J/A+A/589/A36 Carbon stars spectra and photometry values (Gonneau+, 2016)
Carbon stars in the X-shooter Spectral Library.
Gonneau A., Lancon A., Trager S.C, Aringer B., Lyubenova M., Nowotny W.,
Peletier R.F, Prugniel P., Chen Y.-P., Dries M., Choudhury O.S.,
Falcon-Barroso J., Koleva M., Meneses-Goytia S., Sanchez-Blazquez P.,
Vazdekis A.
<Astron. Astrophys. 589, A36 (2016)>
=2016A&A...589A..36G 2016A&A...589A..36G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, carbon ; Spectroscopy
Keywords: stars: AGB and post-AGB - stars: carbon - infrared: stars -
ultraviolet: stars
Abstract:
We provide a new collection of spectra of 35 carbon stars obtained
with the ESO/VLT X-shooter instrument as part of the X-shooter
Spectral Library project. The spectra extend from 0.3um to 2.4um with
a resolving power above ∼8000. The sample contains stars with a
broad range of (J-K) color and pulsation properties located in the
Milky Way and the Magellanic Clouds. We show that the distribution of
spectral properties of carbon stars at a given (J-K) color becomes
bimodal (in our sample) when (J-K) is larger than about 1.5. We
describe the two families of spectra that emerge, characterized by the
presence or absence of the absorption feature at 1.53um, generally
associated with HCN and C2H2. This feature appears essentially
only in large-amplitude variables, though not in all observations.
Associated spectral signatures that we interpret as the result of
veiling by circumstellar matter, indicate that the 1.53um feature
might point to episodes of dust production in carbon-rich Miras.
Description:
The table provided is a merged version of several tables from our
paper. It contains some observational properties as described in Table
1 (e.g., coordinates, MJD, host galaxy) and some other properties
taken from the literature as described in Table B.1 (e.g., period,
amplitude, bolometric magnitudes). The synthetic colors and the values
of the indexes derived from our spectra are also available (as listed
in Tables E.1 and E.2).
The X-shooter spectra originally cover three wavelength ranges,
referred to as arms (ultraviolet-blue (UVB), visible (VIS) and
near-infrared (NIR)) and they are merged to create one single spectrum
that covers the following wavelength range: 300nm to 2400nm.
Therefore, each arm has its own resolution: 9100 for the UVB, 11000
for the VIS and 7700 for the NIR.
The output spectra were heavily smoothed to a common resolution:
R∼2000, in the NIR. The resolution is highest in the two other arms.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 293 35 Properties of our sample of 35 carbon stars
fits/* . 35 *Individual fits spectra
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Note on fits/*: Each spectrum is from 300nm to 2400nm with a size of
1139Kibytes.
