J/ApJ/768/47 Swift/XRT 0.2-10keV observations of SN2009ip (Ofek+, 2013)
SN 2009ip: constraints on the progenitor mass-loss rate.
Ofek E.O., Lin L., Kouveliotou C., Younes G., Gogus E., Kasliwal M.M.,
Cao Y.
<Astrophys. J., 768, 47 (2013)>
=2013ApJ...768...47O 2013ApJ...768...47O
ADC_Keywords: Supernovae ; X-ray sources
Keywords: stars: mass-loss; supernovae: general;
supernovae: individual: SN 2009ip
Abstract:
Some supernovae (SNe) show evidence for mass-loss events taking place
prior to their explosions. Measuring their pre-outburst mass-loss
rates provides essential information regarding the mechanisms that are
responsible for these events. Here we present XMM-Newton and Swift
X-ray observations taken after the latest, and presumably the final,
outburst of SN 2009ip. We use these observations as well as new
near-infrared and visible-light spectra and published radio and
visible-light observations to put six independent order-of-magnitude
constraints on the mass-loss rate of the SN progenitor prior to the
explosion. Our methods utilize the X-ray luminosity, the bound-free
absorption, the Hα luminosity, the SN rise time, free-free
absorption, and the bolometric luminosity of the outburst detected
prior to the explosion. Assuming spherical mass loss with a
wind-density profile, we estimate that the effective mass-loss rate
from the progenitor was between 10-3 and 10-2M☉/yr, over a
few years prior to the explosion, with a velocity of ∼103km/s. This
mass-loss rate corresponds to a total circumstellar matter (CSM) mass
of ∼0.04M☉, within 6x1015cm of the SN. We note that the
mass-loss rate estimate based on the Hα luminosity is higher by
an order of magnitude. This can be explained if the narrow-line
Hα component is generated at radii larger than the shock radius,
or if the CSM has an aspherical geometry. We discuss simple geometries
which are consistent with our results.
Description:
We observed SN 2009ip with XMM-Newton on 2012 November 1 in prime
full-window imaging mode for an effective exposure time of 8ks. Using
data collected with the EPIC-pn detector, we accumulated the source
spectrum from a circular region of 30" centered on the optical
position of SN 2009ip.
The Swift-XRT observed SN 2009ip on an almost daily basis since 2012
September 4 (triggered by Roming/Maragutti). Some of these X-ray
observations have been already reported in, e.g., Margutti et al.
(2012ATel.4414....1M 2012ATel.4414....1M) and Campana (2012ATel.4444....1C 2012ATel.4444....1C). For each
Swift-XRT image of the SN, we extracted the number of X-ray counts in
the 0.2-10keV band within an aperture of 9" radius centered on the SN
position.
Objects:
---------------------------------------------------
RA (ICRS) DE Designation(s)
---------------------------------------------------
22 23 08.26 -28 56 52.4 SN 2009ip = SN 2009ip
---------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 19 112 Swift-XRT observations
--------------------------------------------------------------------------------
See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2012)
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/ApJ/763/L27 : RI light curves of the type IIn SN 2009ip (Prieto+, 2013)
J/ApJ/763/42 : X-ray emission from 28 SNe (IIn, Ibn or SLSN-I) (Ofek+, 2013)
J/MNRAS/433/1312 : SN2009ip UBVRI, UVOR and JHK light curves (Fraser+, 2013)
J/other/Nat/494.65 : SN 2010mc outburst before explosion (Ofek+, 2013)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 d MJD Modified Julian Date of observation
10- 14 F5.2 ks Exp [0.08/18] Swift/XRT integration time
16 I1 ct SC X-ray counts in source aperture (1)
18- 19 I2 ct BC X-ray counts in background annulus (2)
--------------------------------------------------------------------------------
Note (1): A 9" radius aperture of the source position and in the 0.2-10keV band.
Note (2): In the 0.2-10 keV band, with an inner and outer annulus radii of
50" and 100" around the source. The ratio between the background
annulus area and the aperture area is 92.59.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 25-Nov-2014