J/MNRAS/491/655 Photometry and spectroscopy of RN LMC 1968 (Kuin+, 2020)
The 2016 January eruption of recurrent Nova LMC 1968.
Kuin N.P.M., Page K.L., Mroz P., Darnley M.J., Shore S.N., Osborne J.P.,
Walter F., Di Mille F., Morrell N., Munari U., Bohlsen T., Evans A.,
Gehrz R.D., Starrfield S., Henze M., Williams S.C., Schwarz G.J.,
Udalski A., Szymanski M.K., Poleski R., Soszynski I., Ribeiro V.A.R.M.,
Angeloni R., Breeveld A.A., Beardmore A.P., Skowron J.
<Mon. Not. R. Astron. Soc., 491, 655-679 (2020)>
=2020MNRAS.491..655K 2020MNRAS.491..655K (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Photometry, ultraviolet ; Photometry, UBVRI; Spectroscopy
Keywords: binaries: eclipsing - stars: individual: (Nova LMC 1968) -
novae, cataclysmic variables - ultraviolet: stars - X-rays: binaries
Abstract:
We present a comprehensive review of all observations of the eclipsing
recurrent Nova LMC 1968 in the Large Magellanic Cloud which was
previously observed in eruption in 1968, 1990, 2002, 2010, and most
recently in 2016. We derive a probable recurrence time of 6.2±1.2yr
and provide the ephemerides of the eclipse. In the
ultraviolet-optical-IR photometry the light curve shows high
variability right from the first observation around 2 d after
eruption. Therefore no colour changes can be substantiated. Outburst
spectra from 2016 and 1990 are very similar and are dominated by H and
He lines longward of 2000Å. Interstellar reddening is found to be
E(B-V)=0.07±0.01. The super soft X-ray luminosity is lower than the
Eddington luminosity and the X-ray spectra suggest the mass of the
white dwarf (WD) is larger than 1.3M☉. Eclipses in the light
curve suggest that the system is at high orbital inclination. On day 4
after the eruption a recombination wave was observed in FeII
ultraviolet absorption lines. Narrow-line components are seen after
day 6 and explained as being due to reionization of ejecta from a
previous eruption. The UV spectrum varies with orbital phase, in
particular a component of the HeII 1640Å emission line, which
leads us to propose that early-on the inner WD Roche lobe might be
filled with a bound opaque medium prior to the re-formation of an
accretion disc. Both this medium and the ejecta can cause the delay in
the appearance of the soft X-ray source.
Description:
This catalogue is a collection of the data for Nova LMC 1968 up to and
including the 2016 eruption. The data includes the photometry of the
2002 eruption as seen by EROS in addition to the data collected in the
course of the study of the 2016 eruption of the recurrent Nova LMC
1968, with the exception of the IUE spectra which have been processed
and are archived at IUE data repositories in the USA and Europe. This
collection includes the reduced Swift UVOT photometry and spectra, but
not the Swift X-ray data which can be accessed from the USA, Italian
and UK Swift data centres. We present the data from photometry and
spectroscopy by year of eruption and/ or source (for OGLE). Eruptions
were observed in 1968, 1990, 2002, 2010, 2016, and 2020.
Objects:
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RA (2000) DE Designation(s)
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05 09 58.40 -71 39 52.7 Nova LMC 1968 = SV* BV 1261
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
erosblue.dat 28 531 *2002 EROS blue photometry
erosred.dat 28 410 *2002 EROS red photometry
phot1968.dat 38 8 The 1968 photometry (table A3)
phot1990.dat 65 23 The 1990 photometry (table A3)
phot2016.dat 66 434 *2016 photometry: SMART, ANS, UVOT (table A3)
photogle.dat 66 808 The OGLE V and I photometry 2010-2016
t1990_01.dat 20 1000 *Spectrum 1990-02-22.83 day 8.73 SAAO
t1990_03.dat 20 1000 *Spectrum 1990-03-01.86 day 15.76 SAAO
listsp1.dat 150 13 *Observation log for Swift UVOT spectra and
ANS spectrum
listsp2.dat 194 7 List of fits spectra
listimg.dat 94 15 List of EROS fits images
sp1/* . 14 Individual ascii spectra
sp2/* . 7 Individual fits spectra
img/* . 15 Individual EROS fits images
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Note on erosblue.dat and erosred.dat:
The EROS photometry was obtained by a new reduction of the EROS-1 data
by J.-B. Marquette. The photometry in the blue and red bands has been
provided as uncalibrated instrumental mags and errors. The data were
extracted using Emmanuel Bertins astrOmatic pipeline with an arbitrary
zeropoint of 21.
