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J/AJ/128/1233   LkHα 101 and the young cluster in NGC 1579 (Herbig+, 2004)

LkHα 101 and the young cluster in NGC 1579. Herbig G.H., Andrews S.M., Dahm S.E. <Astron. J., 128, 1233-1253 (2004)> =2004AJ....128.1233H
ADC_Keywords: Clusters, open ; Stars, emission ; Stars, pre-main sequence ; Photometry, Cousins ; Photometry, infrared ; Spectroscopy Keywords: open clusters and associations: individual (NGC 1579) - stars: emission-line, Be - stars: formation - stars: individual (LkHα 101) - stars: pre-main-sequence Abstract: The central region of the dark cloud L1482 is illuminated by LkHα 101, a heavily reddened (AV∼10mag) high-luminosity (≥8x103LSun) star having an unusual emission-line spectrum plus a featureless continuum. About 35 much fainter (mostly between R=16 and >21) Hα emitters have been found in the cloud. Their color-magnitude distribution suggests a median age of about 0.5Myr, with considerable dispersion. There are also at least five bright B-type stars in the cloud, presumably of about the same age; none show the peculiarities expected of HAeBe stars. Dereddened, their apparent V magnitudes lead to a distance of about 700pc. Radio observations suggest that the optical object LkHα 101 is in fact a hot star surrounded by a small H II region, both inside an optically thick dust shell. Description: Optical images behind BVRcIc filters, covering an area of about 7.5'x7.5' centered on LkHα 101, were obtained at the f/10 focus of the University of Hawaii (UH) 2.2m telescope in 1999 October. Near-infrared JHK images of NGC 1579 were obtained in 2002 August with the QUIRC (QUick InfraRed Camera) infrared array at the f/10 focus of the UH 2.2m telescope. The spectra of LkHα 101 were obtained with the HIRES spectrograph at the Keck I telescope on three occasions: 2000 February 2, November 5, and 2002 December 16. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 04 30 14.4 +35 16 24 LKHa 101 = HBC 40 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 90 325 Optical and near-infrared photometry of stars in NGC 1579 table4.dat 80 9 Coordinates and Lick UBV photometry of bright stars in L1482 table8.dat 50 219 Emission lines in LkHα 101
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [HAD2004] Star identified as [HAD2004] NGC 1579 NNN in Simbad 5 A1 --- f_[HAD2004] Flag on [HAD2004] (1) 7 I1 h RAh Hour of right ascension (J2000) 9- 10 I2 min RAm Minute of right ascension (J2000) 12- 16 F5.2 s RAs Second of right ascension (J2000) 18 A1 --- DE- Sign of the declination (J2000) 19- 20 I2 deg DEd Degree of declination (J2000) 22- 23 I2 arcmin DEm Arcminute of declination (J2000) 25- 28 F4.1 arcsec DEs Arcsecond of declination (J2000) 30- 34 F5.2 mag Vmag ? The V-band magnitude (2) 36- 40 F5.2 mag B-V ? The (B-V) color index (2) 42 A1 --- f_B-V [)] Flag on B-V (3) 44- 47 F4.2 mag V-Rc ? The (V-Rc) color index (2) 49- 52 F4.2 mag V-Ic ? The (V-Ic) color index (2) 54- 58 F5.2 mag Rcmag ? The R-band magnitude (2) 60- 63 F4.2 mag Rc-Ic ? The (Rc-Ic) color index (2) 65- 69 F5.2 mag Jmag ? The J-band magnitude (2) 71- 75 F5.2 mag J-H ? The (J-H) color index (2) 77 A1 --- f_J-H [)] Flag on J-H (3) 79- 82 F4.2 mag H-K ? The (H-K) color index (2) 84- 89 A6 --- SpType MK spectral type
Note (1): Flag on [HAD2004], defined as follows: c = Integrated magnitudes of an unresolved binary. d = Emission lines including [OI](6300, 6363), [NII](6584), and [SII](6716, 6730) are present. e = Integrated magnitudes of an unresolved triple. f = The IR colors of this star are severely affected by the steep brightness gradient of the LkHα 101 infrared nebulosity; its J and H magnitudes are particularly uncertain. g = This is LkHα 101. Two stars are present within the glare of this star: one to the northeast at RA=4 30 14.76, DE=+35 16 34.5 [J=14.9, (J-H)=1.7, (H-K)=1.0] and one to the southwest at position0 4 30 13.73 +35 16 20.9 [J=16.1, (J-H)=2.2, (H-K)=1.6]. Because of the glare from LkHα 101, the photometry for these objects is rather uncertain. h = This is star D. The spectral type is uncertain, but likely K0 III. See the text for details. i = This is a double star and is saturated in V. Therefore, the B magnitude is flagged with a parenthesis in the (B-V) column. Note (2): The BVRI colors have been converted to the Johnson-Kron-Cousins photometric system, whereas the JHK colors are on the new Mauna Kea filter system. Note (3): A ")" indicates that only one of the magnitudes in the color is available.