Editing Stardome Observatory (section)

== Research by Auckland Astronomical Society ==
In 1969, the observatory constructed a UBV [[Photometry (astronomy)|photoelectric photometer]] with assistance from the [[University of Auckland]]. This photometer on the Zeiss telescope became a very successful instrument and produced a significant number of published research papers. Probably the most important discovery was the phenomenon of "super-humps" in the [[SU Ursae Majoris]] class of [[cataclysmic variable star|cataclysmic binary]] stars<ref>http://www.konkoly.hu/cgi-bin/IBVS?0864 {{Dead link|date=February 2022}}</ref> in 1974.

In 1988, the observatory participated in the discovery of the atmosphere of [[Pluto]] by measuring the brightness change as the planet passed in front of a star.

During the 1980s the Zeiss telescope was used to support several doctoral students from the [[University of Auckland]] (most notably [[Rodger Freeth]]), including the development of a new computer-controlled photon counting photometer. Regular UBV photometry of variable stars continued until 1998 when a [[Charge-coupled device|CCD]] camera was first used.

In 1999, a [[Celestron]] C-14 [[Schmidt-Cassegrain]] telescope was provided by the Nustrini family for installation in the newly built second dome at Stardome Observatory. A grant from the ASB Trust was used to buy a Paramount GT1100s mounting (manufactured by [[Software Bisque]]) and an Apogee AP8p CCD camera. The Apogee camera has a back-illuminated SITe003 CCD (1024×1024 24-[[micrometre]] pixels). The field of view is 22 [[arc-minute]]s. The 0.35 m (f/11) Nustrini telescope is used only for research. In 2006 the [[Celestron]] C-14 telescope was replaced by a 40&nbsp;cm Meade ACF (F/10) and in 2008 CCD camera was replaced by a SBIG ST-6303. The Meade ACF telescope uses an OG530 Orange Schott Optical Glass Filter.

Stardome Observatory & Planetarium is a member of the microFUN collaboration<ref>{{cite web |url=http://www-astronomy.mps.ohio-state.edu/~microfun/ |title=MicroFUN 2005 |access-date=2006-02-08 |archive-url=https://web.archive.org/web/20060102223958/http://www-astronomy.mps.ohio-state.edu/~microfun/ |archive-date=2006-01-02 }}</ref> which attempts to detect [[Extrasolar planet|extra-solar]] planets by [[gravitational microlensing]]. MicroFUN is based at the Astronomy Department of [[Ohio State University]] and coordinates the observation of high-magnification microlensing events. In April 2005, microFUN contributed significantly to the discovery of a Jovian-mass planet ([[OGLE-2005-BLG-071L]]<ref>{{cite journal | bibcode = 2005ApJ...628L.109U | title=A Jovian-Mass Planet in Microlensing Event OGLE-2005-BLG-071 | journal=The Astrophysical Journal | volume=628 | page=L109 | year=2005 |author=Udalski, A. |author2=Jaroszynski, M. |author3=Paczynski, B. |author4=Kubiak, M. |author5=Szymanski, M. K. |author6=Soszynski, I. |author7=Pietrzynski, G. |author8=Ulaczyk, K. |author9=Szewczyk, O. |author10=Wyrzykowski, L. |author11=Christie, G. W. |author12=DePoy, D. L. |author13=Dong, S. |author14=Gal-Yam, A. |author15=Gaudi, B. S. |author16=Gould, A. |author17=Han, C. |author18=Lépine, S. |author19=McCormick, J. |author20=Park, B.-G. |author21=Pogge, R. W. |author22=Bennett, D. P. |author23=Bond, I. A. |author24=Muraki, Y. |author25=Tristram, P. J. |author26=Yock, P. C. M. |author27=Beaulieu, J.-P. |author28=Bramich, D. M. |author29=Dieters, S. W. |author30=Greenhill, J. |author31=Hill, K. |author32=Horne, K. |author33=Kubas, D. | issue=2 | doi=10.1086/432795|arxiv = astro-ph/0505451 | s2cid=7425167 }}</ref><ref>{{Cite journal|arxiv=astro-ph/0505451|doi=10.1086/432795|title=A Jovian-Mass Planet in Microlensing Event OGLE-2005-BLG-071|year=2005|last1=Udalski|first1=A.|last2=Jaroszyński|first2=M.|last3=Paczyński|first3=B.|last4=Kubiak|first4=M.|last5=Szymański|first5=M. K.|last6=Soszyński|first6=I.|last7=Pietrzyński|first7=G.|last8=Ulaczyk|first8=K.|last9=Szewczyk|first9=O.|last10=Wyrzykowski|first10=Ł.|last11=Christie|first11=G. W.|last12=Depoy|first12=D. L.|last13=Dong|first13=S.|last14=Gal-Yam|first14=A.|last15=Gaudi|first15=B. S.|last16=Gould|first16=A.|last17=Han|first17=C.|last18=Lépine|first18=S.|last19=McCormick|first19=J.|last20=Park|first20=B.-G.|last21=Pogge|first21=R. W.|last22=Bennett|first22=D. P.|last23=Bond|first23=I. A.|last24=Muraki|first24=Y.|last25=Tristram|first25=P. J.|last26=Yock|first26=P. C. M.|last27=Beaulieu|first27=J.-P.|last28=Bramich|first28=D. M.|last29=Dieters|first29=S. W.|last30=Greenhill|first30=J.|journal=The Astrophysical Journal|volume=628|issue=2|pages=L109–L112|bibcode=2005ApJ...628L.109U|s2cid=7425167|display-authors=1}}</ref>), the second planet to be detected in this way. In 2005, the Stardome contributed 250 hours of time-series photometry to this collaboration.