Note on phot2016.dat, s1990_02.dat, s2016_04.dat: original ANS photometry here
is the original provided by U. Munari.
Note on t1990_01.dat, t1990_03.dat: SAAO spectra were extracted from
Sekigushi et al. (1990MNRAS.245p..28S 1990MNRAS.245p..28S).
The CTIO spectrum can be found in Williams et al. 2003JAD.....9....3W 2003JAD.....9....3W.
Note on listsp1.dat: The spectral range for the UV grism first order is
1700-2950Å with extended range with possible second order overlap
2950-4500Å, and second + third order overlap 4500-6800Å.
The spectra may be cut short depending on the overlap and strength of the UV.
Order overlap is reduced when the placement is offset from the centre.
Contamination by zeroth and first order from other sources in the field of
view is indicated a quality flag > 0.
Errors are only random errors due to statistics in the total and
background, with an adjustment due to the coincidence loss correction.
There is an additional systematic noise due to centroiding which can be
reduced by summing individual spectra, see Kuin et al. 2015MNRAS.449.2514K 2015MNRAS.449.2514K.
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Byte-by-byte Description of file: erosblue.dat erosred.dat
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Bytes Format Units Label Explanations
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1- 12 F12.5 d MJD Modified Julian Day observation time
14- 21 F8.3 mag mag Uncalibrated EROS instrumental magnitude
23- 28 F6.3 mag e_mag ? Error in magnitude
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Byte-by-byte Description of file: phot*.dat
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Bytes Format Units Label Explanations
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1- 12 F12.4 d JD Observation time (1)
14 A1 --- l_mag [>] Upper limit flag on mag
15- 20 F6.3 mag mag ? Magnitude in Filter
22- 26 F5.3 mag e_mag ? Error in magnitude (1-sigma)
28- 31 A4 --- system [AB/VEGA] magnitude system
33- 38 A6 --- Filter Name of the filter
40- 45 F6.3 --- Phase ? Orbital phase
47- 66 A20 --- Source Name of the observatory/instrument/reference
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Note (1): UVOT times are mid-time of observation; OGLE times are heliocentric
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Byte-by-byte Description of file: t1990_01.dat t1990_03.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda Wavelength
9- 20 E12.5 --- Rflux Relative flux
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Byte-by-byte Description of file: listsp1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- FileName Name of the file in subdirectory sp1
14- 16 A3 --- grism Grism [UV Vis]
18- 26 F9.4 d JD ? Julian date, JD-2450000
28- 32 F5.2 d Day ? Day of observation
34- 41 I8 --- Obsid ? Obsid
43- 48 A6 --- Place [offset ] placement
50-150 A101 --- Title Title
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Byte-by-byte Description of file: sp1/*
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm Lambda Wavelength
9- 20 E12.5 10-2W/m2/nm Flux Flux (in erg/cm2/s/Å)
22- 32 E11.5 10-2W/m2/nm e_Flux ? Error in the flux (in erg/cm2/s/Å)
35 I1 --- q_Flux [0/1]? Quality of flux (1)
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Note (1): Quality flag as follows:
1 = zeroth order contamination
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Byte-by-byte Description of file: listsp2.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Nx Number of pixels along X-axis
6- 24 A19 "datime" Obs.date Observation date
26- 32 F7.2 0.1nm blambda Lower value of wavelength interval
34- 40 F7.2 0.1nm Blambda Upper value of wavelength interval
42- 49 F8.6 0.1nm dlambda Wavelenght resolution
51- 52 I2 Kibyte size Size of FITS file
54- 65 A12 --- FileName Name of FITS file, in subdirectory sp2
67-102 A36 --- Title Title of the FITS file
104-144 A41 --- FileName2 Original file name
146-178 A33 --- Tel Telescope name
180-183 F4.2 arcsec Slit ? Slit
185-188 I4 s ExpTime ? Exposure time
190-194 F5.3 --- Airmass ? Airmass
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Byte-by-byte Description of file: listimg.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 24 F5.3 arcsec/pix scale Scale of the image
26- 28 I3 --- Nx Number of pixels along X-axis
30- 32 I3 --- Ny Number of pixels along Y-axis
34- 56 A23 "datime" Obs.date Observation date
58- 60 I3 Kibyte size Size of FITS file
62- 73 A12 --- FileName Name of FITS file, in subdirectory img
75- 94 A20 --- Title Title of the FITS file
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Acknowledgements:
Paul Kuin, npkuin(at)gmail.com
(End) Paul Kuin [MSSL/UCL], Patricia Vannier [CDS] 10-Aug-2020