Changeset 41333 for trunk/doc/release.2015/ps1.analysis/response.txt
- Timestamp:
- Apr 13, 2020, 2:38:00 PM (6 years ago)
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trunk/doc/release.2015/ps1.analysis/response.txt (modified) (18 diffs)
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trunk/doc/release.2015/ps1.analysis/response.txt
r41324 r41333 16 16 data sets. 17 17 18 ** ** TBD : all of these items until Abstract18 ** added to the end of Section 3 Psphot Design Goals 19 19 20 20 For many of the sections, the reader would benefit by starting with … … 77 77 state the same for galaxy astrometry, fluxes and colors. 78 78 79 **** TBD 79 ** for each section, we have added a summary of where the values may 80 be found, and added an overall summary of this issue to the end of 81 the Basic Analysis section. 80 82 81 83 A detail of the code is presented (variable names, etc) that imply … … 96 98 that the photometric goals are achieved 97 99 98 **** TBD see note section Forced PSF Phot100 **** TBD : discuss relative quality of chip, forced, stack photometry 99 101 100 102 - Sec 7, where the image differencing detections and photometry is used … … 124 126 in one place would be a useful service. 125 127 126 **** TBD 128 **** TBD : summarize the lessons learned 127 129 128 130 Abstract: … … 219 221 applying to bright sources, and another addessing all (==faint) sources. 220 222 221 **** TBD 223 ** We have expanded the discussion in 4.7 (Faint Source Analysis) to 224 explain which of the steps in the bright source pass are repeated 225 and which are skipped. We refer back to the specific sections and 226 explain where there are detailed differences in the bright and 227 faint versions of the same step. 222 228 223 229 Sec 4.1: … … 227 233 of Sec 4.8) that the PSF model for an image is actually selected. 228 234 229 **** TBD230 235 ** The aperture correction is measured at the end of the bright-star 231 ** pass, at which point the PSF model is chosen and fixed. A final 232 ** aperture correction is measured at the end of the full analysis, 233 ** but only for the PSF model class selected earlier. 236 pass, at which point the PSF model is chosen and fixed for the rest 237 of the analysis. A final aperture correction is measured at the 238 end of the full analysis, but only for the PSF model class selected 239 earlier. But for PV3, the PDF model was fixed to the PS1_V1 240 version, so this selection was not performed. We have added text to 241 4.5.3 to explain how the aperture correction is used to select a 242 PSF model, and that only the single model form was used for PV3. 243 We also note in section 4.8 that we re-measure the aperture 244 correction at the end with the other sources subtracted. 234 245 235 246 Sec 4.3: … … 264 275 measure is used. 265 276 266 **** TBD: model? 277 ** added a table showing sky recovery vs stellar density from 278 simulations using the standard psphot analysis vs other methods, 279 added discussion of the results. 267 280 268 281 Sec 4.4.1: … … 319 332 320 333 **** TBD: SHOW SOME EXAMPLES of PSF variations 334 choose 3 exposures: 1 with good IQ, one with bad IQ, but round, one with bad IQ but not round, 335 plot some IQ stats (Mxx - Myy) / (Mxx + Myy) 321 336 322 337 - Please state whether the PSF model is this set of formulae … … 344 359 sources by GAIA. 345 360 346 ***** TBD 361 ** This is an interesting suggestion, but out of the scope of this 362 effort. we have added this to the lessons-learned discussion 347 363 348 364 Sec 4.5.3: … … 419 435 and presented as a future development effort. 420 436 421 **** TBD 437 **** TBD : wording of full PSF model section 4.6.6 422 438 423 439 - Remind the reader that the 4 independent parameters includes a local sky 424 440 value. 425 441 426 **** TBD: double-check if the sky is allowed to float in this step 442 ** in fact, we do not allow the sky to float; fixed the wording to 443 specify the *3* independent parameters and to explain why we do not 444 allow the sky to float. 427 445 428 446 - "remaining flux should be below 1\sigma significance" -> … … 437 455 range. 438 456 439 **** TBD: was the turned on for PV3?457 **** TBD: double-star mode: was this turned on for PV3? ppSim to show recovery 440 458 441 459 Sec 4.7: … … 444 462 could be included here. 445 463 446 **** TBD: include detection limit description 464 ** This was a definitely gap. We have added a subsection (4.9) 465 discussing the completeness and contamination, using both simulated 466 and real data to illustrate these effects 447 467 448 468 Sec 4.8: … … 501 521 atmospheric transparency variations. 502 522 503 **** TBD 523 ** we have added discussion and some plots showing the repeatability 524 of the brightest stars for PSF and aperture magnitudes. We also 525 discuss the long-term site characteristics and the impact of the 526 atmosphere on the photometric calibration, relating back to the 527 ubercal work of Schlaley et al 2012. 504 528 505 529 Sec 5: … … 534 558 compare well to those in the PS1 catalog? 535 559 536 **** TBD: compare to SDSS560 **** TBD: compare Petrosian mags to SDSS for some example 537 561 538 562 Sec 5.3: … … 561 585 error of this approximation should be stated. 562 586 563 **** TBD: model 587 **** TBD: model central pixel errors for Sersic models 564 588 565 589 Sec 5.4: … … 626 650 discussion would be Zackay & Ofek 2016. 627 651 628 ** ** TBD652 ** added references and updated the text 629 653 630 654 - The terms "skycell" and "warp image" are first used here without … … 664 688 and if not, which code would it be most similar to? 665 689 666 **** TBD 690 **** TBD : check on GREAT challenge to compare code 667 691 668 692 - Define "KSB" and "HFK" references in-line … … 789 813 - Some additional references should be included; some suggestions above. 790 814 791 ** ** TBD815 ** added additional references 792 816 793 817 ** Also, we have added Danny Farrow (UK Durham & MPIA) to the authors
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