1. FMOS and UKIDSS Galactic Astronomy Phil Lucas UHerts

2. Outline 1) UKIDSS galactic surveys and FMOS 2) Brown Dwarf Science with FMOS 3) X-ray sources and FMOS 4) Mapping nebulae with FMOS

3. UKIDSS: The UK Infrared Deep Sky Survey WFCAM 0.8-2.5  m imager FOV = 0.76 deg 2 /tile Forward mounted Cass focus on UKIRT UKIDSS UK+ESO+Japan 5 surveys from 2004: UDS 0.76 deg 2 DXS 35 deg 2 GPS 1800 deg 2 GCS >1000 deg 2 LAS 4000 deg 2 - Galactic Plane at |b|<5 degrees. - Galactic Clusters, eg. Orion, Pleiades. - High latitude survey.

4. Brown Dwarfs: background M6L5T8 Brown dwarfs spectral types are a cooling sequence. The spectral types have been determined using 2MASS and SLOAN sources, eg.Kirkpatrick et al.(1999, ApJ 519,802) They range from near M6 soon after formation to T8 and later, not yet discovered types at ages several Gyr. THE GCS and GPS will mostly see young M and L type brown dwarfs.

5. Brown dwarfs, UKIDSS and FMOS (1) The UKIDSS science goals are to measure the IMF in a range of different environments and study brown dwarf formation and kinematics. The GCS will survey 10 nearby clusters at JHK to K=18.4. The younger clusters have high source densities -> FMOS targets. The GPS will survey half the galactic plane at JHK to K=19. Hundreds of clusters will be detected but most will be quite distant and crowded. FMOS will be invaluable for testing cluster membership. SIRTF, ASTRO-F and MSX surveys. Perseus OB2 Taurus-Auriga Orion Scorpio-Centaurus Alpha-Per Pleiades Hyades Praesepe Coma-Ber IC4665

6. Brown Dwarfs, UKIDSS and FMOS (2) Credit: 2MASS All Sky Survey

7. Brown Dwarfs, UKIDSS and FMOS (3) What will FMOS spectra tell us? - confirm cluster membership – reliable LF. - 0.9 – 1.8 um spectra yield Effective Temperature, spectral type and surface gravity. - This allows determination of location on HR diagram, yielding age corrected IMF and the star formation history of the cluster. - Effects of circumstellar matter on spectra, eg. scattered light, and externally excited [SIII] and accretion powered Hydrogen recombination lines will be measured with a large sample (Paschen series). FMOS spare fibres will be vital for good background subraction.

8. Brown Dwarfs, UKIDSS and FMOS (4) (Lucas et al.2001, MNRAS 326,695)

9. Chandra / UKIDSS sources and FMOS The UKIDSS Galactic Plane Survey will identify IR counterparts to thousands of Chandra and XMM X-ray sources. Chandra Galactic Centre study. CVs, Neutron star/White Dwarf binaries, wind accreting binaries, active stars? Background AGN? High source density in the plane: typically 2 sources per Chandra error circle (0.3 to 1 arcsec). FMOS will be needed for a large study to understand the various populations. FMOS science: (1) detect accretion signatures: HI lines; (2) detect and identify faint stellar companion. CHANDRA - ACIS image

10. Chandra sources and FMOS (2) The Chandra Deep Field. Other UKIDSS GPS fields. Nearby spiral galaxies. In all these cases IR spectroscopy is desired to identify X-ray sources.

11. High Mass Star Formation Regions Star formation regions containing O-type stars often have pervasive nebulosity with a wide range of excitation conditions. Analysis of this such regions is important to understand the effect of environment on star and brown dwarf formation and the IMF. FMOS can sample nebular emission lines in 400 places. Useful lines in the ZJH bands are [SIII] at 953 nm, HeI at 1080 nm, and the Paschen series of hydrogen. HST/WFPC1 image of a star forming region

12. SNe remnants, microquasars and PNe FMOS can provide information on the excitation conditions in all types of high excitation nebulae. MOIRCS will be more useful for low excitation nebulae. The UKIDSS GPS will identify the infrared targets for which multi-fibre data will be useful. Multi-epoch FMOS data over a period of a few years will help us to understand the changing excitation conditions in highly excited and fast moving jets and knots, such as those observed in the microquasar SS433 or in planetary nebulae such as the Helix nebula. Rudy et al.(2001, ApJ 121, 362) spectra of a PN…

13. Conclusions FMOS and similar IRMOSes will be essential for the exploitation of data from the UKIDSS Galactic Plane Survey and Galactic Clusters Survey. For Galactic Science optical MOSes are of little use. FMOS will benefit but from a synergy of X-ray, near IR and mid-IR data.