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J/A+A/615/A45       NIR K-corrections                        (Stanishev+, 2018)

Type Ia supernova Hubble diagram with near-infrared and optical observations. Stanishev V., Goobar A., Amanullah R., Bassett B., Fantaye Y.T., Garnavich P., Hlozek R., Nordin J., Okouma P.M., Ostman L., Sako M., Scalzo R., Smith M. <Astron. Astrophys. 615, A45 (2018)> =2018A&A...615A..45S (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, standards ; Photometry, infrared Keywords: supernovae: general - methods: observational - techniques: photometric Abstract: Type Ia Supernovae (SNe Ia) have been used as standardizable candles in the optical wavelengths to measure distances with an accuracy of ∼7% out to redshift z∼1.5. There is evidence that in the near-infrared (NIR) wavelengths SNe Ia are even better standard candles, however, NIR observations are much more time-consuming. We aim to test whether the NIR peak magnitudes could be accurately estimated with only a single observation obtained close to maximum light, provided that the time of B band maximum, the B-V color at maximum and the optical stretch parameter are known. We present multi-epoch UBVRI and single-epoch J and H photometric observations of 16 SNe Ia in the redshift range z=0.037-0.183, doubling the leverage of the current SN Ia NIR Hubble diagram and the number of SNe beyond redshift 0.04. This sample was analyzed together with 102 NIR and 458 optical light curves (LCs) of normal SNe Ia from the literature. Results. The analysis of 45 NIR LCs with well-sampled first maximum shows that a single template accurately describes the LCs if its time axis is stretched with the optical stretch parameter. This allows us to estimate the peak NIR magnitudes of SNe with only few observations obtained within ten days from B-band maximum. The NIR Hubble residuals show weak correlation with ΔM15 and the color excess E(B-V), and for the first time we report a potential dependence on the Jmax-Hmax color. With these corrections, the intrinsic NIR luminosity scatter of SNe Ia is estimated to be ∼0.10mag, which is smaller than what can be derived for a similarly heterogeneous sample at optical wavelengths. Analysis of both NIR and optical data shows that the dust extinction in the host galaxies corresponds to a low RV~=1.8-1.9. We conclude that SNe Ia are at least as good standard candles in the NIR as in the optical and are potentially less affected by systematic uncertainties. We extended the NIR SN Ia Hubble diagram to its nonlinear part at z∼0.2 and confirmed that it is feasible to accomplish this result with very modest sampling of the NIR LCs, if complemented by well-sampled optical LCs. With future facilities it will be possible to extend the NIR Hubble diagram beyond redshift z~=1, and our results suggest that the most efficient way to achieve this would be to obtain a single observation close to the NIR maximum. Description: NIR J-J and H-H K-corrections from MKO to MKO, CSP and 2MASS photometric system s for several redshifts and phases between -16 and +40 days. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file hmko-2m.dat 232 57 NIR H-H K-corrections from MKO to 2MASS photometric systems hmko-csp.dat 232 57 NIR H-H K-corrections from MKO to CSP photometric systems hmko-mko.dat 232 57 NIR H-H K-corrections from MKO to MKO photometric systems jmko-2m.dat 232 57 NIR J-J K-corrections from MKO to 2MASS photometric systems jmko-csp.dat 232 57 NIR J-J K-corrections from MKO to CSP photometric systems jmko-mko.dat 232 57 NIR J-J K-corrections from MKO to MKO photometric systems kcorerr.dat 150 6 K-correction errors
