THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE

Contreras, C.; Hamuy, M.; Phillips, M. M.; Folatelli, G.; Suntzeff, Nicholas B.; Persson, S. E.; Stritzinger, M. D.; Boldt, Luis; González, S.; Krzemiński, W.; Morrell, N.; Roth, M.; Salgado, Francisco; Maureira, María José; Burns, C. R.; Freedman, Wendy L.; Madore, Barry F.; Murphy, D. C.; Wyatt, P.; Li, Weidong; Filippenko, A. V.

doi:10.1088/0004-6256/139/2/519

Cited by 332 publications

(226 citation statements)

References 48 publications

Supporting

Mentioning

224

Contrasting

Order By: Relevance

“…We adjust the SED continuum to match the observed color by comparing synthetic magnitudes with observed magnitudes using the zero points defined in Fukugita et al (1996), Stritzinger et al (2002), and Regnault et al is the zero point of filter X of the CSP-I system (see Contreras et al 2010;Stritzinger et al 2011). The choice of filter X depends on the redshift.…”

Section: Methodsmentioning

confidence: 99%

See 1 more Smart Citation

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

Jaeger

González–Gaitán

Hamuy

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

The coming era of large photometric wide-field surveys will increase the detection rate of supernovae by orders of magnitude. Such numbers will restrict spectroscopic follow-up in the vast majority of cases, and hence new methods based solely on photometric data must be developed. Here, we construct a complete Hubble diagram of Type II supernovae (SNe II) combining data from three different samples: the Carnegie Supernova Project-I, the Sloan Digital Sky Survey II SN, and the Supernova Legacy Survey. Applying the Photometric Color Method (PCM) to 73 SNe II with a redshift range of 0.01-0.5 and with no spectral information, we derive an intrinsic dispersion of 0.35 mag. A comparison with the Standard Candle Method (SCM) using 61 SNeII is also performed and an intrinsic dispersion in the Hubble diagram of 0.27 mag, i.e., 13% in distance uncertainties, is derived. Due to the lack of good statistics at higher redshifts for both methods, only weak constraints on the cosmological parameters are obtained. However, assuming a flat universe and using the PCM, we derive the universe's matter density: W = -+ 0.32 m 0.21 0.30 providing a new independent evidence for dark energy at the level of two sigma.

show abstract

Section: Methodsmentioning

confidence: 99%

“…23 A full description can be found in Hamuy et al (2006), Contreras et al (2010), Stritzinger et al (2011), andFolatelli et al (2013).…”

Section: Carnegie Supernova Project-imentioning

confidence: 99%

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

Jaeger

González–Gaitán

Hamuy

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…At intermediate redshifts (0.1 < z < 0.4), the SDSS-II supernova survey Sako et al, 2008) has discovered and monitored 500 spectroscopically confirmed Type Ia SNe; only the first-year data set (103 SNe) has so far been subjected to a full cosmological analysis (Kessler et al, 2009 present cosmological results from a sample of 752 photometrically classified SDSS-II SNe with spectroscopic host galaxy redshifts, and a joint analysis of the SNLS and SDSS-II samples is in process (J. Frieman, private communication). Finally, the last five years have also seen major efforts to expand the sample of local calibrators and improve their measurements, including rest-frame IR and rest-frame UV photometry (Wood-Vasey et al, 2008;Stritzinger et al, 2011;Contreras et al, 2010;Hicken et al, 2009a).…”

Section: The Current State Of Playmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

View full text Add to dashboard Cite

The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

show abstract

“…The 374 supernovae from SDSS-II and 239 from SNLS were combined with 118 nearby supernovae from [6,[58][59][60][61][62] and nine high-redshift supernovae discovered and studied by HST [63]. We use this set, dubbed Joint Light-curve Analysis (JLA), rather than the Union 2.1 compilation of [64] because of the demonstrated improvement in calibration and corresponding reduction in systematic uncertainties presented in [30].…”

Section: Supernova Datamentioning

confidence: 99%

Cosmological implications of baryon acoustic oscillation measurements

Aubourg¹,

Bailey²,

Bautista³

et al. 2015

Phys. Rev. D

642

513

View full text Add to dashboard Cite

We derive constraints on cosmological parameters and tests of dark energy models from the combination of baryon acoustic oscillation (BAO) measurements with cosmic microwave background (CMB) data and a recent reanalysis of Type Ia supernova (SN) data. In particular, we take advantage of high-precision BAO measurements from galaxy clustering and the Lyman-α forest (LyaF) in the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). Treating the BAO scale as an uncalibrated standard ruler, BAO data alone yield a high confidence detection of dark energy; in combination with the CMB angular acoustic scale they further imply a nearly flat universe. Adding the CMB-calibrated physical scale of the sound horizon, the combination of BAO and SN data into an "inverse distance ladder" yields a measurement of H0 = 67.3 ± 1.1 km s −1 Mpc −1 , with 1.7% precision. This measurement assumes standard pre-recombination physics but is insensitive to assumptions about dark energy or space curvature, so agreement with CMB-based estimates that assume a flat ΛCDM cosmology is an important corroboration of this minimal cosmological model. For constant dark energy (Λ), our BAO+SN+CMB combination yields matter density Ωm = 0.301 ± 0.008 and curvature Ω k = −0.003 ± 0.003. When we allow more general forms of evolving dark energy, the BAO+SN+CMB parameter constraints are always consistent with flat ΛCDM values at ≈ 1σ. While the overall χ 2 of model fits is satisfactory, the LyaF BAO measurements are in moderate (2 − 2.5σ) tension with model predictions. Models with early dark energy that tracks the dominant energy component at high redshift remain consistent with our expansion history constraints, and they yield a higher H0 and lower matter clustering amplitude, improving agreement with some low redshift observations. Expansion history alone yields an upper limit on the summed mass of neutrino species, mν < 0.56 eV (95% confidence), improving to mν < 0.25 eV if we include the lensing signal in the Planck CMB power spectrum. In a flat ΛCDM model that allows extra relativistic species, our data combination yields N eff = 3.43 ± 0.26; while the LyaF BAO data prefer higher N eff when excluding galaxy BAO, the galaxy BAO alone favor N eff ≈ 3. When structure growth is extrapolated forward from the CMB to low redshift, standard dark energy models constrained by our data predict a level of matter clustering that is high compared to most, but not all, observational estimates.

show abstract

THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE

Cited by 332 publications

References 48 publications

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

Observational probes of cosmic acceleration

Cosmological implications of baryon acoustic oscillation measurements

Contact Info

Product

Resources

About