J/ApJ/864/45 Survey of X-ray emission from superluminous SNe (Margutti+, 2018)
Results from a systematic survey of X-ray emission from hydrogen-poor
superluminous SNe.
Margutti R., Chornock R., Metzger B.D., Coppejans D.L., Guidorzi C.,
Migliori G., Milisavljevic D., Berger E., Nicholl M., Zauderer B.A.,
Lunnan R., Kamble A., Drout M., Modjaz M.
<Astrophys. J., 864, 45 (2018)>
=2018ApJ...864...45M 2018ApJ...864...45M
ADC_Keywords: Supernovae; Redshifts; X-ray sources
Keywords: stars: magnetars ; stars: mass-loss ; supernovae: general ;
X-rays: general
Abstract:
We present the results from a sensitive X-ray survey of 26 nearby
hydrogen-poor superluminous supernovae (SLSNe-I) with Swift, Chandra,
and XMM. This data set constrains the SLSN evolution from a few days
until ∼2000d after explosion, reaching a luminosity limit
Lx∼1040erg/s and revealing the presence of significant X-ray
emission possibly associated with PTF 12dam. No SLSN-I is detected
above Lx∼1041erg/s, suggesting that the luminous X-ray emission
Lx∼1045erg/s associated with SCP 60F6 is not common among SLSNe-I.
We constrain the presence of off-axis gamma-ray burst (GRB) jets,
ionization breakouts from magnetar engines and the density in the
sub-parsec environments of SLSNe-I through inverse Compton emission.
The deepest limits rule out the weakest uncollimated GRB outflows,
suggesting that if the similarity of SLSNe-I with GRB/SNe extends to
their fastest ejecta, then SLSNe-I are either powered by energetic
jets pointed far away from our line of sight (θ>30°), or
harbor failed jets that do not successfully break through the stellar
envelope. Furthermore, if a magnetar central engine is responsible for
the exceptional luminosity of SLSNe-I, our X-ray analysis favors large
magnetic fields B>2x1014G and ejecta masses Mej>3M☉, in
agreement with optical/UV studies. Finally, we constrain the
pre-explosion mass-loss rate of stellar progenitors of SLSNe-I. For
PTF 12dam we infer dM/dt<2x10-5M☉/yr, suggesting that the SN
shock interaction with an extended circumstellar medium is unlikely to
supply the main source of energy powering the optical transient and
that some SLSN-I progenitors end their lives as compact stars
surrounded by a low-density medium similar to long GRBs and type Ib/c
SNe.
Description:
Since 2011, we routinely followed up all publicly announced nearby
(z≲0.5) hydrogen-poor superluminous supernovae (SLSNe-I) with
Swift-XRT with a series of observations acquired between the time of
discovery and ∼360 days (rest-frame) after explosion. For a subset of
events we acquired deep X-ray observations with dedicated programs on
the CXO and XMM-Newton. Additionally, we searched the Swift-XRT, CXO,
and XMM archives for serendipitous or unpublished observations of
SLSNe-I discovered before 2016 May. Our final sample consists of 26
SLSNe-I discovered between 2006 and 2016 May. The data set covers the
time range between ∼days after explosion until ∼2000 days (rest-frame)
and comprises ∼700hr of observations.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
slsne.dat 81 26 Nearby hydrogen-poor superluminous supernovae
(SLSNe-I) sample (Tables 1-3)
table5.dat 70 254 X-ray observations of SLSNe-I
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
B/xmm : XMM-Newton Obs. Log (XMM-Newton Science Operation Center, 2012)
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
