Issues which must be closed out before software implementation in 2MAPPS v3.0
subsystems can be completed and final uniform processing can begin.
Most require Science Team decisions or further analysis.
CogE/T: Cognizant Engineers, Analysts and Science Team members assigned to
task.
PRI(ority): Priority for meeting start of final processing. 1=Highest.
ST(atus): C=Analysis complete, coding and testing in progress.
P=Pending - Analysis and discussion in progress.
O=Open - Needs attention
Subsystem PRI ST Description and References
(CogE/T)
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1. RDFRAME 1 P Finalize saturation level derivation. Derive saturation
(Wheaton, maps for relevant hardware periods.
Skrutskie) (see: http://spider.ipac.caltech.edu/staff/waw/2mass/thresholds/index.html)
2. PIXCAL 1 P Demonstrate algorithm and calibration of saturated R1 star
(Kopan,Xu, photometry.
Tam) (see: http://spider.ipac.caltech.edu/staff/raymond/2mass/bootstrap/history.html
and http://spider.ipac.caltech.edu/staff/cxu/2mass/bstar/new_effort/new_effort.html )
3. PIXPHOT 1 P Characterize completeness and reliability of meteor trail
(Kopan,Hurt) detection/blanking. Tune parameters.
(see: http://spider.ipac.caltech.edu/staff/gene/analysis/meteor.html)
4. PIXPHOT 1 P Define requirements for Atlas Image coverage/mask maps.
(Chester,
Huchra)
5. PIXPHOT 1 C Decide whether or not to allow n=1 sample pixels into
(Kopan,Jarrett) Atlas Images. Decision is to allow n=1 samples into
Atlas Images. Coverage maps will track.
6. PROPHOT 1 P Decide whether or not to deblend. Deblending completeness,
(Marsh,Rho reliability and photometric accuracy demonstrated with
Weinberg) simulations, high resolution truth data, and repeatability.
Decision is to proceed with deblending. Properties of
deblended population to be examined in detail.
(see: http://spider.ipac.caltech.edu/staff/kam/2mass/deblending/deblend_list.html)
7. PROPHOT 1 P Incorporate confusion noise term in photometric noise model.
(Marsh) (see: http://spider.ipac.caltech.edu/staff/kam/2mass/confusion/confusion.html)
8. MAPCOR 1 P Complete analyses to refine confusion flagging parameters
(Evans,Howard, to flag for biased photometry.
Stiening,Beichman) (see: http://spider.ipac.caltech.edu/staff/evans/2mass.index.html,
and http://kutath.phast.umass.edu/%7eehwd/2mass/snowflake.html)
9. MAPCOR 1 P Perform analysis to derive artifact flagging parameters.
(Evans,Nelson, Include source density terms to improve completeness in
Tam,Beichman) Galactic Plane.
(see: http://spider.ipac.caltech.edu/staff/evans/2mass.index.html)
10. MAPCOR 1 P Determine whether PSF normalization will use a look-up
(Evans,Gizis) table, like aperture corrections, or be empirically
determined in each scan. If empirically, what to do about
scans that get skewed values because of bright stars and
other problems?
(see: http://spider.ipac.caltech.edu/staff/gizis/2mass/detap.html)
11. MAPCOR 1 P Decide how to treat deblended sources in artifact
(Evans,Cutri) identification and photometric correction process.
12. BANDMERGE 1 P Decide how to treat deblended sources consistently.
(Fowler,Cutri) Applicable for both passive and active deblending.
Proposal is to "accept" only if deblend is consistent for
all bands in which a sources is detected, and "reject"
if not self-consistent. If deblend is rejected,
quote upper limits formed from photometry in bands
in which the deblend is inconsistent.
13. POSMAN 1 C Decide on how distortion model will be implemented
(McCallon, Plan described in:
Kopan,Marsh, http://spider.ipac.caltech.edu/staff/waw/2mass/misc/distortion.html
Wheaton,Monet)
14. GALWORKS 1 P Decide on processing thresholds in high source density
(Jarrett, regions.
Chester,Huchra, (see: http://spider.ipac.caltech.edu/staff/jarrett/2mass/3chan/v3/galworks.html)
Schneider)
15. GALWORKS 2 P Should bright star masking in GALWORKS be aligned with
(Jarrett, MAPCOR artifact flagging?
Chester,Huchra, (see: http://spider.ipac.caltech.edu/staff/jarrett/2mass/3chan/v3/galworks.html)
Schneider)
16. GALWORKS 2 P Should proposed change to postage stamp images be adopted?
(Jarrett, (see: http://spider.ipac.caltech.edu/staff/jarrett/2mass/3chan/v3/galworks.html)
Chester,Huchra,
Schneider)
17. CALMON 2 C Decide if time-dependent atmospheric extinction terms
(Wheelock, should be used. If so, what model - look-up table or
Gizis,Seitzer) smoothly varying function. Decided that monthly
look-up table will be used for extinction coefficients.
Table to be derived from final global calibration analysis.
18. CALMON 1 P Determine if higher order fits, or continguous multiple
(Wheelock, linear fits should be used in nightly photometric zero-point
Skrutskie, fitting.
Cutri)
19. MPCAT 2 O Decide if comet matching should be handled differently than
(Fowler, asteroids (e.g. larger search radius?).
Sykes,Tholen,
Price)
20. QA 2 P Finalize pre-processing triage requirements. (e.g. what
(Cutri, data will go through final processing - Q>0 Q>5,
Kirkpatrick) repeated tiles, ancillary science observations?)
21. QA 2 O Define final QA criteria and requirements, if different
(Kirkpatrick) from current ones.
22. CATGEN 3 O Selection - Decide on SNR thresholds for final catalog
(Cutri) selection.
23. CATGEN 3 O Decide if any global photometric homogenizing is
(?) possible/desirable.
24. CATGEN 3 O How to deal with increased extended source "chaff" due to
(Jarrett) GALWORKS unrestrained processing of big galaxies.
Last Updated: 27 November 2000
R. Cutri - IPAC