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J/ApJS/120/247      Supernova remnants in M33                (Gordon+, 1999)

A new sample of radio-selected and optically confirmed supernova remnants in M33 Gordon S.M., Duric N., Kirshner R.P., Goss W.M., Viallefond F. <Astrophys. J. Suppl. Ser. 120, 247 (1999)> =1999ApJS..120..247G
ADC_Keywords: Supernova remnants ; Radio sources Keywords: galaxies: individual (M33) - galaxies: ISM - radio continuum: ISM - supernova remnants Abstract: Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&AS...99..217D). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 68 186 Radio sources in M 33 table4.dat 67 53 Radio-selected sample of supernova remnants
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [GDK99] Identification number ([GDK99] NNN in Simbad) 5- 6 I2 h RAh Right ascension (J2000) 8- 9 I2 min RAm Right ascension (J2000) 11- 15 F5.2 s RAs Right ascension (J2000) 17 A1 --- DE- Declination sign (J2000) 18- 19 I2 deg DEd Declination (J2000) 21- 22 I2 arcmin DEm Declination (J2000) 24- 28 F5.2 arcsec DEs Declination (J2000) 30- 34 F5.1 mJy S20cm Total flux at 20cm (1.5GHz) 36- 38 F3.1 mJy e_S20cm rms uncertainty on S20cm 40 A1 --- l_S6cm Limit flag on S6cm 41- 44 F4.1 mJy S6cm Total flux at 6cm (5GHz) 46- 48 F3.1 mJy e_S6cm ? rms uncertainty on S6cm 50 A1 --- l_Sp+Index Limit flag on Sp+Index 51- 54 F4.1 --- Sp+Index Spectral index of the source 56- 58 F3.1 --- e_Sp+Index ? rms uncertainty on Sp+Index 60- 68 A9 --- OptID Optical identification (1)
Note (1): the symbols have the following meaning: OI denotes the radiosurces that where outside the ield of view of the optical image SNR denotes the confirmed SNR SNRc denotes the SNR candidate H II denotes the H II region BGND-NOE denotes the background, no optical emission BGND-FOE denotes the background, faint optical emission BGND-STR denotes the background, stellar-like source GC denotes the galactic center * represent the H II regions with nonthermal spectral indices
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [GDK99] Identification number ([GDK99] NNN in Simbad) 5- 6 I2 --- M33SNR Gordon et al. (1998ApJS..117...89G) identification number (M33SNR NN in Simbad) 8- 9 I2 h RAh right ascension (J2000) 11- 12 I2 min RAm right ascension (J2000) 14- 17 F4.1 s RAs right ascension (J2000) 19 A1 --- DE- Declination sign (J2000) 20- 21 I2 deg DEd Declination (J2000) 23- 24 I2 arcmin DEm Declination (J2000) 26- 27 I2 arcsec DEs Declination (J2000) 29- 31 I3 pc Diam Diameter (1) 32 A1 --- n_Diam [*] Note on Diam (1) 34 A1 --- l_S20cm Limit flag on S20cm 35- 37 F3.1 mJy S20cm Total flux at 20cm (1.5GHz) 39- 41 F3.1 mJy e_S20cm ? rms uncertainty on S20cm 43 A1 --- l_S6cm Limit flag on S6cm 44- 46 F3.1 mJy S6cm Total flux at 6cm (5GHz) 48- 50 F3.1 mJy e_S6cm ? rms uncertainty on S6cm 52 A1 --- l_Sp+Index Limit flag on Sp+Index 53- 56 F4.1 --- Sp+Index Spectral index 58- 60 F3.1 --- e_Sp+Index ? rms uncertainty on Sp+Index 62 A1 --- Tc [x] Thermal correction (2) 64- 67 A4 --- SpConf Spectral confirmation (3)
Note (1): Diameters as measured from optical images. Geometric mean for noncircular objects. * indicates that measurement is highly uncertain due to optical confusion. At 840 kpc, 1"=4.08pc Note (2): x indicates that the radio fluxes are corrected for thermal contamination Note (3): Sources for optical spectroscopy: G98: Gordon et al., 1998ApJS..117...89G (<M33SNR NN>) S93: Smith et al., 1993ApJ...407..564S BK85: Blair & Kirshner, 1985ApJ...289..582B
History: From ApJS electronic version
(End) James Marcout, Patricia Bauer [CDS] 27-May-1999
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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