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 20 A20 --- SName Simbad designation 23 A1 --- n_SName Illuminating star (1) 25 A1 --- f_SName Individual notes (2) 27 I1 h RAh Hour of Right Ascension (J2000) 29- 30 I2 min RAm Minute of Right Ascension (J2000) 32- 35 F4.1 s RAs Second of Right Ascension (J2000) 37 A1 --- DE- Sign of the Declination (J2000) 38- 39 I2 deg DEd Degree of Declination (J2000) 41- 42 I2 arcmin DEm Arcminute of Declination (J2000) 44- 45 I2 arcsec DEs Arcsecond of Declination (J2000) 48- 52 F5.2 mag Vmag V magnitude 55- 58 F4.2 mag B-V B-V color index 61- 64 F4.2 mag U-B ? U-B color index 65 A1 --- u_U-B [:] Uncertainty on U-B 68- 69 A2 --- SpType MK spectral type 70 A1 --- u_SpType [:] Uncertainty on SpType 73- 74 I2 km/s RV ? Radial velocity 75 A1 --- u_RV [:] Uncertainty on RV 78- 80 I3 km/s vsini ? Projected rotational velocity
Note (1): Those stars that illuminate individual reflection nebulae are marked with asterisks Note (2): Flag on ID, defined as follows: b = HD 279899. It is star A of Barsony et al. (1990ApJ...362..674B). The V, B-V values in their Table 2 must be in error. It is S222, star 1 of Hunter & Massey (1990AJ.....99..846H); they classified it as B37 V. c = This is star B of Barsony et al. (1990ApJ...362..674B), for which they give V=13.92, B-V=1.34. Our values (Table 1/249) are 13.43, 1.87. d = The nebulosity at H is IC 2067. e = Our values (Table 1/40) are V=14.63, B-V=1.06. f = The V and B-V for LkHα101 are from Table 1. Published values are 15.67, 1.99 from Barsony et al. (1990ApJ...362..674B), and 14.76, 0.90 from Bergner et al. (1995A&AS..112..221B).
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm lambdaMean Intensity-weighted mean wavelength of the line (1) 8 A1 --- u_lambdaMean [:] Uncertainty on lambdaMean 10- 14 A5 --- f_lambdaMean Flag on lambdaMean (2) 16- 20 F5.2 0.1nm EW ? Equivalent width of the entire line, in angstroms, or lower value if EW exists. 21 A1 --- u_EW [:] Uncertainty on EW 23 I1 0.1nm EWu ? Upper limit of equivalent width when interval 24 A1 --- u_EWu [:] Uncertainty on EWu 26- 40 A15 --- Ion The likely identification (with RMT number in parentheses) (3) 42- 49 F8.3 0.1nm lambdaLab ? Laboratory wavelength 50 A1 --- f_lambdaLab [?] Flag on lambdaLab
Note (1): The intensity-weighted mean wavelength of the line, not the wavelength of the intensity peak, and not corrected for the stellar velocity. This mean wavelength will change as the line structure varies. Note (2): Flag on lambdaMean, defined as follows: d = double peaks; t = triple peaks; br = the line is broad; bl = the line is blended with another; as = the line is asymmetric; 1 = the line measured on only one spectrogram, usually because it falls in an interorder gap on the others; n1 = Line 5264 has a shortward wing, probably FeII(5264.176); n2 = Line 5746: the measurements include a shortward wing, possibly FeII(5746.578); n3 = Line 6456: the measurements include a distinct subsidiary peak on the shortward edge at about 6455.69, probably a blend of two weaker FeII lines, plus a contribution from OI RMT 9; n4 = Line 6548: The [NII] line is confused by an overlapping atmospheric H2O line; n5 = Line 6562: see the text for a discussion of Hα; n6 = Line 6678 falls in a corner of the frame and possibly for that reason measurements are discordant; Note (3): A plus sign means that there is probably another contributor. The [Fe II] and Fe II wavelengths are from Johansson (1977PhyS...15..183J) and (1978PhyS...18..217J), respectively.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 08-Jun-2005
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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