J/MNRAS/483/5459 SNe II as distance indicators at near-IR (Rodriguez+, 2019) ================================================================================ Type II supernovae as distance indicators at near-IR wavelengths. Rodriguez O., Pignata G., Hamuy M., Clocchiatti A., Phillips M.M., Krisciunas K., Morrell N.I., Folatelli G., Roth M., Castellon S., Jang I.S., Apostolovski Y., Lopez P., Marchi S., Ramirez R., Sanchez P. =2019MNRAS.483.5459R (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Supernovae ; Galaxies ; Redshifts Keywords: supernovae: general - galaxies: distances and redshifts - distance scale Abstract: Motivated by the advantages of observing at near-IR wavelengths, we investigate Type II supernovae (SNe II) as distance indicators at those wavelengths through the Photospheric Magnitude Method (PMM). For the analysis, we use BVIJH photometry and optical spectroscopy of 24 SNe II during the photospheric phase. To correct photometry for extinction and redshift effects, we compute total-to-selective broad-band extinction ratios and K-corrections up to z=0.032. To estimate host galaxy colour excesses, we use the colour-colour curve method with the V-I versus B-V as colour combination. We calibrate the PMM using four SNe II in galaxies having Tip of the Red Giant Branch distances. Among our 24 SNe II, nine are at cz>2000km/s, which we use to construct Hubble diagrams (HDs). To further explore the PMM distance precision, we include into HDs the four SNe used for calibration and other two in galaxies with Cepheid and SN Ia distances. With a set of 15 SNe II we obtain an HD rms of 0.13mag for the J-band, which compares to the rms of 0.15-0.26mag for optical bands. This reflects the benefits of measuring PMM distances with near-IR instead of optical photometry. With the evidence we have, we can set the PMM distance precision with J-band below 10 per cent with a confidence level of 99 per cent. Description: We base our work on data obtained over the course of the Carnegie Type II Supernova Survey (CATS; PI: Hamuy, 2002-2003), a program whose main objective was to study nearby (z<0.05) SNe II. Optical photometry and spectroscopy, along with some near-IR photometry, were obtained with the 1-m Swope, 2.5-m du Pont, and 6.5-m Magellan Baade and Clay telescopes at Las Campanas Observatory. A few additional optical images were obtained with the 0.9-m and 1.5-m telescopes at Cerro Tololo Inter-American Observatory. During the CATS survey, 34 SNe II were observed. Optical photometry and spectroscopy of these SNe II, along with the description of the data reduction, is presented in Galbany et al. (2016AJ....151...33G, Cat. J/AJ/151/33) and Gutierrez et al. (2017ApJ...850...89G), respectively. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablef3.dat 134 24 SN II parameters tablef4.dat 138 24 CMB redshifts and PMM distance moduli tablef5.dat 38 46 SN II spectra library tablef6.dat 108 56 SNID templates -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablef3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 A9 --- Name Supernova name (SN YYYYAA) 11- 16 F6.3 mag B-V Host galaxy colour excesses estimated with the V-I versus B-V colour-colour curve 18- 22 F5.3 mag E_B-V Upper error on B-V (80 per cent confidence interval) 24- 28 F5.3 mag e_B-V Lower error on B-V (80 per cent confidence interval) 30- 34 F5.3 mag rmsB-V rms uncertainty on B-V 36- 40 F5.3 mag B-VO10 ? Host galaxy colour excesses from Olivares et al. (2010ApJ...715..833O) recalibrated