First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters

Abbott, T. M. C.; Allam, S.; Andersen, Per H.; Angus, C.; Asorey, J.; Avelino, Arturo; Ávila, S.; Bassett, Bruce A.; Bechtol, K.; Bernstein, G. M.; Bertin, E.; Brooks, D.; Brout, D.; Brown, P. J.; Burke, D. L.; Calcino, Josh; Rosell, A. Carnero; Carollo, D.; Kind, M. Carrasco; Carretero, J.; Casas, R.; Castander, F. J.; Cawthon, R.; Challis, P.; Childress, M.; Clocchiatti, A.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; Davis, C.; Davis, Tamara M.; Vicente, J. De; DePoy, D. L.; Desai, S.; Diehl, H. T.; Doel, P.; Drlica-Wagner, A.; Eifler, T. F.; Evrard, A. E.; Fernández, E.; Filippenko, A. V.; Finley, D. A.; Flaugher, B.; Foley, R. J.; Fosalba, P.; Frieman, J.; Galbany, L.; García-Bellido, J.; Gaztañaga, E.; Giannantonio, T.; Glazebrook, Karl; Goldstein, D.; González–Gaitán, S.; Gruen, David; Gruendl, R. A.; Gschwend, J.; Gupta, R.; Gutiérrez, G.; Hartley, W. G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hoormann, J. K.; Hoyle, B.; James, D. J.; Jeltema, T.; Johnson, M. W. G.; Johnson, Michael D.; Kasai, E.; Kent, S.; Kessler, R.; Kim, A. G.; Kirshner, R.; Kovacs, E.; Krause, E.; Krön, Richard G.; Kuêhn, K.; Kuhlmann, S. E.; Kuropatkin, N.; Lahav, O.; Lasker, J.; Lewis, Geraint F.; Li, T. S.; Lidman, C.; Lima, M.; Lin, Hai-Nan; Macaulay, E.; Maia, M. A. G.; Mandel, Kaisey S.; March, M.; Marriner, J.; Marshall, J. L.; Martini, Paul; Menanteau, F.; Miller, C. J.; Miquel, R.; Miranda, V.; Mohr, J. J.; Morganson, E.; Muthukrishna, Daniel; Möller, A.; Neilsen, Eric H.; Nichol, R. C.; Nord, B.; Nugent, P.; Ogando, R. L. C.; Palmese, A.; Pan, Y.-C.; Plazas, A. A.; Pursiainen, M.; Romer, A. K.; Roodman, A.; Rozo, Eduardo; Rykoff, E. S.; Šako, M.; Sánchez, E.; Scarpine, V.; Schindler, R. H.; Schubnell, M.; Scolnic, D.; Serrano, S.; Sevilla-Noarbe, I.; Sharp, Robert; Smith, M.; Soares-Santos, M.; Sobreira, F.; Sommer, N. E.; Spinka, H.; Suchyta, E.; Sullivan, M.; Swann, E.; Tarlè, G.; Thomas, Daniel B.; Thomas, R. C.; Troxel, M. A.; Tucker, B.; Uddin, S. A.; Walker, A. R.; Wester, W.; Wiseman, P.; Wolf, R. C.; Yanny, B.; Zhang, B.; Zhang, Y

doi:10.3847/2041-8213/ab04fa

Cited by 270 publications

(197 citation statements)

References 58 publications

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“…In our calculations we takew Y,0 = −0.80 +0.09 −0.11 , as derived from a combination of multiple observational probes in the Dark Energy Survey (DES) supernovae program (including 207 type Ia supernovae light curves, the BAO feature, weak gravitational lensing, and galaxy clustered, but independent of CMB measurements) [91]. This value ofw Y,0 is consistent at the 1σ level with the one derived from a combination of DES data and CMB measurements [92].…”

Section: Relaxing the H 0 Tension With Fading Dark Mattersupporting

confidence: 77%

H0 tension and the string swampland

et al. 2020

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We realize the Agrawal-Obied-Vafa swampland proposal of fading dark matter for solving the H 0 tension by the model of Salam-Sezgin and its string realization of Cvetič-Gibbons-Pope. The model describes a compactification of six-dimensional supergravity with a monopole background on a 2sphere. In four dimensions, there are two scalar fields, X and Y , and the effective potential in the Einstein frame is an exponential with respect to Y times a quadratic polynomial in the field e −X . When making the volume of the 2-sphere large, namely for large values of Y , there appears a tower of states, which according to the infinite distance swampland conjecture becomes exponentially massless. We confront the model with recent cosmological observations. We show that this set up is well equipped to explain the overall data even when considering local measurements of H 0 , and that it can potentially ameliorate the tension between low-redshift observations and measurements of the cosmic microwave background. Indeed, the tower of string states that emerges from the rolling of Y constitutes a portion of the dark matter, and the way in which the X particle and its KK excitations evolve over time (refer to as fading dark matter) is responsible for reducing the H 0 tension.

