First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant

Macaulay, E.; Nichol, R. C.; Bacon, David; Brout, D.; Davis, Tamara M.; Zhang, B.; Bassett, Bruce A.; Scolnic, Dan; Möller, A.; D’Andrea, C. B.; Hinton, S. R.; Keßler, R.; Kim, A. G.; Lasker, J.; Lidman, C.; Šako, M.; Smith, M.; Sullivan, M.; Abbott, T. M. C.; Allam, S.; Annis, J.; Asorey, J.; Ávila, S.; Bechtol, K.; Brooks, D.; Brown, P. J.; Burke, D. L.; Calcino, Josh; Rosell, A. Carnero; Carollo, D.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Collett, Thomas E.; Crocce, M.; Cunha, C. E.; Costa, L. N. da; Davis, C.; Vicente, J. De; Diehl, H. T.; Doel, P.; Drlica-Wagner, A.; Eifler, T. F.; Estrada, J.; Evrard, A. E.; Filippenko, A. V.; Finley, D. A.; Flaugher, B.; Foley, R. J.; Fosalba, P.; Frieman, Joshua A.; Galbany, L.; García-Bellido, J.; Gaztañaga, E.; Glazebrook, Karl; González–Gaitán, S.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutiérrez, G.; Hartley, W. G.; Hollowood, D. L.; Honscheid, K.; Hoormann, J. K.; Hoyle, B.; Huterer, Dragan; Jain, Bhuvnesh; James, D. J.; Jeltema, T.; Kasai, E.; Krause, E.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Lewis, Geraint F.; Li, T. S.; Lima, M.; Lin, Huan; Maia, M. A. G.; Marshall, J. L.; Martini, Paul; Miquel, R.; Nugent, P.; Palmese, A.; Pan, Y. C.; Plazas, A. A.; Romer, A. K.; Roodman, A.; Sanchez, E. J.; Scarpine, V.; Schindler, R. H.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Sharp, Robert; Soares-Santos, M.; Sobreira, F.; Sommer, N. E.; Suchyta, E.; Swann, E.; Swanson, M. E. C.; Tarlè, G.; Thomas, Daniel; Thomas, R. C.; Tucker, B.; Uddin, S. A.; Vikram, V.; Walker, A. R.; Wiseman, P.

doi:10.1093/mnras/stz978

Cited by 200 publications

(85 citation statements)

References 78 publications

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“…For this analysis the apparent magnitudes given in equations (3) and (22) are used. Finally, it is important to note that, although the CMB prior of equation (14) corresponds to the analysis based on the ΛCDM model, this does not ensure that the H0 value that we will obtain is in agreement with CMB determinations, see Macaulay et al (2019).…”

Section: Sne + Bao + Cmb Priormentioning

confidence: 95%

“…We now discuss the so-called "inverse distance ladder" (see, e.g., Macaulay et al 2019;Feeney et al 2018b). BAO needs to be calibrated in order to provide a pure geometrical distance, that is, a standard ruler.…”

Section: Sne + Bao + Cmb Priormentioning

confidence: 99%

“…We will now compare our inverse distance ladder of Section 4.2 with previous results. The standard way to extend the cosmic ladder to high-redshift observations is via a cosmographic approach (see, e.g., Macaulay et al 2019;Feeney et al 2018b); we call "cosmographic method" this way of building the comic ladder. As discussed earlier, our method uses the cosmographic expansion only at low redshifts (z ≤ 0.15) and exploits the distance-duality relation for calibrating BAO and SNe data; we name it the "distance-duality method."…”

Section: Comparison With Previous Inverse Distance Laddersmentioning

confidence: 99%

“…Here, we will discuss how the cosmic distance ladder can be extended from our galaxy to the CMB. This allows one to use it as an "inverse distance ladder", that is, to calibrate the supernovae via CMB and BAO instead of Cepheids and geometrical distances (Cuesta et al 2015;Aubourg et al 2015;Verde et al 2017;Lemos et al 2018;Feeney et al 2018b;Macaulay et al 2019;Tutusaus et al 2019). Although this method allows one to avoid possible unknown systematics, most of the approaches requires a fiducial model to convert redshifts into distances (Cuesta et al 2015;Aubourg et al 2015;Verde et al 2017;Lemos et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Although this method allows one to avoid possible unknown systematics, most of the approaches requires a fiducial model to convert redshifts into distances (Cuesta et al 2015;Aubourg et al 2015;Verde et al 2017;Lemos et al 2018). A few cases have been built using a cosmographic expansion (Feeney et al 2018b;Macaulay et al 2019), which could be problematic at 0 z 2 (Zhang et al 2017). Most importantly, the standard approach cannot provide a truly local value of H0 as supernovae beyond z = 0.15 are used.…”

