Main criteria for classical PDRs are:

1
Canadian Involvement in the Herschel Space
Telescope Key Program The Warm and Dense ISM
(WADI)
Kevin France Peter G. Martin (CITA/U of
Toronto) for the WADI Consortium
Abstract We report on Canadian involvement in the
Herschel Space Telescope Guaranteed Time Key
Programme The Warm Dense ISM' (WADI). WADI
explores the roles of UV photons from massive
stars and shocks from supernova outflows in
shaping the Galactic ISM. WADI will use HIFI and
PACS observations to provide a set of far-IR
atomic and molecular line diagnostics that can be
used as templates for the interpretation of data
from more distant star-forming galaxies. CITA is
part of the WADI consortium, coordinating the
observing strategy and supporting observations of
the nearby PDR IC 59. We present an overview of
the WADI project and ongoing efforts to obtain
complementary imaging and spectral observations
of IC 59, from IR to UV wavelengths.
CITA Involvement-IC63/IC59
The emission nebula IC 63 is a prototypical
object for studies of molecular photoexcitation
in the local interstellar medium. In order to
better understand the influence of density
structure on the PDR energy balance and
kinematics, we have applied the Canadian WADI
time to the nearby cloud IC 59. Both clouds are
under the influence of ? Cas (B0.5IVe).
Comparing IC 59 and IC 63 will allow us to
remove uncertainties about the shape of the
illuminating radiation field when modeling the
spectral characteristics of these objects. WADI
observations of IC 63/IC 59 are being coordinated
by Marco Spaans, with the IC 59 observing
strategy being defined at CITA. To date, we
have created the Herschel Astronomical
Observation Requests (AORs) for IC 59, compiled
supporting visible to far-IR observations, and
have submitted a proposal to acquire
Discretionary Time observations of possible
fluorescent H2 emission with FUSE. The AORs
target numerous atomic, molecular, and dust
emissions, including C II, O I, O III, N II, N
III, HD, CH, CH, OH, CO, NH, NH3, several
species of H2O, and far-IR dust continuum from
72-210 um. These observations will be
complemented by Herschel-SPIRE and PACS imaging
as part of the "Evolution of Interstellar Dust"
KP.
AV
IC 63 IC 59
Fig2- PDR models for H and C abundances across
the interface
3.6(B), 5.8(G), 8.0(R) µm
WADI Targets - PDRs
WADI Science Goals
IRAC 8 ?m
MIPS 24 ?m

• The WADI project studies feedback processes from
  the life and death of massive stars, exploring
  the role of UV photons from massive stars and
  shocks from supernova outflows in shaping the
  Galactic ISM. The KP has four primary science
  goals
• to determine the energy balance in
  photodissociation regions (PDRs), comparing the
  energy input by UV photons with the cooling
  through dust continuum and far-IR line emission.
  
• 2) photo-induced chemistry in the ISM, where
  processing by UV photons can catalyze reactions
  with light hydrides, e.g., involving the chemical
  chains of carbon (CH, CH2, CH3), oxygen (OH,
  H2O, H3O), and nitrogen (NH, NH2, NH3).
• 3) PDR dynamics and kinematics, focusing on the
  photoevaporation of PDR interfaces and advection
  of molecular material into a region where it can
  be dissociated by UV photons.
• 4) shock waves driven by supernovae, an
  important source of mechanical energy input into
  the ISM.
• This study will provide an understanding of a
  rich set of far-IR atomic and molecular line
  diagnostics the at can be used as templates for
  the interpretation of data from more distant
  star-forming galaxies.
• Along with the KP team effort to prepare the GT
  proposal in detail, we have coordinated the
  observing strategy and supporting observations
  for the nearby PDR IC 59, a complementary target
  to the prototypical H2 emission nebula IC 63. We
  will use Herschel HIFI and PACS spectroscopic
  observations in order to develop better models of
  PDR interfaces, constraining the processes that
  affect the evolution of the ISM.

Fig4-Wide field B-band image of the IC63/IC59
system (top), and individual Spitzer-IRAC (left)
and MIPS (right) images
WADI Targets
Main criteria for classical PDRs are - the
sources cover a wide range of FUV field
intensities and spectral shapes. - the sources
have a well defined geometry and orientation with
respect to the observer illuminating star,
preferably edge-on. - high spatial resolution is
an asset, favoring nearby sources unfortunately
closer PDRs tend to have lower UV fields. -
complementary chemical information. All proposed
source have been extensively studied with
ground-based observations, so that a large set of
complementary data is available. As a reference,
we plan to perform complementary observations of
one dense cloud which is exposed to the standard
interstellar radiation field only and not
influenced by shocks (B68). The list presented
above is ordered by the intensity of the UV
radiation field, where the value given here is
the field at the edge of the clouds, relative to
the interstellar radiation field (ISRF Draine
1978). All of the sources exhibit particular
features that further underline the value of
their observation. Comparing Carina and NGC7023
shows the impact of the spectral shape of the
illuminating field, comparing S140 and Rosette
shows the influence of X-rays on the PDR
chemistry, and Ced201 will provide clues to
time-dependent PDR chemistry due to the high
proper motion of the illuminating source.
Fig5-Overlay of the Spitzer-IRS mapping
observations (above) and the IRS spectra (right)
FUSE Discretionary Time IC 59 - H2 Fluorescence
Image courtesy of David Teyssier
WADI Consortium
Herschel/WADI -- Consortium members Volker
Ossenkoph-PI KOSMA/SRON DE/NL M. Roellig
KOSMA-DE M. Gerin
LERMA FR R. Simon
KOSMA-DE A. Gusten
MPIR-DE M. Spaans Kapteyn-NL A. Benz
ETH-CH J. Stutzki
KOSMA-DE F. Boulanger
IAS-FR D. Teyssier ESA-ES A. Fuente
OAN-ES H. Yorke
JPL-US A. Harris
UMD-US O. Berne CESR-FR Ch. Joblin
CNRS-FR J. LeBourlot
CNRS-FR Th. Klein
MPIR-DE S. Bruderer ETH-CH S. Lord
JPL-US K. France
CITA-CAN C. Kramer
KOSMA-DE J. Coicoechea LERMA-FR P. G. Martin
CITA CAN B. Mookerjea
UMD-US J. Martin-Pintado CSIC-ES F.
LePetit LUTH-FR D. Neufeld
JHU US D. Poelman Kapteyn-NL S.
Philipp MPIR-DE R. Rizzo
UEM-ES T. Phillips
JPL-US
B 8 ?m 24 ?m
Fig3 Sample Herschel AORs for IC 59. The blue
stripes are HIFI maps (CH-536 and CII-1900 GHz),
the green and red squares are PACS, and the cyan
squares are proposed for FUSE
For More Information france_at_cita.utoronto.ca www.
cita.utoronto.ca/france/
Fig1 Example of typical HIFI mapping
strategy. Cuts sample the PDR interface as they
cross from the HII region onto the molecular
cloud.
Fig6 Fluorescent H2 emission in IC 63 from HUT
(left) and FUSE (right)