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J/AJ/127/1943       KISS Hα survey list 2                (Gronwall+, 2004)

The KPNO International Spectroscopic Survey. IV. Hα-selected survey list 2. Gronwall C., Salzer J.J., Sarajedini V.L., Jangren A., Chomiuk L., Moody J.W., Frattare L.M., Boroson T.A. <Astron. J., 127, 1943-1958 (2004)> =2004AJ....127.1943G
ADC_Keywords: Surveys ; Galaxies, Seyfert ; Photometry, H-alpha 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 is the first purely digital objective-prism survey for emission-line galaxies. Here we present the second list of emission-line galaxy candidates selected from our red spectral data, which cover the wavelength range 6400 to 7200Å. In most cases, the detected emission line is Hα. The current survey list covers a 1.6°-wide strip located at δ=43°30'(B1950) and spans the right ascension range 11h55m to 16h15m. The survey strip runs through the center of the Bootes void and has enough depth to adequately sample the far side of the void. An area of 65.8deg2 is covered. A total of 1029 candidate emission-line objects have been selected for inclusion in the survey list (15.6deg-2). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data. Although the current survey covers only a modest fraction of the total volume of the Bootes void, we catalog at least 12 objects that appear to be located within the void. Only one of these objects has been recognized previously as a void galaxy. Description: All survey data were acquired using the 0.61 m Burrell Schmidt telescope. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 95 1029 List of Candidate ELGs table4.dat 95 291 List of 4 σ Candidate ELGs
See also: J/AJ/121/66 : KISS Hα survey list 1 (Salzer+, 2001) J/AJ/123/1292 : KISS [O III]-selected survey list (Salzer+, 2002) Table 1: KISS 43° red survey observing runs ---------------------------------------------------------------- Dates Nights Direct fields Spectral fields ---------------------------------------------------------------- 1998 April 19-May 4 15 43 40 1998 Jun 19-21 3 7 --- 1999 May 7-14 8 12 22 Byte-by-byte Description of file: table2.dat table4.dat
Bytes Format Units Label Explanations
1- 4 I4 --- KISSR KISS-red running identification number 6- 10 A5 --- Field KISS database table survey field identification number 12- 15 I4 --- ID KISS database table identification number 17- 18 I2 h RAh Hour of right ascension (J2000) 20- 21 I2 min RAm Minute of right ascension (J2000) 23- 26 F4.1 s RAs Second of right ascension (J2000) (1) 27 A1 --- DE- Sign of declination (J2000) 28- 29 I2 deg DEd Degree of declination (J2000) 31- 32 I2 arcmin DEm Arcminute of declination (J2000) 34- 37 F4.1 arcsec DEs Arcsecond of declination (J2000) (1) 39- 43 F5.2 mag Bmag The B-band magnitude (2) 45- 49 F5.2 mag B-V The (B-V) color 51- 57 F7.4 --- z Spectroscopic redshift estimate (3) 59- 62 I4 10-19W/m2 Flux Halpha emission-line flux in units of 10-16 ergs/s/cm-2 (4) 64- 67 I4 0.1nm EW Halpha equivalent width in angstroms (5) 69 I1 --- Qual Estimate of the reliability of source (6) 71- 95 A25 --- AName Alternate identification
Note (1): The formal uncertainties in the coordinates are 0.25arcsec in RAs and 0.20 arcseconds in DEs. Note (2): For brighter objects, the magnitude estimates typically have uncertainties of 0.05mag, increasing to ∼0.10mag at B=20. Note (3): Based on its objective-prism spectrum. This estimate assumes that the emission line seen in the objective-prism spectrum is Hα. Follow-up spectra for over 1200 ELG candidates from the two red survey lists (KR1 and the current list) show that this assumption is correct in the vast majority of cases. Only 35 ELGs with follow-up spectra (2.8%) are high-redshift objects in which a different line (typically [O III], Hβ, or both) appears in the objective-prism spectrum. Nine objects in the table have negative redshifts, although only two of these are more than 1σ below 0.0000. We have obtained follow-up spectra for four of the nine: three are high-redshift objects in which the detected line is not Hα, and one is a low-z star-forming galaxy with an actual redshift of 0.0006. The formal uncertainty in the redshift estimates is σz=0.0028 (see section 4.1.3). Note (4): Measured from objective-prism spectra and hence have fairly large certainties. The calibration of the fluxes is discussed in section 4.1.2. Note (5): Measured from objective-prism spectra and hence have fairly large uncertainties. Note (6): Reliability of source is coded as follows: 1 = High-quality source 2 = Lower quality but still reliable object 3 = Somewhat less reliable source
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 Salzer et al., Paper III 2002AJ....123.1292S, Cat. J/AJ/123/1292
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 02-Jul-2004
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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