J/ApJ/830/13 Host-galaxy NUV-NIR data of 32 superluminous SNe (Perley+, 2016)
Host-galaxy properties of 32 low-redshift superluminous supernovae from the
Palomar Transient Factory.
Perley D.A., Quimby R.M., Yan L., Vreeswijk P.M., De Cia A., Lunnan R.,
Gal-Yam A., Yaron O., Filippenko A.V., Graham M.L., Laher R., Nugent P.E.
<Astrophys. J., 830, 13-13 (2016)>
=2016ApJ...830...13P 2016ApJ...830...13P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Supernovae ; Photometry, SDSS ; Redshifts ;
Photometry, infrared ; Photometry, HST ; Abundances
Keywords: galaxies: abundances; galaxies: dwarf; galaxies: photometry;
supernovae: general
Abstract:
We present ultraviolet through near-infrared photometry and
spectroscopy of the host galaxies of all superluminous supernovae
(SLSNe) discovered by the Palomar Transient Factory prior to 2013 and
derive measurements of their luminosities, star formation rates,
stellar masses, and gas-phase metallicities. We find that Type I
(hydrogen-poor) SLSNe (SLSNe I) are found almost exclusively in
low-mass (M*<2x109M☉) and metal-poor (12+log10[O/H]<8.4)
galaxies. We compare the mass and metallicity distributions of our
sample to nearby galaxy catalogs in detail and conclude that the rate
of SLSNe I as a fraction of all SNe is heavily suppressed in galaxies
with metallicities ≳0.5Z☉. Extremely low metallicities are not
required and indeed provide no further increase in the relative SLSN
rate. Several SLSN I hosts are undergoing vigorous starbursts, but
this may simply be a side effect of metallicity dependence: dwarf
galaxies tend to have bursty star formation histories. Type II
(hydrogen-rich) SLSNe (SLSNe II) are found over the entire range of
galaxy masses and metallicities, and their integrated properties do
not suggest a strong preference for (or against)
low-mass/low-metallicity galaxies. Two hosts exhibit unusual
properties: PTF 10uhf is an SLSN I in a massive, luminous infrared
galaxy at redshift z=0.29, while PTF 10tpz is an SLSN II located in
the nucleus of an early-type host at z=0.04.
Description:
The superluminous supernovae (SLSNe) in the PTF sample were targeted
for late-time imaging in a variety of wavebands spanning the near-UV
to the NIR. Several host galaxies were bright enough to be well
recovered in SDSS (at least in the gri filters). For fainter hosts and
for other filters we observed with other facilities: the Palomar
60-inch (P60) telescope imaging camera, the Large Format Camera or the
Wide-Field Infrared Camera (WIRC) on the Palomar 5-m Hale telescope,
or the Low-Resolution Imaging Spectrometer (LRIS) or the Multi-Object
Spectrometer for Infrared Exploration (MOSFIRE) on the Keck I 10m
telescope.
All ground-based images used for the host-galaxy spectral energy
distribution (SED) analysis were acquired either pre-explosion or long
after the SN peak time (at least 2yr, typically 3-4yr).
Several host galaxies of slowly declining (Type I-R) hydrogen-poor
SLSNe were observed with HST as part of our team's approved programs
(GO-12983, PI O. Yaron; GO-13858, PI A. De Cia).
Some of our HST observations were conducted within 1-2yr after the SN
in order to follow the late-time evolution of the light curve, and the
SN is still clearly detected.
Additional UV and NIR observations of various events in the sample
(PTF 09atu, PTF 09cnd, PTF 09cwl, PTF 11dij, PTF 11dsf, PTF 11rks)
were obtained as part of programs GO-13025 and GO-13480 (PI A. Levan).
Several host galaxies in our sample were observed with IRAC on the
Spitzer Space Telescope during Cycle 10 (GO-10056, PI R. Lunnan).