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Section: Relaxing the H 0 Tension With Fading Dark Mattersupporting

confidence: 77%

H0 tension and the string swampland

et al. 2020

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“…Transient events were detected using a differenceimaging pipeline (Kessler et al 2015), with machine-learning algorithms used to remove spurious candidates (Goldstein et al 2015). During the first three years, 251 SNe Ia were spectroscopically classified (D'Andrea et al 2018). The SN Ia light curve fluxes were measured using a 'Scene Model Photometry' (SMP) technique (Brout et al 2019a), and the photometric calibration is described in Burke et al (2018) and Lasker et al (2019).…”

Section: Sn and Host Galaxy Datamentioning

confidence: 99%

“…As part of the real-time survey operations, DES preferentially targeted SN-like events in low luminosity environments (D'Andrea et al 2018), potentially biasing the DES-SN sample with respect to host galaxy properties. In contrast, the SDSS and SNLS surveys spectroscopically confirmed SNe Ia using targeting programs principally agnostic to local environment.…”

Section: Estimates Of Stellar Massmentioning

confidence: 99%

“…With the DES-SN sample likely biased with respect to M stellar (D'Andrea et al 2018), to do this, we use instead the near-complete SDSS+SNLS sample of SN Ia hosts (as described in §5.2.1). For each galaxy in the HOSTLIB, with given stellar mass, we draw a random value of x 1 and c from the corresponding CDF in bins of log M stellar /M with width 0.25.…”

Section: Including Intrinsic Correlations Between Sn and Hostmentioning

confidence: 99%

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First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

Smith

Sullivan

Wiseman

et al. 2020

Monthly Notices of the Royal Astronomical Society

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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, α, β) bias correction, we find evidence of a Hubble residual 'mass step', where SNe Ia in high mass galaxies (> 10 10 M ) are intrinsically more luminous (after correction) than their low mass counterparts by γ = 0.040 ± 0.019mag. This value is consistent with other recent supernova samples that use a 5D correction, and is larger by 0.031mag 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 hostgalaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with γ = 0.066 ± 0.020mag. The 1D-5D γ difference for DES-SN is 0.026 ± 0.009mag. 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 γ with −9mmag bias compared to a +2mmag 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 γ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST.

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“…As the best distance indicator, the observation of Type Ia supernovae (SNe Ia) leads to the discovery of an accelerating-expansion Universe, which implies that there is a mysterious dark energy in the Universe and the evolution of the Universe is dominated by the dark energy (Riess et al 1998;Perlmutter et al 1999). Now, SNe Ia are becoming the center of a kind of scientific industry, such as measuring the equation of dark energy (Sullivan et al 2011;Abbott et al 2019), and constraining the cosmological model and basic physics via comparing the Hubble constant value from SNe Ia with the one from Planck satellite (Riess et al 2016;Planck Collaboration et al 2018). The cosmological utility of SNe Ia as distance indicators is dependent on one property of SNe Ia, i.e.…”

Section: Introductionmentioning

confidence: 99%

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

Meng

2019

ApJ

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Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact nature is still unclear, e.g. the progenitor and explosion models. The high-velocity features (HVFs) in optical spectra of SNe Ia could provide some meaningful information to constrain the nature of SNe Ia. Here, I show strong evidence that the SNe Ia with strong CaII infrared triple (CaII IR3) HVF around maximum brightness associate with relatively younger population than those with weak CaII IR3 HVF, e.g. the SNe Ia with strong CaII IR3 HVF tend to occur in late-type galaxy, or early-type galaxy with significant star formation. In addition, using pixel statistics I find that the SNe Ia with strong maximum-light CaII IR3 HVF show a higher degree of association with star formation index, e.g. Hα or near-UV emission, than those with weak CaII IR3 HVF. Moreover, I find that the strength of the CaII IR3 HVF is linearly dependent on the difference of the absorption-weighted velocities between CaII IR3 and SiII 635.5 nm absorption lines, which then is a good index to diagnose whether or not there is a high-velocity component in the CaII IR3 absorption feature in the spectra of SNe Ia. I finally discussed the origin of the HVFs and the constraints from our discoveries on the progenitor model of SNe Ia.

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First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters

Cited by 270 publications

References 58 publications

H0 tension and the string swampland

H0 tension and the string swampland

First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

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