J/ApJ/830/30 HDS spectrum of nova V2659 Cyg (Nova Cyg 2014) (Arai+, 2016)
Origins of absorption systems of classical nova V2659 Cyg (Nova Cyg 2014).
Arai A., Kawakita H., Shinnaka Y., Tajitsu A.
<Astrophys. J., 830, 30-30 (2016)>
=2016ApJ...830...30A 2016ApJ...830...30A (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Spectroscopy
Keywords: novae, cataclysmic variables; stars: individual: V2659 Cyg;
stars: winds, outflows
Abstract:
We report on high-dispersion spectroscopy results of a classical nova
V2659 Cyg (Nova Cyg 2014) that are taken 33.05 days after the V-band
maximum. The spectrum shows two distinct blueshifted absorption
systems originating from H I, Fe II, Ca II, etc. The radial velocities
of the absorption systems are -620km/s, and -1100 to -1500km/s. The
higher velocity component corresponds to the P-Cygni absorption
features frequently observed in low-resolution spectra. Much larger
numbers of absorption lines are identified at the lower velocity.
These mainly originate from neutral or singly ionized Fe-peak elements
(Fe I, Ti II, Cr II, etc.). Based on the results of our spectroscopic
observations, we discuss the structure of the ejecta of V2659 Cyg. We
conclude that the low- and high-velocity components are likely to be
produced by the outflow wind and the ballistic nova ejecta,
respectively.
Description:
The nova V2659 Cyg (Nova Cyg 2014 = PNV J20214234+3103296) was
discovered on UT 2014 March 31.790 (JD 2456748.29) by K. Nishiyama and
F. Kabashima.
The nova showed a slow rising (trise=11 days) up to the first V-band
maximum at JD 2456758.0±0.5 (2014 Apr 10; t=0; V=9.3).
We obtained the post-outburst spectrum of V2659 Cyg at t=33.05d in the
early decline phase using the High Dispersion Spectrograph (HDS)
mounted on the 8.2m Subaru Telescope.
Objects:
-------------------------------------------------------
RA (ICRS) DE Designation(s)
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20 21 42.34 +31 03 29.6 V2659 Cyg = NOVA Cyg 2014
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 61 264 *List of identified absorption lines of
lower velocity component (LVC)
fig2/* . 3 HDS spectrum of V2659 Cyg obtained 33.05 days
after visual maximum
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Note on table5.dat: Two distinct velocity components are detected for each
transition at velocities of vrad=-620km/s and vrad -1100 to -1500km/s
(the LVCs and HVCs (higher velocity components), respectively).
See section 4 for further discussions.
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Description of file: In subdirectory fig2/*:
Subaru Telescope/High Dispersion Spectrograph spectrum of V2659 Cyg
obtained 33.05 days after visual maximum. The FITS files provide the
Data behind Figure 2a (V2659CygUT201405133562-4394A.fits) and
2b (V2659CygUT201405134444-5289A.fits).
The spectrum covers the wavelength regions from 3561 to 5288 Angstroms
with a gap at 4394-4444 Angstroms. The spectral resolving power was
R∼72000 with a 0.50 arcsec (0.25mm) slit width. Data reduction was
conducted using the Image Reduction and Analysis Facility (IRAF)
software with the standard procedure.
See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Line Line identifier
14- 15 I2 --- Blend [1/22]?=- Blend Number
17- 25 F9.4 0.1nm lambda [3576.3/5284.1] Wavelength in Angstroms
27- 33 F7.4 eV Ei [0/10.2]? Lower energy level
35- 41 F7.4 eV Ek [2.9/13.6]? Upper energy level
43- 50 A8 --- Termi Lower term symbols
52- 59 A8 --- Termk Upper term symbols
61 I1 --- Ref ? Reference for energy and term values (1)
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Note (1): Reference as follows:
1 = NIST database - Kramida et al. (2016APS..DMP.Q1202K);
2 = Moore (1972mtai.book.....M 1972mtai.book.....M);
3 = Kurucz & Bell (1995all..book.....K 1995all..book.....K).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-Jan-2017