Primary measurements, Chris L. Peterson Cloudbait Observatory, Colorado, The coma size values plotted at the bottom of this page are primary measurements. They were obtained using conventional methods: individual short CCDs images were made in order to avoid saturation, and these were then calibrated with bias, flat, and dark frames and summed to increase the image dynamic range. Each stacked image (for the 5 nights of data) was astrometrically calibrated (using Pinpoint) for scale, and the intensity profile of the coma measured with a standard tool (in this case, the line profile tool in MaximDL). The resulting profiles were exported to Excel, normalized to the same gain, and the width measured against the noise floor. The best reference is the plotted data itself. نسخة محفوظة 26 ديسمبر 2017 على موقع واي باك مشين. [وصلة مكسورة]
Davidson, J. E. "Comet e, 1889," The Observatory, July 1890, Vol. 13, pp. 247. Retrieved 27 October 2007. نسخة محفوظة 14 أبريل 2020 على موقع واي باك مشين.
Altenhoff، W. J.؛ Kreysa, E.؛ Menten, K. M.؛ Sievers, A.؛ Thum, C.؛ Weiss, A. (2009). "Why did Comet 17P/Holmes burst out? Nucleus splitting or delayed sublimation?". Astronomy and Astrophysics. ج. 495 ع. 3: 975–978. arXiv:0901.2739. Bibcode:2009A&A...495..975A. DOI:10.1051/0004-6361:200810458.
Jewitt، David (9 نوفمبر 2007). "Comet Holmes Bigger Than The Sun". Institute for Astronomy at the University of Hawaii. مؤرشف من الأصل في 2019-05-02. اطلع عليه بتاريخ 2007-11-17.
Jewitt، David (9 نوفمبر 2007). "Comet Holmes Bigger Than The Sun". Institute for Astronomy at the University of Hawaii. مؤرشف من الأصل في 2019-05-02. اطلع عليه بتاريخ 2007-11-17.
Davidson, J. E. "Comet e, 1889," The Observatory, July 1890, Vol. 13, pp. 247. Retrieved 27 October 2007. نسخة محفوظة 14 أبريل 2020 على موقع واي باك مشين.
Primary measurements, Chris L. Peterson Cloudbait Observatory, Colorado, The coma size values plotted at the bottom of this page are primary measurements. They were obtained using conventional methods: individual short CCDs images were made in order to avoid saturation, and these were then calibrated with bias, flat, and dark frames and summed to increase the image dynamic range. Each stacked image (for the 5 nights of data) was astrometrically calibrated (using Pinpoint) for scale, and the intensity profile of the coma measured with a standard tool (in this case, the line profile tool in MaximDL). The resulting profiles were exported to Excel, normalized to the same gain, and the width measured against the noise floor. The best reference is the plotted data itself. نسخة محفوظة 26 ديسمبر 2017 على موقع واي باك مشين. [وصلة مكسورة]
