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II/187A             30 Doradus OB Associations    (Parker 1992)

30 Doradus in the Large Magellanic Cloud: The Stellar Content and Initial Mass Function Parker, J. W. <Publ. Astron. Soc. Pac. 104, 1107 (1992)> <Astron. J. 106, 560 (1993)> <Astron. J. 106, 1471 (1993)> =1992PASP..104.1107P =1993AJ....106..560P =1993AJ....106.1471P
ADC_Keywords: Magellanic Clouds; Clusters, open; Photometry, UBV Abstract: Johnson UBV photometry is presented for 2395 stars in the OB associations of 30 Doradus in the Large Magellanic Cloud. The CCD fields cover an area of 50 square arcminutes in the central region. The entire catalog (exclusive of the dense core cluster R136) is photometrically complete to V=B=18mag and U=17mag, although the completeness magnitudes are fainter for regions with less nebular contamination. Description: These data have been reduced from 39 CCD frames (with short, medium, and long exposure times ranging from 3 to 1000 seconds) using the photometry program DAOPHOT (Peter Stetson, 1987PASP...99..191S). The photometric errors listed in these tables are the errors derived by DAOPHOT using the relative magnitude of the star on the CCD and the goodness of the fit of the point spread function. Most stars appear on more than one CCD frame per filter, and their resulting tabulated magnitudes are the averages of the individual measurements inversely weighted by the squares of their errors. The stars in these tables are from two regions: the central region and a non-overlapping northern region. The latter are designated by four digit numbers starting with 9. The X,Y coordinates are the positions relative to the northwestern-most corner of each region. Notes and remarks (B. Skiff): Precise coordinates on the ICRS system were determined by B. Skiff in March 2008, by identifying 68 relatively bright and isolated stars in either UCAC2 (Cat. I/289) or 2MASS (Cat. II/246). The x,y coordinates were transformed using a quadratic least-squares fit, giving resulting rms residuals of 0.14arcsec. A separate reduction was done on the 'north' field (stars numbered 9001-9045), which gave similar results from a linear fit. It should be noticed too that in the original table 5, the positions are offset by three lines, such that, for example, the bright star 9009 actually has the coordinates of star 9006. This error has been removed in this revised version. (The coordinates for these stars are correct in Tables 11 and 12.) It was apparent while checking the data for individual stars that the catalogue includes false detections. This was first discussed by Parker & Garmany (1993AJ....106.1471P, sec 3.2 and Figure 5) shortly after the catalogue itself was published. Many of the faint entries having V≳17 result from the star-finding algorithm having picked up small clumps in the overlying nebulosity. Among the distinguishing characteristics of the false entries are non-physical photometric colors. Rubio et al (1998AJ....116.1708R) also report that a match-up of HST images against the Parker list shows blank sky at the positions for most of the faintest stars. The original data can be retrieved from the file "tables.ori". File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file photo.dat 106 2395 Positional and photometric data (tables 4 and 5) spectro.dat 125 302 Spectroscopic data (tables 11 and 12) tables.ori 134 3178 Original data material from J.W. Parker
See also: J/A+A/341/98 : The ionizing cluster of 30 Doradus. I. (Selman+ 1999) J/A+A/443/851 : Effective temperature of 30 Dor population (Selman+, 2005) J/AJ/107/1054 : UBV photometry of the 30 Dor region (Malumuth+, 1994) Byte-by-byte Description of file: photo.dat
Bytes Format Units Label Explanations
