Index: /trunk/doc/release.2015/ps1.calibration/calibration.tex =================================================================== --- /trunk/doc/release.2015/ps1.calibration/calibration.tex (revision 41275) +++ /trunk/doc/release.2015/ps1.calibration/calibration.tex (revision 41276) @@ -21,6 +21,6 @@ %% NOTE: 2019 Feb versions of the figures are generated in /data/kukui.1/eugene/cal.paper.20190217 -%\def\picdir{pics} -\def\picdir{.} +\def\picdir{pics} +%\def\picdir{.} % Pick a terse version of the title here; @@ -106,9 +106,9 @@ consistent zero points over the entire area surveyed, the \approx 30,000 square degrees north of $\delta = -30$\degrees. \textadd{Using external -comparisons, we demonstrate that the resulting photometic system is -consistent across the sky to between 7 and 12.4 millimags depending on +comparisons, we demonstrate that the resulting photometric system is +consistent across the sky to between 7 and 12.4 millimagnitudes depending on the filter. For bright stars, the systematic error floor for -individual measurementsis $(\sigma_g, \sigma_r, \sigma_i, \sigma_z, -\sigma_y) = (14, 14, 15, 15, 18)$ millimags.} The astrometric +individual measurements is $(\sigma_g, \sigma_r, \sigma_i, \sigma_z, +\sigma_y) = (14, 14, 15, 15, 18)$ millimagnitudes.} The astrometric calibration compensates for similar systematic effects so that positions, proper motions, and parallaxes are reliable as well. \textadd{The @@ -385,5 +385,5 @@ Coordinates and calibrated magnitudes of stars from the reference -database are loaded by \ippprog{pasastro}. A model for the positions of +database are loaded by \ippprog{psastro}. A model for the positions of the 60 chips in the focal plane is used to determine the expected astrometry for each chip based on the boresite coordinates and @@ -488,7 +488,7 @@ (changes from over time). The spatial scale on which the astrometric deviations due to atmosphere are varying is related to - the isoplanetic patch size. We note that, in the typical conditions + the isoplanatic patch size. We note that, in the typical conditions at the \PSONE\ site, if the seeing is due to low-lying atmospheric - layers, the isoplanetic patch scale will be at most a few arcminutes + layers, the isoplanatic patch scale will be at most a few arcminutes \citep{1988ESOC...30..693B}, and smaller when the seeing comes from higher altitudes.} @@ -886,5 +886,5 @@ measurements of the same stars from different nights to tie nights together. \textadd{This analysis relies on the chemical and - thermodynamic stability of the atmosphere during a photometic night + thermodynamic stability of the atmosphere during a photometric night so that the zero point and extinction slope are stable as a result.} Flat-field corrections are also determined as part of the minimization @@ -916,5 +916,5 @@ SDSS as an external reference, with standard deviations of (8.0, 7.0, 9.0, 10.7, 12.4) millimags in (\grizy). Internal comparisons - show the zero-points of indidual exposures to be consistent with the + show the zero-points of individual exposures to be consistent with the Ubercal solution with a standard deviation of 5 millimags. The former is an upper limit on the overall system zero-point stability, @@ -2395,5 +2395,5 @@ rotation curve and set a fixed proper motion.} If we do not have a distance modulus from the Green et al analysis, we assume a value of -500pc. \textadd{We find that applying our Galactic rotatation model improves +500pc. \textadd{We find that applying our Galactic rotation model improves the systematic proper motion errors to some extent. The standard deviation of the quasar proper motions (averaged on 12 arcminute @@ -2452,5 +2452,5 @@ astrometric analysis to provide a measurement which is robust against failures. In addition to the detector effects artifacts which affect -astrometry, the astrometric measurments may have non-Gaussian outliers +astrometry, the astrometric measurements may have non-Gaussian outliers due to the high degree of structure in the astrometric transformations introduced by the camera optics and the atmosphere. We have again @@ -3118,5 +3118,5 @@ Canada-France Imaging Survey, or CFIS, collaborations) is expected to release deep photometry in the {\it ugriz} bands for roughly 5000 -square degrees of the northern hemisphere with agressive photometric +square degrees of the northern hemisphere with aggressive photometric precision goals. This collaboration is in part motivated to support the Euclid satellite mission, which requires deep 8-band photometry to @@ -3137,5 +3137,5 @@ \textadd{Second, cross-comparisons between independent datasets are critical to reveal the limitations. This lesson has appeared several times in our -intestigations, in the comparison between Pan-STARRS and Gaia above, +investigations, in the comparison between Pan-STARRS and Gaia above, between Pan-STARRS and SDSS \citep{2016ApJ...822...66F}, and in the comparison between Pan-STARRS and 2MASS \citep{2013ApJS..205...20M}. Index: /trunk/doc/release.2015/ps1.calibration/response.txt =================================================================== --- /trunk/doc/release.2015/ps1.calibration/response.txt (revision 41275) +++ /trunk/doc/release.2015/ps1.calibration/response.txt (revision 41276) @@ -1,35 +1,14 @@ - -** We are resubmitting our article "Pan-STARRS Photometric and - Astrometric Calibration" after addressing suggestions raised by the - referee. We thank the referee for detailed comments and - suggestions. Below are our responses to the referee's suggestions. - In the response below, our responses are preceeded by "**". - Modified portions of the article text are highlighted with boldface - type. Reviewer's Comments: -The paper "Pan-STARRS Photometric and Astrometric Calibration" by -Magnier et al. describes the calibration of a major modern sky survey. -The