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J/A+A/314/615       Maps of the 36 GHz methanol emission (Liechti+, 1996)

Maps of the 36 GHz methanol emission Liechti S., Wilson T.L. <Astron. Astrophys. 314, 615 (1996)> =1996A&A...314..615L (SIMBAD/NED BibCode)
ADC_Keywords: Masers Keywords: ISM: molecules - ISM: clouds - ISM: HII regions - radio lines: ISM Abstract: We have used the Effelsberg 100-meter telescope to map the 36GHz 4-1->30E methanol transition in galactic star forming regions where methanol masers were previously detected. In most sources, the emission consists in one or several narrow (maser) features superimposed on a broader, presumably quasi-thermal component. The line shapes and positions of the narrow features are often similar to those observed in the other ClassI methanol maser transitions (at 25, 44, 84 and 95GHz), but with some exceptions. Our observations confirm that, unlike the strong ClassII methanol masers (at 12.2, and 6.6GHz), the ClassI methanol masers are offset from the compact HII regions, infrared sources and OH/H2O masers. In outflow sources, these are located at the edge of the molecular lobes. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1 115 116 Line parameters for detected sources table1.tex 88 423 LaTeX version of table1 table2 42 7 Non detected sources table3 33 29 Main detected features in Sgr B2 table4 33 18 Main detected features in Sgr A-A figure1.ps 130 1581 Postscript file of figure 1 (with caption) figure3.ps 130 1821 Postscript file of figure 3 (with caption) figure5.ps 130 729 Postscript file of figure 5 (with caption) figure7.ps 130 983 Postscript file of figure 7 (with caption) figure8.ps 131 1078 Postscript file of figure 8 (with caption) figure9.ps 130 1306 Postscript file of figure 9 (with caption) figure10.ps 130 937 Postscript file of figure 10 (with caption) figure11.ps 130 1399 Postscript file of figure 11 (with caption)
Byte-by-byte Description of file: table1
Bytes Format Units Label Explanations
1- 14 A14 --- Name Source name (1) 16- 17 I2 h RAh Right ascension 1950 (hours) (1) 19- 20 I2 min RAm Right ascension 1950 (minutes) (1) 22- 25 F4.1 s RAs Right ascension 1950 (seconds) (1) 27 A1 --- DE- Declination sign 28- 29 I2 deg DEd Declination 1950 (degrees) (1) 31- 32 I2 arcmin DEm Declination 1950 (arcminutes) (1) 34- 35 I2 arcsec DEs Declination 1950 (arcseconds) (1) 37- 41 F5.1 Jy.km/s S ? Integrated flux density of the feature (2) 43- 46 F4.1 Jy.km/s e_S ? 1 sigma uncertainty on integrated flux 49- 54 F6.2 km/s V ? Center velocity of the feature (3) 56- 59 F4.2 km/s e_V ? 1 sigma uncertainty on center velocity 61- 65 F5.2 km/s W ? Width of the feature (3) 67- 70 F4.2 km/s e_W ? 1 sigma uncertainty on width 72- 74 I3 arcsec dRA ? R.A. position offset of the feature (4) 76 I1 arcsec e_dRA ? 1 sigma uncertainty on R.A. position offset 79- 81 I3 arcsec dDE ? Dec. position offset of the feature (4) 83 I1 arcsec e_dDE ? 1 sigma uncertainty on dec. position offset 87- 88 I2 arcsec theta ? Angular size of the feature (5) 90 I1 arcsec e_theta ? 1 sigma uncertainty on angular size 93-103 A11 --- Rem Remarks (6) 105-115 A11 --- F-name Other name for the position of the feature
Note (1): The source name and coordinates are repeated for each detected feature. The sources are ordered in increasing right ascension. Note (2): The integrated flux density (determined from spectral gaussian fit of the feature) is the one at the peak position (see note (3)). If no peak position was determined, it is the maximum integrated area of the different observed positions. Note (3): The velocity (with respect to the l.s.r.) and width is the mean over the all the observed positions and the 1 sigma uncertainty is the statistical error of this mean. Note (4): The offset is with respect to the R.A. and Dec. position of the source.The position of the emission peak of the feature has been determined by a spatial 2-dimension gaussian fit on the integrated area of the line. The error is the error of the fit and does not include pointing errors. When no fit was performed (line too weak, extended or on the edge of the map), the position given is the position where the maximum flux density has been detected. Note (5): Theta is the mean size of the source assuming a gaussian shape, calculated from the mean of the minor and major axis half power width of the elliptical 2-dimensional gaussian fitted on the line area contour map (assuming a 26" HPBW for the telescope beam). Theta is not given when the peak of the detected emission is on the edge of the map, or when the 2-dimension gaussian fit was not performed (2 peaks, too extended, line too weak, ...). Note (6): P: point-like source in our beam (i.e. < 10") td: tentative detection em: peak of the detected emission on the edge of the observed map ex: extended emission uncomp: map uncomplete mf: many features, only the strongest are given
Byte-by-byte Description of file: table2
Bytes Format Units Label Explanations
1- 9 A9 --- Name Source name 11- 12 I2 h RAh Right ascension 1950 14- 15 I2 min RAm Right ascension 1950 17- 20 F4.1 s RAs Right ascension 1950 22 A1 --- DE- Declination sign 23- 24 I2 deg DEd Declination 1950 26- 27 I2 arcmin DEm Declination 1950 29- 30 I2 arcsec DEs Declination 1950 33- 37 F5.1 km/s Vcen Center velocity of observation 39- 41 F3.1 Jy rms 1 sigma upper limit (spectrum r.m.s. noise)
Byte-by-byte Description of file: table3 table4
Bytes Format Units Label Explanations
1- 4 I4 Jy Fpeak Peak flux density of the feature 6- 10 F5.1 km/s Vcen Center velocity of the feature 12- 14 F3.1 km/s e_Vcen 1 sigma uncertainty on center velocity 17- 20 F4.1 km/s Width Width of the feature 22- 24 F3.1 km/s e_Width 1 sigma uncertainty on width 27- 29 I3 arcsec dRA Feature right ascension position offset (1) 31- 33 I3 arcsec dDE Feature declination position offset (1)
Note (1): The offsets are with respect to the position given in Table 1 for Sgr B2 (Table 3) and Sgr A-A (Table 4).
Courtesy: Stella Liechti
(End) Patricia Bauer [CDS] 16-Apr-1996
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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