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J/ApJ/668/331       OH masers in W3(OH)                      (Fish+, 2007)

Structure of W3(OH) from very high spectral resolution observations of 5 centimeter OH masers. Fish V.L., Sjouwerman L.O. <Astrophys. J., 668, 331-347 (2007)> =2007ApJ...668..331F
ADC_Keywords: Interstellar medium; Masers Keywords: ISM: individual (W3(OH)) - line: profiles - magnetic fields - masers - radio lines: ISM - stars: formation Abstract: Recent studies of methanol and ground-state OH masers at very high spectral resolution have shed new light on small-scale maser processes. The nearby source W3(OH), which contains numerous bright masers in several different transitions, provides an excellent laboratory for high spectral resolution techniques. We present a model of W3(OH) based on European VLBI Network (EVN) observations of the rotationally excited 6030 and 6035MHz OH masers taken at 0.024km/s spectral resolution. Description: The European VLBI Network (EVN) was used to observe the 6030.747 and 6035.092MHz OH main-line masers in dual circular polarization in W3(OH). Eight stations were used: the Mk II telescope at Jodrell Bank, Effelsberg, the Onsala 25m telescope, Medicina, Torun, Noto, Darnhall, and a single Westerbork antenna. No usable data were obtained in left circular polarization (LCP) at 6030MHz at the Mk II telescope due to a hardware failure. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 57 292 Detected 6030 and 6035MHz masers in W3(OH) table2.dat 41 117 Zeeman pairs and associations
See also: J/ApJ/647/418 : Ground-state OH masers in W3(OH) study (Fish+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [FS2007b] Spot number 5- 8 I4 MHz Freq Transition frequency (6030 or 6035) 10 A1 --- Pol [LR] Left or Right circular polarization 12- 18 F7.2 mas oRA Right Ascension offset (G1) 20- 27 F8.2 mas oDE Declination offset (G1) 29- 34 F6.2 km/s Vel LSR velocity of channel of peak emission 36- 41 F6.2 Jy Sp Peak brightness of Gaussian fit in channel of peak emission in units of Jy/beam 43- 47 F5.3 km/s/mas Vgrad ? Velocity gradient 49- 52 I4 deg PA [-180/180]? Position angle of Vgrad (2) 54- 55 I2 --- Zg ? Zeeman group from Table 2 57 A1 --- f_[FS2007b] [fgp] Flag on [FS2007b] (3)
Note (2): Position angle east of north in direction of increasing line-of-sight velocity across the maser spot. Note (3): Flag as follows: f = Reference feature g = Consistent with B=8.3mG, vLSR=-43.26km/s if interpreted as a multi-transition Zeeman association p = Unpaired maser in one transitions consistent with the central velocity and magnetic field strength derived from a Zeeman pair in the other transitions
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Zg Zeeman group sequential number 3 A1 --- n_Zg [d] in a Zeeman association (1) 5- 11 F7.2 mas oRA Right Ascension offset (G1) (2) 13- 20 F8.2 mas oDE Declination offset (G1) (2) 22- 25 I4 MHz Freq Frequency (6030 or 6035) 27- 32 F6.2 km/s Vel Center LSR velocity of the Zeeman pair 34- 37 F4.1 10-7T B Magnetic field, in milli-Gauss (3) 39- 41 F3.1 mas Sep Separation
Note (1): d = See Sect. 3.3 for a discussion of this Zeeman association Note (2): Average of the right ascension and declination offsets of the left circular (LCP) and right circular (RCP) polarization components of the Zeeman pair. Note (3): Positive values indicate magnetic fields oriented in the hemisphere pointing away from the observer.
Global notes: Note (G1): Centroid of Gaussian fit in channel of peak emission. Right Ascension and Declination offsets are with respect to 02:27:03.8343, +61:52:25.300 ± 0.01". Errors range from <0.01mas for the strongest maser spots to ∼1mas for the weakest detections.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 29-Nov-2009
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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