paper is well written and provides sufficient technical detail to not -only for the reader to understand what was done, but also to inform -future surveys. Given this legacy aspect, my only major comment is -that it would be prudent to discuss the performance of Pan-STARRS -calibration in comparison to other major optical surveys, such as SDSS, -DES and HSC surveys. Such a discussion would illuminate all your -advances and provide direction for future work. My other, much more -minor comments are listed below. +The paper "Pan-STARRS Photometric and Astrometric Calibration" by Magnier et al. describes the calibration of a major modern sky survey. The paper is well written and provides sufficient technical detail to not only for the reader to understand what was done, but also to inform future surveys. Given this legacy aspect, my only major comment is that it would be prudent to discuss the performance of Pan-STARRS calibration in comparison to other major optical surveys, such as SDSS, DES and HSC surveys. Such a discussion would illuminate all your advances and provide direction for future work. My other, much more minor comments are listed below. -** We agree with this suggestion and have substantially extended the - Conclusion section to put this article in the context of other - recent and future surveys. +** We agree with this suggestion and have substantially extended the Conclusion section to put this article in the context of other recent and future surveys. -- Abstract: it would be good to provide quantitative summary of photometric -and astrometric performance (such as values listed in fig. 4 caption) +- Abstract: it would be good to provide quantitative summary of photometric and astrometric performance (such as values listed in fig. 4 caption) ** we added this to the abstract. -- after eqs. 5 and 6: I was puzzled why there was no source color -dependence in these equations; you may want to clarify that early +- after eqs. 5 and 6: I was puzzled why there was no source color dependence in these equations; you may want to clarify that early ** clarification added to the end of section 3.3 @@ -39,52 +18,32 @@ ** fixed -- page 8, left column, 1st paragraph: you may want to state that your -fundamental assumption is that the chemical and thermodynamical -state of the atmosphere is constant throughout a night +- page 8, left column, 1st paragraph: you may want to state that your fundamental assumption is that the chemical and thermodynamical state of the atmosphere is constant throughout a night ** clarification added -- page 8, left column, 3rd paragraph: what does word "reliability" mean -in this context? It's certainly not standard statistical usage. +- page 8, left column, 3rd paragraph: what does word "reliability" mean in this context? It's certainly not standard statistical usage. -** This paragraph was reworded to describe the reliablity of the - Schlafly et al results more clearly. +** This paragraph was reworded to describe the reliablity of the Schlafly et al results more clearly. -- page 8, left column, last paragraph: this result (20-35 mmag) is -discrepant by a factor of ~3 compared to Schlafly et al. results; -please comment and clarify +- page 8, left column, last paragraph: this result (20-35 mmag) is discrepant by a factor of ~3 compared to Schlafly et al. results; please comment and clarify -** The Schlafly et al results do not constrain the absolute zero - points, relying on a tie via SDSS. The Scolnic et al analysis - determines the absolute zero points directly. This has been +** The Schlafly et al results do not constrain the absolute zero points, relying on a tie via SDSS. The Scolnic et al analysis determines the absolute zero points directly. This has been explained at the end of Section 5.1. -- page 9, right column, 2nd paragraph: this clipping procedure sounds -like an ad hoc hocus pocus; can you provide at least some statistical -justification (e.g. what is the distribution model you had in your mind)? -perhaps even more ad hoc procedure is assigning weights of 10x their -default; why 10 and not 5, or 50, or? +- page 9, right column, 2nd paragraph: this clipping procedure sounds like an ad hoc hocus pocus; can you provide at least some statistical justification (e.g. what is the distribution model you had in your mind)? perhaps even more ad hoc procedure is assigning weights of 10x their default; why 10 and not 5, or 50, or? -** Text has been added to 5.3 (p. 10) to explain the outlier - rejection process and rationale. +** Text has been added to 5.3 (p. 10) to explain the outlier rejection process and rationale. -- similarly to the above comments; what statistical outlier model are eqs. -17 and 18 supposed to model/address? +- similarly to the above comments; what statistical outlier model are eqs. 17 and 18 supposed to model/address? -** Clarification has been added to the text in section 5.4.2 to - explain the outliers. +** Clarification has been added to the text in section 5.4.2 to explain the outliers. -- comment about proper motions after introducing eqs. 21-24 is not -entirely correct because a lot of your observations are far from the -galactic plane and thus are sensitive to the asymmetric drift effects +- comment about proper motions after introducing eqs. 21-24 is not entirely correct because a lot of your observations are far from the galactic plane and thus are sensitive to the asymmetric drift effects for disk stars -** This is a good point. We have updated the text in section 6.2 to - address this concern. +** This is a good point. We have updated the text in section 6.2 to address this concern. -- last paragraph in section 6.2: so how much improvement did you get -from eqs. 21-24? +- last paragraph in section 6.2: so how much improvement did you get from eqs. 21-24? ** The improvement is noted now in section 6.2. -