1. AKARI IRC survey of the Large Magellanic Cloud Yoshifusa Ita, Daisuke Kato,Takashi Onaka, & AKARI LMC team 2012/Feb/27-29AKARI2 @ Jeju1

2. Index Part 1 A brief summary of the AKARI IRC LMC survey Part 2 A brief description of the AKARI LMC point source catalog Part 3 A brief introduction of published results using the early survey data 2012/Feb/27-29AKARI2 @ Jeju2

3. Part 1: A brief summary of the AKARI IRC LMC survey 2012/Feb/27-29AKARI2 @ Jeju3

4. The AKARI IRC LMC survey PI. Prof. Onaka Takashi Observation ~600 pointings 2006/Feb - 2007/July About 10 degree^2 Photometry 3.2, 7, 11, 15, 24 um Spectroscopy NP (2.5 - 5.0 um) λ/Δλ ~ 20 2012/Feb/27-29AKARI2 @ Jeju4 Observed area = 10’ x 10‘

5. Comparison to the other surveys Orange AKARI survey ~10 deg^2 Pink South Africa IRSF/SIRIUS JHK survey ~ 6.3 deg x 6.3 deg Green Spitzer SAGE survey~ 7 deg x 7 deg Cyan Zaritsky Optical (UBVI) survey ~ 8.5 x 7.5 deg 2012/Feb/27-29AKARI2 @ Jeju5

6. Comparison to the SAGE survey: λ and spectroscopy AKARI has 11 and 15μm imaging bands, which fill the gap between the IRAC and MIPS. see next page In addition to the photometric data, we also took low resolution (λ/Δλ ~ 20) 2.5 ~ 5 μm spectral data. 2012/Feb/27-29AKARI2 @ Jeju6 AKARI SAGE/Spitzer An o-rich AGB star A c-rich AGB star

7. 5 sigma detection limits 2012/Feb/27-29AKARI2 @ Jeju7 IRC+10216: an extreme c-rich AGB star AB Aur : a Herbig Ae/Be star β And: a tip of the RGB star

8. 2.5-5um spectra for sources in the observed 10 deg^2 field. 2012/Feb/27-29AKARI2 @ Jeju8 Refer to Shimonishi’s Talk for initial results using the spectroscopic data FOV = 10’ x 10’

9. Summary of the survey A 10 deg^2 area was observed with AKARI Imaging data 3.2, 7.0, 11, 15, 24 um detection limits are comparable to those of the SAGE survey Spectroscopic data 2.5 – 5.0 um, λ/Δλ ~ 20 The point source catalog is coming soon. (Kato, Ita, and Onaka et al.) 2012/Feb/27-29AKARI2 @ Jeju9 Unique to AKARI

10. Part 2: A brief description of the AKARI IRC LMC point source catalog 2012/Feb/27-29AKARI2 @ Jeju10

11. Catalog compilation (1) Image data reduction The latest IRC imaging data reduction toolkit ver.20110304 was used. Ask Egusa-san for details.

12. Catalog compilation (2) Source detection and photometry Source detection IRAF/DAOFIND Photometry IRAF/DAOPHOT PSF fitting photometry N3: satellite jitter → PSF vary in each image S7~L24: insensitive to the jitter → grand PSF Calibration ADU to Jy conversion factors (Tanabe et al. 2008)

13. Catalog compilation (3) Detection limits and Completeness Detection Limits (10σ, vega-mag) Completeness Limits (90% recovery limit) Add artificial sources to images Dense, Medium, Blank region (source number density) Source extraction Count the recovery rate Comparable to the 10σ detection limits except N3, which is about 2mag shallower.

14. an example : N3 magnitude vs. error 2012/Feb/27-29AKARI2 @ Jeju14

15. Catalog compilation (4) Astrometric Calibration Referenced to 2MASS catalog positions with a condition that at least 5 sources should be mached. If matching with 2MASS positions failed Alternative reference : Spitzer SAGE catalog In some cases, matching with SAGE catalog failed due to small number of sources in the FOV  S11 : 1 images, L15 : 5 images, L24 : 74 images Internal Positional Accuracy 0.6” at N3, 0.3” at S7, and S11, 1.0” at L15 and L24

16. Catalog compilation (5) Flagging Artifact Identification mux-bleed, column pulldown, and ghosts any sources within ±5 pixel belt area are flagged ghosts (inc. suspected ones) are flagged Multi-detected sources Only the best S/N data is adopted Final Products Archive lists all detected sources  more fainter sources, but with false detections Catalog only lists sources with SAGE counterparts  more reliable

