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ChaMPlane: The Chandra Multiwavelength Plane Survey
Servillat Mathieu, Grindlay J.E., van den Berg M., CfA, Cambridge, USA, Hong J., Zhao P., Allen B. (CfA), Laycock S. (Gemini) mservillat@cfa.harvard.edu

The Chandra Multiwavelength Plane Survey (ChaMPlane) is designed to identify the point X-ray sources discovered by the C h a n d r a X-ray Observatory in the Galactic Plane and in particular in the Galactic Center [1]. Based on a multiwavelength dataset, we aim to identify peculiar Galactic populations of objects such as accreting white dwarfs, neutron stars and black holes in order to study the distribution and the evolution of those populations. The X-ray survey has now extended through 10 years of Chandra data. 193 pointings were processed specifically in order to produce a catalog of serendipitous sources [2]. We obtained o p t i c a l i m a g i n g data for 74 fields (Mosaic @ CTIO 4m, see [3]), and we are now conducting a follow-up s p e c t r o s c o p y and n e a r i n f r a r e d i m a g i n g (ISPI @ CTIO 4m) program in order to detect counterparts to the X-ray sources and identify their nature (latest observations performed in the summer 2009 and being processed). We also focus on the Galactic bulge with the B u l g e L a t i t u d e S u r v e y (BLS) and deep observations of 3 l o w e x t i n c t i o n w i n d o w s at 1.4° (Limiting Window), 2° (Stanek's Window) and 4° (Baade's Window) below the Galactic Center.

ChaMPlane fields in Galactic coordinates. B l a c k d o t s : fields observed in optical, red dots: fields observed in near-infrared, blue dots: mutiobject spectroscopy performed for selected sources.

Zoom on the low extinction windows

X-ray Chandra ACIS-I -S Latitude |b| < 12° Exposure time > 20 ks (AO1-10, ~295 obsids)

Optical (V, R, I, H) 74 pointings with Mosaic @ CTIO 4m (2001-2009)

Near infrared (J, H. K) 19 pointings with ISPI @ CTIO 4m (2007-2009) Multi-objects spectroscopy 25 pointings Hydra @ CTIO 4m (2004-2009)

The Bulge Latitude Survey (3°x1°) Completed in 2009 in X-ray and near-infrared

Chandra Discovery of an Intermediate Polar in Baade's Window
Hong J, van den Berg M, Laycock S, Grindlay JE, Zhao P, 2 0 0 9 , ApJ, 699, 1053
· In the Baade's window (BW), a low extinction region at about 4 south of the Galactic center · Large X-ray modulations at a p e r i o d o f 1 0 2 8 . 4 s in the 0.3­8 keV band · H a r d X - r a y s p e c t r u m (photon index = 0.44 ± 0.05, NH = 1.5 ± 1.0 в 1021 cm-2) · F a i n t (V 22), relatively b l u e (B0 - V0 0.05) counterpart with IMACS @ Magellan 6.5m · Bright I n t e r m e d i a t e P o l a r (1033 erg s-1 at 8 kpc) in the Galactic bulge

Radi near

Hong J, van den Berg M, Grindlay JE, Laycock S, 2 0 0 9 , ApJ, accepted
· L o g N - L o g S and s p a t i a l d i s t r i b u t i o n s of X-ray point sources in seven Galactic Bulge (GB) fields within 4 deg from the Galactic Center (GC) · Highly c o n c e n t r a t e d a t t h e c e n t e r , more heavily than stellar distribution models · X-ray luminosity and spectral properties support the idea that the most likely candidate is m a g n e t i c c a t a c l y s m i c v a r i a b l e s (CVs), primarily i n t e r m e d i a t e p o l a r s (IPs)

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ChaMPlane accretion-dr

van den Berg M, Hong J, Grindlay JE, 2 0 0 9 , ApJ, 700.1702
· Identification through b l u e o p t i c a l c o l o r s , excess H fluxes, and high X-ray to optical · 3 compact binaries, · 22 candidates accreting · Possibly a majority of m flux ratios probably cataclysmic variables binaries agnetic cataclysmic variables [2] Hong et al. 2005

deep Gal iven bina

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ulge survey. the Limiting

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Quantile diagram [4] Absorbed sources

Hard sources




[3] Zhao et al. 2005 [4] Hong et al. 2004

References

[1] Grindlay et al. 2005

See also the website: http://hea-www.harvard.edu/ChaMPlane/index.html