J/ApJ/938/83 Multiepoch opt. obs. of 91T/99aa-like SNe Ia (Yang+, 2022)
Using 1991T/1999aa-like Type Ia supernovae as standardizable candles.
Yang J., Wang L., Suntzeff N., Hu L., Aldoroty L., Brown P.J.,
Krisciunas K., Arcavi I., Burke J., Galbany L., Hiramatsu D.,
Hosseinzadeh G., Howell D.A., McCully C., Pellegrino C., Valenti S.
<Astrophys. J., 938, 83 (2022)>
=2022ApJ...938...83Y 2022ApJ...938...83Y
ADC_Keywords: Supernovae; Photometry; Optical; Redshifts
Keywords: Supernovae ; Type Ia supernovae
Abstract:
We present the photometry of 16 91T/99aa-like Type Ia Supernovae
(SNeIa) observed by the Las Cumbres Observatory. We also use an
additional set of 21 91T/99aa-like SNe Ia and 87 normal SNe Ia from
the literature for an analysis of the standardizability of the
luminosity of 91T/99aa-like SNe. We find that 91T/99aa-like SNe are
0.2mag brighter than normal SNe Ia, even when fully corrected by the
light-curve shapes and colors. The weighted rms of the 91T/99aa-like
SNe (with zCMB>0.01) Hubble residuals is 0.25±0.03mag, suggesting
that 91T/99aa-like SNe are also excellent relative distance indicators
to ±12%. We compare the Hubble residuals with the pseudo-equivalent
width (pEW) of SiIIλλ6355 around the date of maximum
brightness. We find that there is a broken linear correlation between
those two measurements for our sample including both 91T/99aa-like and
normal SNe Ia. As the pEWmax(SiIIλλ6355) increases,
the Hubble residual increases when
pEWmax(SiIIλλ6355)<55.6Å. However, the Hubble
residual stays constant beyond this. Given that 91T/99aa-like SNe
possess shallower SiII lines than normal SNe Ia, the linear
correlation at pEWmax(SiIIλλ6355)<55.6Å can account
for the overall discrepancy of Hubble residuals derived from the two
subgroups. Such a systematic effect needs to be taken into account
when using SNe Ia to measure luminosity distances.
Description:
The general properties of our 16 Las Cumbres Observatory 91T/99aa-like
supernovae are given in Table 1.
The Las Cumbres Observatory (LCO) operates a fleet of 1m class
telescopes distributed around the globe. The Las Cumbres Observatory
magnitudes presented here are based on the Vega standard system for B
and V, and the Sloan BD17 system for g'r'i' commonly called AB
magnitudes. Photometry in U and R filters without color term
corrections and S-corrections is also provided in Table 5 for
completeness. See Section 2.1.1.
To supplement our 91T/99aa-like SNe sample, we gathered all SNe Ia
that are classified as 91T/99aa-like from at least one source and
have at least one B-band data point in the Open Supernova Catalogue
(Guillochon+ 2017ApJ...835...64G 2017ApJ...835...64G). See Section 2.1.3.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 103 16 General properties of Las Cumbres 91T/99aa-like
supernovae
table2.dat 65 22 General properties of 91T/99aa-like SNe Ia in
the literature
table3.dat 49 3810 *Las Cumbres 91T/99aa-like SNe photometry in
natural systems
table4.dat 35 3810 Las Cumbres 91T/99aa-like SNe photometry in
standard systems using S-corrections;
See Section 2.2
table5.dat 49 150 Las Cumbres 91T/99aa-like SNe photometry in UR bands
table7.dat 158 36 *Parameters of 91T/99aa-like SNe Ia in our sample
table8.dat 160 87 Parameters of normal SNe Ia in our sample
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Note on table3.dat: Photometric coefficients appropriate to the Las Cumbres
Observatory 1m telescopes (see Table B1 in Valenti+ 2016MNRAS.459.3939V 2016MNRAS.459.3939V)
were used to convert APASS catalog magnitudes to values in the Las
Cumbres Observatory natural system. We use the color terms to convert
the APASS magnitude to Las Cumbres Observatory natural system
magnitude as follows:
mnat=mAPASS+C*color (Equation (1))
where mnat is the natural system magnitude, mAPASS is the APASS
magnitude, and C and "color" are the appropriate color term and color
for each filter. See Section 2.1.1.
