Developing Tools to Search for PNe in the J­PAS Survey

The Javalambre Physics of the Accelerating Universe Astrophysical Survey
(J-PAS) is a new astronomical facility dedicated to mapping the
observable Universe in 59 colors, and will produce high-quality images
and an unique spectral resolution over the 8000 deg^2. It will consist
of two telescopes. One of 2.5-m (J-PAS) and another of 0.8-m (J-PLUS,
mainly for calibrations). The former will have a dedicated 1.2-G pixel
survey camera (containing an array of 14 CCDs) with a FoV of 5 deg^2. It
is planned to take 4–5 years and is expected to map the above area
to a 5σ magnitude depth for point sources equivalent to
i˜23.3 over an aperture of 2 arcsec^2. The J-PAS filter system
consists of 54 contiguous narrow band filters of 100-Å FWHM, from
3,500 to 10,000Å. To those filters 2 broad-band ones will be at
the extremes, UV and IR, plus 3 SDSS g, r, and i filters. J-PLUS, on the
other hand, comprise 12 filters, including g, r, i and z SDSS ones.
Though about 2,500 PNe (confirmed spectroscopically) are known in the
Galaxy, only about 20 objects have been identified as halo PNe. They
were found from their location, kinematics and chemistry. Halo PNe are
able to reveal precious information for the study of low- and
intermediate-mass star evolution and the early chemical conditions of
the Galaxy. The characteristic low continuum and intense line emissions
of PNe make them good objects to be searched for by J-PAS. For instance,
the halo PNe BoBn 1, DdDm 1 and PS 1, located somewhere between 11 and
24 kpc from the Sun, have B magnitudes of 16, 14 and 13.4, respectively.
Such values are easily encompassed by J-PAS, given the typical limit
magnitude of the survey. Because of the low number of halo PNe detected
so far, we are developing tools to find these objects by using
J-PAS/J-PLUS, and planning a follow-up study for any possible candidate
identified by the survey. Color magnitudes diagram able to separate PNe
from other strong line emission objects are being explored by the group
and results are discussed in this contribution.