J/A+A/171/261 Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)
Southern HII Regions: an extensive study of radio recombination line emission Caswell J.L., Haynes R.F. <Astron. Astrophys. 171, 261 (1987)> =1987A&A...171..261C
ADC_Keywords: H II regions; Radial velocities; Radio lines; Radio sources Keywords: H II regions; radio recombination lines; galactic structure Description: We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109α and H110α) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 152 317 Hydrogen recombination line data (1)
Note (1): One of the sources in the table, G326.230+0.976, may be part of the next source in the table, G326.315+0.689.
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 F7.3 deg GLON Galactic longitude (1) 8- 13 F6.3 deg GLAT Galactic latitude (1) 14 A1 --- m_V [ab]? Recombination line velocity component 16- 17 I2 h RAh Right Ascension (1950) (1) 18- 19 I2 min RAm Right Ascension (1950) 20- 23 F4.1 s RAs Right Ascension (1950) 24 A1 --- DE- Declination sign (1950) 25- 26 I2 deg DEd Declination (1950) (1) 27- 28 I2 arcmin DEm Declination (1950) 29- 30 I2 arcsec DEs Declination (1950) 32- 37 F6.2 K Tc Peak 5GHz continuum brightness temperature 38 A1 --- u_Tc [ :] Uncertainty flag on Tc 41- 44 F4.1 arcmin Diam1 ? Angular size (first dimension) (2) 45 A1 --- u_Diam1 [ :] Uncertainty flag on Diam1 48- 51 F4.1 arcmin Diam2 ? Angular size (second dimension) (2) 52 A1 --- u_Diam2 [ :] Uncertainty flag on Diam2 55- 60 F6.2 Jy S ? 5GHz continuum flux density 61 A1 --- u_S [ :] Uncertainty flag on S 62- 67 F6.1 km/s V1-H2CO ? LSR velocity of H2CO absorption line, first velocity component 68- 73 F6.1 km/s V2-H2CO ? LSR velocity of H2CO absorption line, second velocity component 74- 79 F6.1 km/s V3-H2CO ? LSR velocity of H2CO absorption line, third velocity component 80- 84 F5.1 km/s V4-H2CO ? LSR velocity of H2CO absorption line, fourth velocity component 85- 86 A2 --- nH2CO ? Note on H2CO measurements: ND: no detectable H2CO absorption, NA: no available H2CO measurement 88- 89 A2 --- rH2CO ? Reference for H2CO results: CH: this survey, Caswell and Haynes (1987), WG: Whiteoak and Gardner 1974A&A....37..389W Gardner and Whiteoak 1984MNRAS.210...23G 91- 95 F5.3 K TL Peak recombination line brightness temperature (3) 96 A1 --- u_TL [ :] Uncertainty flag on TL 98- 99 I2 km/s DV Width of recombination line, full width at half intensity (3) 100 A1 --- u_DV [ :] Uncertainty flag on DV 101-104 I4 km/s V LSR velocity of recombination line (3) 105 A1 --- u_V [ :] Uncertainty flag on V 107-111 I5 K Te LTE Electron Temperature 112 A1 --- u_Te [ :] Uncertainty flag on Te 115-118 F4.1 kpc Rg ? Galactocentric radius (4) 119 A1 --- u_Rg [ :] Uncertainty flag on Rg 122-125 F4.1 kpc d1 ? Kinematic distance, or near kinematic distance (4) (5) 126 A1 --- u_d1 [ :] Uncertainty flag on d1 128-131 F4.1 kpc d2 ? Far kinematic distance (4) (5) 133 A1 --- f_d1 ? Near/far preference flag, N: near kinematic distance is significantly more likely, F: far kinematic distance is significantly more likely 135-136 A2 --- n_d1 ? HI absorption flag, HI: near/far preference is based on 21 cm absorption line data 138-140 A3 --- ref ? Reference for recombination line results if cited from another source (6) 142 A1 --- Note [ N] Source comments, N indicates that section 4 of Caswell and Haynes (1987) contains additional information or discussion for this source 145-152 A8 --- Opt Optical counterpart (7)