17. Figures from Kato’s paper Two-Color diagram 2012/Feb/27-29AKARI2 @ Jeju17 pink: YSO candidates cyan: background galaxy Gruendl & Chi(2009) blue: Naked stars orange: dusty O-rich stars green: dusty C-rich stars red: YSOs

18. Figures from Kato’s paper Color-Magnitude diagram 2012/Feb/27-29AKARI2 @ Jeju18 pink: YSO candidates cyan: background galaxy Gruendl & Chi(2009)

19. Summary of the point source catalog Two types of point source catalogs. Archive include all detected sources Catalog only include sources with SAGE counterparts The point source catalog will be in public right after the acceptance of paper. (submitted to ApJ soon) We want to release imaging data as well. an GUI I/F to search images is needed.

20. Part 3: A brief introduction of published results using the survey data 2012/Feb/27-29AKARI2 @ Jeju20

21. Refereed Papers using AKARI/LMC data published so far. Mori, Tamami I. et al., 2012,ApJ,744,68 Observations of the near- to Mid-infrared Unidentified Emission Bands in the Interstellar Medium of the Large Magellanic Cloud Ngeow, Chow-Choong et al., 2010,MNRAS,408,983 Cepheid period-luminosity relation from the AKARI observations Shimonishi, T. et al., 2010,A&A,514,12 Spectroscopic observations of ices around embedded young stellar objects in the Large Magellanic Cloud with AKARI Seok, Ji Yeon et al., 2008,PASJ,60,453 Supernova Remnants in the AKARI IRC Survey of the Large Magellanic Cloud Shimonishi, T., et al., 2008,ApJ,686,99 AKARI Near-Infrared Spectroscopy: Detection of H2O and CO2 Ices toward Young Stellar Objects in the Large Magellanic Cloud Ita, Y., et al., 2008,PASJ,60,435, AKARI IRC Survey of the Large Magellanic Cloud: Outline of the Survey and Initial Results 2012/Feb/27-29AKARI2 @ Jeju21

22. Ngeow, Chow-Choong et al., 2010,MNRAS,408,983 Matched catalog with known Cepheid variables in the LMC. P-L relation is derived. important results to the evaluation of data reduction software Linearity Photometry 2012/Feb/27-29AKARI2 @ Jeju22

23. There should be more to come. There are six refereed paper published so far using the AKARI LMC catalog. We hope you to write papers using the AKARI/LMC Point Source Catalog. 2012/Feb/27-29AKARI2 @ Jeju23

24. Acknowledgements Special thanks to: Dr. Fumihiko Usui He kindly helped us a lot to make our observations effectively and smoothly. 2012/Feb/27-29AKARI2 @ Jeju24

25. Appendix 2012/Feb/27-29AKARI2 @ Jeju25

26. LMC phase-3 observation Observe almost the same region as in phase1&2 Bar region × too crowded Total 515 pointing ΔΦ = π Photometry & Spectroscopy N3, NP 2012/Feb/27-29AKARI2 @ Jeju26 Green: April – May 2008 Blue: May – July 2008 Red: October 2008 Magenta: November - January 2008 Phase1&2 phase3

27. SMC observation overview Open time program PI: Y. ITA “Role of pulsation along the AGB” Patchy area survey Photometry&Spectro scopy N3,N4,S7,S11,L15,L 24 NP,SG1,SG2 2012/Feb/27-29AKARI2 @ Jeju27 Red: NIR,MIRS,MIRL available Cyan: NIR,MIRS available Breen: only MIRL available

28. SMC spectroscopy results Total 500 arcmin^2 NP, SG1, SG2 spectroscopy Detected many point-like sources with PAH features Upper panel DSS image with equatorial coordinate grid Lower panel IRAS 100um image with galactic coordinate grid 2012/Feb/27-29AKARI2 @ Jeju28

29. SMC 0059-7230H blue:N3 green:S7 red: S11 2012/Feb/27-29AKARI2 @ Jeju29 A D B C E A B C D E

30. SMC 0050-7250H blue:N3 green:S7 red: S11 2012/Feb/27-29AKARI2 @ Jeju30 A B C D A B C D

31. SMC 0055-7250D blue:N3 green:S9W red: L15 2012/Feb/27-29AKARI2 @ Jeju31 A B C D A B C D E E F F

32. SMC 0050-7310E blue:N3 green:S11 red: L15 2012/Feb/27-29AKARI2 @ Jeju32 A B C D A B C D

33. SMC 0055-7230D blue:K green:N3 red: S9W 2012/Feb/27-29AKARI2 @ Jeju33 A B C D A B C D