Spectra were obtained for most host galaxies within the sample using
LRIS on the Keck I telescope (continuous coverage between the near-UV
and 10300Å; spanning 2012 Jul - 2016 Jan - see table 3).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 104 32 Superluminous Supernovae from PTF
table2.dat 74 273 Photometry of SLSN hosts
table3.dat 71 39 Log of spectroscopic observations
table4.dat 115 32 Photometric properties of PTF SLSN hosts
table5.dat 149 35 Emission-line fluxes for SLSN hosts
table6.dat 255 32 Emission-line diagnostics for SLSN hosts
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
II/328 : AllWISE Data Release (Cutri+ 2013)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
J/ApJ/828/3 : The superluminous SNI ASASSN-15lh with Swift (Brown+, 2016)
J/ApJ/819/35 : LCs of four transients from PTF + SNLS (Arcavi+, 2016)
J/MNRAS/448/1206 : Superluminous supernovae in faint galaxies (McCrum+, 2015)
J/MNRAS/445/899 : LVL SEDs and physical properties (Cook+, 2014)
J/MNRAS/445/881 : LVL global optical photometry (Cook+, 2014)
J/other/Nat/491.228 : Light curves of 2 superluminous supernovae (Cooke+, 2012)
J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)
J/other/Nat/474.484 : Ligth curves of 4 supernovae (Quimby+, 2011)
J/ApJS/192/6 : A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)
J/ApJ/715/506 : Aromatic inventory of the local volume (Marble+, 2010)
J/ApJ/703/517 : The Spitzer Local Volume Legacy: IR photometry (Dale+, 2009)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/ApJS/178/247 : Hα and [NII] survey in local 11 Mpc (Kennicutt+, 2008)
J/A+A/459/85 : O/H & gas densities in star-forming galaxies (Nagao+, 2006)
J/A+A/448/955 : Abundances of emission galaxies in SDSS-DR3 (Izotov+, 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF Identifier (YYaaaa)
8- 9 I2 h RAh Hour of Right Ascension (J2000) (1)
11- 12 I2 min RAm Minute of Right Ascension (J2000) (1)
14- 19 F6.3 s RAs Second of Right Ascension (J2000) (1)
21 A1 --- DE- Sign of the Declination (J2000)(1)
22- 23 I2 deg DEd Degree of Declination (J2000) (1)
25- 26 I2 arcmin DEm Arcminute of Declination (J2000) (1)
28- 32 F5.2 arcsec DEs Arcsecond of Declination (J2000) (1)
34- 36 A3 --- Class Supernova classification (15 "I", 14 "II" and
3 "I-R")
38- 43 F6.4 --- z [0.03/0.6] SN redshift
45- 46 A2 --- l_Vmag [≪ ] Limit flag on Vmag
47- 52 F6.1 mag Vmag [-23/-19] Approximate peak absolute visual
magnitude of the supernova (2)
54 A1 --- l_tpeak Limit flag on tpeak
55- 64 A10 "Y-M-D" tpeak Approximate UT date of peak visual
magnitude (2)
66- 70 F5.3 mag E(B-V) [0.008/0.5] Galactic (foreground) selective
extinction; from Schlafly+ (2011ApJ...737..103S 2011ApJ...737..103S)
72-104 A33 --- Notes Notes on object
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Note (1): Supernova position
Note (2): More refined measurements will be presented by De Cia+, in prep.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF Identifier (YYaaaa)
8- 12 A5 --- Filt Filter
14 A1 --- l_omag Limit flag on omag
16- 20 F5.2 mag omag [11.7/27.1] Magnitude, in Filt (1)
22- 25 F4.2 mag e_omag [0.04/0.6]? Uncertainty in omag
27 A1 --- l_Fnu Limit flag on Fnu
28- 35 F8.2 uJy Fnu [0.07/10326] Flux density, in Filt (2)
37- 43 F7.2 uJy e_Fnu [0.02/1257]? Uncertainty in Fnu (2)
45- 54 A10 "Y-M-D" Obs Observation date
56- 72 A17 --- Inst Instrument used
74 I1 --- Ref [1/5] Photometry reference (3)
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Note (1): Magnitudes are expressed in the conventional frame for each
relevant filter and are not corrected for foreground extinction:
ugriz = SDSS system;
BVRI = Johnson-Cousins in Vega magnitudes.