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Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Name of the star (from table 1)
25- 26 I2 h RAh Right ascension (J2000) (from table 1)
28- 29 I2 min RAm Right ascension (J2000) (from table 1)
31- 35 F5.2 s RAs Right ascension (J2000) (from table 1)
37 A1 --- DE- Declination sign (J2000) (from table 1)
38- 39 I2 deg DEd Declination (J2000) (from table 1)
41- 42 I2 arcmin DEm Declination (J2000) (from table 1)
44- 47 F4.1 arcsec DEs Declination (J2000) (from table 1)
49- 51 A3 --- Host Host galaxy (from table 1)
53- 55 A3 --- ESOPer ESO observing period (from table 1)
57- 62 I6 --- OBid ESO observing block identification number
(from table 1)
64- 71 F8.2 d MJD Modified Julian Date (from table 1)
73- 75 A3 --- FluxIssue Note about the flux calibration issue
(from table 1) (1)
77 I1 --- Group ? Group classification (from table 1)
79 A1 --- 1.53um? [Y] Presence of the 1.53 micron feature
(from table 1) (2)
81 A1 --- InputCat Input catalog used in the initial construction
of the X-shooter sample (from table B.1) (3)
83- 86 I4 d Per ? Period of the star (from table B.1) (4)
87 A1 --- u_Per Uncertainty flag on Per
89 A1 --- l_Amp [~<] Limit flag on Amp
90- 93 F4.2 mag Amp ? Amplitude of variation (from table B.1) (5)
94- 99 A6 --- n_Amp Note on amplitude
101 A1 --- Band [VIK] Band used for the period and amplitude
determination (from table B.1)
103-105 A3 --- r_Amp Reference used for the period and amplitude
determination (from table B.1) (3)
107-111 A5 --- VarType Variability types (from table B.1) (6)
113-117 A5 --- r_LC Light curves references (from table B.1)
119-125 A7 --- n_LC Light curves description (from table B.1) (7)
127-131 F5.2 mag Kmag K magnitude taken from 2MASS (Cutri et al.,
2003, Cat. II/246) (from table B.1)
133-136 F4.2 mag J-K (J-K) color taken from 2MASS (Cutri et al.,
2003, Cat. II/246) (from Table B.1)
138-142 F5.2 mag Mbol Absolute bolometric magnitude
(from table B.1) (8)
143 A1 --- n_Mbol [)] ) indicates apparent bolometric magnitude
145 A1 --- r_Mbol References used for the bolometric magnitudes
(from table B.1) (3)
147-150 F4.2 mag R-I ? R-I color index derived by us
(from table E.1) (9)
152-155 F4.2 mag R-H ? R-H color index derived by us
(from table E.1) (9)
157-160 F4.2 mag I-H ? I-H color index derived by us
(from table E.1) (9)
162-165 F4.2 mag I-Ks ? I-Ks color index derived by us
(from table E.1) (9)
167-170 F4.2 mag J-H ? J-H color index derived by us
(from table E.1) (9)
172-175 F4.2 mag H-Ks ? H-Ks color index derived by us
(from table E.1) (9)
177-180 F4.2 mag J-Ks ? J-Ks color dindex derived by us
(from table E.1) (9)
182-185 F4.2 --- COH ? Calculation of the 12CO index in the
H band (from table E.2)
187-190 F4.2 --- CO12 ? Calculation of the 12CO(2,0) index in the
K band (at 2.29 micron) (from table E.2)
192-195 F4.2 --- CO13 ? Calculation of the 13CO(2,0) index in the
K band (at 2.53 micron) (from table E.2)
197-200 F4.2 --- CN ? Calculation of the CN index at 1.11 micron
(from table E.2)
202-205 F4.2 --- C2U ? Calculation of the C2U index at
0.5165 micron (from table E.2)
207-210 F4.2 --- C2 ? Calculation of the C2 index at 1.77 micron
(from table E.2)
212-216 F5.2 --- DIP153 ? Calculation of the HCN+C2H2 index at
1.53 micron (from table E.2)
218-221 F4.2 --- rmsH ? Calculation of the high-frequency structure
in the H band (from table E.2)
223-226 F4.2 --- rmsK ? Calculation of the high-frequency structure
in the K band (from table E.2)
228-251 A24 --- Obs.date Observation date
253-293 A41 --- FileName Name of FITS file, in subdirectory fits
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Note (1): The letter indicates for which X-shooter arm no absolute
flux-calibration was possible, as follows:
V = visible,
N = near-infrared
S = spectrum is saturated in the K-band
Note (2): Y = presence of the 1.53 micron absorption band.
