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J/AJ/103/1205 Stellar Content of LH 9 and 10 in the LMC (Parker+ 1992)
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The Stellar Content of LH 9 and 10 (N 11) in the LMC: A Case for Sequential
Star Formation
Parker J.WM., Garmany C.D., Massey P., Walborn N.R.
<Astron. J. 103, 1205 (1992)>
=1992AJ....103.1205P (SIMBAD/NED Reference)
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ADC_Keywords: Magellanic Clouds; Associations, stellar; Photometry, CCD;
Photometry, UBV; Spectroscopy; Spectral types
Description:
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 ~18mag in all
three filters) for 795 stars and BV-only photometry (complete to
~19mag in both filters) for an additional 434 stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
ubv.dat 97 1229 UBV data from Tables 3-6 in the paper
stars.dat 133 795 All stars with UBV photometry with their
bolometric magnitudes and effective
temperatures which were not listed in the
original tables (tables 10 to 12).
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Byte-by-byte Description of file: ubv.dat
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Bytes Format Units Label Explanations
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2- 5 A4 --- Star Star number (1)
9 I1 h RAh Right ascension (2000)
11- 12 I2 min RAm Right ascension (2000)
14- 18 F5.2 s RAs Right ascension (2000)
21 A1 --- DE- Declination sign
22- 23 I2 deg DEd Declination (2000)
25- 26 I2 arcmin DEm Declination (2000)
28- 31 F4.1 arcsec DEs Declination (2000)
36- 41 F6.2 pix Xpos X position (2)
44- 49 F6.2 pix Ypos Y position (2)
52- 57 F6.3 mag Vmag V magnitude
60- 65 F6.3 mag B-V B-V colour index
68- 73 F6.3 mag U-B ?=99.000 U-B colour index (3)
77- 81 F5.3 mag e_Vmag Error on V magnitude
85- 89 F5.3 mag e_B-V Error on B-V colour
93- 97 F5.3 mag e_U-B ?=9.000 Error on U-B colour (3)
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Note (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.
Note (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.
Note (3): Stars without U photometry are flagged by U-B = 99.000 and
U-B err = 9.000.
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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2- 5 A4 --- Star Star number (1)
9 I1 h RAh Right ascension (2000)
11- 12 I2 min RAm Right ascension (2000)
14- 18 F5.2 s RAs Right ascension (2000)
21 A1 --- DE- Declination sign
22- 23 I2 deg DEd Declination (2000)
25- 26 I2 arcmin DEm Declination (2000)
28- 31 F4.1 arcsec DEs Declination (2000)
36- 40 F5.1 pix Xpos X position (2)
43- 47 F5.1 pix Ypos Y position (2)
50- 54 F5.2 mag Vmag V magnitude
57- 61 F5.2 mag B-V B-V colour index
64- 68 F5.2 mag U-B U-B colour index
71- 75 F5.2 mag Q (U-B)-0.72(B-V)
79- 82 F4.2 mag E(B-V) Color excess calculated from Q or spectral
type or mean reddening as discussed in
Section 3.1 of the article.
84- 89 F6.2 mag Mv Absolute V magnitude=V-Rv*E(B-V)-DM where
Rv=3.1, and the distance modulus DM=18.3 mag
93- 96 F4.2 [K] log(Teff) log10 of the effective temperature: is
calculated from Q or (B-V)0 as discussed in
Section 3.2 of the article.
98-103 F6.2 mag Mbol Bolometric magnitude=Mv+BC, where BC is
calculated from Teff as discussed in
Section 3.2 of the article.
106-118 A13 --- Sp Spectral type and luminosity class as
determined from spectroscopic observations (3)
120-132 A13 --- Comments Comments (4)
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Note (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.
Note (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.
Note (3): One colon ":" indicates an uncertainty of one spectral subtype or
luminosity class, and two colons "::" indicate a larger uncertainty.
Note (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
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Courtesy: Joel Wm. Parker <joel.parker@gsfc.nasa.gov>
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(End) Simona Mei [CDS] 04-Apr-1995