Section: Introductionmentioning

confidence: 99%

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A new method to build the (inverse) distance ladder

Camarena

Marra

2020

Monthly Notices of the Royal Astronomical Society

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The cosmic distance ladder is the succession of techniques by which it is possible to determine distances to astronomical objects. Here, we present a new method to build the cosmic distance ladder, going from local astrophysical measurements to the CMB. Instead of relying on cosmography in order to model the luminosity-distance relation and calibrate supernovae with BAO, we exploit the distance-duality relation d L = (1 + z) 2 d A -valid if photon number is conserved and gravity is described by a metric theory. The advantage is that the results will not depend on the parametrization of the luminosity-distance relation: no model is adopted in order to calibrate BAO with supernovae. This method yields measurements of the Hubble constant and deceleration parameter that only use local observations. Furthermore, it can directly assess the impact of BAO observations on the strong 4-5σ tension between local and global H 0 . Using the latest supernova, BAO and CMB observations, we found a consistently low value of q 0 and strong inconsistency between angular and anisotropic BAO measurements, which are, or not, in agreement with CMB depending on the kind of analysis. We conclude that, in order to understand the reasons behind the H 0 crisis, a first step should be clarifying the tension between angular and anisotropic BAO as this will help understanding if new physics is required at the pre-recombination epoch or/and during the dark energy era.

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Section: Sne + Bao + Cmb Priormentioning

confidence: 95%

Section: Sne + Bao + Cmb Priormentioning

confidence: 99%

Section: Comparison With Previous Inverse Distance Laddersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A new method to build the (inverse) distance ladder

Camarena

Marra

2020

Monthly Notices of the Royal Astronomical Society

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Kilonova afterglow rate from spherical and axisymmetrical models

Kóbori

2019

Astron Nachr

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Detecting the afterglows of double-neutron star merger events is a challenging task because of the quick fading of the observed flux. In order to create an efficient observing strategy for their observing method, it is crucial to know their intrinsic rate. Unfortunately, the numerous models existing today predict this rate on a very wide range. Our goal in this paper is to compare the different levels of approximations in order to determine their reliability. We find that there is a significant discrepancy in the expected detection rate between the spherical and axisymmetrical models (∼18 and ≲ 1 yr −1 , respectively). In addition, choosing different models for the input parameters (for example, redshift and time delay distribution) has also a strong effect on the results. K E Y W O R D Sgamma rays: bursts, methods: numerical, methods: statisticalThis is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited.

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Dynamical System Approach and Thermodynamical Perspective of Hořava‐Lifshitz Gravity

Samaddar,

Singh

2024

Fortschritte der Physik

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The authors have examined a Friedmann Robertson Walker cosmological model in Hořava‐Lifshitz gravity by using a dynamical system approach. A set of autonomous equations is derived and their solutions are calculated. The critical points from these equations and find the characteristics values with the analysis of the physical interpretation of the phase space for this system are assessed. Three stable critical points are found and the values of the physical parameters and the scale factor's expressions at each critical points are displayed in Tables 1, 2, and 3. A hybrid scale factor to develop the model, which results in a phase transition from deceleration to acceleration is used. The suitable values of the parameters are governed by applying the Monte Chain Monte Carlo method technique to the Hubble 46 and joint Hubble 46 and Baryon Acoustic Oscillations 15 datasets. In contrast to the negative behavior of pressure, the positive behavior of energy density and illustrate the Universe's acceleration epoch and the model is represented by the EoS parameter . The authors investigated that the energy conditions and their model violates the strong energy condition. Utilizing diagnostic test, it is found that the model represents phantom behavior. The thermodynamical perspective for the model is also examined. The model accurately explained the Universe's propagation history and fits well with contemporary cosmic data.

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First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant

Cited by 200 publications

References 78 publications

A new method to build the (inverse) distance ladder

A new method to build the (inverse) distance ladder

Kilonova afterglow rate from spherical and axisymmetrical models

Dynamical System Approach and Thermodynamical Perspective of Hořava‐Lifshitz Gravity

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