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AKARI IRC surveyof the Large Magellanic Cloud
Yoshifusa Ita,
Daisuke Kato,Takashi Onaka,
&
AKARI LMC team
2012/Feb/27-29 AKARI2 @ Jeju 1
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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
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Part 1: A brief summary of the AKARI IRC LMC survey
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The AKARI IRC LMC surveyPI. 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
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Observed area
= 10’ x 10‘
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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
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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.
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AKARI
SAGE/Spitzer
An o-rich AGBstar
A c-rich AGBstar
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5 sigma detection limits
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IRC+10216: an extreme c-rich AGB star
AB Aur : a Herbig Ae/Be star
β And: a tip of the RGB star
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2.5-5um spectra for sources in the observed 10 deg^2 field.
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Refer to Shimonishi’s Talk for initial results using thespectroscopic data
FOV = 10’ x 10’
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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.)
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Unique to AKARI
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Part 2: A brief description of the AKARI IRC LMC point source catalog
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Catalog compilation (1)Image data reduction
The latest IRC imaging data reduction toolkit ver.20110304 was used. Ask Egusa-san for details.
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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)
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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.
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an example : N3magnitude vs. error
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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
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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
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Figures from Kato’s paperTwo-Color diagram
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pink: YSO candidatescyan: background galaxyGruendl & Chi(2009)
blue: Naked starsorange: dusty O-rich starsgreen: dusty C-rich starsred: YSOs
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Figures from Kato’s paperColor-Magnitude diagram
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pink: YSO candidatescyan: background galaxyGruendl & Chi(2009)
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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.
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Part 3: A brief introduction of published results using the survey data
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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
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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
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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.
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Acknowledgements
Special thanks to: Dr. Fumihiko Usui
He kindly helped us a lot to make our observations effectively and smoothly.
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Appendix
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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
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Green: April – May 2008Blue: May – July 2008Red: October 2008Magenta: November - January 2008
Phase1&2
phase3
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SMC observationoverview
Open time program PI: Y. ITA
“Role of pulsation along the AGB”
Patchy area survey Photometry&Spectro
scopy N3,N4,S7,S11,L15,L2
4 NP,SG1,SG2
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Red: NIR,MIRS,MIRL availableCyan: NIR,MIRS availableBreen: only MIRL available
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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
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SMC 0059-7230H
blue:N3 green:S7 red: S11
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A
D
B
CE
A
B
C
D
E
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SMC 0050-7250H
blue:N3 green:S7 red: S11
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A
B
C
D
A
B
C
D
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SMC 0055-7250D
blue:N3 green:S9W red: L15
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A
BC
D
A
B
C
D
E
E F
F
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SMC 0050-7310E
blue:N3 green:S11 red: L15
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A
B
C
D
A
B
C
D
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SMC 0055-7230D
blue:K green:N3 red: S9W
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AB
C
D
A
B
C
D