Halpha image of NGC 1156 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 1569 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 2366 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 6822 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of IC 4662 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of NGC 1569 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of NGC 1156 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of IC 4662 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
The spectra of IC 4662 include two observations of each line.
The two observations differ markedly in the continuum levels
due to calibration uncertainties in the dark current subtraction.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 1156.
The LW2 filter was centered at 6.75 microns.
The object labeled "star" is a foreground star.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 1569.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
The four plus signs mark the positions of
the 5 giant molecular clouds mapped by Taylor et al. (1999),
where two of the clouds are given as one position,
and the two five-pointed stars mark the positions of the super
star clusters.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 2366.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars, and the object labeled "Gal"
is a background galaxy.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
Named HII regions are labeled.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 6822.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
Named HII regions are labeled.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of IC 4662.
The LW2 filter was centered at 6.75 microns.
The object labeled "star" is a
foreground star.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 1569 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 2366 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of NGC 6822 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Halpha image of IC 4662 with V-band contours superposed.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of NGC 1569 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of NGC 1156 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Spectra of FIR emission lines of IC 4662 observed with
ISO. The y-axes are in units of
10e-14 W/cm^2/micron.
The spectra of IC 4662 include two observations of each line.
The two observations differ markedly in the continuum levels
due to calibration uncertainties in the dark current subtraction.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 1156.
The LW2 filter was centered at 6.75 microns.
The object labeled "star" is a foreground star.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 1569.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
The four plus signs mark the positions of
the 5 giant molecular clouds mapped by Taylor et al. (1999),
where two of the clouds are given as one position,
and the two five-pointed stars mark the positions of the super
star clusters.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 2366.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars, and the object labeled "Gal"
is a background galaxy.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
Named HII regions are labeled.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of NGC 6822.
The LW2 filter was centered at 6.75 microns.
Objects labeled "star" are
foreground stars.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
Named HII regions are labeled.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)
Mid-infrared CAM images of IC 4662.
The LW2 filter was centered at 6.75 microns.
The object labeled "star" is a
foreground star.
Contours are of Halpha emission
where the Halpha images have been transformed to the
geometry of the CAM images and pixel scale.
(Supported in part by ISO data analysis funding from the
US National Aeronautics and Space Administration through the Jet Propulsion
Laboratory of the California Institute of Technology, by
the Lowell Research
Fund, and by grant AST-9802193 from the National Science
Foundation.)