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J/A+A/453/1003      SCUBA ultracompact HII regions           (Thompson+, 2006)

A SCUBA imaging survey of ultracompact HII regions. The environments of massive star formation. Thompson M.A., Hatchell J., Walsh A.J., Macdonald G.H., Millar T.J. <Astron. Astrophys., 453, 1003-1026 (2006)> =2006A&A...453.1003T
ADC_Keywords: H II regions ; Millimetric/submm sources Keywords: stars: formation - ISM: HII regions - ISM: dust, extinction - submillimeter - radio continuum: ISM Abstract: We present a SCUBA submillimetre (450 and 850µm) survey of the environment of 105 IRAS point sources, selected from the Wood and Churchwell (1989ApJS...69..831W) and Kurtz et al. (1994, Cat. J/ApJS/91/659) radio ultracompact (UC) HII region surveys. We detected a total of 155 sub-mm clumps associated with the IRAS point sources and identified three distinct types of object: ultracompact cm-wave sources that are not associated with any sub-mm emission (sub-mm quiet objects), sub-mm clumps that are associated with ultracompact cm-wave sources (radio-loud clumps); and sub-mm clumps that are not associated with any known ultracompact cm-wave sources (radio-quiet clumps). 90% of the sample of IRAS point sources were found to be associated with strong sub-mm emission. We consider the sub-mm colours, morphologies and distance-scaled fluxes of the sample of sub-mm clumps and show that the sub-mm quiet objects are unlikely to represent embedded UC HII regions unless they are located at large heliocentric distances. Description: Our observations were carried out using the SCUBA common-user bolometer array in operation at the James Clerk Maxwell Telescope (JCMT). The observations were performed in a flexibly-scheduled mode whereby observations are not scheduled over a pre-defined period but are carried out over a 6-month observing semester according to the appropriate weather (atmospheric opacity) band, the visibility of the sources from the telescope and the scientific priority of the observations. The survey data were thus obtained by visiting observers over several separate periods across the 98B (Aug.-Jan.) and 99A (Feb.-July) observing semesters at the JCMT. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 54 105 UC HII fields observed during the survey, their central coordinates and estimated distance to the UC HIIs in each field refs.dat 144 19 References table2.dat 105 159 Identifications, coordinates, peak and integrated fluxes of each submillimetre source detected in the survey
See also: J/ApJS/91/659 : Ultracompact HII regions radio images (Kurtz+ 1994) J/A+A/336/339 : VLA observations of UC HII regions (Molinari+ 1998) J/A+AS/133/29 : Molecular line survey towards UC HII (Hatchell+ 1998) J/A+AS/120/283 : Water maser features in UC HII regions (Hofner+ 1996) J/ApJS/155/123 : JHKs photometry of UC HII regions (Alvarez+, 2004) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Field UC HII field designation 14 A1 --- n_Field [+] Note on Field (1) 15 A1 --- f_Field [*] Note on Field (2) 17- 18 I2 h RAh Right ascension (J2000) 20- 21 I2 min RAm Right ascension (J2000) 23- 26 F4.1 s RAs Right ascension (J2000) 28 A1 --- DE- Declination sign (J2000) 29- 30 I2 deg DEd Declination (J2000) 32- 33 I2 arcmin DEm Declination (J2000) 35- 38 F4.1 arcsec DEs Declination (J2000) 40- 43 F4.1 kpc Dist ?=- Distance or near distance (3) 44 A1 --- --- [/] 45- 48 F4.1 kpc Dist2 ? Far distance (3) 50- 54 A5 --- r_Dist Distance reference
Note (1): Fields indicated with a dagger (+) show no evidence for UC HII regions in the Wood & Churchwell (1989ApJS...69..831W) and Hofner et al. (1994ApJ...429L..85H) surveys, or in the literature search described in Sect. 2.1 Note (2): Fields indicated by an asterisk (*) were subject to the 450µm calibration problems described in Sect. 2.3. Note (3): In cases where there is an ambiguity between the near and far kinematic distance both values are listed.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode BibCode 24- 43 A20 --- Aut Author's name 47-144 A98 --- Com Comments
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Field UCH II field designation 15 A1 --- m_Field [a-d] Multiplicity index on Field 17- 34 A18 --- Source Source designation (1) 36 A1 --- n_Source [a-e] Note on Source (2) 38- 39 I2 h RAh Right ascension (J2000) 41- 42 I2 min RAm Right ascension (J2000) 44- 47 F4.1 s RAs Right ascension (J2000) 49 A1 --- DE- Declination sign (J2000) 50- 51 I2 deg DEd Declination (J2000) 53- 54 I2 arcmin DEm Declination (J2000) 56- 57 I2 arcsec DEs Declination (J2000) 59 A1 --- l_Fp450um Limit flag on Fp450um (3) 60- 64 F5.1 Jy Fp450um ?=- Peak flux density at 450um (in Jy/beam) (6) 66- 69 F4.1 Jy e_Fp450um ? rms uncertainty in Fp450um (in Jy/beam) (4) 70 A1 --- n_Fp450um [+] Note on Fp450um (5) 72- 75 F4.1 Jy Fp850um ?=- Peak flux density at 850um (in Jy/beam) (6) 77- 79 F3.1 Jy e_Fp850um ? rms uncertainty in Fp850um (in Jy/beam) (4) 81 A1 --- l_Fi450um Limit flag on F450umI (3) 82- 87 F6.1 Jy Fi450um ?=- Integrated flux density at 450um (in Jy/beam) (6) 89- 93 F5.1 Jy e_Fi450um ? rms uncertainty in F450umI (in Jy/beam) (4) 94 A1 --- n_Fi450um [+] Note on Fi450um (5) 96-100 F5.1 Jy Fi850um ?=- Integrated flux density at 850um (in Jy/beam) (6) 102-105 F4.1 Jy e_Fi850um ? rms uncertainty in F850umI (in Jy/beam) (4)
Note (1): All source positions were measured from the 850µm images unless otherwise stated. Note (2): Notes as follows: a = A noisy bolometer clipped from the final rebinned image is located close to this source and thus the measured flux is a lower limit to the true flux. b = These sources are separable in the unsmoothed 450µm image but blended in the 850µm image. The quoted 850µm flux is that of the blended single source. The coordinates quoted are measured from the 450µm image. c = These sources are separable in the 850µm images but blended into one source in the smoothed 450µm images. The quoted 450µm flux is the flux of the blended single source. d = A noisy bolometer clipped from the final rebinned 850µm image lies over this source and it was not possible to masure any sensible peak or integrated 850µm flux. e = This sources lies on the edge of the field of view and thus one or more of the quoted fluxes is a lower limit to the true flux. Note (3): Upper limits for non-detections at 450um Note (4): Quoted errors include calibration uncertainties of 30% at 450µm and 10% at 850µm. Note (5): 450µm peak flux measurements indicated by a dagger (+) are measured from smoothed images and the flux density unit in this case is Janskys per 14" beam. The resolution of the unsmoothed images is 8" at 450 µm and 14" at 850 µm. Note (6): Where it was not possible to measure a 450µm flux, either due to the smaller FOV of the short wavelength array or calibration problems this is indicated by an ellipsis (---).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 16-Jan-2007
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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