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J/AJ/123/1292       KISS III. [O III]-selected survey list   (Salzer+, 2002)

The KPNO International Spectroscopic Survey. III. [O III]-selected survey list. Salzer J.J., Gronwall C., Sarajedini V.L., Lipovetsky V.A., Kniazev A., Moody J.W., Boroson T.A., Thuan T.X., Izotov Y.I., Herrero J.L., Frattare L.M. <Astron. J. 123, 1292 (2002)> =2002AJ....123.1292S
ADC_Keywords: Galaxies, Seyfert ; Surveys ; Redshifts ; Equivalent widths Keywords: galaxies: Seyfert - galaxies: starburst - surveys Abstract: The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500Å. In most cases, the detected emission line is [O III] λ5007. The current survey list covers a 1°-wide strip located at δ=29°30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d°2 is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91°-2). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 104 223 List of Candidate Emission-Line Galaxies table3.dat 103 91 List of 4 σ Candidate ELGs
See also: J/AJ/121/66 : KISS Hα survey list 1 (Salzer+, 2001) J/AJ/127/1943 : KISS Hα survey list 2 (Gronwall+, 2004) Byte-by-byte Description of file: table2.dat table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- KISS The running KISS blue survey number (KISSB NNN in table2, KISSBx NN in table3) 5- 9 A5 --- Field Object survey field number identification 11- 15 I5 --- ID KISS survey database identification number (1) 17- 18 I2 h RAh Hour of Right Ascension (J2000) (2) 20- 21 I2 min RAm Minute of Right Ascension (J2000) (2) 23- 26 F4.1 s RAs Second of Right Ascension (J2000) (2) 27 A1 --- DE- Sign of Declination (J2000) (2) 28- 29 I2 deg DEd Degree of Declination (J2000) (2) 31- 32 I2 arcmin DEm Arcminute of Declination (J2000) (2) 34- 37 F4.1 arcsec DEs Arcsecond of Declination (J2000) (2) 39- 43 F5.2 mag Bmag The B band magnitude (3) 45- 48 F4.2 mag B-V The (B-V) color (3) 50- 56 F7.4 --- z Estimated redshift from the objective-prism spectrum (4) 58- 61 I4 10-16mW/m2 Flux Objective-prism spectrum emission-line flux in units of 10-16erg/cm2/s 63- 66 I4 0.1nm EW Objective-prism spectrum equivalent width 68 I1 --- Qual The objective-prism spectrum quality flag (5) 70- 73 A4 --- KISSR The KISS red survey number (only in table2.dat) 75-103 A29 --- Com Previously catalogued alternate identification
Note (1): Necessary for locating the KISS ELGs within the survey database tables Note (2): The formal uncertainties in the coordinates are 0.25" in right ascension and 0.20" in declination. Note (3): For brighter objects the magnitude estimates have uncertainties of typically 0.05 magnitude, increasing to ∼0.10 magnitude at B=20. Note (4): Estimate assumes that the emission line seen in the objective-prism spectrum is [O III]. Follow-up spectra for 123 ELG candidates from the current list show that this assumption is correct in the vast majority of cases. The formal uncertainty in these redshift estimates is σz=0.0049 (see Section 4.1.3). There are three objects in the table with negative redshifts listed. In all three cases the measured value is just slightly negative (i.e., within the error quoted above), and two of the three have redshifts measured from follow-up spectra that are both small but positive. Note (5): Assigned during the line measurement step of the data processing, is given the value of 1 for high quality sources, 2 for lower quality but still reliable objects, and 3 for somewhat less reliable sources.
History: From electronic version of the journal References: Salzer et al., Paper I 2000AJ....120...80S Salzer et al., Paper II 2001AJ....121...66S, Cat. J/AJ/121/66 Gronwall et al., Paper IV 2004AJ....127.1943G, Cat. J/AJ/127/1943
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 27-May-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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