Note (1): Coordinates are the position of peak 5GHz continuum intensity from Haynes et al. (1979AuJPA..48....1H, Cat. VIII/20). Note (2): Angular sizes quoted for small diameter sources are widths to half maximum intensity of the equivalent deconvolved Gaussian source. For large irregular sources the quoted sizes are the average major and minor dimensions, and are very approximate. Note (3): Determined from a Gaussian fit to the observed line profile. Note (4): Derived from the recombination line LSR velocity assuming the Schmidt (1965) rotation curve inside the solar circle, a flat rotation curve (V=250 km/s) outside the solar circle, and 10 kpc for the distance of the Sun from the Galactic center. Sources in the first or fourth quadrants with velocities exceeding, or within 5 km/s of, the terminal velocity as defined by the Schmidt rotation curve are assigned to the tangent point. Note (5): For sources with two possible kinematic distance solutions, d1 contains the near distance and d2 contains the far distance. For other sources, d1 contains the kinematic distance and d2 is blank. Note (6): C: Caswell (1972AuJPh..25..443C), CC: Caswell and Clark (1975AuJPA.......57C), Ch: Churchwell et al. (1974A&A....32..283C), CHC: Caswell et al. (1975AuJPh..28..633C), HD: Huchtmeier and Day (1975A&A....41..153H), S: Shaver at el. (1983MNRAS.204...53S), W: Wilson et al. (1970A&A.....6..364W). Note (7): 'V', or a specific nebula name, denotes the presence of a visible optical counterpart, and 'A' indicates the absence of an optical counterpart.
Acknowledgements: H. Andernach and S. Trushkin scanned the published data table, made format changes, and provided a copy of their electronic version to ADC. References: Caswell, J. L. 1972, Australian J. Phys., 25, 443. Caswell, J. L., and Clark, D. H. 1975, Australian J. Phys. Astrophys. Suppl., No. 37, 57 =1975AuJPA.......57C Caswell, J. L., and Haynes, R. F. 1987, Astr. Ap., 171, 261 =1987A&A...171..261C Caswell, J. L., Haynes, R. F., and Clark, D. H. 1975, Australian J. Phys., 28, 633 =1975AuJPh..28..633C Churchwell, E., Mezger, P. G., and Huchtmeier, W. 1974, Astr. Ap., 32, 283 =1974A&A....32..283C Gardner, F. F., and Whiteoak, J. B. 1984, M.N.R.A.S., 210, 23 =1984MNRAS.210...23G Haynes, R. F., Caswell, J. L., and Simons, L. W. J. 1978, Australian J. Phys. Astrophys. Suppl., No. 45, 1 =1978AuJPA..45....1H Haynes, R. F., Caswell, J. L., and Simons, L. W. J. 1979, Australian J. Phys. Astrophys. Suppl., No. 48, 1 =1979AuJPA..48....1H Huchtmeier, W. K. and Day, G. A. 1975, Astr. Ap., 41, 153 =1975A&A....41..153H Schmidt, M. 1965, in Galactic Structure, eds. A. Blauuw, M. Schmidt, Univ. Chicago Press, p. 513 =1965QB819.B55...... Shaver, P. A., McGee, R. X., Newton, L. M., Danks, A. C., and Pottasch, S. R. 1983, M.N.R.A.S., 204, 53 =1983MNRAS.204...53S Whiteoak, J. B., and Gardner, F F. 1974, Astr. Ap., 37, 389 =1974A&A....37..389W Wilson, T. L., Mezger, P. G., Gardner, F. F., Milne, D. K. 1970, Astr. Ap., 6, 364 =1970A&A.....6..364W
(End) Nils Odegard [SSDOO/ADC] 01-Aug-1999
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