B/swift : Swift Master Catalog (HEASARC, 2004-)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
J/ApJ/690/1358 : Transient SCP 06F6 unusual opt. spectra (Barbary+, 2009)
J/other/Nat/463.513 : Radio observations of SN 2009bb (Soderberg+, 2010)
J/other/Nat/474.484 : Ligth curves of 4 supernovae (Quimby+, 2011)
J/MNRAS/428/729 : GRB Swift X-ray light curves analysis (Margutti+, 2013)
J/ApJ/782/42 : Panchromatic observations of PTF11qcj (Corsi+, 2014)
J/ApJ/781/42 : Optical photometry of SN 2010jl (Ofek+, 2014)
J/MNRAS/448/1206 : Superluminous supernovae in faint galaxies (McCrum+, 2015)
J/MNRAS/458/84 : Host galaxies of Superluminous Supernovae (Angus+, 2016)
J/ApJ/821/57 : Photometry of the Type Ib/c SN2013ge (Drout+, 2016)
J/ApJ/830/13 : Host-galaxy NUV-NIR data of SNe (Perley+, 2016)
J/ApJ/845/85 : Absorption vel. for 21 super-luminous SNe Ic (Liu+, 2017)
J/ApJ/836/25 : Swift UVOT light curves of ASASSN-15lh (Margutti+, 2017)
J/ApJ/835/58 : PTF 12dam & iPTF 13dcc follow-up (Vreeswijk+, 2017)
J/ApJ/852/81 : PS1 superluminous SNe LCs + classif. spectra (Lunnan+, 2018)
J/ApJ/860/100 : LCs of 26 hydrogen-poor superluminous SNe (De Cia+, 2018)
Byte-by-byte Description of file: slsne.dat
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Bytes Format Units Label Explanations
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1 A1 --- Set Sample identifier (1)
3- 18 A16 --- SN SN name
20- 28 A9 --- OName Other name
30- 35 F6.4 --- z [0.09/1.2] Redshift
36 A1 --- f_z [p] Flag on z (2)
38- 43 F6.1 Mpc Dist [463/8310] Luminosity distance
45- 51 F7.1 d MJD [53787/57438]? Discovery date
53- 54 A2 --- f_MJD Flag on MJD (2)
56- 62 F7.1 d MJDe [53767/57393] Inferred explosion date
64- 65 A2 --- f_MJDe Flag on MJDe (2)
67- 71 F5.3 10+20cm-2 NHmw [0.7/9.5] Hydrogen column density NHMW
73- 81 A9 --- Inst Instrument
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Note (1): Sample code as follows:
g = the "gold sample" contains 4 SLSNe-I with X-ray detections or
well-sampled optical bolometric light curve and deep X-ray limits
obtained with XMM or the CXO.
b = the "bronze sample" contains 12 SLSNe-I with sparser optical data
but with good Swift-XRT X-ray coverage.
i = the "iron sample" comprises 10 SLSNe-I with very sparse optical and
X-ray data.
Note (2): Flag as follows:
a = From Levan et al. (2013ApJ...771..136L 2013ApJ...771..136L).
b = The time of the peak is MJD 53872. The rise-time is ∼50d in the
rest-frame (Barbary et al. 2009, J/ApJ/690/1358).
c = The light curve reached maximum light on MJD 56088 and the rest-frame
rise-time is ∼60d (Nicholl et al. 2013Natur.502..346N 2013Natur.502..346N).
d = From Lunnan et al. (2016ApJ...831..144L 2016ApJ...831..144L).
e = Lunnan+ (2016ApJ...831..144L 2016ApJ...831..144L) estimate a peak time on MJD 56801.3 and
a rest-frame rise-time ≳125d.
f = From Nicholl et al. (2016ApJ...826...39N 2016ApJ...826...39N).
g = The SN reached r-band maximum light on MJD 57102
(Nicholl+ 2016ApJ...826...39N 2016ApJ...826...39N); the rise-time inferred is ∼80d
in the rest-frame.
bb = From Quimby+ (2011, J/other/Nat/474.484), the peak time is MJD 55069.145
and the rest-frame rise-time is ∼50 days.
bc = From Quimby+ (2011, J/other/Nat/474.484), the peak time is MJD 55279 and
the rest-frame rise-time is ∼23 days.
bd = Vinko et al. (2012AAS...21943604V) report that SN 2010kd reached maximum
light 40 days after discovery. We assume a 50 day rest-frame rise-time.
