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J/A+A/378/556       UVES/VLT spectra of white dwarfs         (Koester+, 2001)

High-resolution UVES/VLT spectra of white dwarfs for the ESO SN Ia progenitor survey (SPY). I. Koester D., Napiwotzki R., Christlieb N., Drechsel H., Hagen H.J., Heber U., Homeier D., Karl C., Leibundgut B., Moehler S., Nelemans G., Reimers D., Reinecke E-M., Renzini A., Yungelson L. <Astron. Astrophys. 378, 556 (2001)> =2001A&A...378..556K
ADC_Keywords: Stars, white dwarf ; Magnitudes ; Effective temperatures ; Stars, masses Keywords: stars: white dwarfs - stars: supernovae: general Abstract: We have started a large survey for radial velocity variations in white dwarfs (PI R. Napiwotzki) with the aim of finding close double degenerates, which could be precursor systems for SNe Ia. The UVES spectrograph at the ESO VLT is used to obtain high resolution spectra with good S/N. During this project 1500 white dwarfs will be observed. This unique data set will also allow to derive atmospheric parameters and masses for the largest sample of white dwarfs ever analyzed in a homogeneous way. In this paper we present a catalog of objects and report results for the first sample of about 200 white dwarfs, many of which are spectroscopic confirmations of candidates from the Hamburg ESO Quasar Survey (HE, Cat. J/A+AS/115/235), Montreal-Cambridge-Tololo Survey (MCT), and Edinburgh-Cape Survey (EC, Cat. J/MNRAS/287/867) surveys. Among the peculiar spectra we identify two new magnetic DA, one previously known magnetic DA, several DA with emission cores, in some cases due to a late-type companion, and two new DBA. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 79 261 Observed DA and parameters from spectral fitting
See also: J/A+AS/115/235 : The Hamburg/ESO survey for bright QSOs. II. (Reimers+, 1996) J/MNRAS/287/867 : Edinburgh-Cape Blue Object Survey. Zone 1. (Kilkenny+ 1997) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Object name, based on B1950 coordinates (1) 13 A1 --- n_Name [j] j: Name based on J2000 coordinates 15- 16 I2 h RAh Right ascension (J2000) 17 A1 --- --- [:] 18- 19 I2 min RAm Right ascension (J2000) 20 A1 --- --- [:] 21- 24 F4.1 s RAs Right ascension (J2000) 26 A1 --- DE- Declination sign (J2000) 27- 28 I2 deg DEd Declination (J2000) 29 A1 --- --- [:] 30- 31 I2 arcmin DEm Declination (J2000) 32 A1 --- --- [:] 33- 34 I2 arcsec DEs Declination (J2000) 36- 40 F5.2 mag Vmag V magnitude (or B or v, see n_Vmag) 41 A1 --- n_Vmag [Bv] B: photographic B magnitude in Vmag v: multichannel v magnitude in vmag 44- 48 I5 K Teff Effective temperature 50- 53 I4 K e_Teff rms uncertainty on Teff 55- 58 F4.2 [cm/s2] logg Surface gravity 61- 64 F4.2 [cm/s2] e_logg rms uncertainty on logg 66- 70 F5.2 --- chi2 χ2 of the best fit 72- 75 F4.2 solMass Mass Mass 77- 79 A3 --- Rem Remark (2)
Note (1): Object names: WDHHMM+DDd: White Dwarf (Cat. III/129, III/210) MCTHHMM+DDMM: Montreal-Cambridge-Tololo survey ECHHMMm-DDMM: Edinburgh-Cape survey HEHHMM+DDMM : Hamburg-ESO Survey Note (2): Remarks: 1: no good fit to Balmer line cores 2: no good fit possible; although the fitting routine gives a solution with reasonable χ2, which we have kept in the table, visual inspection shows that the fit does not reproduce a correct Balmer decrement. The mass value is not included in the table and in the calculation of the mass distribution. The core of Hα may be different between the two spectra 3: known double-degenerate G271-115 = EG11 = GJ 64 (Bergeron et al., 1989ApJ...345L..91B) 4: Hα and Hβ with core filled-in (emission core?) 5: Hα emission core 6: known DAB (Jordan et al., 1993A&A...273L..27J) fit is with pure hydrogen models 7: double core in Hα variable between the two spectra 8: interstellar CaII 9: narrow CaII; possibly interstellar, but velocity difference to Balmer lines <10km/s 10: strong CaII K; Hα with emission core 11: change in line profiles between two spectra; core filled in? 12: CaII, Hα and Hβ with emission cores 13: possibly weak broad CaII N: parameters from fit with NLTE atmosphere grid.
Acknowledgements: Detlev Koester
(End) Patricia Bauer [CDS] 27-Sep-2001
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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