J/PAZh/41/665 V1016 Cyg light curves and spectroscopy (Arkhipova+, 2015)
Symbiotic nova V1016 Cygni: Evolution of the dust envelope and the gaseous
nebula.
Arkhipova V.P., Taranova O.G., Ikonnikova N.P., Esipov V.F.,
Komissarova G.V., Shenavrin V.I.
<Pis'ma Astron. Zh. 41, 665 (2015)>
=2015PAZh...41..665A 2015PAZh...41..665A (SIMBAD/NED BibCode)
=2015AstL...41..613A 2015AstL...41..613A
ADC_Keywords: Novae ; Photometry, UBV ; Spectroscopy
Keywords: symbiotic stars - UBV observations - infrared observations -
fluxes in emission lines - nebular continuum -
post-outburst spectroscopic evolution, V1016 Cyg
Abstract:
As a result of the next cycle of our long-term monitoring, we present
our UBV JHKLM photometry for the symbiotic nova V1016 Cyg in
2008-2014. The star continued to systematically fade and redden in
UBV: over this period, the brightness declined by 0.1m in V and by
0.2m in B and U ,the B-V color index increased by 0.1m, and
U-B barely changed. On the color-color (U-B, B-V) diagram, the star
moved approximately horizontally rightward with a slight bluing in U-B
starting from 2000. Our JHKLM photometry has shown a decline in the
mean infrared (IR) brightness and a rise in the mean IR color indices
after 2004 due to an increase in the optical depth of the dust
envelope. The brightness decline and reddening of the Mira in the near
infrared reached their extreme values over the entire period of the
system's observations by the end of 2014.
The pulsation period of the Mira is determined with confidence:
P=465±5-days. The distance to the Mira, D=2.92±0.16kpc, ant its
parameters, the radius R*=(470±50)R☉ and luminosity
L*=(9200+/=1900)L☉, have been estimated from the observations of
V1016 Cyg at its maximum J brightness and at its minimum J-H color
index. The temperature of the star during its pulsations varied within
the range T* =2100-2700K. We have estimated the parameters of the dust
envelope near its maximum (in 2004) and minimum (in 2012-2014) IR
brightness. The mass of the dust envelope almost doubled in ten years,
with the rate of dust supply being ΔMd∼10-7M☉/yr.
Using a low-resolution spectrograph, we performed absolute
spectrophotometry for V1016 Cyg in 1995-2013 in the range
λ4340-7130Å. We have shown that almost all absolute fluxes
in lines and in continuum at λ4400Å decrease monotonically
after 2000, while the relative intensities of [OIII], [FeVII], and
[CaVII] lines increase after the minimum that probably occurred in the
1990s. The significant (approximately by a factor of 10 from 1995 to
2013) decrease of the flux in the Raman OVI λ6825 line reflects
a change of conditions in the formation zone of this line due to the
absorption of some OVI λ1032 photons in the newly forming dust
envelope of the cool component.
Description:
Our UBV observations of V1016 Cyg have been performed since 1971
(Arkhipova, 1983PZ.....22...25A 1983PZ.....22...25A) with an automated photon-counting UBV
photometer at the Cassegrain focus of the Zeiss-600 telescope at the
Crimean Station of the Sternberg Astronomical Institute.
The spectroscopic observations of V1016 Cyg were performed at the
Cassegrain focus of the 125-cm reflector at the Crimean Station of
the Sternberg Astronomical Institute with a fast spectrograph in
the range ~λ4000-7500Å.
Objects:
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RA (2000) DE Designation(s)
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19 57 05.03 +39 49 36.3 V1016 Cyg = NOVA Cyg 1964
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 41 70 UBV observations V1016 Cyg in 2008-2014
table6.dat 134 17 Observed absolute emission-line fluxes in the
spectrum of V1016 Cyg
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See also:
J/PAZh/26/695 : IR photometry of V1016 Cyg and HM Sge (Taranova+, 2000)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 I7 d JD Julian date
9- 14 F6.3 mag Vmag V magnitude
16- 21 F6.3 mag Bmag B magnitude
23- 28 F6.3 mag Umag U magnitude
30- 34 F5.3 mag B-V B-V colour index
36- 41 F6.3 mag U-B U-B colour index
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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- 7 I7 d JD Julian date
9- 13 F5.2 10-15W/m2 F4340 ?=- Absolute intensity of 4340 HI
15- 18 F4.2 10-15W/m2 F4363 ?=- Absolute intensity of 4363 [OIII]
20- 24 F5.2 10-15W/m2 F4686 ?=- Absolute intensity of 4686 HeII
26- 30 F5.2 10-15W/m2 F4861 ?=- Absolute intensity of 4861 HI
32- 36 F5.2 10-15W/m2 F4959 ?=- Absolute intensity of 4959 [OIII]
38- 42 F5.2 10-15W/m2 F5007 ?=- Absolute intensity of 5007 [OIII]
44- 47 F4.2 10-15W/m2 F5412 ?=- Absolute intensity of 5412 HeII
49- 52 F4.2 10-15W/m2 F5616 ?=- Absolute intensity of 5616 [CaVII]
54- 57 F4.2 10-15W/m2 F5721 ?=- Absolute intensity of 5721 [FeVII]
59- 62 F4.2 10-15W/m2 F5876 ?=- Absolute intensity of 5876 HeI
64- 67 F4.2 10-15W/m2 F6087 ?=- Absolute intensity of 6087 [FeVII]
69- 72 F4.2 10-15W/m2 F6300 ?=- Absolute intensity of 6300 [OI]
74- 77 F4.2 10-15W/m2 F6312 ?=- Absolute intensity of 6312 [SIII]
79- 82 F4.2 10-15W/m2 F6363 ?=- Absolute intensity of 6363 [OI]
84- 87 F4.2 10-15W/m2 F6435 ?=- Absolute intensity of 6435 [AV]
89- 94 F6.2 10-15W/m2 F6563 ?=- Absolute intensity of 6563 HI
96- 99 F4.2 10-15W/m2 F6678 ?=- Absolute intensity of 6678 HeI
101-104 F4.2 10-15W/m2 F6716 ?=- Absolute intensity of 6716 [SII]
106-109 F4.2 10-15W/m2 F6731 ?=- Absolute intensity of 6731 [SII]
111-114 F4.2 10-15W/m2 F6825 ?=- Absolute intensity of 6825 OVI
116-119 F4.2 10-15W/m2 F7005 ?=- Absolute intensity of 7005 [AV]
121-124 F4.2 10-15W/m2 F7065 ?=- Absolute intensity of 7065 HeI
126-129 F4.2 10-15W/m2 F7136 ?=- Absolute intensity of 7136 [ArIII]
131-134 F4.2 10-15W/m2 F7325 ?=- Absolute intensity of 7325 [OII]
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Acknowledgements:
Natalia Ikonnikova, ikonnikova(at)gmail.com
(End) Patricia Vannier [CDS] 28-Jan-2016