J/AJ/103/1205 J/AJ/103/1205 Stellar Content of LH 9 and 10 in the LMC J W Parker C D Garmany P Massey N R Walborn Astron. J. 103 1205 1992 1992AJ....103.1205P Magellanic Clouds Photometry, UBV We present CCD photometry and spectroscopy for stars in Lucke-Hodge 9 and 10, two adjacent OB association in the northwest corner of the LMC. Our catalog contains UBV photometry (complete to ~18min in all three filters) for 795 stars and BV-only photometry (complete to ~19min in both filters) for an additional 434 stars.

Star Star number number=1 Stars with numbers <3000 are in LH 9, and numbers >3000 are in LH 10. Star numbers 1001 through 1522 are from Table 3. Star numbers 2001 through 2345 are from Table 4. Star numbers 3001 through 3273 are from Table 5. Star numbers 4001 through 4089 are from Table 6. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Xpos X position number=2 Since the CCD frames for these fields (LH 9 and 10) are not contiguous, the X and Y coordinates refer to different coordinate systems for LH 9 and LH10; for orientation of the coordinate systems see the CCD finder charts in the article. Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Ypos Y position number=2 Since the CCD frames for these fields (LH 9 and 10) are not contiguous, the X and Y coordinates refer to different coordinate systems for LH 9 and LH10; for orientation of the coordinate systems see the CCD finder charts in the article. Pixel sizes (in X and Y columns) are approximately 0.49 arcsec/pixel. pix Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag e_Vmag Error on V magnitude mag e_B-V Error on B-V colour mag e_U-B Error on U-B colour mag Star Star number number=1 Stars numbers 1001 through 1522 are located in LH 9 (Table 10), and 3001 through 3273 in LH 10 (Table 11). In the journal article, Tables 10 and 11 listed the Bluest (Q<-0.7) and Brightest (V<16) Stars in LH 9 and 10, and Table 12 listed other stars with known spectral types. The table here contains ALL stars with UBV photometry (e.g., all stars that are listed in Tables 3 and 5), and includes their bolometric magnitudes and effective temperatures which were not listed in the original tables. --- RAh Right ascension (2000) h RAm Right ascension (2000) min RAs Right ascension (2000) s DE- Declination sign --- DEd Declination (2000) deg DEm Declination (2000) arcmin DEs Declination (2000) arcsec Xpos X position number=2 Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems: they are from the CCD finder charts in the article. Pixel sizes are approximately 0.49 arcsec/pixel. pix Ypos Y position number=2 Since these fields are not contiguous, the X,Y coordinates refer to different coordinate systems: they are from the CCD finder charts in the article. Pixel sizes are approximately 0.49 arcsec/pixel. pix Vmag V magnitude mag B-V B-V colour index mag U-B U-B colour index mag Q (U-B)-0.72(B-V) mag E(B-V) Color excess calculated from Q or spectral type or mean reddening as discussed in Section 3.1 of the article. mag Mv Absolute V magnitude=V-Rv*E(B-V)-DM where Rv=3.1, and the distance modulus DM=18.3 mag mag log(Teff) log10 of the effective temperature: is calculated from Q or (B-V)0 as discussed in Section 3.2 of the article. K Mbol Bolometric magnitude=Mv+BC, where BC is calculated from Teff as discussed in Section 3.2 of the article. mag Sp Spectral type and luminosity class as determined from spectroscopic observations number=3 One colon ":" indicates an uncertainty of one spectral subtype or luminosity class, and two colons "::" indicate a larger uncertainty. --- Comments Comments number=4 Comments in square brackets, [], are indicated by the following codes (note that these codes are somewhat different than those that appear in the original paper): [a]: strong Balmer lines [b]: possible composite / blend; spectrum contaminated by nearby star (in some cases the number of the other star is given in parentheses) [c]: cosmic ray hits / bad pixels [d]: weak Balmer lines [e]: strong nebular emission in the Balmer lines [g]: weak N lines [p]: Star 3264 is a ZAMS star with extremely strong nebular emission lines and is located in the compact HII knot N 11A (see text) [z]: ZAMS O star --- Simona Mei CDS 1995Apr04Joel Wm. Parker <joel.parker@gsfc.nasa.gov> J_AJ_103_1205.xml