JHKs = 2MASS;
HST/Spitzer/WISE = AB magnitudes, Oke (1983ApJ...266..713O 1983ApJ...266..713O).
Note (2): Flux densities in uJy calculated from our standard magnitudes
via Fukugita (1995PASP..107..945F 1995PASP..107..945F), and corrected for
foreground extinction.
Note (3): Photometry reference as follows:
1 = This work;
2 = Angus et al. (2016MNRAS.458...84A 2016MNRAS.458...84A);
3 = Cutri et al. (2012, II/311);
4 = Lunnan et al. (2014ApJ...787..138L 2014ApJ...787..138L);
5 = ALLWISE (Cutri+ 2013, II/328).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF Identifier
8- 17 A10 "Y-M-D" Obs Observation UT date
19 A1 --- flag Observation flag (1)
21- 38 A18 --- Setup Setup (2)
40- 65 A26 --- Exp Exposure sequence (3)
67- 71 F5.1 deg PA Sky position angle (4)
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Note (1): Observation flag as follows:
d = Spectrum contains significant supernova contribution;
e = Slit centered on the SN and not aligned with the host nucleus.
Note (2): LRIS-B grism and LRIS-R grating, unless another instrument is
specified.
Note (3): Exposure sequence (seconds per exposure). Comma denotes separate
sequences for LRIS-B and LRIS-R.
Note (4): Sky position angle used for the slit. Zero = North up,
with a positive angle indicating rotation counterclockwise on the sky.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF Identifier
8- 13 F6.2 mag Mg [-22.1/-13.5] Integrated galaxy magnitude (5)
15- 15 A1 --- l_SFR Limit flag on SFR (5)
16- 21 F6.3 Msun/yr SFR [0.004/11.2]? Star formation rate (5)
23- 28 F6.3 Msun/yr E_SFR ? Upper uncertainty on SFR (5)
30- 35 F6.3 Msun/yr e_SFR ? Lower uncertainty on SFR (5)
37- 41 F5.2 [Msun] logM* [6/11.3] Stellar Galaxy Mass (5)
43- 47 F5.2 [Msun] E_logM* Upper uncertainty on logM* (5)
49- 53 F5.2 [Msun] e_logM* Lower uncertainty on logM* (5)
55- 55 A1 --- l_Av Limit flag on Av (5)
57- 60 F4.2 mag Av [0/1.6]? Total extinction (5)
62- 66 F5.2 mag E_Av ? Upper uncertainty on Av (5)
68- 72 F5.2 mag e_Av ? Lower uncertainty on Av (5)
74-115 A42 --- Morph Morphology (6)
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Note (5): Properties derived from SED fitting to the photometry in Table 2.
Uncertainties are derived from the distribution of Monte-Carlo trials
plus (for SFR and M* estimates) an additional systematic uncertainty
of 10%. An Av value of 0 with no uncertainty indicates that this
parameter was fixed.
Note (6): Informal morphological properties from visual inspection and from
estimates of the size, luminosity, and environment of each host
galaxy.
