J/AJ/155/58 2006-2016 CCD photometry of V723 Cassiopeia (Hamilton-Drager+, 2018)
The photometric evolution of the classical nova V723 Cassiopeia from 2006
through 2016.
Hamilton-Drager C.M., Lane R.I., Recine K.A., Ljungquist L.S., Grant J.A.,
Shrader K., Frymark D.G., Dornbush E.M., Richey-Yowell T., Boyle R.J.,
Schwarz G.J., Page K.L.
<Astron. J., 155, 58 (2018)>
=2018AJ....155...58H 2018AJ....155...58H (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Binaries, cataclysmic ; Photometry, UBVRI ;
Photometry, ultraviolet ; X-ray sources
Keywords: novae, cataclysmic variables - stars: individual (V723 Cas)
Abstract:
We present photometric data of the classical nova, V723 Cas
(Nova Cas 1995), over a span of 10 years (2006 through 2016) taken
with the 0.9 m telescope at Lowell Observatory, operated as the
National Undergraduate Research Observatory (NURO) on Anderson Mesa
near Flagstaff, Arizona. A photometric analysis of the data produced
light curves in the optical bands (Bessel B, V, and R filters). The
data analyzed here reveal an asymmetric light curve (steep rise to
maximum, followed by a slow decline to minimum), the overall structure
of which exhibits pronounced evolution including a decrease in
magnitude from year to year, at the rate of ∼0.15 mag/yr. We model
these data with an irradiated secondary and an accretion disk with a
hot spot using the eclipsing binary modeling program Nightfall. We
find that we can model reasonably well each season of observation by
changing very few parameters. The longitude of the hot spot on the
disk and the brightness of the irradiated spot on the companion are
largely responsible for the majority of the observed changes in the
light curve shape and amplitude until 2009. After that, a decrease in
the temperature of the white dwarf is required to model the observed
light curves. This is supported by Swift/X-Ray Telescope observations,
which indicate that nuclear fusion has ceased, and that V723 Cas is no
longer detectable in the X-ray.
Description:
In 2006 October, we began a program to observe V723 Cas (RA=01:05:05.4,
DE=+54:00:40.3 J2000.0) photometrically during the months of October and
January with the 0.9 m telescope at the National Undergraduate Research
Observatory (NURO) located at Lowell Observatory on Anderson Mesa in
Flagstaff, Arizona as a part of our undergraduate research program.
The observing runs generally spanned four-night periods, which allowed
for observations of four distinct epochs per run on average. The Lowell
0.9 m f/15.7 telescope is equipped with standard Bessel UBVRI filters
manufactured by Omega Optical.
Swift (Gehrels et al. 2004ApJ...611.1005G 2004ApJ...611.1005G) observations of V723 Cas
were obtained intermittently between 2006 January and 2014 September
while V723 Cas was in the SSS phase. Observations after 2008 September
12 (with the exception of 2014 April 01) were taken using one or more
of the UV/Optical Telescope (UVOT; Roming et al. 2005SSRv..120...95R 2005SSRv..120...95R)
UV filters. The XRT (Burrows et al. 2005SSRv..120..165B 2005SSRv..120..165B) collected
data in Photon Counting (PC) mode throughout all of the observations.
Objects:
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RA (ICRS) DE Designation(s)
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01 05 05.36 +54 00 40.2 V723 Cas = NOVA Cas 1995
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 27 2320 2006 October-2016 October R-band CCD Photometry
of V723 Cas
table5.dat 85 25 Swift X-Ray and UV Data
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See also:
J/A+A/338/1006 : V723 Cas equivalent widths (Iijima+ 1998)
J/AJ/140/34 : Classification of nova light curves (Strope+, 2010)
J/ApJS/197/31 : Swift X-ray observations of classical novae. II.
(Schwarz+, 2011)
J/MNRAS/454/123 : BVRI light curves of Nova V723 Cas (Ochner+, 2015)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1 A1 --- Filter Filter used (Bessel B, V or R)
3- 14 F12.4 d JD Julian Date of the observation
16- 21 F6.3 mag mag [14.205/17.152] Apparent magnitude in Filter (1)
23- 27 F5.3 mag e_mag [0.003/0.048] Uncertainty in mag
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Note (1): In the paper, the October 2016 R band data are adjusted by subtracting
0.1 magnitudes. This is done to correct for the effects of soot in
air from nearby prescribed fires (see Section 7).
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Date UT date(s) of the observation
16- 27 F12.4 d JD Julian Date of the observation
29- 39 I11 --- ObsID Observation identification number
41 A1 --- l_CtX [<] Limit flag on CtX
42- 46 F5.3 ct/s CtX [0.002/0.043] Swift/XRT X-ray count
48- 52 F5.3 ct/s e_CtX [0.001/0.007]? Uncertainty in CtX
54- 58 F5.2 mag UVW1 [14.77/16.09]? Swift-UVOT UVW1 magnitude
60- 63 F4.2 mag e_UVW1 [0.01/0.04]? Uncertainty in UVW1
65- 69 F5.2 mag UVM2 [15.36/16.23]? Swift-UVOT UVM2 magnitude
71- 74 F4.2 mag e_UVM2 [0.02/0.06]? Uncertainty in UVM2
76- 80 F5.2 mag UVW2 [15.24/16.12]? Swift-UVOT UVW2 magnitude
82- 85 F4.2 mag e_UVW2 [0.02/0.05]? Uncertainty in UVW2
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 03-Oct-2018