Response to Mike DiSanti’s comments on the Hyakutake spectra 1. a. Flux vs. flux density. Yes - flux density is the better term for the column in the table. b. Aperture - yes it is ±3.7 arcsec orthogonal to the offset direction (see diagram in the AJ paper appendix), which can certainly be spelled out here. It is ±0.43 arcsec in the offset (sunward) direction. 2. Each offset is the weighted average of several different exposures (except I think the 7-arcsec offset was a single long exposure). The log of individual spectra that have been combined is in the AJ paper. I thought that table of individual exposures had been included in the dataset, but perhaps not. It should be. A LaTeX version of the table is below, which will allow cutting and pasting into xml instead of retyping (& thus minimizing the chance of typos). I leave it to Anne/Ludmilla to decide whether to change the start-end times in each product or just explain that the start-end times refer to the entire collection with the details spelled out in the separate tables. Note that the table gives mid-times so start-end times are mid-time of first exposure of a given offset - half the exposure time and mid-time of the last exposure of that same offset plus half its exposure time. Probably editing the individual products is better technically but for searching purposes, noting that the different offsets are interspersed, the whole window is probably best. 3. Agreed. 4. Cosmetic: I have looked at the individual pages, each only 50Å long, that were used to make these and they also show the problem at this particular point. It is possible that Dennis Wellnitz has the original form, which was a continuous plot for the entire spectrum. If he does, that can be substituted for this. 5. Labelling features: As best I can recall, looking again at the spectra, is that the purple identifications are firm but the blue ones were an attempt to see if other species were the right species - some match and some don’t match observed peaks but none of these identifications is really firm. The ones labelled ?A and ?B in pox0 are now identified as prompt emission by OH (the AJ paper). 6. Agreed - “Over most of the spectral range, the wavelength was calibrated using exposures on a thorium-argon lamp, with careful matching in the overlap between orders of the echelon. At the shortest wavelengths there are not enough lines from the thorium-argon lamp so the wavelength was calibrated using readily identified cometary emission lines of OH.” ********************************* Details for item 2 response \begin{tabular}{ccccc} \tableline\tableline Exp ID & mid-UTC & Exp Time & AirMass & Offset \\ & & [s] & & [arcsc] \\ \tableline coo23 &6:02:57 &600 &1.530 &0 \\ coo24 &6:16:02 &600 &1.513 &0 \\ coo35 &7:04:45 &600 &1.468 &7 \\ coo36 &7:17:27 &600 &1.460 &7 \\ coo37 &7:31:14 &600 &1.453 &10 \\ coo38 &7:44:05 &600 &1.449 &10 \\ coo39 &8:31:03 &600 &1.443 &10 \\ coo40 &8:54:26 &1800 &1.445 &10 \\ coo41 &9:27:58 &1800 &1.458 &10 \\ coo42 &10:15:54 &3600 &1.489 &2 \\ coo43 &11:04:23 &1800 &1.544 &0 \\ \tableline \end{tabular} *********************************** Additional changes In collection.xml: The last reference (A’Hearn, Krishna Swamy, et al) should be updated since it has now been published. Astron.J. 150, 5. DOI:10.1088/0004-6256/150/1/5. In collection_description.txt: several English issues a. Under Parameters: The data are presented as ascii tables (plural verb and object), also flux —> flux density b. Under Ancillary: flux —> flux density c. Under Spectra: The original spectra are available at KPNO.