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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- 6 A6 --- PTF PTF Identifier
8- 8 A1 --- Fl [bcds] Measurement flag (7)
10- 10 A1 --- l_FHa Limit flag on FHa
11- 16 F6.1 mW/m2 FHa ? Emission line flux, Hα 6563 (8)
18- 22 F5.1 mW/m2 e_FHa ? Uncertainty in FHa (9)
24- 24 A1 --- l_FHb Limit flag on FHb
25- 30 F6.1 mW/m2 FHb ? Emission line flux, Hβ 4861 (8)
32- 35 F4.1 mW/m2 e_FHb ? Uncertainty in FHb (9)
37- 37 A1 --- l_FHg Limit flag on FHg
38- 42 F5.1 mW/m2 FHg ? Emission line flux, Hγ 4340 (8)
44- 47 F4.1 mW/m2 e_FHg ? Uncertainty in FHg (9)
49- 49 A1 --- l_F[OII]3727 Limit flag on F[OII]3727
50- 56 F7.2 mW/m2 F[OII]3727 ? Emission line flux, [O II] 3727 (8)
58- 61 F4.1 mW/m2 e_F[OII]3727 ? Uncertainty in F[OII]3727 (9)
63- 63 A1 --- l_F[OIII]4363 Limit flag on F[OIII]4363
64- 68 F5.1 mW/m2 F[OIII]4363 ? Emission line flux, [O III] 4363 (8)
70- 72 F3.1 mW/m2 e_F[OIII]4363 ? Uncertainty in F[OIII]4363 (9)
74- 74 A1 --- l_F[OIII]4959 Limit flag on F[OIII]4959
75- 80 F6.1 mW/m2 F[OIII]4959 ? Emission line flux, [O III] 4959 (8)
82- 85 F4.1 mW/m2 e_F[OIII]4959 ? Uncertainty in F[OIII]4959 (9)
87- 87 A1 --- l_F[OIII]5007 Limit flag on F[OIII]5007
88- 93 F6.1 mW/m2 F[OIII]5007 ? Emission line flux, [O III] 5007 (8)
95- 98 F4.1 mW/m2 e_F[OIII]5007 ? Uncertainty in F[OIII]5007 (9)
100-100 A1 --- l_F[NII]6548 Limit flag on F[NII]6548
101-105 F5.1 mW/m2 F[NII]6548 ? Emission line flux, [N II] 6548 (8)
107-110 F4.1 mW/m2 e_F[NII]6548 ? Uncertainty in F[NII]6548 (9)
112-112 A1 --- l_F[NII]6584 Limit flag on F[NII]6584
113-118 F6.1 mW/m2 F[NII]6584 ? Emission line flux, [N II] 6584 (8)
120-124 F5.1 mW/m2 e_F[NII]6584 ? Uncertainty in F[NII]6584 (9)
126-126 A1 --- l_F[SII]6716 Limit flag on F[SII]6716
127-132 F6.1 mW/m2 F[SII]6716 ? Emission line flux, [S II] 6716 (8)
134-137 F4.1 mW/m2 e_F[SII]6716 ? Uncertainty in F[SII]6716 (9)
139-139 A1 --- l_F[SII]6731 Limit flag on F[SII]6731
140-144 F5.1 mW/m2 F[SII]6731 ? Emission line flux, [S II] 6731 (8)
146-149 F4.1 mW/m2 e_F[SII]6731 ? Uncertainty in F[SII]6731 (9)
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Note (7): Measurement flag as follows:
b = For the large disk galaxy near the SLSN position;
c = From the sum of extractions from a slit through the nucleus of the
"major" and "minor" components of the merger;
d = From a slit that passes through the "primary" galaxy, although not
through its nucleus;
s = Measurement at the SLSN site.
Note (8): Emission line fluxes in units of erg/cm2/s, corrected for Galactic
extinction.
