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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 95 1029 List of Candidate ELGs
table4.dat 71 291 List of 4 σ Candidate ELGs
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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
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Dates Nights Direct fields Spectral fields
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1998 April 19-May 4 15 43 40
1998 Jun 19-21 3 7 ---
1999 May 7-14 8 12 22
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Byte-by-byte Description of file: table2.dat table4.dat
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Bytes Format Units Label Explanations
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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 Hα emission-line flux in units
of 10-16 ergs/s/cm-2 (4)
64- 67 I4 0.1nm EW Hα equivalent width in angstroms (5)
69 I1 --- Qual Estimate of the reliability of source (6)
71- 95 A25 --- AName Alternate identification
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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
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History:
From electronic version of the journal
References:
Salzer et al., Paper I 2000AJ....120...80S 2000AJ....120...80S
Salzer et al., Paper II 2001AJ....121...66S 2001AJ....121...66S, Cat. J/AJ/121/66
Salzer et al., Paper III 2002AJ....123.1292S 2002AJ....123.1292S, Cat. J/AJ/123/1292
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 02-Jul-2004