples. We show that a 5D fit recovers $\gamma$ with $-9$mmag bias compared to a $+2$mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modeling correlations between galaxy properties and SN is necessary to determine the implications for $\gamma$ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST.
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|b AC02-07CH11359.
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|a 79 astronomy and astrophysics
|2 local.
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2 |
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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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| 856 |
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|u http://www.osti.gov/servlets/purl/1606223
|z Full Text (via OSTI)
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|a .b110067459
|b 11-30-21
|c 05-11-20
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|a web
|b 05-11-20
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| 952 |
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|p Can circulate
|a University of Colorado Boulder
|b Online
|c Online
|d Online
|e E 1.99: des-2018-0402
|h Superintendent of Documents classification
|i web
|n 1
|