Note (9): 1σ statistical uncertainties shown. These do not include
uncertainties associated with the overall flux calibration, which for
sources with SN contamination or weak continuum (09atu, 09cwl, 10hgi,
10qwu, 10scc, 10vwg, 12mue, 12mxx) may be significant but will affect
all lines proportionally.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF Identifier
8- 8 A1 --- l_SFRd Limit flag on SFRd
9- 14 F6.3 Msun/yr SFRd [0.01/19.4] Dust-corrected Hα SFR
16- 21 F6.3 Msun/yr E_SFRd ? Upper uncertainty in SFRd
23- 28 F6.3 Msun/yr e_SFRd ? Lower uncertainty in SFRd
30- 30 A1 --- l_Avd ? Limit flag on Avd
31- 35 F5.2 mag Avd [0/2.9]? Balmer-decrement dust extinction
37- 41 F5.2 mag E_Avd ? Upper uncertainty in Avd
43- 47 F5.2 mag e_Avd ? Upper uncertainty in Avd
49- 49 A1 --- l_Best ? Limit flag on Best
50- 54 F5.2 [-] Best [7.4/9.3]? Best Metallicity, 12+log(O/H) (10)
56- 60 F5.2 [-] E_Best ? Upper uncertainty in Best
62- 66 F5.2 [-] e_Best ? Lower uncertainty in Best
68- 71 F4.2 [-] Te [7.4/8.3]? Te Metallicity, 12+log(O/H)
73- 77 F5.2 [-] E_Te ? Upper uncertainty in Te
79- 83 F5.2 [-] e_Te ? Lower uncertainty in Te
85- 85 A1 --- l_N06N2 ? Limit flag on N06N2
86- 90 F5.2 [-] N06N2 [7.6/9.3]? N06N2 Metallicity, 12+log(O/H)
92- 96 F5.2 [-] E_N06N2 ? Upper uncertainty in N06N2
98-102 F5.2 [-] e_N06N2 ? Lower uncertainty in N06N2
104-107 F4.2 [-] N06R23 [6.9/9.3]? N06R23 Metallicity, 12+log(O/H)
109-113 F5.2 [-] E_N06R23 ? Upper uncertainty in N06R23
115-119 F5.2 [-] e_N06R23 ? Lower uncertainty in N06R23
121-124 F4.2 [-] D02 [7.7/9]? D02 Metallicity, 12+log(O/H)
126-130 F5.2 [-] E_D02 ? Upper uncertainty in D02
132-136 F5.2 [-] e_D02 ? Lower uncertainty in D02
138-141 F4.2 [-] PP04N2 [7.9/8.9]? PP04N2 Metallicity, 12+log(O/H)
143-147 F5.2 [-] E_PP04N2 ? Upper uncertainty in PP04N2
149-153 F5.2 [-] e_PP04N2 ? Lower uncertainty in PP04N2
155-158 F4.2 [-] PP04O3 [7.9/8.9]? PP04O3 Metallicity, 12+log(O/H)
160-164 F5.2 [-] E_PP04O3 ? Upper uncertainty in PP04O3
166-170 F5.2 [-] e_PP04O3 ? Lower uncertainty in PP04O3
172-175 F4.2 [-] M08 [7.8/9]? M08 Metallicity, 12+log(O/H)
177-181 F5.2 [-] E_M08 ? Upper uncertainty in M08
183-187 F5.2 [-] e_M08 ? Lower uncertainty in M08
189-192 F4.2 [-] M13O3 [7.9/8.7]? M13O3 Metallicity, 12+log(O/H)
194-198 F5.2 [-] E_M13O3 ? Upper uncertainty in M13O3
200-204 F5.2 [-] e_M13O3 ? Lower uncertainty in M13O3
206-209 F4.2 [-] M13N2 [7.9/9.2]? M13N2 Metallicity, 12+log(O/H)
211-215 F5.2 [-] E_M13N2 ? Upper uncertainty in M13N2
217-221 F5.2 [-] e_M13N2 ? Lower uncertainty in M13N2
223-226 F4.2 [-] KK04 [7.7/9]? KK04 Metallicity, 12+log(O/H)
228-232 F5.2 [-] E_KK04 ? Upper uncertainty in KK04
234-238 F5.2 [-] e_KK04 ? Lower uncertainty in KK04
240-243 F4.2 [-] KD02 [7.7/8.5]? KD02 Metallicity, 12+log(O/H)
245-249 F5.2 [-] E_KD02 ? Upper uncertainty in KD02
251-255 F5.2 [-] e_KD02 ? Lower uncertainty in KD02
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Note (10): The "best" metallicity (the value presented in plots and elsewhere
in the discussion) is the Te metallicity when a high-significance detection
of the [OIII]λ{4363} auroral line is available, else the N06
(N2Hα) metallicity if [NII] is detected. The mass-metallicity
relation is used if neither of these lines is detected.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Jan-2017