Note (3): References as follows:
a = Hughes & Wood (1990AJ.....99..784H 1990AJ.....99..784H, Cat. J/AJ/99/784)
b = Bergeat et al. (2002A&A...390..967B 2002A&A...390..967B, Cat. J/A+A/390/967). Stars found
non-variable by these authors based on Hipparcos satellite photometry
are labelled nv in Col. VarType.
c = Lancon & Wood (2000A&AS..146..217L 2000A&AS..146..217L, Cat. J/A+AS/146/217)
e = Christlieb et al. (2001A&A...375..366C 2001A&A...375..366C, Cat. J/A+A/375/366)
f = Whitelock et al. (2006MNRAS.369..751W 2006MNRAS.369..751W, Cat. J/MNRAS/369/751)
g = Cioni et al. (2003A&A...406...51C 2003A&A...406...51C, Cat. J/A+A/406/51/) with updates from
Raimondo et al. (2005A&A...438..521R 2005A&A...438..521R, Cat. J/A+A/438/521)
h = Frogel et al. (1990ApJ...352...96F 1990ApJ...352...96F) with the distance moduli (m-M)=18.90
for SMC cluster NGC 419 (Sloan et al. 2016, in prep.) and
(m-M)=19.06 for NGC 121 (Glatt et al. 2008AJ....136.1703G 2008AJ....136.1703G,
Cat. J/AJ/136/1703)
i = General Catalog of Variable Stars (GCVS) (Samus et al., 2007-2012,
Cat. B/gcvs)
k = OGLE LMC data in V and I (Soszynski et al., 2009AcA....59..239S 2009AcA....59..239S,
Cat. J/AcA/59/239, via Vizier)
l = OGLE SMC data in V and I (Soszynski et al., 2011AcA....61..217S 2011AcA....61..217S,
Cat. J/AcA/61/217, via Vizier)
m = EROS data in B and R (Kim et al., 2014A&A...566A..43K 2014A&A...566A..43K,
Cat. J/A+A/566/A43)
n = MACHO data in B and R (Alcock et al., 1996MNRAS.280L..49A 1996MNRAS.280L..49A,
2001, Cat. J/ApJ/562/337, via Vizier).
o = DIRBE data in J and K (Price et al., 2010ApJS..190..203P 2010ApJS..190..203P,
Cat. J/ApJS/190/203, via Vizier).
p = Association Francaise des Observateurs d'Etoiles Variables (AFOEV).
q = American Association of Variable Star Observers (AAVSO).
r = ASAS data in V (Pojmanski, 2002AcA....52..397P 2002AcA....52..397P, Cat. II/264, via Vizier)
s = Our estimate based on (J-K) and Nowotny et al. (2013A&A...552A..20N 2013A&A...552A..20N)
Note (4): Periods followed by a colon are highly uncertain, as the corresponding
light curves are very irregular (for most of these stars, a detailed
literature search produces half a dozen of very different periods depending
on passband, method, and time of observation).
Note (5): The amplitudes given are representative of the peak-to-peak variations
over long time spans rather than single-period fits of sine functions (for
V CrA, the amplitude given does not include the deep obscuration events).
Note (6): The SR and M variability types are based on amplitude (as is common
practice), not on the shape of the light curve.
Note (7): Light curves description flags as follows:
irr = irregular
irr.d = irregular with marked dips in brightness
irr.a = irregular with marked changes in amplitude
reg = mostly regular
reg.d1 = mostly regular with one dip near the end of the available time
series
reg.at = mostly regular with variations in amplitude and mean magnitude
comparable to half the mean amplitude
reg.atV = same as reg.at but with larger variations in the OGLE V light curve
reg.t = mostly regular short period pattern, but long term trends in the
mean that are comparable or larger than the amplitude (possibly
associated with a secondary long period)
Note (8): The bolometric magnitudes are apparent when followed by a parenthesis,
absolute otherwise.
Note (9): The synthetic magnitudes were derived using the Bessell filters R and
I (1990PASP..102.1181), and the 2MASS filters (Cohen et al.,
2003AJ....126.1090C 2003AJ....126.1090C) J, H and Ks.
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Acknowledgements:
Anais Gonneau, anais.gonneau(at)astro.unistra.fr
(End) Patricia Vannier [CDS] 24-Feb-2016