CDROM/AJ/V106/P0560 30 Doradus. I. (Parker 1993) ================================================================================ The OB Associations of 30 Doradus in the Large Magellanic Cloud. I. Stellar Observations and Data Reductions Joel Wm. Parker <1993, AJ, 106, 560> =1993AJ....106..560P ================================================================================ Abstract: UBV photometry is presented for 2400 stars in the OB associations of 30 Doradus in the Large Magellanic Cloud, and I discuss new spectroscopic observations of 54 stars including 24 O stars. The CCD fields cover an area of 50 square arcminutes in the central region. The entire catalog (exclusive of the dense core cluster R 136) is photometrically complete to V = B = 18 mag and U = 17 mag, although the completeness magnitudes are fainter for regions with less nebular contamination. File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table4.dat 101 2350 UBV photometry of the stars in 30 Doradus table5.dat 101 45 UBV photometry of the stars in the northern region of 30 Doradus table11.dat 126 267 The bluest (Q < -0.7) and brightest (V < 16) stars in 30 Doradus table12.dat 126 35 Other stars with spectral classifications -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 1X --- --- Blank 2- 6 I5 --- Star Running ID number 7- 8 2X --- --- Blank 9 I2 h RAh Right ascension (2000.0) 11 1X --- --- : separator 12- 13 I2 min RAm Right ascension 14 1X --- --- : separator 15- 18 F4.1 s RAs Right ascension 19- 20 2X --- --- Blank 21 A1 --- DE- Sign of declination (2000.0) 22- 23 I2 deg DEd Declination 24 1X --- --- : separator 25- 26 I2 arcmin DEm Declination 27 1X --- --- : separator 28- 29 I2 arcsec DEs Declination 30- 38 F9.2 pix X *X pixel coordinate 39- 47 F9.2 pix Y *Y pixel coordinate 48- 56 F9.3 mag V V magnitude 57- 65 F9.3 mag B-V B-V color 66- 74 F9.3 mag U-B []? U-B color 75- 83 F9.3 mag e_V Error in V 84- 92 F9.3 mag e_B-V Error in B-V 93-101 F9.3 mag e_U-B []? Error in U-B -------------------------------------------------------------------------------- Notes for file: table4.dat -------------------------------------------------------------------------------- X, Y: X and Y coordinates are from the CCD finder charts in the printed paper. Pixel sizes are approximately 0.49 arcsec/pixel. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 1X --- --- Blank 2- 6 I5 --- Star Running ID number 7- 8 2X --- --- Blank 9- 10 I2 h RAh Right ascension (2000.0) 11 1X --- --- : separator 12- 13 I2 min RAm Right ascension 14 1X --- --- : separator 15- 18 F4.1 s RAs Right ascension 19- 20 2X --- --- Blank 21 A1 --- DE- Sign of declination (2000.0) 22- 23 I2 deg DEd Declination 24 1X --- --- : separator 25- 26 I2 arcmin DEm Declination 27 1X --- --- : separator 28- 29 I2 arcsec DEs Declination 30- 38 F9.2 pixel X *X pixel coordinate 39- 47 F9.2 pixel Y *Y pixel coordinate 48- 56 F9.3 mag V V magnitude 57- 65 F9.3 mag B-V B-V color 66- 74 F9.3 mag U-B U-B color 75- 83 F9.3 mag e_V Error in V 84- 92 F9.3 mag e_B-V Error in B-V 93-101 F9.3 mag e_U-B Error in U-B -------------------------------------------------------------------------------- Notes for file: table5.dat -------------------------------------------------------------------------------- X, Y: X and Y coordinates are from the CCD finder charts in the printed paper. Pixel sizes are approximately 0.49 arcsec/pixel. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table11.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- Star *Running ID number 6 1X --- --- Blank 7- 8 I2 h RAh Right ascension (2000.0) 9 1X --- --- : separator 10- 11 I2 min RAm Right ascension 12 1X --- --- : separator 13- 16 F4.1 s RAs Right ascension 17- 18 2X --- --- Blank 19 A1 --- DE- Sign of declination (2000.0) 20- 21 I2 deg DEd Declination 22 1X --- --- : separator 23- 24 I2 arcmin DEm Declination 25 1X --- --- : separator 26- 27 I2 arcsec DEs Declination 28- 35 F8.2 pix X *X pixel coordinate 36- 43 F8.2 pix Y *Y pixel coordinate 44- 50 F7.4 mag V Johnson V magnitude 51- 57 F7.4 mag B-V Johnson B-V color 58- 64 F7.4 mag U-B Johnson U-B color 65- 71 F7.4 mag Q Q value = (U-B) - 0.72(B-V) 72- 78 F7.4 mag E_B-V *Color excess calculated from Q 79- 85 F7.4 mag MV *Absolute visual magnitude 86- 91 F6.2 K Teff *Effective temperature 92- 98 F7.2 mag Mbol *Bolometric magnitude 99-100 2X --- --- Blank 101-112 A12 --- Sp *Spectral type 113-114 2X --- --- Blank 115-126 A12 --- Comments *Miscellaneous notes and comments -------------------------------------------------------------------------------- Notes for file: table11.dat -------------------------------------------------------------------------------- Star: Stars with ID numbers 1 through 2350 are located in the central field, Table 4 of Paper I (this paper), and 9001 through 9045 are in the northern field of 30 Doradus. Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems. X, Y: Pixel coordinates are from the CCD finder charts in the printed paper. Pixel sizes are approximately 0.49 arcsec/pixel. E_B-V: E(B-V) color excess calculated from Q as discussed in Section 2 of Paper II. MV: Absolute V magnitude = V - Rv * E(B-V) - DM where Rv = 3.1, and the distance modulus DM = 18.5 mag. Teff: log10 of the effective temperature, and is calculated from Q or (B-V)0 as discussed in Section 3.1 of Paper II [Parker 1993, AJ, 106, 1471]. Mbol: Mbol = Mv + BC, where BC is calculated from Teff as discussed in Section 3.1 of Paper II. Sp: Spectral type and luminosity class as determined from spectroscopic observations. One colon ":" indicates an uncertainty of one spectral subtype or luminosity class, and two colons "::" indicate a larger uncertainty. Comments: Indicated by the following codes: a --- strong / over-subtracted Balmer lines b --- blend c --- possible composite / spectrum contaminated by nearby star e --- strong nebular emission in the Balmer lines f --- foreground star j,J --- has been observed by the author and the spectrogram appears in Figure 6 or 7 of Paper I. p --- peculiar (details in text of Paper I) m,M --- has been observed by Melnick (1985, A&A, 153, 235) w,W --- has been observed by Walborn (1986, IAU symp 116, p. 185; 1992 unpublished classifications) or Walborn & Blades (1987, ApJ, 323, L65) z --- ZAMS O star The uppercase letters "J", "M", "W", indicate the sources of the spectral types listed in Column 14; two or all three letters may be uppercase if they agree on the same classification. -------------------------------------------------------------------------------- Comments for file: table12.dat -------------------------------------------------------------------------------- These are stars in 30 Doradus that have been classified spectroscopically but are not listed in Table 11 because they either are not blue enough (Q > -0.7) or bright enough (V > 16). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table12.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- Star *Running ID number 6 1X --- --- Blank 7- 8 I2 h RAh Right ascension (2000.0) 9 1X --- --- : separator 10- 11 I2 min RAm Right ascension 12 1X --- --- : separator 13- 16 F4.1 s RAs Right ascension 17- 18 2X --- --- Blank 19 A1 --- DE- Sign of declination (2000.0) 20- 21 I2 deg DEd Declination 22 1X --- --- : separator 23- 24 I2 arcmin DEm Declination 25 1X --- --- : separator 26- 27 I2 arcsec DEs Declination 28- 35 F8.2 pix X *X pixel coordinate 36- 43 F8.2 pix Y *Y pixel coordinate 44- 50 F7.4 mag V V magnitude 51- 57 F7.4 mag B-V B-V color 58- 64 F7.4 mag U-B U-B color 65- 71 F7.4 mag Q Q value 72- 78 F7.4 mag E_B-V *Color excess 79- 85 F7.4 mag MV *Absolute visual magnitude 86- 91 F6.2 K Teff *Effective temperature 92- 98 F7.2 mag Mbol *Bolometric magnitude 99-100 2X --- --- Blank 101-112 A12 --- Sp *Spectral type 113-114 2X --- --- Blank 115-126 A12 --- Comments *Miscellaneous notes and comments -------------------------------------------------------------------------------- Notes for file: table12.dat -------------------------------------------------------------------------------- Star: Stars with ID numbers 1 through 2350 are located in the central field, Table 4 of Paper I (this paper) and 9001 through 9045 are in the northern field of 30 Doradus. Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems. X, Y: Pixel coordinates are from the CCD finder charts in the article given above. Pixel sizes are approximately 0.49 arcsec/pixel. E_B-V: E(B-V) color excess calculated from Q as discussed in Section 2 of Paper II (Parker 1993, AJ, 106, 1471) MV: Absolute V magnitude = V - Rv * E(B-V) - DM where Rv = 3.1, and the distance modulus DM = 18.5 mag. Teff: log10 of the effective temperature, and is calculated from Q or (B-V)0 as discussed in Section 3.1 of Paper II. Mbol: Mbol = Mv + BC, where BC is calculated from Teff as discussed in Section 3.1 of Paper II. Sp: Spectral type and luminosity class as determined from spectroscopic observations. One colon ":" indicates an uncertainty of one spectral subtype or luminosity class, and two colons "::" indicate a larger uncertainty. Comments: Indicated by the following codes: a --- strong / over-subtracted Balmer lines b --- blend c --- possible composite / spectrum contaminated by nearby star e --- strong nebular emission in the Balmer lines f --- foreground star j,J --- has been observed by the author and the spectrogram appears in Figure 6 or 7 of Paper I. p --- peculiar (details in text of Paper I) m,M --- has been observed by Melnick (1985, A&A, 153, 235) w,W --- has been observed by Walborn (1986, IAU symp 116, p. 185; 1992 unpublished classifications) or Walborn & Blades (1987, ApJ, 323, L65) z --- ZAMS O star The uppercase letters "J", "M", "W", indicate the sources of the spectral types listed in Column 14; two or all three letters may be uppercase if they agree on the same classification. -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 15-Mar-1994