be = From Inserra et al. (2013ApJ...770..128I 2013ApJ...770..128I).
bf = From Yan et al. (2015ApJ...814..108Y 2015ApJ...814..108Y).
bg = Yan et al. (2015ApJ...814..108Y 2015ApJ...814..108Y) report a range of explosion dates
between MJD 56470.8 and MJD 56522.0. We use the middle date MJD 56496.4.
bh = From Leloudas et al. (2015ApJ...815L..10L 2015ApJ...815L..10L).
bi = Peak time on MJD 56699 (Leloudas et al. 2015ApJ...815L..10L 2015ApJ...815L..10L); the
pre-max evolution is only sparsely sampled. We assume a 50d rest-frame
rise-time, similar to other SLSNe-I.
bj = From Jerkstrand et al. (2017ApJ...835...13J 2017ApJ...835...13J).
bk = From the CRTS source catalog:
http://nesssi.cacr.caltech.edu/catalina/AllSN.arch.html
bl = From Smith et al. (2014ATel.6739....1S 2014ATel.6739....1S).
bm = According to Smith et al. (2014ATel.6739....1S 2014ATel.6739....1S), on 2014 Nov 22 the
transient was 4-5 weeks rest-frame after maximum light. The inferred
time of maximum light is MJD 56940. We assume a 50d rest-frame rise-time.
bn = From D'Andrea et al. (2015ATel.8092....1D 2015ATel.8092....1D).
bo = Very sparse photometric coverage.
On MJD 57286 D'Andrea et al. (2015ATel.8092....1D 2015ATel.8092....1D) reported that the
transient is still before the peak. We adopt the discovery date as a
rough proxy for the explosion date here.
p = From P. Blanchard et al. (2018, in preparation).
bq = From http://star.pst.qub.ac.uk/ps1threepi/psdb/public/.
br = The peak time is MJD 57453 from:
http://star.pst.qub.ac.uk/ps1threepi/psdb/public/. We assume a 50d
rest-frame rise-time.
cb = The time of the peak is MJD 55081 and the rise-time is ∼50d in
the rest-frame (Quimby et al. 2011, J/other/Nat/474.484).
cc = The time of maximum light is MJD 55063 (Quimby+ 2011 J/other/Nat/474.484).
We assume a 50 day rise-time in the rest-frame.
cd = The time of maximum light is MJD 55473 (Perley+ 2016, J/ApJ/830/13).
We assume a 50 day rise-time in the rest-frame.
cf = From Lunnan+ (2018, J/ApJ/852/81).
cg = From Challis et al. (2016ATel.8952....1C 2016ATel.8952....1C).
ch = From Challis et al. (2016ATel.8952....1C 2016ATel.8952....1C) the peak time is MJD 57340.
We assume a 50 day rest-frame rise-time.
ci = From http://ogle.astrouw.edu.pl/ogle4/transients/transients.html.
cj = From Dimitriadis et al. (2016ATel.8555....1D 2016ATel.8555....1D).
ck = The peak time is MJD 57397 (Dimitriadis+ 2016ATel.8555....1D 2016ATel.8555....1D).
We assume a 50 day rest-frame rise-time.
un = unclear.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- SN SN name (1)
18- 25 A8 --- OName Other name
27- 35 F9.3 d MJDst [53949/57667.1] Modified Julian Date of
observation start
37- 45 F9.3 d MJDend [53949/57667.1] Modified Julian Date of
observation ending
47 A1 --- l_Flux Limit flag on Flux
49- 55 F7.2 10-17W/m2 Flux [0.06/2412] Unabsorbed flux in 0.3-10keV
band (2)
57- 60 F4.2 10-17W/m2 e_Flux [0.03]? The 1σ uncertainty in Flux
62- 70 A9 --- Inst Instrument used in the observation
(Swift-XRT, XMM or Chandra)
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Note (1): The XMM observation of SCP06F6 is from Levan+ (2013ApJ...771..136L 2013ApJ...771..136L).
Note (2): In units of 1e-14erg/s/cm2.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 14-Aug-2019