Stardome also contributes to the [[Center for Backyard Astrophysics]] (CBA)<ref>{{cite web |url=http://cba.phys.columbia.edu/ |title=CBA - Center for Backyard Astrophysics |access-date=2006-02-20 |archive-url=https://web.archive.org/web/20060220021210/http://cba.phys.columbia.edu/ |archive-date=2006-02-20 }}</ref> in [[New York City]] as CBA-Auckland.<ref>{{cite web |url=http://cba.phys.columbia.edu/data/archive/auckland.html |title=CBA - Center for Backyard Astrophysics |access-date=2006-02-09 |archive-url=https://archive.today/20060907150833/http://cba.phys.columbia.edu/data/archive/auckland.html |archive-date=2006-09-07 }}</ref> This professional-amateur network monitors selected [[cataclysmic variable star|cataclysmic binary]] stars and contributes to the understanding of these objects. During 2005, over 250 hours of observations where contributed to the CBA.

The research telescope at Stardome is used to make regular astrometric observations of [[comet]]s and [[near-Earth object]]s (NEOs) for the [[Minor Planet Center]].<ref>[http://www.minorplanetcenter.net/iau/mpc.html Minor Planet Center (MPC) – About, Services and Publications]</ref> In 2004, observations were made of the NEO [[2004 FH]] which was at the time the closest natural object detected from [[Earth]] (43,000&nbsp;km). CCD photometry obtained at Stardome showed that the object was rotating in 3 minutes, the fastest rotation rate measured for any solar system object.<ref>[http://cbat.eps.harvard.edu/iauc/08300/08310.html#Item4 Central Bureau for Astronomical Telegrams (Circular No. 8310) – 2004 FH]</ref>

Research at Stardome is performed on a voluntary basis by members of the [https://www.astronomy.org.nz/ Auckland Astronomical Society].
{| class="wikitable floatright" style="font-size: 0.9em;"
|+ '''Edith Winstone Blackwell Telescope'''
|-
! align="left" | Organization
| Stardome Observatory
|-
! align="left" | Location
| One Tree Hill, Auckland, New Zealand
|-
! align="left" | Wavelength regime
| optical
|-
! align="left" | Completion date
| 1966
|-
! align="left" | Webpage
| {{URL|http://www.stardome.org.nz}}
|-
! colspan="2" bgcolor="#green" | Physical characteristics
|-
! align="left" | Telescope style
| Cassegrain
|-
! align="left" | Diameter
| 0.5 m
|-
! align="left" | Collecting area
| 0.72 m²
|-
! align="left" | Focal length
| 6.65 m
|-
! align="left" | Mounting
| equatorial
|-
! align="left" | Dome
| spherical
|}