1. Large surveys and estimation of interstellar extinction Oleg Malkov Institute of Astronomy, Moscow Moscow, Apr 10-11, 2006

2. Galactic extinction models Three-dimensional models (A v = f [l,b,d]) are used to study Galaxy stellar populations. They are based –on spectral and photometric stellar data (Sharov 1963, Arenou et al. 1992) –on open cluster data (Pandey and Mahra 1987) –on star counts (Mendez and van Altena 1998) –on the Galactic dust distribution model (Chen et al. 1999, Drimmel et al. 2003) Total Galactic extinction maps (A v = f [l,b], see, e.g., Burstein and Heiles 1982, Schleger et al. 1998) are most appropriate for extragalactic studies

3. Galactic extinction models Three-dimensional models (A v = f [l,b,d]) are used to study Galaxy stellar populations. They are based –on spectral and photometric stellar data (Sharov 1963, Arenou et al. 1992) –on open cluster data (Pandey and Mahra 1987) –on star counts (Mendez and van Altena 1998) –on the Galactic dust distribution model (Chen et al. 1999, Drimmel et al. 2003) Total Galactic extinction maps (A v = f [l,b], see, e.g., Burstein and Heiles 1982, Schleger et al. 1998) are most appropriate for extragalactic studies

4. Large surveys are on hand / coming While 3D models, using spectral and photometric data, were based on 10 4 – 10 5 stars.......... modern surveys (2MASS, DENIS, SDSS,...) contain photometric (3 to 5 bands) data for 10 7 – 10 9 stars. But –one needs cross-identification between surveys –the surveys do not contain spectral data

5. Catalog cross-correlation services The identification of objects requires the federation of multiple surveys obtained at different wavelengths and with different observational techniques. Such cross- matching of catalogs is currently laborious and time consuming Using VO data access and cross-correlation technologies a search for counterparts in a subset of different catalogues can be carried out in a few minutes

6. Scientific output A search for brown dwarf candidates in the Sloan and 2MASS catalogs (US NVO prototype) and a search for type 2 QSOs in the VLT, HST and Chandra data (AVO prototype) demonstrated the exciting result of a new object discovery Information on interstellar extinction may be obtained from modern large photometric surveys data

7. Our goal is to design a procedure for construction of a 3D model of the galactic interstellar extinction. Assumption: uniform interstellar extinction law

8. Interstellar extinction law Rieke and Lebofsky 1985 BVRIJHK E(  V)/ E(B  V) 1.0.-0.78-1.60-2.22-2.55-2.74   V   k 0.1.1.782.603.223.553.74

9. Procedure For every available in photometric survey: –calculate (B  ) –E(B  ) = (B  (B  ) 0 –E(B  V) = E(B  k (B  ) 0 – intrinsic color indices (they depend on spectral type, see, e.g., Straizys 1977 tables) Assuming that a star satisfies the interstellar extinction law, we can expect E(B  V) be identical   if we guessed spectral type So we should determine a spectral type that yields the most appropriate set of (B- ) 0 to produce as close values of E(B-V) as possible

10. The procedure repeated for all spectral types Mean E(B  V) calculation, E = n -1  E(B  V)  n Minimization of  E 2 =  ( E(B  V)  n  E ) 2 n n

11. When spectral type is determined M B = M B (Sp) A V = 3.1 · E(B-V) A B = 1.324 · A V log r = (B – M B + 5 – A B ) / 5 …and construct a “r – A V ” diagram

12. 2’ test area: l=323, b=+6 (Lupus) Low latitude: to compare not only with “all- sky” maps (Sharov 1963, Arenou et al. 1992), but also with “galactic plane” maps (FitzGerald 1968, Neckel and Klare 1980) No dense molecular clouds Southern sky (DENIS covers)

13. Multicolor surveys DENIS (I, J, K’) 2MASS (J, H, Ks) USNO-B (SERC-J, ESO-R, AAO-R, SERC-I)

14. Mean wavelengths BRIJHK UBVRIJHKLMNQ440070008800125001620022000 DENIS80001250022000 2MASS123501662021590 SERC + ESO-R (USNO-B) 462566008075 AAO-R (USNO-B)6400

15. R- and I-bands problems (B-I) observed colors produce systematically smaller E(B-V); while (B-R) observed colors produce systematically larger E(B-V) R and I photometry was excluded from the investigation

16. H-band calibration problem Straizys (1977) tables provide (B-H) 0 for the following spectra: A2V-K5V, M0III-M5III, K5I-M4I If the procedure reveals another spectrum (based, in that case, on only two colors, B-J and B-K), the object is excluded from the investigation

17. Number of objects Two-arc-minute test area contains 134 objects cross-identified in all three surveys (2MASS, DENIS, USNO-B) For 36 of them all required photometry is available: B(USNO-B), J(DENIS), H(2MASS), K(DENIS) For 7 objects “(B-H) 0 -covered” spectra are revealed Compare with 0.0007 objects (on average) used in previous models

18. Error budget Observational photometry errors: 0.01 for USNO and 0.001 for IR surveys Calibration tables errors (depending on spectral type): 0.05 – 0.1 for intrinsic color indices and 0.2 – 0.5 for absolute magnitudes Interstellar extinction law coefficients (k ) error: 0.03 Difference between calculated E(B-V)  does not exceed 0.05 ( = J, H, K)

19. Uncertainties of final parameters The uncertainty of A V is about 0.1 depending primarily on the errors of (B- ) 0 The relative error of the distance is about 25%, depending primarily on the errors of absolute magnitudes

21. Conclusion 1. Advantages of the method No need for spectral type data and trigonometric parallaxes 10 4 – 10 6 times more stars are used, than in “classical” models “On-line” model can be constructed Other (future) multi-wavelength surveys like DPOSS (3 bands), SDSS (5 bands), … can be incorporated using VO techniques

22. Conclusion 2. Requirements Regions of very high density of interstellar matter should be excepted (or regional variations in the uniform interstellar extinction law should be taken into account) Intrinsic color indices tables should be available for all survey wavelength (e.g., substitution K DENIS for K 2MASS would increase the number of objects by at least 10 times) Variable stars, some types of double stars, solar system and extragalactic objects should be somehow removed from the sample

23. Conclusion 3. Future plans SDSS, DENIS, 2MASS, DPOSS, USNO-B data can be recalculated to the 13-color system, using appropriate calibration relations Modern (B- ) 0 calibration tables should be used Modern VO facilities (OpenSkyQuerry, RVO SkyNode tool, GAVO matcher, etc.) for cross- matching will be / are available