3- 6 I4 --- Num [1/9045] Running number ([P93] in Simbad) 11- 12 I2 h RAh Right ascension J2000 (1) 14- 15 I2 min RAm Right ascension J2000 (1) 17- 22 F6.3 s RAs Right ascension J2000 (1) 24 A1 --- DE- Declination sign J2000 (1) 25- 26 I2 deg DEd Declination J2000 (1) 28- 29 I2 arcmin DEm Declination J2000 (1) 31- 35 F5.2 arcsec DEs Declination J2000 (1) 38- 43 F6.2 pix Xpos X position (2) 46- 52 F7.2 pix Ypos Y position (2) 56- 61 F6.3 mag Vmag V magnitude, in Johnson system 65- 70 F6.3 mag B-V B-V color, in Johnson system 74- 79 F6.3 mag U-B ?=99.000 U-B color, in Johnson system (3) 84- 88 F5.3 mag e_Vmag Vmag accuracy 93- 97 F5.3 mag e_B-V B-V accuracy 102-106 F5.3 mag e_U-B ?=9.000 U-B accuracy
Note (1): Position recomputed in March, 2008, see some details in the "Notes and remarks" section above. Note (2): coordinates are from the CCD finder charts in the reference. Pixel sizes (in X and Y columns) are approximately 0.49arcsec/pixel Note (3): 99.000 indicates no value for U-B. Note that most of the stars having U-B < -1.3 tend to have large errors in U because they are relatively faint or are blended
Byte-by-byte Description of file: spectro.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Num [1/9045] Running number (7) 6 A1 --- n_Num [r] indicates a star too faint or red (7) 7- 8 I2 h RAh Original Right ascension 2000 (1) 10- 11 I2 min RAm Original Right ascension 2000 (1) 13- 16 F4.1 s RAs Original Right ascension 2000 (1) 19 A1 --- DE- Original Declination sign 2000 (1) 20- 21 I2 deg DEd Original Declination 2000 (1) 23- 24 I2 arcmin DEm Original Declination 2000 (1) 26- 27 I2 arcsec DEs Original Declination 2000 (1) 31- 35 F5.1 pix Xpos X position 39- 43 F5.1 pix Ypos Y position 46- 50 F5.2 mag Vmag V magnitude in Johnson system 53- 57 F5.2 mag B-V B-V color in Johnson system 60- 64 F5.2 mag U-B U-B color in Johnson system 67- 71 F5.2 mag Q Q = (U-B) - 0.72(B-V) 75- 78 F4.2 mag E(B-V) Color excess in B-V calculated from Q 81- 85 F5.2 mag Mv Absolute V magnitude (2) 88- 91 F4.2 [K] Teff Log effective temperature (3) 93- 98 F6.2 mag Mbol Bolometric absolute magnitude (4) 101-112 A12 --- Sp MK spectral type (5) 115-125 A11 --- Com Comments (6)
Note (1): a more accurate position is available from the "photo.dat" file, see the "Notes and remarks" section above. Note on (2): Mv is the absolute V magnitude = V - Rv * E(B-V) - DM where Rv = 3.1, and the distance modulus DM = 18.5 mag. Note (3): is the log10 of the effective temperature, and is calculated from Q or (B-V)0 as discussed in Section 3.1 of Paper II (1993AJ....106.1471P) Note (4): is the bolometric magnitude = Mv + BC, where BC is calculated from Teff as discussed in Section 3.1 of Paper II (1993AJ....106.1471P) Note (5): Sp is the 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. Note (6): Comments are 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 = has been observed by the author and the spectrogram appears in Figure 6 or 7 of Paper I (1993AJ....106..560P) J = as j, with spectral type agreement. p = peculiar (details in text of Paper I, 1993AJ....106..560P) m = has been observed by Melnick (1985A&A...153..235M) M = as m, with spectral type agreement. w = has been observed by Walborn (1986, IAU Symp. 116, 185; 1992 - unpublished classifications) or Walborn & Blades (1987ApJ...323L..65W) W = as w, with spectral type agreement. z = ZAMS O star The uppercase letters "J", "M", "W", indicate the sources of the spectral types listed in the 'Sp' column; two or all three letters may be uppercase if they agree on the same classification. Note (7): stars without the suffix 'r' are the Bluest (Q←0.7) and Brightest (V<16) Stars in 30 Doradus.
Courtesy: Joel Parker <joel(at)> Historical Notes: * 17-May-1994: First archived (Nancy G. Roman, NASA/NSSDC/ADC) * 15-Mar-1995: Corrected reference (PASP 104) and standardized this file (CDS) * 20-Jul-1995: Removed the colons (:) between RAh:RAm:RAs and DEd:DEm:DEs in data files (Francois Ochsenbein, CDS) * 05-Mar-2008: accurate position by B. Skiff in the photo.dat file (catalog renumbered II/187A)
(End) Joel Parker, Nancy G. Roman, Brian Skiff, Francois Ochsenbein 05-Mar-2008
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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