by Rodriguez et al. (2014AJ....148..107R) 42- 46 F5.3 mag rmsB-VO10 ? rms uncertainty on BVO10 48- 58 F11.3 d JD Date of the discovery 60- 67 F8.3 d tln ? Last non detection epoch (1) 69 A1 --- f_tln [a] Flag on tln (2) 71- 76 F6.3 d tfd First detection epoch (1) 78 A1 --- f_tfd [a] Flag on tfd (2) 80- 85 F6.2 d t0SNID ? Explosion epoch estimated with SNID without any prior 87- 90 F4.2 d rmst0SNID ? rms uncertainty on t0SNID 92 A1 --- f_t0SNID [b] Flag on t0SNID (3) 94- 99 F6.2 d t0final Explosion epoch estimated with our SN II template library with photometric priors 101-104 F4.2 d E_t0final Upper error on t0final 106-109 F4.2 d e_t0final Lower error on t0final 111-134 A24 --- Ref References for Jd, tln and tfd (4) -------------------------------------------------------------------------------- Note (1): Epochs with respect to the discovery epoch Note (2): Flag as follows: a = Value obtained through polynomial fits to pre-maximum VRI photometry Note (3): Flag as follows: b = Optical spectra not published Note (4): References as follows: E03: Elmhamdi et al. (2003MNRAS.338..939E) P09: Pastorello et al. (2009MNRAS.394.2266P, Cat. J/MNRAS/394/2266) R11: Roy et al. (2011ApJ...736...76R) F11: Fraser et al. (2011MNRAS.417.1417F) CF: C. Feliciano report on the Bright Supernova website (http://www.rochesterastronomy.org/snimages/) -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablef4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 A14 --- Host Host galaxy 16- 19 I4 km/s czCMB CMB redshift 21- 23 I3 km/s e_czCMB Error on czCMB 25- 33 A9 --- Name Supernova name (SN YYYYAA) 35- 39 F5.2 mag muB B-band distance modulus obtained with the Photospheric Magnitude Method 41- 44 F4.2 mag E_muB Upper error on muB (80 per cent confidence interval) 46- 49 F4.2 mag e_muB Lower error on muB (80 per cent confidence interval) 51- 54 F4.2 mag rmsmuB rms uncertainty on muB 56- 60 F5.2 mag muV V-band distance modulus obtained with the Photospheric Magnitude Method 62- 65 F4.2 mag E_muV Upper error on muV (80 per cent confidence interval) 67- 70 F4.2 mag e_muV Lower error on muV (80 per cent confidence interval) 72- 75 F4.2 mag rmsmuV rms uncertainty on muV 77- 81 F5.2 mag muI I-band distance modulus obtained with the Photospheric Magnitude Method 83- 86 F4.2 mag E_muI Upper error on muI (80 per cent confidence interval) 88- 91 F4.2 mag e_muI Lower error on muI (80 per cent confidence interval) 93- 96 F4.2 mag rmsmuI rms uncertainty on muI 98-102 F5.2 mag muJ J-band distance modulus obtained with the Photospheric Magnitude Method 104-107 F4.2 mag E_muJ Upper error on muJ (80 per cent confidence interval) 109-112 F4.2 mag e_muJ Lower error on muJ (80 per cent confidence interval) 114-117 F4.2 mag rmsmuJ rms uncertainty on muJ 119-123 F5.2 mag muH H-band distance modulus obtained with the Photospheric Magnitude Method 125-128 F4.2 mag E_muH Upper error on muH (80 per cent confidence interval) 130-133 F4.2 mag e_muH Lower error on muH (80 per cent confidence interval) 135-138 F4.2 mag rmsmuH rms uncertainty on muH -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablef5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 A9 --- Name Supernova name (SN YYYYAA) 11 A1 --- f_Name [c] Flag on Name (1) 13- 17 F5.3 mag B-VG Galactic coulour excess from Schlafly & Finkbeiner (2011ApJ...737..103S) 19- 22 I4 km/s czhelio Heliocentric SN redshift 24- 29 F6.3 mag B-Vh Host galaxy colour excess computed in this work 31- 38 A8 --- Ref References (2) -------------------------------------------------------------------------------- Note (1): Flag a follows: c = SN with useful near-IR spectra Note (2): References as follows: 1 = Schmidt et al. (1993AJ....105.2236S) 2 = Gutierrez et al. (2017ApJ...850...89G) 3 = Inserra et al. (2013A&A...555A.142I, Cat. J/A+A/555/A142) 4 = Pastorello et al. (2004MNRAS.347...74P) 5 = Faran et al. (2014MNRAS.442..844F, Cat. J/MNRAS/442/844) 6 = Faran et al. (2014MNRAS.445..554F) 7 = Spiro et al. (2014MNRAS.439.2873S) 8 = Pastorello et al. (2006MNRAS.370.1752P) 9 = Pastorello et al. (2009MNRAS.394.2266P, Cat. J/MNRAS/394/2266) 10 = Takats et al. (2014MNRAS.438..368T) 11 = Takats et al. (2015MNRAS.450.3137T, Cat. J/MNRAS/450/3137) 12 = Dall'Ora et al. (2014ApJ...787..139D) 13 = Barbarino et al. (2015MNRAS.448.2312B) 14 = Valenti et al. (2014MNRAS.438L.101V, Cat. J/MNRAS/438/L101) 15 = Dhungana et al. (2016ApJ...822....6D) 16 = Yuan et al. (2016MNRAS.461.2003Y, Cat. J/MNRAS/461/2003) 17 = Terreran et al. (2016MNRAS.462..137T) -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablef6.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- Name Supernova name (SN YYYYAA) except LSQ14gv 9 A1 --- f_Name Flag on Name (1) 11- 21 F11.3 d td Discovery epoch 23- 29 F7.3 d tln-td Last non detection with respect to the discovery epoch 31- 37 F7.3 d tfd-td First detection with respect to the discovery epoch 39- 73 A35 d t-t0ln Spectra phase values with respect to the explosion epoch (2) 75-108 A34 --- Ref References for data (3) -------------------------------------------------------------------------------- Note (1): Flag as follows: a = Explosion time constraint obtained through polynomial fit to pre-maximum VRI photometry Note (2): We assume the spectra phase as the midpoint between the last non-detection and the first detection. Adjacent ages are listed in brackets Note (3): References as follows: 1 = Gutierrez et al. (2017ApJ...850...89G) 2 = Schmidt et al. (1993AJ....105.2236S) 3 = Pastorello et al. (2004MNRAS.347...74P) 4 = Elmhamdi et al. (2003MNRAS.338..939E) 5 = Faran et al. (2014MNRAS.442..844F, Cat. J/MNRAS/442/844) 6 = Shivvers et al. (2017PASP..129e4201S) 7 = Faran et al. (2014MNRAS.445..554F) 8 = Hicken et al. (2017ApJS..233....6H, Cat. J/ApJS/233/6) 9 = Harutyunyan et al. (2008A&A...488..383H) 10 = Spiro et al. (2014MNRAS.439.2873S) 11 = Sahu et al. (2006MNRAS.372.1315S, Cat. J/MNRAS/372/1315) 12 = Gal-Yam et al. (2008ApJ...685L.117G) 13 = Pastorello et al. (2009MNRAS.394.2266P, Cat. J/MNRAS/394/2266) 14 = Pastorello et al. (2006MNRAS.370.1752P) 15 = Quimby et al. (2007ApJ...666.1093Q) 16 = Sako et al. (2018PASP..130f4002S, Cat. II/333) 17 = Inserra et al. (2013A&A...555A.142I, , Cat. J/A+A/555/A142) 18 = Gal-Yam et al. (2011ApJ...736..159G, Cat. J/ApJ/736/159) 19 = Dall'Ora et al. (2014ApJ...787..139D) 20 = Tomasella et al. (2018MNRAS.475.1937T) 21 = Zhang et al. (2014ApJ...797....5Z) 22 = Valenti et al. (2015MNRAS.448.2608V, Cat. J/MNRAS/448/2608) 23 = Valenti et al. (2014MNRAS.438L.101V, Cat. J/MNRAS/438/L101) 24 = Childress et al. (2016PASA...33...55C) 25 = Dhungana et al. (2016ApJ...822....6D) 26 = Yuan et al. (2016MNRAS.461.2003Y, Cat. J/MNRAS/461/2003) 27 = Yaron et al. (2017NatPh..13..510Y) 28 = Terreran et al. (2016MNRAS.462..137T) 29 = Valenti et al. (2016MNRAS.459.3939V, Cat. J/MNRAS/459/3939) CF = C. Feliciano report on the Bright Supernova website (http://www.rochesterastronomy.org/snimages/) -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Ana Fiallos [CDS] 04-Aug-2022