Access to Astronomical Catalogues

← Click to display the menu
J/MNRAS/331/474  ubvyβ photometry in the Lupus dark cloud    (Franco, 2002)

On the infrared void in the Lupus dark clouds. Franco G.A.P. <Mon. Not. R. Astron. Soc. 331, 474 (2002)> =2002MNRAS.331..474F
ADC_Keywords: Molecular clouds ; Photometry, uvby, beta Keywords: stars: distances - ISM: clouds - dust, extinction - ISM: individual: Lupus Abstract: Stroemgren uvbyβ photometry observations obtained for 205 stars in the general direction of a void in the IRAS 100-µm emission from the Lupus dark cloud complex are presented and analysed. The colour excess versus distance diagram confirms the existence of a region depleted from interstellar material, which is also seen in the ROSAT soft X-ray background emission map. The distance to the surrounding material is estimated as being within the interval from 60 to 100pc. This result is in disagreement with previous distance estimates to the supposed supernova that has been suggested as responsible for clearing the region from dust. As an alternative, the data presented support the suggestion that the void may have been produced by the detachment of material from the interface between LoopI and the Local Bubble as a consequence of hydromagnetic instabilities. Moreover, the distribution of colour excess as a function of distance supports a value of ∼150pc as the most probable distance to the dark cloud known as Lupus1. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 97 201 Stroemgren photometry of stars earlier than G0 towards Lupus (SAO stars) table1b.dat 77 4 Stroemgren photometry of stars earlier than G0 towards Lupus (SA stars)
See also: J/A+A/320/185 : UBVRIcJHKL photometry in Lup (Wichmann+ 1997) I/131 : SAO Star Catalog J2000 (SAO Staff 1966; USNO, ADC 1990) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- SAO SAO (I/131) Catalog number 8- 13 I6 --- HD ? HD (III/135) number 15- 29 A15 --- SpType MK spectral type 31- 32 I2 h RAh Right ascension (1950) 34- 35 I2 min RAm Right ascension (1950) 37- 38 I2 s RAs Right ascension (1950) 40 A1 --- DE- Declination sign (1950) 41- 42 I2 deg DEd Declination (1950) 44- 45 I2 arcmin DEm Declination (1950) 47- 52 F6.3 mag Vmag Johnson computed V magnitude 54- 55 I2 mmag e_Vmag rms uncertainty on Vmag 57- 62 F6.3 mag b-y b-y Stroemgren colour index 64- 65 I2 mmag e_b-y rms uncertainty on b-y 67- 71 F5.3 mag m1 m1 Stroemgren colour index 73- 74 I2 mmag e_m1 rms uncertainty on m1 76- 80 F5.3 mag c1 c1 Stroemgren colour index 82- 83 I2 mmag e_c1 rms uncertainty on c1 85 I1 --- o_b-y Number of nights in which the star was observed in uvby 87- 91 F5.3 mag beta ? Hβ Stroemgren index 93- 94 I2 mmag e_beta ? rms uncertainty on beta 96- 97 I2 --- o_beta Number of nights in which the star was observed in Hbeta
Byte-by-byte Description of file: table1b.dat
Bytes Format Units Label Explanations
1- 10 A10 --- SA SA name 12- 13 I2 h RAh Right ascension (1900) 15- 16 I2 min RAm Right ascension (1900) 18- 19 I2 s RAs Right ascension (1900) 21 A1 --- DE- Declination sign (1900) 22- 23 I2 deg DEd Declination (1900) 25- 26 I2 arcmin DEm Declination (1900) 28- 33 F6.3 mag Vmag Johnson computed V magnitude 35- 36 I2 mmag e_Vmag rms uncertainty on Vmag 38- 42 F5.3 mag b-y b-y Stroemgren colour index 44- 45 I2 mmag e_b-y rms uncertainty on b-y 47- 51 F5.3 mag m1 m1 Stroemgren colour index 53- 54 I2 mmag e_m1 rms uncertainty on m1 56- 60 F5.3 mag c1 c1 Stroemgren colour index 62- 63 I2 mmag e_c1 rms uncertainty on c1 65 I1 --- o_b-y Number of nights in which the star was observed in uvby 67- 71 F5.3 mag beta ? Stroemgren Hβ index 73- 74 I2 mmag e_beta ? rms uncertainty on Hbeta 76- 77 I2 --- o_beta Number of nights in which the star was observed in Hbeta
History: From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 22-Apr-2002
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

catalogue service

© UDS/CNRS

Contact