Note on table7.dat: For SN 2018apo we do not have B-band photometry, so the
maximum date was determined using g-band photometry and the SN is not
included in Figure 6 or in Table 7.
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See also:
J/AJ/131/527 : UBVRI light curves of 44 type Ia supernovae (Jha+, 2006)
J/ApJ/700/331 : Light curves of type Ia supernovae (CfA3) (Hicken+, 2009)
J/ApJ/699/L139 : Spectral parameters of SNe Ia (Wang+, 2009)
J/ApJS/190/418 : Light curves for 165 SNe (Ganeshalingam+, 2010)
J/A+A/523/A7 : Light curves of type Ia supernovae in SNLS (Guy+, 2010)
J/ApJ/722/566 : Host galaxies of SNIa in SDSS-II SN survey (Lampeitl+, 2010)
J/MNRAS/406/782 : Type Ia supernovae luminosities (Sullivan+, 2010)
J/ApJ/740/92 : SN.Ia host galaxies properties (Gupta+, 2011)
J/AJ/143/126 : Spectroscopy of nearby Type Ia supernovae (Blondin+, 2012)
J/ApJS/200/12 : CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)
J/MNRAS/425/1789 : Berkeley supernova Ia program. I. (Silverman+, 2012)
J/MNRAS/435/1680 : SN Ia host galaxy properties (Johansson+, 2013)
J/A+A/568/A22 : Joint analysis of SDSS-II and SNLS SNe Ia (Betoule+, 2014)
J/ApJ/813/30 : UV-Opt light curves of the SNIa iPTF14bdn (Smitka+, 2015)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/AJ/154/211 : The CSP (DR3): phot. of low-z SNe Ia (Krisciunas+, 2017)
J/MNRAS/475/193 : Foundation Supernova Survey 1st data release (Foley+, 2018)
J/ApJ/869/167 : Improved empirical models for Type Ia SNe (Saunders+, 2018)
J/ApJ/876/85 : HST observations for LMC Cepheids (Riess+, 2019)
J/MNRAS/499/1424 : Properties of 407 SNe and their 394 hosts (Hakobyan+, 2020)
J/A+A/636/A46 : The SUGAR model. Training dataset (Leget+, 2020)
J/ApJ/902/46 : LCO network light curves of SN Ia 2018gv (Yang+, 2020)
J/ApJ/930/70 : A compilation of optical spectra from 361 SNe Ia (Hu+, 2022)
http://www.wis-tns.org/ : Transient Name Server (TNS) homepage
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Supernova name
11- 12 I2 h RAh Hour of right ascension (J2000) (1)
14- 15 I2 min RAm Minute of right ascension (J2000)
17- 21 F5.2 s RAs Second of right ascension (J2000)
23 A1 --- DE- Sign of declination (J2000) (1)
24- 25 I2 deg DEd Degree of declination (J2000) (1)
27- 28 I2 arcmin DEm Arcminute of declination (J2000)
30- 33 F4.1 arcsec DEs Arcsecond of declination (J2000)
35- 62 A28 --- Gal Host galaxy name (1)
64- 71 F8.6 --- zHelio [0.011/0.06] Host-galaxy heliocentric redshift
from NED or TNS unless flagged
73 A1 --- r_zHelio [c] c: From Phillips+ 2019PASP..131a4001P 2019PASP..131a4001P
75- 88 A14 --- DiscRef Discovery reference
90-103 A14 --- SpRef Spectroscopic reference
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Note (1): Basic information for each SN, including its J2000 R.A. and decl.,
and its host galaxy, were sourced from TNS or the discovery references.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Supernova name
11- 34 A24 --- Gal Host galaxy name
36- 42 F7.5 --- zHelio Heliocentric redshift from the NED unless
indicated otherwise
44 A1 --- r_zHelio Reference for zHelio (1)
46- 55 A10 --- PhotRef Photometry reference(s) (1)
57- 65 A9 --- ClRef Classification reference (1)
