In this poster paper we report on our observing programme to obtain
integrated spectrophotometry, intermediate and high resolution major
axis spectra, and UBR surface photometry of a representative
sample of ~200 galaxies in the nearby field. The main goal of this
programme is to provide a comparison sample for high redshift studies
and to study the variation in star formation rates (SFR), star formation
history (SFH), excitation, metallicity, and internal kinematics over a
large range in galaxy luminosity and morphological type. In particular,
we extend the work of Kennicutt (1992) to lower luminosity systems.
Here, we present two atlases: one of images and radial surface
brightness- and colour profiles (left
panel), another of images and integrated spectra (right panel). Furthermore, we present the main
results of our analysis sofar (middle panel). Each of the separate
panels can be accessed directly by clicking on the appropriate region in
the poster miniature above.
As galaxies are now routinely sampled at fainter magnitudes and higher
redshifts than ever before, one of the major problems with the
interpretation of distant spectroscopic data has become the difficulty
of obtaining good comparison samples in the local universe. Distant
galaxies subtend a small angle on the sky and their spectra are
unavoidably integrated spectra, while most spectra of nearby galaxies
are nuclear spectra only. A direct comparison of distant and nearby
galaxy spectra, therefore, is difficult.
In a pioneering effort, Kennicutt (1992) obtained integrated
spectrophotometry for 90 galaxies spanning the entire Hubble sequence.
His study has been a benchmark for the interpretation of spectra at both
high and low redshift. The range in luminosity sampled per type,
however, was limited to the brightest galaxies, and no uniform surface
photometry nor internal kinematical data is available. Also, only 44
out of 90 galaxies were observed at intermediate spectral resolution
(5–7 Å), the remainder at lower resolution (15–20
Å). Large homogeneous samples of intermediate or high
resolution nuclear and integrated spectrophotometry, supplemented by
multi-filter surface photometry, for galaxies spanning the entire Hubble
sequence and with a large range in luminosity, are absent in the
literature to date.
With our Nearby Field Galaxy Survey (NFGS) we aim to remedy this
situation. The purpose of our study is to obtain integrated and nuclear
spectrophotometry over the entire optical regime, as well as U,B,R,
H and K' surface photometry, and high resolution
spectroscopy, for a sample of 196 galaxies in the nearby field,
including galaxies of all types and spanning a large range in
luminosity. With "field" we imply a selection that includes galaxies in
clusters, groups an low density environments, as opposed to a selection
favoring any single one of these.
The data will be used to study the emission and absorption line
strengths, star formation rate and star formation history, morphologies,
structural parameters, colours, magnitudes and internal kinematics of
gas and stars, both globally and as a function of radius within a
galaxy. We thus aim to extend the work of Kennicutt to lower luminosity
galaxies accross the Hubble sequence and to study the variation in
galaxy properties over a large range in absolute magnitude and type.
The data can be used as a benchmark for galaxy evolution modelling and
comparison with observations of high redshift galaxies, as will result
from future observations with large ground-based telescopes and the
NGST.
The 196 target galaxies in this survey have been objectively selected
from the CfA redshift catalog (CfA I, Huchra et al. 1983) to span the
full range in absolute B magnitude present in the CfA I (−14
< MB < −22), while sampling fairly the
changing mix of morphological types as a function of luminosity. Absolute
magnitudes were calculated directly from blue photographic magnitudes and
radial velocities in the Local Group rest-frame, assuming H0 = 100
km s-1 Mpc-1.
To avoid a sampling bias favoring a cluster population we excluded
galaxies in the direction of the Virgo Cluster with velocities smaller
than 2000 km/sec. We also minimized the number of galaxies larger than
3 arcmin (the slit length of the FAST spectrograph) by imposing a
luminosity dependent lower limit on the radial velocity. Thus, we do
not impose a strict diameter limit, while avoiding selecting the
nearest high luminosity galaxies (which tend to be the largest on the
sky). We sorted the 1006 galaxies remaining after our Virgo Cluster and
radial velocity cuts into 1 magnitude wide bins of absolute magnitude,
which in turn were sorted according to Hubble type. We then drew from
each bin a number of galaxies chosen to approximately reproduce the
local galaxy luminosity function, while preserving the mix of
morphological types in each luminosity bin. The total number of
galaxies selected is 196, with a median redshift of 0.01 and a maximum
redshift of 0.07 . Only 8 of these have major axis optical diameters
larger than the slit length.
With very few caveats this sample can be considered a fair
representation of the local galaxy population.
The photometric observations were obtained at the FLWO 1.2 m telescope,
on Mt.Hopkins, Arizona, during 50 dark nights between 1994 March and
1997 March. U filter images were obtained with a thinned
backside illuminated CCD, while most B and R images
were obtained with an older camera and a front illuminated CCD.
Typically, we exposed 2 × 450, 2 × 900 and 1 × 900 seconds
in R, B, and U. Limiting surface brightnesses average
µR=26.1,
µB=27.2,
and µU=26.7
mag/arcsec2.
Radial surface brightness profiles were extracted using an ellipse
fitting procedure where center, position angle and ellipticity were
fixed at all radii to the average values in the outer parts. Total,
effective and isophotal magnitudes were calculated from the radial
surface brightness profiles. Tests of the internal and external
accuracy of our photometry indicate typical errors of 0.02 mag and 0.05
mag for isophotal and total magnitudes, respectively.
