J/A+A/544/A26 CI Aql spectra during 2000 outburst (Iijima, 2012)
Spectroscopic observations of the recurrent nova CI Aquilae during the 2000
outburst.
Iijima T.
<Astron. Astrophys. 544, A26 (2012)>
=2012A&A...544A..26I 2012A&A...544A..26I
ADC_Keywords: Stars, variable ; Spectroscopy
Keywords: stars: individual: CI Aql - novae, cataclysmic variables
Abstract:
High- and low-resolution optical spectra of CI Aql were obtained
during the outburst in 2000. Multiple absorption components of HI and
FeII lines were detected at the early decline stage. Their radial
velocities were roughly -2500km/s, -2200km/s , -1700km/s, and
-1400km/s, among which only the last components were likely still
accelerating during the early decline stage. Prominent emission lines
of [OIII] and [NII] appeared about one month after light maximum. The
duration of the nebular stage, however, was only one month and a few
weeks. The ejected gas shells seem to have started to shrink about 70
days after light maximum. The amount of interstellar extinction is
estimated to be E(B-V)=0.92±0.15 from the equivalent widths of the
diffuse interstellar absorption bands. The helium abundance in the
ejecta is estimated to be N(He)=0.19±0.05 and the mass of the
ejecta to be about 2x10-6M☉. This object has been classified
as a U Sco type recurrent nova, but its spectral evolution during the
outburst resembled those of T Pyx type recurrent novae. It is doubtful
whether the peak of mV∼9mag on 2000 May 5 was the true light maximum
or an earlier brighter peak had been overlooked, because the spectral
data suggest that the ejections of gas shells occurred prior to the
discovery of the outburst on 2000 April 28.
Description:
The high-resolution spectra were obtained with a Reosc echelle
spectrograph mounted on the 182cm telescope at the Mount Ekar station
of the Astronomical Observatory of Padova.
The low-resolution spectra were obtained at the Bisei Astronomical
Observatory in Okayama Japan. A grating spectrograph Bisei mounted on
the Cassegrain focus of the 101cm telescope was used.
The low-resolution spectra are not uploaded, because those belong to
Matsumoto et al. (2001A&A...378..487M 2001A&A...378..487M).
The spectra are given in the Fits format. The sensitivity of the
spectrograph was calibrated using the spectra of the standard star
HR7596 obtained during the same nights of the observations. The
wavelengths are given in the heliocentric frame, while no correction
is applied for the interstellar extinction.
Objects:
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RA (2000) DE Designation(s)
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18 52 03.57 -01 28 39.4 CI Aql = NOVA Aql 1917
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 69 11 Log of spectroscopic observations of CI Aql
ciaql001.dat 20 9967 Calibrated high-resolution spectrum, May/14, 01:06
ciaql002.dat 20 9965 Calibrated high-resolution spectrum, May/15, 00:56
ciaql003.dat 20 9965 Calibrated high-resolution spectrum, May/15, 01:08
ciaql004.dat 20 12832 Calibrated high-resolution spectrum, May/16, 01:05
ciaql005.dat 20 12832 Calibrated high-resolution spectrum, May/16, 01:17
ciaql006.dat 20 12832 Calibrated high-resolution spectrum, Jun/09, 00:19
ciaql007.dat 20 9960 Calibrated high-resolution spectrum, Jun/10, 00:49
fits/* . 7 FITS files of spectra
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 "YYYY/MMM/DD" Obs.date Observation date
13- 17 A5 "h:m" Obs.time UT time
19- 25 F7.2 d JD Julian date (JD-2450000)
27- 30 F4.1 d Days Number of days from light maximum on
2005 May 5 (JD=2451669.5)
32- 35 I4 s Texp Exposure time
37- 41 A5 --- Inst Instrument
43- 49 A7 --- Range Spectral range (nm)
51- 56 A6 --- Sky Sky information (cloudy)
58- 69 A12 --- FileName Name of the file with spectrum
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Byte-by-byte Description of file: ciaql*.dat
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Bytes Format Units Label Explanations
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2- 7 F6.1 0.1nm lambda [4329/6896] Wavelength
9- 20 E12.6 10-14W/m2/nm Flux Flux (in 10-12ergs/cm2/s/Å)
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Acknowledgements:
Takashi Iijima, takashi.iijima(at)oapd.inaf.it
(End) Patricia Vannier [CDS] 13-Jul-2012