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Note (1): Reference as follows:
1 = Lira et al. (1998AJ....115..234L 1998AJ....115..234L)
2 = Riess et al. (1999AJ....117..707R 1999AJ....117..707R)
3 = Altavilla et al. (2004MNRAS.349.1344A 2004MNRAS.349.1344A)
4 = Jha et al. (2006, J/AJ/131/527)
5 = Ganeshalingam et al. (2010, J/ApJS/190/418)
6 = Hicken et al. (2009, J/ApJ/700/331)
7 = Blondin et al. (2012, J/AJ/143/126)
8 = Strolger et al. (2002AJ....124.2905S 2002AJ....124.2905S)
9 = Blondin et al. 2012, J/AJ/143/126
10 = Silverman et al. (2012, J/MNRAS/425/1789)
11 = Krisciunas et al. (2017, J/AJ/154/211)
12 = Brown et al. (2014Ap&SS.354...89B 2014Ap&SS.354...89B)
13 = Zhang et al. (2016ApJ...817..114Z 2016ApJ...817..114Z)
14 = Stahl et al. (2019MNRAS.490.3882S 2019MNRAS.490.3882S)
15 = Foley et al. (2018, J/MNRAS/475/193)
16 = Baltay et al. (2021PASP..133d4002B 2021PASP..133d4002B)
17 = Smitka et al. (2015, J/ApJ/813/30)
IAUC 5239 = 1991IAUC.5239....1W 1991IAUC.5239....1W
IAUC 6278 = 1995IAUC.6278....1P 1995IAUC.6278....1P
IAUC 7054 = 1998IAUC.7054....2J 1998IAUC.7054....2J
IAUC 7108 = 1999IAUC.7108....2F 1999IAUC.7108....2F & 1999IAUC.7108....1A 1999IAUC.7108....1A
IAUC 7122 = 1999IAUC.7122....2P 1999IAUC.7122....2P & 1999IAUC.7122....3K 1999IAUC.7122....3K
IAUC 7250 = 1999IAUC.7250....1J 1999IAUC.7250....1J
IAUC 8474 = 2005IAUC.8474....4T 2005IAUC.8474....4T
CBET 839 = 2007CBET..839....1B 2007CBET..839....1B
CBET 2901 = 2011CBET.2901....1N 2011CBET.2901....1N & 2011CBET.2901....2Z 2011CBET.2901....2Z
ATEL 9720 = 2016ATel.9702....1W 2016ATel.9702....1W
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Supernova identifier
11- 11 A1 --- Filt Filter used (B,V,g,r,i)
13- 22 F10.4 d MJD [56929.38/58931.75] Modified Julian Date
24- 29 F6.3 mag mag [14.38/22.22] Apparent magnitude in Filter
31- 35 F5.3 mag e_mag [0.015/0.8] Uncertainty in mag
37- 49 A13 --- Inst Site, Telescope and Instrument information (G1)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Supernova identifier
11- 11 A1 --- Filt Filter used (B,V,g,r,i)
13- 22 F10.4 d MJD [56929.38/58931.75] Modified Julian Date
24- 29 F6.3 mag mag [14.36/22.2] Apparent magnitude in Filt
31- 35 F5.3 mag e_mag [0.025/0.8] Uncertainty in mag
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova identifier
11- 11 A1 --- Filt Filter used (U,R)
13- 22 F10.4 d MJD [58287.36/58931.74] Modified Julian Date
24- 29 F6.3 mag mag [13.88/18.8] Apparent magnitude in Filter
31- 35 F5.3 mag e_mag [0.02/1.01] Uncertainty in mag
37- 49 A13 --- Inst Site, Telescope and Instrument information (G1)
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Supernova identifier
11 I1 --- f_Name [0/8]? Subtype flag on Name (G2)
13- 18 F6.4 --- zCMB [0.0069/0.06] CMB frame redshift
20- 23 F4.1 0.1nm pEW [4.5/80.4]? SiII 6355Å equivalent width near
maximum; Angstroms
25- 28 F4.2 mag E(B-V) [0.01/0.5] Host galaxy B-V color excess
30- 33 F4.2 mag e_E(B-V) [0.01/0.06] Uncertainty in E(B-V)
35- 39 F5.2 mag HRes [-2/0.5] Hubble residual
41- 44 F4.2 mag e_HRes [0.29/0.5] Uncertainty in HRes
46- 53 F8.2 d tMaxB [48375.5/58830.9] Modified Julian Date of B
band maximum
55- 58 F4.2 d e_tMaxB [0.03/1.01] Uncertainty in tMaxB
60- 63 F4.2 mag Delm15B [0.68/1.2] Decline in B band after 15 days
