J/ApJ/763/42 X-ray emission from 28 SNe (IIn, Ibn or SLSN-I) (Ofek+, 2013)
X-ray emission from supernovae in dense circumstellar matter environments:
a search for collisionless shocks.
Ofek E.O., Fox D., Cenko S.B., Sullivan M., Gnat O., Frail D.A., Horesh A.,
Corsi A., Quimby R.M., Gehrels N., Kulkarni S.R., Gal-Yam A., Nugent P.E.,
Yaron O., Filippenko A.V., Kasliwal M.M., Bildsten L., Bloom J.S.,
Poznanski D., Arcavi I., Laher R.R., Levitan D., Sesar B., Surace J.
<Astrophys. J., 763, 42 (2013)>
=2013ApJ...763...42O 2013ApJ...763...42O
ADC_Keywords: Supernovae ; X-ray sources
Keywords: stars: mass-loss; supernovae: general;
supernovae: individual (SN 2006jc, SN 2010jl)
Abstract:
Here we report on a search, using Swift/XRT and Chandra, for X-ray
emission from 28 SNe that belong to classes whose progenitors are
suspected to be embedded in dense circumstellar matter (CSM). Our
sample includes 19 Type IIn SNe, one Type Ibn SN, and eight
hydrogen-poor superluminous SNe (SLSN-I such as SN 2005ap). Two SNe
(SN 2006jc and SN 2010jl) have X-ray properties that are roughly
consistent with the expectation for X-rays from a collisionless shock
in optically thick CSM. However, the X-ray emission from SN 2006jc can
also be explained as originating in an optically thin region. Thus, we
propose that the optical light curve of SN 2010jl is powered by shock
breakout in CSM. We suggest that two other events (SN 2010al and SN
2011ht) were too X-ray bright during the SN maximum optical light to
be explained by the shock-breakout model. We conclude that the light
curves of some, but not all, SNe IIn/Ibn are powered by shock breakout
in CSM. For the rest of the SNe in our sample, including all of the
SLSN-I events, our X-ray limits are not deep enough and were typically
obtained too early (i.e., near the SN maximum light) for definitive
conclusions about their nature. Late-time X-ray observations are
required in order to further test whether these SNe are indeed
embedded in dense CSM.
Description:
For each Swift/XRT image of an SN, we extracted the number of X-ray
counts in the 0.2-10keV band within an aperture of 7.2" (3 pixels)
radius centered on the SN position. For each SN that has Swift/XRT
observations, we searched for Chandra observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 132 28 SN sample
table2.dat 76 306 Swift-XRT X-ray measurements
refs.dat 43 58 References
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
II/313 : Palomar Transient Factory (PTF) phot. catalog 1.0 (Ofek+, 2012)
J/AJ/144/131 : Photometry and spectroscopy of SN 2010jl (Zhang+, 2012)
J/other/Nat/474.484 : Ligth curves of 4 supernovae (Quimby+, 2011)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/ApJ/690/1358 : Spectra of unusual optical transient SCP 06F6 (Barbary+, 2009)
http://www.cbat.eps.harvard.edu/lists/Supernovae.html : List of IAU SNe
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name SN name
10- 19 A10 --- OName Other name of the SN
21- 26 A6 --- Type SN type (Ibn, IIbn, or SLSN-I=superluminous SN)
28- 36 F9.5 deg RAdeg Right ascension in decimal degrees (J2000)
38- 46 F9.5 deg DEdeg Declination in decimal degrees (J2000)
48 A1 --- l_Tr Limit flag on Tr
50- 51 I2 d Tr ? Approximate rise time of the SN optical
light curve (trise) (1)
52 A1 --- u_Tr Uncertainty flag on Tr
54- 55 I2 d TrUp [23/60]? Upper range in Tr
57- 61 F5.1 mag RMag [-23/-14] Absolute R-band magnitude at
maximum light (ignoring K-corrections)
62 A1 --- u_RMag Uncertainty flag on RMag
64- 69 F6.4 --- z [0.004/0.6] Redshift (2)
71- 75 I5 d Tpk Modified Julian Date of maximum light (tpeak)
76 A1 --- u_Tpk Uncertainty flag on Tpk
78- 82 F5.2 10+20cm-2 NH [0.7/11] Galactic neutral hydrogen column
density (3)
84 A1 --- l_LX [≲] 2σ upper limit flag on LX or
uncertainty flag
86- 91 E6.2 10-7W LX 0.2-10keV band X-ray luminosity in erg/s
93- 97 F5.3 --- LX/LO [0.004/1.2] X-ray to optical luminosity
ratio (4)
99-102 F4.2 --- FAP [0/1] Minimum false-alarm probability value
(FAPmin) (5)
104-130 A27 --- Ref Reference(s) (see refs.dat file)
132 A1 --- Note [nuse] Note (6)
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Note (1): The rise time is deduced from various sources including PTF and
Katzman Automatic Imaging Telescope (KAIT; Filippenko et al.
2001ASPC..246..121F 2001ASPC..246..121F) photometry and the literature listed in the
references.
Note (2): The object redshift. If the galaxy is nearby and has a direct distance
measurement in the NASA Extragalactic Database (NED), we replaced the
observed redshift by the redshift corresponding to the luminosity
distance of the galaxy.
Note (3): The Galactic neutral hydrogen column density for the source position
(Dickey & Lockman 1990ARA&A..28..215D 1990ARA&A..28..215D).
Note (4): LX/LO is the ratio between the X-ray measurements or limit (LX) and
the peak visible-light luminosity.
Note (5): Sources with FAPmin<0.01 indicate a possible detection of an X-ray
source at the position of the SN. As discussed in the text, some of
these possible detections are chance coincidences or due to emission
from the SN host galaxy.
Note (6): Flag as follows:
n = Reported here for the first time
u = tpeak and trise are based on unpublished KAIT photometry
s = Spectrum is similar to SN 1997cy
e = Spectrum is similar to SN 1983K with HeII, NIII, and HI emission lines
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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- 8 A8 --- Name Supernova name
10- 16 F7.1 d Start ?=-99.99 Start date (1)
18- 24 F7.2 d End ?=-99.99 End date (1)
26- 33 F8.1 s Exp [1/207967] Swift/XRT integration time
35- 39 F5.2 ct/ks CR [-1.2/8.4] Count rate in the 0.2-10keV band
41- 46 F6.2 ct/ks e_CR ?=-99.99 The 1σ lower error on CR
48- 53 F6.2 ct/ks E_CR ?=-99.99 The 1σ upper error on CR
55- 61 F7.2 ct/ks CRUL ?=-99.99 The 2σ upper limit on a nondetection
63- 66 F4.2 --- FAP [0/1] Detection false-alarm probability
68 A1 --- l_LX Upper limit flag on LX
69- 76 E8.2 10-7W LX X-ray luminosity in the 0.2-10keV band; erg/s
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Note (1): Relative to maximum optical light (indicated in Table 1).
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Ref Reference code
6- 24 A19 --- BibCode Bibcode
26- 43 A18 --- Auth Author's name(s)
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Oct-2014