Digitization and astrophysical use of Hewitt Camera Archive

Hudec, R.; Hudec, L.; Howarth, J. J.

doi:10.1002/asna.201813516

Cited by 3 publications

(4 citation statements)

References 5 publications

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“…The device based on the DSLR 39 Mpx digital camera is fast and accurate enough for photometry—for example, Tuorla Observatory plate archive, 11,000 plates fully digitized in just 1 week in March 2017; Hewitt camera plate archive UK, 1,700 plates digitized in 2 days (Hudec et al ); and UNAM Mexico, 2000 CdC plates digitized in 2 days.…”

Section: Digitization Of Astronomical Plates: Current Statusmentioning

confidence: 99%

Astronomical photographic data archives: Recent status

Hudec

2019

Astron Nachr

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I briefly present and discuss the recent status (with emphasis on digitization and data access) of astronomical photographic data archives worldwide, both photometric and spectroscopic, including various digitization techniques, automated data evaluation pipelines, astrophysical use, and public access. Although there are two major astronomical plate digitization projects (Harvard DASCH USA and APPLAUSE representing German Bamberg, Potsdam and Hamburg plate collections), the majority of astronomical photographic data archives are still awaiting digitization. Numerous plate archives have been visited, and in many of them, the glass plates are affected by various degradation types such as gold decease, sometimes progressing so fast that digitization is of great importance, taking into account the enormous scientific value of these databases.

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Section: Digitization Of Astronomical Plates: Current Statusmentioning

confidence: 99%

Astronomical photographic data archives: Recent status

Hudec

2019

Astron Nachr

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“…V627 Peg (=OT J213806.6+261957) was discovered in 2010 (Yamaoka 2010;Nakano 2010), and spectroscopically confirmed as a DN outburst by Arai (2010); Graham et al (2010); Tovmassian et al (2010). Three outbursts of V627 Peg have been reported in literature so far: in 1942; Hudec (2010Hudec ( ), in 2010Kato et al (2010); Chochol et al (2012); Zemko and Kato (2013); Mitrofanova et al (2014), andin 2014;. Although the outburst profile of the 1942 outburst is unknown, those of the 2010 and 2014 superoutbursts showed large differences.…”

Section: Introductionmentioning

confidence: 96%

2021 superoutburst of the WZ Sge-type dwarf nova V627 Pegasi lacks an early superhump phase

Tampo

Kato

Kojiguchi

et al. 2023

Publications of the Astronomical Society of Japan

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Superoutbursts in WZ Sge-type dwarf novae (DNe) are characterized by both early superhumps and ordinary superhumps originating from the 2 : 1 and 3 : 1 resonances, respectively. However, some WZ Sge-type DNe show a superoutburst lacking early superhumps; it is not well established how these differ from superoutbursts with an early superhump phase. We report time-resolved photometric observations of the WZ Sge-type DN V627 Peg during its 2021 superoutburst. The detection of ordinary superhumps before the superoutburst peak highlights that this 2021 superoutburst of V627 Peg, like that in 2014, did not feature an early superhump phase. The duration of stage B superhumps was slightly longer in the 2010 superoutburst accompanied by early superhumps than that in the 2014 and 2021 superoutbursts, which lacked early superhumps. This result suggests that an accretion disk experiencing the 2 : 1 resonance may have a larger mass at the inner part of the disk and hence needs more time for the inner disk to become eccentric. The presence of a precursor outburst in the 2021 superoutburst suggests that the maximum disk radius should be smaller than that of the 2014 superoutburst, even though the duration of quiescence was longer than that before the 2021 superoutburst. This could be accomplished if the 2021 superoutburst was triggered as an inside-out outburst or if the mass transfer rate in quiescence changes by a factor of two, suggesting that the outburst mechanism and quiescence state of WZ Sge-type DNe may have more variety than ever thought.

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“…The astronomical plate archives represent the only method to study the behavior of objects over very long (100 years or even more) time intervals, and the only method to go back in time (like a time machine) (Hudec ). In addition, the archived photographic data provide huge monitoring times (up to 30,000 hr of continuous monitoring) for a particular sky position, allowing the detection and study of rare events such as flares.…”

Section: Introductionmentioning

confidence: 99%

“…With historical photographic data, we can follow the evolution of the source over almost 100 years (Figure ). We note that a considerable fraction of X‐ray and even γ‐ray sources are also emitters of optical emission, often variable, hence the photographic data archives provide supplementary data also for objects of frontier astrophysics (Hudec ).…”

Section: Introductionmentioning

confidence: 99%