IPHAS now, VPHAS to come

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(IPHAS now, VPHAS to come)

• Surveying the Galactic Plane in r, i and Ha

Janet Drew Imperial College London
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Public Website at Imperial http//www.iphas.org
/
NGC 6888
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Acronyms IPHAS The INT Photometric Ha Survey of
the northern Galactic Plane Filters
r,i,Ha Instrument Wide Field Camera, on the
Isaac Newton Telescope started August
2003 VPHAS The VST Photometric Ha survey of
the southern Galactic Plane (augmented to include
ug filters from UVEX-S proposal) Filters
ug,r,i,Ha Instrument OmegaCam, on the VLT
Survey Telescope from end 2007?
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Numbers of catalogued emission line stars by
magnitude, north (Kohoutek/Wehmeyer) and south
(Stephenson/Sanduleak)

• over 10,000 to be found?

South
south
North
north
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SHS IPHASs older (southern) brother .breaking
the 13th mag barrier
The AAO/UKST Ha survey of the southern Galactic
Plane 4o x 4o Ha, and broad-band red exposures on
film 1-2 arcsec spatial resolution (complete)
UKST Ha image of survey field 233
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Definition of IPHAS Survey area all northern
Plane longitudes latitude range 5o lt b lt 5o
(1800 sq deg) Magnitude limit (10s) r
20 Required observations Ha (120 sec),
Sloan r (30 sec) and i (10 sec) at 2
overlapping pointings Seeing lt 2.0 arcsec
(finally?)
.started using INT bright time .5-10 A EW
detectable
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IPHAS observations up to 19/1/2006
Target completion date end 2007
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Release of IPHAS data

• Reduced images already available from CASU to
  UK/Netherlands/Spain
• Partial/early release of point source
  catalogues to be announced here
• Final target photometrically uniform
  point-source catalogue (..and nebulae?)

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IPHAS filters
Transmission v. wavelength
r
i
(WFC)
lc FWHM r 6240
1347 Ha 6568 95 i 7743
1519 units Angstrom
Ha
(5000A)
(9000A)
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The (r-Ha, r-i) plane delivered by IPHAS-
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Changes in (r Ha) as Ha emission EW is grown
on top of a continuum
E(B-V)
Ha EW (Ang)
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• MMT/HectoSpec multi-fibre and other single-slit
  spectroscopic follow-up-
• IPHAS gives highly reliable lists of candidate
  emission line objects
• Positioning of main object classes in IPHAS
  colour-colour plane well-understood
• Ha minimum objects easily selected too (WDs,
  early-A stars, carbon stars, )

ITP programme now underway
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• ITP goals/component programmes-
• To use early-type emission line stars to map
  Galactic structure (in 06B the Outer Arm in
  Perseus at 6 kpc)
• Identify PNe outside the Solar Circle
• To search for IBs among the faint emission line
  candidates.
• To find missing WDs in the Galactic Plane
• 5. To map the chemistry of extreme red giants
  at a range of Galactocentric radii (EROs)
• 6. To demonstrate BD searching capability.

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An early result from ITP programme a young BD
(M6) with extremely strong Ha emission (EW 440
A)
(ISIS observation Aug 06 from E. Martin)
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Nebular astrophysics the Princes Nebula
(tomorrow)
(Deep follow-up optical image, Mampaso et al, AA
in press)
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To start end 2007 (?) VPHAS The VST photometric
Ha survey of the southern Galactic Plane
ugri and Ha, to AB mag 21 22
? can explore metallicity, and anomalous
extinction better discrimination of compact
(blue) objects
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VPHAS preparation-

• Negotiation of management plan first revision
  with ESO, currently
• Procurement of 4-segment Ha filter for OmegaCam.
  on order with Barr Associates, over half of
  80,000 already paid.

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Consortium organisation . evolution to EGAPS
to be discussed here

• Present IPHAS working-group structure
• Survey science and the structure of the Galaxy
• Nebulae and their progenitor objects
• Young populations (massive stars and YSOs at all
  masses)
• Binaries and compact objects
• Stellar variability and proper motion

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Closing acknowledgments-
to Robert Greimel for keeping the
observing/monitoring show on the road to the
Irwins and CASU supporting staff for
data-processing/interface to Nick Wright, for
the continuing production of beautiful IPHAS
mosaics