LVL Data Products
LVL consist of a sample of 258 galaxies, which are being mapped with both IRAC (4 bands) and
MIPS (3 bands). In addition,
ancillary data products consisting of images in the narrow-band H
1. IRAC : four astrometrically aligned images (one image per band) for
each galaxy, as a single extension FITS file, calibrated in Myr/sr,
and with standard WCS information.
2. MIPS :
three astrometrically aligned images, one for each MIPS channel,
per galaxy, with pixels size of 1.5, 4.5, and 9.0 arcsec (24, 70,
and 160
1. Optical data: Optical imaging data in the standard R broad-band filter and in narrow-band filters at
the wavelength of the H
2. GALEX UV images: GALEX ultraviolet imaging for the
LVL galaxies had been/is being obtained through the 11 Mpc H
3. High level products of the HST optical images obtained as part of the
ACS Nearby Galaxy Survey Treasury (ANGST) will be available from XXX
line emission and broad-band R (from the ground) and the UV continuum (2 bands from GALEX )
are also available for most of the sample,
and will be delivered as part of the LVL project.
A fraction of galaxies in LVL sample is already available in the Spitzer
Archive (57 for MIPS
and 78 for IRAC ); the archival
images will be re-processed by our team to provide a common product together with the rest of the LVL sample. Of the galaxies with
Spitzer images, 33 are from the SINGS project.
We will deliver 256 of the galaxies in the LVL sample. The two remaining galaxies, the Magellanic Clouds (SMC and LMC),
are already being observed and delivered as part of other Spitzer Legacy Programs, SAGE (P.I.:Meixner) and
SAGE-SMC (P.I.:Gordan).
The final list of data products is as follows:
a. IRAC mosaics of 256 galaxies;
b. MIPS mosaics of 256 galaxies;
c. Optical images in H and R for 170 galaxies.
For the majority of the remaining galaxies, H
images are already available to the community through NED .
d. GALEX FUV (1529 A) and NUV (2312 A) images of 251 galaxies. The remaining galaxies are unobservable by GALEX due
to the bright object limit constraints.
The Data products from the Spitzer observations will be delivered to
the Spitzer Science Center and available from the
Spitzer Center's website.
They will consist of:
m, respectively), calibrated in MJy/sr and with constant
background level removed. FITS files will have the same characteristics
as the IRAC data products.
Ancillary Data
+[NII] emission, plus
continuum-substracted H+[NII] images, will
be delivered to the SSC , all of which are original observations of the
LVL team (described in Lee 2006, PhD thesis; Kennicutt et al. 2008, ApJS submitted). The
optical images will be single-extension FITS files and will be flux
and astrometrically calibrated (with standard WCS headers). The
H-alpha images will be continuum-subtracted.
UV Galaxy Survey (11HUGS) Cycle 1 (P.I.: R. C. Kennicutt) and Cycle 4 (P.I.: J. C. Lee) programs, through a Cycle 3 ACS Nearby Galaxies
Treasury Survey program (P.I.: E. Skillman), as well as from the GALEX PI-programs Nearby Galaxaies Survey (NGS), Medium-deep
Imaging Survey (MIS), and all-sky Imaging Survey (AIS), plus a handful of GO archival data. The combined programs will provide UV
data for 251 of the 258 galaxies in the LVL sample. The remaining 7 galaxies cannot be observed due to bright-object avoidance
constraints. Observations remain to be taken for 51 galaxies and these are expected to be completed by the end of 2008.
For each galaxy, 4 intensity images, two for each GALEX band (one image per band containing the full
GALEX field-of-view, 1.2 degrees,
and the other cropped to a radius of 4 times D_25), will be deileved, with 5 arcsec resolution.
GALEX pipeline processed images will also be available at
Multimission Archive at Space Telescope .