J/MNRAS/440/3402 Nova Cep 2013 (V809 Cep) UBVRI light curves (Munari+, 2014)
Study of three 2013 novae: V1830 Aql, V556 Ser and V809 Cep.
Munari U., Ochner P., Dallaporta S., Valisa P., Graziani M., Righetti G.L.,
Cherini G., Castellani F., Cetrulo G., Englaro A.
<Mon. Not. R. Astron. Soc., 440, 3402-3415 (2014)>
=2014MNRAS.440.3402M 2014MNRAS.440.3402M (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Photometry, UBVRI
Keywords: Stars: novae
Abstract:
BVRCIC photometry and low-, medium- and high-resolution echelle
fluxed spectroscopy is presented and discussed for three faint,
heavily reddened novae of the Feii-type which erupted in 2013. V1830
Nova Aql 2013 reached a peak V=15.2mag on 2013 Oct 30.3 UT and
suffered from a huge E(B-V)∼2.6mag reddening. After a rapid decline,
when the nova was ΔV=1.7mag below maximum, it entered a flat
plateau where it remained for a month until solar conjunction
prevented further observations. Similar values were observed for V556
Nova Ser 2013, that peaked near RC∼12.3 around 2013 Nov 25 and soon
went lost in the glare of sunset sky. A lot more observations were
obtained for V809 Nova Cep 2013, that peaked at V=11.18 on 2013 Feb
3.6. The reddening is E(B-V)∼1.7 and the nova is located within or
immediately behind the spiral Outer Arm, at a distance of ∼6.5kpc as
constrained by the velocity of interstellar atomic lines and the rate
of decline from maximum. While passing at t3, the nova begun to form
a thick dust layer that caused a peak extinction of ΔV>5mag, and
took 125d to completely dissolve. The dust extinction turned from
neutral to selective around 6000Å. Monitoring the time evolution of
the integrated flux of emission lines allowed us to constrain the
region of dust formation in the ejecta to be above the region of
formation of OI 7774Å and below that of CaII triplet. Along the
decline from maximum and before the dust obscuration, the emission
line profiles of Nova Cep 2013 developed a narrow component
(FWHM=210km/s) superimposed on to the much larger normal profile,
making it a member of the so-far exclusive but growing club of novae
displaying this peculiar feature. Constrains based on the optical
thickness of the innermost part of the ejecta and on the radiated
flux, place the origin of the narrow feature within highly structured
internal ejecta and well away from the central binary.
Description:
BVRCIC photometry of the programme novae was obtained with the
Asiago 67/92 cm Schmidt camera and various telescopes operated by ANS
Collaboration (N. 11, 30, 62, 73, 157).
Objects:
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RA (2000) DE Designation(s)
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23 08 04.71 +60 46 52.1 Nova Cep 2013 = V* V809 Cep
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 107 71 BVRCIC photometric observations of
Nova Cep 2013
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 12 F12.4 d HJD Heliocentric Julian date
14- 19 F6.3 mag Bmag ? Johnson B magnitude
21- 25 F5.3 mag e_Bmag ? rms uncertainty on Bmag
27- 32 F6.3 mag Vmag ? Johnson V magnitude
34- 38 F5.3 mag e_Vmag ? rms uncertainty on Vmag
40- 45 F6.3 mag Rcmag ? Cousins R magnitude
47- 51 F5.3 mag e_Rcmag ? rms uncertainty on Rcmag
53- 58 F6.3 mag Icmag ? Cousins I magnitude
60- 64 F5.3 mag e_Icmag ? rms uncertainty on Icmag
66- 71 F6.3 mag B-V ? Johnson B-V colour index
73- 77 F5.3 mag e_B-V ? rms uncertainty on B-V
79- 84 F6.3 mag V-Rc ? Johnson-Cousins V-R colour index
86- 90 F5.3 mag e_V-Rc ? rms uncertainty on V-Rc
92- 97 F6.3 mag V-Ic ? Johnson-Cousins V-I colour index
99-103 F5.3 mag e_V-Ic ? rms uncertainty on V-Ic
105-107 I3 --- Tel Telescope code number
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-May-2017