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J/A+A/615/A68         Type Ia supernova luminosities              (Roman+, 2018)

Dependence of Type Ia supernova luminosities on their local environment. Roman M., Hardin D., Betoule M., Astier P., Balland C., Ellis R.S., Fabbro S., Guy J., Hook I.M., Howell D.A., Lidman C., Mitra A., Moeller A., Mourao A.M., Neveu J., Palanque-Delabrouille N., Pritchet C.J., Regnault N., Ruhlmann-Kleider V., Saunders C., Sullivan M. <Astron. Astrophys. 615, A68 (2018)> =2018A&A...615A..68R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Supernovae ; Photometry, SDSS Keywords: supernovae: general - techniques: image processing - techniques: photometric - dark energy - methods: data analysis - galaxies: photometry Abstract: We present a fully consistent catalog of local and global properties of host galaxies of 882 Type Ia supernovae (SNIa) that were selected based on their light-curve properties, spanning the redshift range 0.01<z<1. This catalog corresponds to a preliminary version of the compilation sample and includes Supernova Legacy Survey (SNLS) 5-year data, Sloan Digital Sky Survey (SDSS), and low-redshift surveys. We measured low- and moderate-redshift host galaxy photometry in SDSS stacked and single-epoch images and used spectral energy distribution (SED) fitting techniques to derive host properties such as stellar mass and U-V rest-frame colors; the latter are an indicator of the luminosity-weighted age of the stellar population in a galaxy. We combined these results with high-redshift host photometry from the SNLS survey and thus obtained a consistent catalog of host stellar masses and colors across a wide redshift range. We also estimated the local observed fluxes at the supernova location within a proper distance radius of 3kpc, corresponding to the SNLS imaging resolution, and transposed them into local U-V rest-frame colors. This is the first time that local environments surrounding SNIa have been measured at redshifts spanning the entire Hubble diagram. Selecting SNIa based on host photometry quality, we then performed cosmological fits using local color as a third standardization variable, for which we split the sample at the median value. We find a local color step significance of -0.091±0.013mag (7σ), which effect is as significant as the maximum mass step effect. This indicates that the remaining luminosity variations in SNIa samples can be reduced with a third standardization variable that takes the environment into account. Correcting for the maximum mass step correction of -0.094±0.013mag, we find a local color effect of -0.057±0.012mag (5σ), which shows that additional information is provided by the close environment of SNIa. Departures from the initial choices were investigated and showed that the local color effect is still present, although less pronounced. We discuss the possible implications for cosmology and find that using the local color in place of the stellar mass results in a change in the measured value of the dark energy equation-of-state parameter of 0.6%. Standardization using local U-V color in addition to stretch and color reduces the total dispersion in the Hubble diagram from 0.15 to 0.14mag. This will be of tremendous importance for the forthcoming SNIa surveys, and in particular for the Large Synoptic Survey Telescope (LSST), for which uncertainties on the dark energy equation of state will be comparable to the effects reported here. Description: Host photometry (magnitudes) and local photometry (magnitudes and fluxes) measured on SNLS and SDSS images, with derived U-V global and local colors, and host stellar masses. Local color is measured within a 3kpc radius. Projected distance to the centre is also estimated. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file snprop.dat 551 881 *Properties of the SNIa sample snprop.fits 2880 107 Fits version of snprop.dat
Note on snprop.dat: For one SNLS SNIa, host identification was uncertain so no measurement was done. It is nonetheless taken into account in the numbers shown in the paper, but never enters any of the samples we study. Therefore, the file contains 881 entries and not 882 (including 396 SNLS SNIa).