Integrated and nuclear spectra were obtained with the FAST spectrograph
at the FLWO 1.5 m telescope during 41 nights between 1995 March and 1997
March. The 2720 × 512 pixel thinned CCD of the FAST in combination
with a 300 l/mm grating allowed coverage of the entire near-UV through
optical range (3500–7250Å) in a single exposure, at a resolution
(FWHM) of ~6Å. We approximately aligned the spectrograph slit with
the major axis of each galaxy. The integrated spectra were obtained by
drift scanning the slit over a total distance of half the minor axis
optical diameter and extracting over 0.7 times the major axis optical
diameter. Thus, on average, we sample over 80% of the total galaxy
light.
Based on tests of the internal and external accuracy of the data (see
fig.7), we claim an overal relative spectrophotometric accuracy of 6%.
Kannappan, Fabricant and Franx have obtained high resolution spectra in
the range 6000–7000Å (emission line galaxies) at a resolution
(FWHM) of 1Å, and in the range 4000–6000Å (no or relatively
little emission) at a resolution (FWHM) of 2.3Å. Rotation curves
were derived from the former by simultaneously fitting the wavelengths
of Hα, [N II], [S II] and
[O I] lines as a function of radius in a galaxy.
Velocity dispersions were fit using a velocity broadened stellar template
and a Fourier fitting algorithm in the latter spectra.
The main goals of these measurements are to study galaxy mass profiles
as a function of morphological and spectrophotometric properties, to
compare gas and stellar kinematics, and investigate kinematic evidence
of galaxy interactions, mergers and mass infall.
Pahre, Jansen, Kannappan, Fabricant & Willner are obtaining
H and K filter photometry for the NFGS galaxies to
determine the relative contributions of spheroids and disks to the
luminosity density of the local universe. Near-infrared data for half
of the sample is now available.
Previous measurement of this parameter (Schechter & Dressler 1987)
relied on visual total magnitude and bulge estimates from photographic
plates and suffered from relatively poor knowledge of the luminosity
functions of different morphological types. Combination of U,B,R,
H and K photometry and our spectrophotometry will allow a
better separation of age and metallicity effects, as well as internal
extinction, while inversion of our selection and comparison with a
deeper complete spectroscopic sample (Carter et al. (in prep.)) allows
us to infer volume densities as a function of type and luminosity.
Figure 1: Overview of the global properties
of the selected galaxy sample. Presented are the number distributions as
a function of:
a) absolute B magnitude; b) galaxy type (note that we choose to place
the unclassified early type galaxies at T=−4 (cD) rather than −7,
as we do not have any cD galaxies in our sample, and this placement seems more
natural with respect to the compact ellipticals at T=−6); c) the surface
brightness at the effective radius in B; and d) the effective
(B−R) colour, measured within the effective radius in B.
In panels c) and d) the open (blue) histograms represent the selected
sample, and the shaded (red) ones the subsample of galaxies with types
later than S0/a.
We observe a strong trend of (B−R)e color with
morphological type, with later type galaxies becoming progressively
bluer (Figure 2). The observed scatter on this trend is 0.19 mag, which
is smaller than the 0.24 mag scatter on the color–magnitude trend where
intrinsically fainter systems tend to be bluer than brighter systems.
Estimating a galaxy's broad type class (E,S,Irr) from its color can,
therefore, be as accurate as estimates based on galaxy asymmetry and
central concentration of the light (Abraham et al. 1996).
We find that color–magnitude relations are useful for early type
systems and to a lesser degree for very late type systems, but not
useful for intermediate type spirals.
Figure 4: An example of the geometry of the periodic driftscan to obtain integrated spectra. The total distance over which the slit is moved back and forth is half the blue minor axis optical diameter. This distance was chosen to match the expected surface brightness limit of the 1.5 m telescope and FAST spectrograph. The spectra were extracted into 1-D spectra using an objectively defined aperture of size 0.7 times the major axis diameter at µB=26 mag/arcsec2, as determined from our B-filter photometry. The ellipse drawn into the image was fit to the B26 isophote. In the case of galaxy A10368+4811, we sample ~80% of the light within this isophote, or 68% of the total galaxian light.
These findings add to the work by other authors (e.g., Hammer
et al. 1997; CFRS) and show that the excess strength
of [OII]3727 with respect to Hα is not restricted
to higher redshifts.
Figure 9: Overview of high resolution
spectroscopic data obtained with the FAST spectrograph at the 1.5 m
telescope of the F.L. Whipple Observatory, Mt.Hopkins, Arizona.
The NFGS sample galaxies have been ordered according to morphological
type and per type according to their absolute B filter
magnitude.
Note the significant sizes of these files!
Caption to atlas 1: The atlas of images and
radial profiles. Greyscale renditions of a B filter image and
the radial dependence of the surface brightness in U,B,R (top
panel) and corresponding colours (bottom panel) are presented for each
of the observed galaxies. The galaxies have been ordered according to
their morphological type from left (early) to right (late) and per type
according to their absolute B magnitude from top (bright) to
bottom (faint). North is up and East is to the left. The original
CCD images were much larger than the portion centered on the galaxies
presented here. The image scale is indicated by a scale bar, 1 minute of
arc in length.
Caption to atlas 2: The atlas of images and
rest-frame integrated spectra. Greyscale renditions of a B
filter image, with the aperture sampled in the spectra overlayed, are
presented for each of the observed galaxies. The spectra were obtained
by drift-scanning the spectrograph slit accross the face of a galaxy
while exposing and span the range 3600–7200Å at a resolution
(FWHM) of 6Å. The galaxies were ordered according to morphological
type and luminosity as in the photometric atlas. The fluxes are
normalized to the flux at 5500Å prior to plotting. On average, the
apertures indicated encompass more than 85% of the blue light contained
within the optical radius of a galaxy.
More information on the Nearby Field Galaxy Survey and its results may
be found on the Nearby Field Galaxy Survey
homepage (http://www.public.asu.edu/~rjansen/nfgs/ ) or by contacting one
of the NFGS team members:
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