See also: J/A+A/611/A68 : 3D correction in 5 photometric systems (Bonifacio+, 2018) J/A+AS/122/399 : K and evolutionary corrections (Poggianti, 1997) Byte-by-byte Description of file (# headlines): [hj]*.dat
Bytes Format Units Label Explanations
1- 3 I3 d Phase [-16/40] Supernova phase from -16 day to +40 day 7- 12 F6.3 mag Kcor1 K-correction for z=0.003 (1) 17- 22 F6.3 mag Kcor2 K-correction for z=0.005 (1) 27- 32 F6.3 mag Kcor3 K-correction for z=0.007 (1) 37- 42 F6.3 mag Kcor4 K-correction for z=0.010 (1) 47- 52 F6.3 mag Kcor5 K-correction for z=0.015 (1) 57- 62 F6.3 mag Kcor6 K-correction for z=0.020 (1) 67- 72 F6.3 mag Kcor7 K-correction for z=0.025 (1) 77- 82 F6.3 mag Kcor8 K-correction for z=0.030 (1) 87- 92 F6.3 mag Kcor9 K-correction for z=0.035 (1) 97-102 F6.3 mag Kcor10 K-correction for z=0.040 (1) 107-112 F6.3 mag Kcor11 K-correction for z=0.045 (1) 117-122 F6.3 mag Kcor12 K-correction for z=0.050 (1) 127-132 F6.3 mag Kcor13 K-correction for z=0.055 (1) 137-142 F6.3 mag Kcor14 K-correction for z=0.060 (1) 147-152 F6.3 mag Kcor15 ? K-correction for z=0.070 (1) 157-162 F6.3 mag Kcor16 ? K-correction for z=0.080 (1) 167-172 F6.3 mag Kcor17 ? K-correction for z=0.090 (1) 177-182 F6.3 mag Kcor18 ? K-correction for z=0.100 (1) 187-192 F6.3 mag Kcor19 ? K-correction for z=0.110 (1) 197-202 F6.3 mag Kcor20 ? K-correction for z=0.120 (1) 207-212 F6.3 mag Kcor21 ? K-correction for z=0.130 (1) 217-222 F6.3 mag Kcor22 ? K-correction for z=0.140 (1) 227-232 F6.3 mag Kcor23 ? K-correction for z=0.171 (1)
Note (1): Typical error on Kcorrection in kcorerr.dat file.
Byte-by-byte Description of file (# headlines): kcorerr.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Table Table name 14- 18 F5.3 mag eKcor0.003 K-correction error for z=0.003 20- 24 F5.3 mag eKcor0.005 K-correction error for z=0.005 26- 30 F5.3 mag eKcor0.007 K-correction error for z=0.007 32- 36 F5.3 mag eKcor0.010 K-correction error for z=0.010 38- 42 F5.3 mag eKcor0.015 K-correction error for z=0.015 44- 48 F5.3 mag eKcor0.020 K-correction error for z=0.020 50- 54 F5.3 mag eKcor0.025 K-correction error for z=0.025 56- 60 F5.3 mag eKcor0.030 K-correction error for z=0.030 62- 66 F5.3 mag eKcor0.035 K-correction error for z=0.035 68- 72 F5.3 mag eKcor0.040 K-correction error for z=0.040 74- 78 F5.3 mag eKcor0.045 K-correction error for z=0.045 80- 84 F5.3 mag eKcor0.050 K-correction error for z=0.050 86- 90 F5.3 mag eKcor0.055 K-correction error for z=0.055 92- 96 F5.3 mag eKcor0.060 ? K-correction error for z=0.060 98-102 F5.3 mag eKcor0.070 ? K-correction error for z=0.070 104-108 F5.3 mag eKcor0.080 ? K-correction error for z=0.080 110-114 F5.3 mag eKcor0.090 ? K-correction error for z=0.090 116-120 F5.3 mag eKcor0.100 ? K-correction error for z=0.100 122-126 F5.3 mag eKcor0.110 ? K-correction error for z=0.110 128-132 F5.3 mag eKcor0.120 ? K-correction error for z=0.120 134-138 F5.3 mag eKcor0.130 ? K-correction error for z=0.130 140-144 F5.3 mag eKcor0.140 ? K-correction error for z=0.140 146-150 F5.3 mag eKcor0.171 ? K-correction error for z=0.171
Acknowledgements: Vallery Stanishev, vallery.stanishev(at)gmail.com
(End) Patricia Vannier [CDS] 02-May-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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