65- 68 F4.2 mag e_Delm15B [0.01/0.4] Uncertainty in Delm15B
70- 74 F5.2 mag maxB [11.6/17.77] B band magnitude at maximum
76- 79 F4.2 mag e_maxB [0/0.05] Uncertainty in maxB
81- 85 F5.2 --- PC1B [-1.9/1.96] First B band principle component
parameter
87- 90 F4.2 --- e_PC1B [0.05/6.5] Uncertainty in PC1B
92- 96 F5.2 --- PC2B [-1.1/0.24] Second B band principle component
parameter
98- 101 F4.2 --- e_PC2B [0.03/3.8] Uncertainty in PC2B
103- 110 F8.2 d tMaxV [48378.19/58832.31] Modified Julian Date of V
band maximum
112- 115 F4.2 d e_tMaxV [0.05/0.8] Uncertainty in tMaxV
117- 120 F4.2 mag Delm15V [0.5/0.73] Decline in V band after 15 days
122- 125 F4.2 mag e_Delm15V [0.01/0.08] Uncertainty in Delm15V
127- 131 F5.2 mag maxV [11.41/17.51] V band magnitude at maximum
133- 136 F4.2 mag e_maxV [0/0.04] Uncertainty in maxV
138- 142 F5.2 --- PC1V [-1.42/1.1] First V band principle component
parameter
144- 147 F4.2 --- e_PC1V [0.04/1.7] Uncertainty in PC1V
149- 153 F5.2 --- PC2V [-0.32/0.5] Second V band principle component
parameter
155- 158 F4.2 --- e_PC2V [0.02/0.9] Uncertainty in PC2V
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova identifier
11 A1 --- f_Name ? Subtype flag on Name (G2)
13- 18 F6.4 --- zCMB [0.0014/0.062] CMB frame redshift
20- 24 F5.1 0.1nm pEW [28.6/136.6]? SiII 6355 equivalent width near
maximum; Angstroms
26- 30 F5.2 mag E(B-V) [-0.05/1.3] Host galaxy B-V color excess
32- 35 F4.2 mag e_E(B-V) [0.01/0.11] Uncertainty in E (B-V)
37- 41 F5.2 mag HRes [-0.73/1.16] Hubble residual
43- 46 F4.2 mag e_HRes [0.1/0.8] Uncertainty in HRes
48- 55 F8.2 d tMaxB [51029.19/58149.54] Modified Julian Date of B
band maximum
57- 60 F4.2 d e_tMaxB [0.02/1.21] Uncertainty in tMaxB
62- 65 F4.2 mag Delm15B [0.66/2.1] Decline in B band after 15 days
67- 70 F4.2 mag e_Delm15B [0.01/0.32] Uncertainty in Delm15B
72- 76 F5.2 mag maxB [9.89/18.11] B band magnitude at maximum
78- 81 F4.2 mag e_maxB [0/0.09] Uncertainty in maxB
83- 87 F5.2 --- PC1B [-2/5] First B band principle component
parameter
89- 92 F4.2 --- e_PC1B [0/6.6] Uncertainty in PC1B
94- 98 F5.2 --- PC2B [-2/1.9] Second B band principle component
parameter
100- 103 F4.2 --- e_PC2B [0.02/4.8] Uncertainty in PC2B
105- 112 F8.2 d tMaxV [51031.57/58151.59] Modified Julian Date of V
band maximum
114- 117 F4.2 d e_tMaxV [0.03/1] Uncertainty in tMaxV
119- 122 F4.2 mag Delm15V [0.46/1.4] Decline in V band after 15 days
124- 127 F4.2 mag e_Delm15V [0.01/0.22] Uncertainty in Delm15V
129- 133 F5.2 mag maxV [9.9/17.91] V band magnitude at maximum
135- 138 F4.2 mag e_maxV [0/0.06] Uncertainty in maxV
140- 144 F5.2 --- PC1V [-2/5] First V band principle component
parameter
146- 149 F4.2 --- e_PC1V [0/2.7] Uncertainty in PC1V
151- 155 F5.2 --- PC2V [-0.97/0.61] Second V band principle component
parameter
157- 160 F4.2 --- e_PC2V [0.02/1.2] Uncertainty in PC2V
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Global notes:
Note (G1): Las Cumbres Observatory (LCO) site are:
coj = Siding Spring, Australia
cpt = Sutherland, South Africa
elp = McDonald, Texas
lsc = Cerro Tololo, Chile
Note (G2): The classification is the floor hexadecimal integer of pEW/10
(see subsection 5.3 for more details).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Aug-2024