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J/A+A/342/313     ISO HDF observations from PRETI method    (Aussel+, 1999)

Provisional ISOCAM observations of the Hubble Deep Field reduced with the PRETI method Aussel H., Cesarsky C.J., Elbaz D., Starck J.L. <Astron. Astrophys. 342, 313 (1999)> =1999A&A...342..313A
ADC_Keywords: Infrared sources ; Surveys Mission_Name: ISO Keywords: infrared: galaxies - galaxies: evolution - methods: data analysis Abstract: We have developed a new ISOCAM data reduction technique based on wavelet analysis, especially designed for the detection of faint sources in mid-infrared surveys. This method, the Pattern REcognition Technique for Isocam data (PRETI) has been used to reduce the observations of the Hubble Deep Field (HDF) and flanking fields with ISOCAM at 6.75 (LW2) and 15µm (LW3) (Rowan-Robinson et al. 1997MNRAS.289..490R). Simulations of ISOCAM data allow us to test the photometric accuracy and completeness of the reduction. According to these simulations, the PRETI source list is 95% complete in the 15µm band at 200µJy and in the 6.75µm band at 65µJy, using detection thresholds which minimize the number of false detections. We detect 49 objects in the ISO-HDF at high confidence secure level, 42 in the LW3 filter, 3 in the LW2 filter, and 4 in both filters. An additional, less secure, list of 100 sources is presented, of which 89 are detected at 15µm only, 7 at 6.75µm only and 4 in both filters. All ISO-HDF objects detected in the HDF itself have optical or infrared counterparts, except for one from the additional list. All except one of the radio sources detected in the field by Fomalont et al. (1997ApJ...475L...5F) are detected with ISOCAM. Using a precise correction for the field of view distortion of ISOCAM allows us to separate blended sources. This, together with the fact that PRETI allows to correct data on the tail of cosmic rays glitches, lead us to produce deeper source lists than previous authors. Our list of bright sources agree with those of Desert et al. (1999A&A...342..363D) in both filters, and with those of Goldschmidt et al. (1997MNRAS.289..465G) in the LW3 filter, with systematic difference in photometry. ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands and the United Kingdom) and with participation of ISAS and NASA. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file isocat.dat 54 100 Provisional PRETI catalogue 7um.dat 43 100 7µm data 15um.dat 43 100 15µm data
See also: B/iso : ISO Observation Log of validated data (ISO Data Centre, 2001) Byte-by-byte Description of file: isocat.dat
Bytes Format Units Label Explanations
1- 11 A11 --- ID Catalogue ID. (1) 13- 14 I2 h RAh Hour of Right Ascension (J2000) 16- 17 I2 min RAm Minute of Right Ascension (J2000) 19- 22 F4.1 s RAs Second of Right Ascension (J2000) 24 A1 --- DE- Sign of Declination (J2000) 25- 26 I2 deg DEd Degree of Declination (J2000) 28- 29 I2 arcmin DEm Arcminute of Declination (J2000) 31- 32 I2 arcsec DEs Arcsecond of Declination (J2000) 34 A1 --- l_7um 6.7 micron flux is upper limit 35- 37 I3 uJy 7um ? 6.7 micron flux in 3 arcmin aperture 39- 40 I2 uJy E_7um ? Upper error bound to 6.7 micron flux 42- 43 I2 uJy e_7um ? Lower error bound to 6.7 micron flux 45 A1 --- l_15um 15 micron flux is upper limit 46- 48 I3 uJy 15um 15 micron flux in 6 arcsec aperture 50- 51 I2 uJy E_15um ? Upper error bound to 15 micron flux 53- 54 I2 uJy e_15um ? Lower error bound to 15 micron flux
Note (1): the ID starts by HDF_PM2 = detection at 6.5µm at above 7 times noise level in wavelet space HDF_PM3 = detection at 15µmat at above 7 times noise level in wavelet space HDF_PS2 = detection at 6.5µm at above 5 times noise level in wavelet space HDF_PS3 = detection at 15µm at above 3 times noise level in wavelet space
Byte-by-byte Description of file: 7um.dat
Bytes Format Units Label Explanations
1- 11 A11 --- ID Catalogue ID. (1) 13- 14 I2 h RAh Hour of Right Ascension (J2000) 16- 17 I2 min RAm Minute of Right Ascension (J2000) 19- 22 F4.1 s RAs Second of Right Ascension (J2000) 24 A1 --- DE- Sign of Declination (J2000) 25- 26 I2 deg DEd Degree of Declination (J2000) 28- 29 I2 arcmin DEm Arcminute of Declination (J2000) 31- 32 I2 arcsec DEs Arcsecond of Declination (J2000) 34 A1 --- l_7um 6.7 micron flux is upper limit 35- 37 I3 uJy 7um ? 6.7 micron flux in 3 arcmin aperture 39- 40 I2 uJy E_7um ? Upper error bound to 6.7 micron flux 42- 43 I2 uJy e_7um ? Lower error bound to 6.7 micron flux
Note (1): the ID starts by HDF_PM2 = detection at 6.5µm at above 7 times noise level in wavelet space HDF_PM3 = detection at 15µmat at above 7 times noise level in wavelet space HDF_PS2 = detection at 6.5µm at above 5 times noise level in wavelet space HDF_PS3 = detection at 15µm at above 3 times noise level in wavelet space
Byte-by-byte Description of file: 15um.dat
Bytes Format Units Label Explanations
1- 11 A11 --- ID Catalogue ID. (1) 13- 14 I2 h RAh Hour of Right Ascension (J2000) 16- 17 I2 min RAm Minute of Right Ascension (J2000) 19- 22 F4.1 s RAs Second of Right Ascension (J2000) 24 A1 --- DE- Sign of Declination (J2000) 25- 26 I2 deg DEd Degree of Declination (J2000) 28- 29 I2 arcmin DEm Arcminute of Declination (J2000) 31- 32 I2 arcsec DEs Arcsecond of Declination (J2000) 34 A1 --- l_15um 15 micron flux is upper limit 35- 37 I3 uJy 15um 15 micron flux in 6 arcsec aperture 39- 40 I2 uJy E_15um ? Upper error bound to 15 micron flux 42- 43 I2 uJy e_15um ? Lower error bound to 15 micron flux
Note (1): the ID starts by HDF_PM2 = detection at 6.5µm at above 7 times noise level in wavelet space HDF_PM3 = detection at 15µmat at above 7 times noise level in wavelet space HDF_PS2 = detection at 6.5µm at above 5 times noise level in wavelet space HDF_PS3 = detection at 15µm at above 3 times noise level in wavelet space
History: Entered by A Richards (Jodrell Bank Observatory)
(End) A Richards [Jodrell Bank] 20-Dec-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

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