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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 (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: ------------------------------------------------------------ RA (2000) DE Designation(s) ------------------------------------------------------------ 23 08 04.71 +60 46 52.1 Nova Cep 2013 = V* V809 Cep ------------------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 107 71 BVRCIC photometric observations of Nova Cep 2013
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 22-May-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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