J/ApJS/166/505 Hα photometry of face-on galaxies (Andersen+, 2006)
The photometric and kinematic structure of face-on disk galaxies.
I. Sample definition, H-alpha integral field spectroscopy, and HI line widths.
Andersen D.R., Bershady M.A., Sparke L.S., Gallagher J.S.III, Wilcots E.M.,
Van Driel W., Monnier-Ragaigne D.
<Astrophys. J. Suppl. Ser., 166, 505-525 (2006)>
=2006ApJS..166..505A 2006ApJS..166..505A
ADC_Keywords: Galaxies, nearby ; Spectroscopy
Keywords: galaxies: kinematics and dynamics - galaxies: spiral -
galaxies: structure
Abstract:
We present a survey of the photometric and kinematic properties
of 39 nearby, nearly face-on disk galaxies. Our approach exploits
echelle-resolution integral-field spectroscopy of the Hα
regions, obtained with DensePak on the WIYN 3.5m telescope Bench
Spectrograph. These data are complemented by HI line profiles observed
with the Nancay radio telescope for 25 of these sample galaxies.
Twelve additional line widths are available for sample galaxies from
the literature. In this paper, we introduce the goals of this survey,
define the sample selection algorithm, and amass the integral field
spectroscopic data and HI line widths. We establish spatially
integrated Hα line widths for the sample. We test the veracity
of these spatially integrated line profiles by convolving narrowband
imaging data with velocity field information for one of the sample
galaxies, PGC 38268, and also by comparing to HI line profiles.
Description:
We observed 39 sample galaxies with DensePak during 11 nights on 6
separate observing runs (Table 2). The DensePak IFU is a fiber optic
array mounted at the Nasmyth f/6.3 focus imaging port on the WIYN 3.5m
telescope. The WIYN Observatory, located on Kitt Peak south of Tucson,
Arizona, stands 6875 feet above sea level and is home to the second
largest telescope on the mountain.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 48 45 DensePak Observing Log
table3.dat 57 7560 Gaussian Fits to Hα emission-lines
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See also:
J/A+AS/106/451 : Face-on disk galaxies photometry. I. (de Jong+, 1994)
J/A+AS/118/557 : Near-IR photometry of 86 galaxies. II. (de Jong 1996)
J/A+A/313/377 : Near-IR photometry of 86 galaxies. IV. (de Jong 1996)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [PGC]
5- 9 I5 --- PGC PGC number
11 A1 --- Run Run identification (1)
13- 22 A10 "YYYY/MM/DD" Date UT Date of exposure
24- 27 I4 s ExpT1 Exposure Time (first exposure)
28 A1 --- --- [,]
30- 33 I4 s ExpT2 ? Exposure Time (second exposure)
34 A1 --- --- [,]
36- 39 I4 s ExpT3 ? Exposure Time (third exposure)
40 A1 --- --- [,]
42- 45 I4 s ExpT4 ? Exposure Time (fourth exposure)
48 I1 --- Nexp Number of pointings
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Note (1): The run identification identifies the principal investigator (PI) and
observers for each run as follows:
a = PI: M.A. Bershady (UW allocation),
Observers: M.A. Bershady & D.R. Andersen
b = PI: M.A. Bershady, J.S. Gallagher, L.S. Sparke, & E.M. Wilcots
(UW allocation), Observer: D.R. Andersen
c = PI: M.A. Bershady, J.S. Gallagher, L.S. Sparke, & E.M. Wilcots
(UW allocation), Observers: D.R. Andersen & G. Madsen
d = PI: M.A. Bershady (UW allocation), Observer: D.R. Andersen
e = PI: D.R. Andersen (NOAO allocation), Observer: D.R. Andersen
f = PI: M.A. Bershady & D.R. Andersen (UW allocation),
Observer: D.R. Andersen
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [PGC]
5- 9 I5 --- PGC PGC number
11- 12 I2 --- Fiber Fiber number
14 I1 --- Point [1,4] Pointing number
16- 21 F6.2 arcsec West Offset West of the kinematic center (1)
23- 28 F6.2 arcsec North Offset North of the kinematic center (1)
30- 36 F7.2 0.1nm lambda.c ? Gaussian center of Hα line (Å)
38- 42 F5.2 0.1nm e_lambda.c ? Error in lambda.c
44- 48 I5 h-1 Flux ? Flux of Hα line (electrons/hour)
50- 53 F4.2 0.1nm sig ? Gaussian width of Hα line (Å)
55- 57 I3 h-1 Fcont Continuum flux density in units of
electrons/hour/resolution element
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Note (1): Based on our model fits to the velocity fields described in the
relevant forthcoming paper in this series, and the astrometric
information regarding relative fiber positions described in Section 3.1.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 16-May-2008