See also: V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015) Byte-by-byte Description of file: snprop.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Name of the SNIa (name) 10- 23 F14.12 --- z Redshift (redshift) 25- 30 A6 --- Survey Survey (survey) 32- 44 F13.9 deg RAdeg [-56/359] Right ascension of the SNIa location (J2000) (ra) 46- 58 F13.9 deg DEdeg Delcination of the SNIa location (J2000) (dec) 60- 71 F12.6 mag umagg ?=- Host galaxy SDSS u magnitude (magglobalu) (1) 73- 84 F12.6 mag gmagg ?=- Host galaxy SDSS g magnitude (magglobalg) (1) 86- 97 F12.6 mag rmagg ?=- Host galaxy SDSS r magnitude (magglobalr) (1) 99-110 F12.6 mag imagg ?=- Host galaxy SDSS i magnitude (magglobali) (1) 112-123 F12.6 mag zmagg ?=- Host galaxy SDSS z magnitude (magglobalz) (1) 125-136 F12.6 mag e_umagg ?=- rms uncertainty on umagg (emagglobalu) (1) 138-149 F12.6 mag e_gmagg ?=-rms uncertainty on gmagg (emagglobalg) (1) 151-162 F12.6 mag e_rmagg ?=- rms uncertainty on rmagg (emagglobalr) (1) 164-175 F12.6 mag e_imagg ?=- rms uncertainty on imagg (emagglobali) (1) 177-188 F12.6 mag e_zmagg ?=- rms uncertainty on zmagg (emagglobalz) (1) 190-201 F12.6 mag umagl ? SDSS u magnitude within 3kpc radius (maglocalu) (1) 203-214 F12.6 mag gmagl ? SDSS g magnitude within 3kpc radius (maglocalg) (1) 216-227 F12.6 mag rmagl ? SDSS r magnitude within 3kpc radius (maglocalr) (1) 229-240 F12.6 mag imagl ? SDSS i magnitude within 3kpc radius (maglocali) (1) 242-253 F12.6 mag zmagl ? SDSS z magnitude within 3kpc radius (maglocalz) (1) 255-266 F12.6 mag e_umagl ? rms uncertainty on ugmal (emaglocalu) (1) 268-279 F12.6 mag e_gmagl ? rms uncertainty on ggmal (emaglocalg) (1) 281-292 F12.6 mag e_rmagl ? rms uncertainty on rgmal (emaglocalr) (1) 294-305 F12.6 mag e_imagl ? rms uncertainty on igmal (emaglocali) (1) 307-318 F12.6 mag e_zmagl ? rms uncertainty on zgmal (emaglocalz) (1) 320-331 F12.6 --- Ful ?=0 Flux in SDSS u band within 3kpc radius (fluxlocalu) (1) 333-344 F12.6 --- Fgl ?=0 Flux in SDSS g band within 3kpc radius (fluxlocalg) (1) 346-357 F12.6 --- Frl ?=0 Flux in SDSS r band within 3kpc radius (fluxlocalr) (1) 359-370 F12.6 --- Fil ?=0 Flux in SDSS i band within 3kpc radius (fluxlocali) (1) 372-383 F12.6 --- Fzl ?=0 Flux in SDSS z band within 3kpc radius (fluxlocalz) (1) 385-396 F12.6 --- e_Ful []?=0 rms uncertainty on Ful (efluxlocalu) (1) 398-409 F12.6 --- e_Fgl []?=0 rms uncertainty on Fgl (efluxlocalg) (1) 411-422 F12.6 --- e_Frl []?=0 rms uncertainty on Frl (efluxlocalr) (1) 424-435 F12.6 --- e_Fil []?=0 rms uncertainty on Fil (efluxlocali) (1) 437-448 F12.6 --- e_Fzl []?=0 rms uncertainty on Fzl (efluxlocalz) (1) 450-463 F14.11 mag U-Vl ?=99 Local U-V colour index within 3kpc radius (uv_local) 465-478 F14.11 mag e_U-Vl ?=-1 rms uncertainty on U-Vl (euv_local) 480-493 F14.11 mag U-Vg ?=99 Host galaxy U-V colour index (uv_global) 495-508 F14.11 mag e_U-Vg ?=-1 rms uncertainty on U-Vg (euv_global) 510-524 F15.10 [Msun] logMs ?=-999 Stellar mass of the host galaxy (stellar_mass) 526-540 F15.10 [Msun] e_logMs ?=-999 rms uncertainty on logMs (estellar_mass) 542-551 F10.6 kpc Dist Projected distance of the SNIa to the galactic center (d_kpc)
Note (1): For SN from SDSS, CSP, CfAIII and CfAIV, magnitudes are in AB system and fluxes in nanomaggies (∼3.631x10-6Jy). For SN from SNLS5, magnitudes are in Vega system and fluxes are in Vega-flux unit. To transform SNLS5 fluxes in maggies unit, use Flux(Vega)*10^(-0.4DeltaZP), with the following DeltaZP values: u : 10.197 g : 9.596 r : 9.342 i : 9.250 z : 9.238
Acknowledgements: Matthieu Roman, matthieu.roman(at)lpnhe.in2p3.fr, roman.matthieu(at)gmail.com
(End) Matthieu Roman [LPNHE, France], Patricia Vannier [CDS] 20-Mar-2018
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