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== Early life and education ==
== Early life and education ==
Charlene Heisler was born in [[Calgary|Calgary, Canada]]<ref name=":0">{{Cite journal|last=Norris|first=Ray P.|last2=De Robertis|first2=Michael|last3=Kwok|first3=Sun|date=2000-01-01|title=Obituary: Charlene Anne Heisler, 1961-1999|url=https://ui.adsabs.harvard.edu/abs/2000BAAS...32.1668N|journal=Bulletin of the American Astronomical Society|volume=32|pages=1668–1669}}</ref>. Heisler graduated from the [[University of Calgary]] with a BSc in applied maths and physics in 1985<ref name=":0" /><ref name=":1">{{Cite journal|date=2000|title=Charlene Heisler (1961–1999)|url=https://www.cambridge.org/core/product/identifier/S1323358000002460/type/journal_article|journal=Publications of the Astronomical Society of Australia|language=en|volume=17|issue=1|pages=109–111|doi=10.1071/AS00109|issn=1323-3580}}</ref>. During her time at Calgary, she worked as a summer research assistant for [[Sun Kwok]] and Gene (Eugene) Couch as well as working at the [[Calgary Centennial Planetarium]]<ref name=":0" />. Before starting her PhD, Heisler was diagnosed with [[cystic fibrosis]] and was informed by her doctor she would not live more that two years and that she should abandon her PhD studies<ref name=":0" /><ref name=":1" />. However, she went on to live 8 more years and she completed her PhD at [[Yale University|Yale]] under the supervision of Jeanette Patricia Vader in 1991<ref name=":0" /><ref name=":1" />. The focus of her thesis was on the properties galaxies with spectral energy distributions that peaked at sixty microns, referred to as "Sixty Micron Peakers"<ref name=":1" />.
Charlene Heisler was born in [[Calgary|Calgary, Canada]].<ref name=":0">{{Cite journal|last=Norris|first=Ray P.|last2=De Robertis|first2=Michael|last3=Kwok|first3=Sun|date=2000-01-01|title=Obituary: Charlene Anne Heisler, 1961-1999|url=https://ui.adsabs.harvard.edu/abs/2000BAAS...32.1668N|journal=Bulletin of the American Astronomical Society|volume=32|pages=1668–1669}}</ref> Heisler graduated from the [[University of Calgary]] with a BSc in applied maths and physics in 1985.<ref name=":0" /><ref name=":1">{{Cite journal|date=2000|title=Charlene Heisler (1961–1999)|url=https://www.cambridge.org/core/product/identifier/S1323358000002460/type/journal_article|journal=Publications of the Astronomical Society of Australia|language=en|volume=17|issue=1|pages=109–111|doi=10.1071/AS00109|issn=1323-3580}}</ref> During her time at Calgary, she worked as a summer research assistant for [[Sun Kwok]] and Gene (Eugene) Couch as well as working at the [[Calgary Centennial Planetarium]].<ref name=":0" /> Before starting her PhD, Heisler was diagnosed with [[cystic fibrosis]] and was informed by her doctor she would not live more that two years and that she should abandon her PhD studies.<ref name=":0" /><ref name=":1" /> However, she went on to live 8 more years and she completed her PhD at [[Yale University|Yale]] under the supervision of Jeanette Patricia Vader in 1991.<ref name=":0" /><ref name=":1" /> The focus of her thesis was on the properties galaxies with spectral energy distributions that peaked at sixty microns, referred to as "Sixty Micron Peakers".<ref name=":1" />


== Research and career ==
== Research and career ==
Charlene Heisler spent two years as a post doctoral researcher at [[York University]] with Mike De Robertis where she also began her work in science education<ref name=":0" /><ref name=":1" />. She extended her research of "Peakers" to infrared wavelengths, making use of the [[Mauna Kea Observatories|Mauna Kea]] telescopes, with the belief that "Peakers" contained key information about the early stages of AGN<ref>{{Cite journal|last=Heisler|first=C. A.|last2=De Robertis|first2=M. M.|last3=Nadeau|first3=D.|date=1996-05-11|title=Near-infrared surface photometry of 'Sixty Micron Peaker' galaxies|url=https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/280.2.579|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=280|issue=2|pages=579–615|doi=10.1093/mnras/280.2.579|issn=0035-8711}}</ref><ref name=":0" /><ref>{{Cite journal|last=Heisler|first=Charlene A.|last2=De Robertis|first2=Michael M.|date=1999|title=A Near-Infrared Spectroscopic Study of 60 Micron Peakers|url=https://iopscience.iop.org/article/10.1086/301073|journal=The Astronomical Journal|volume=118|issue=5|pages=2038–2054|doi=10.1086/301073}}</ref><ref name=":1" />. Using a combination of infrared imaging and spectroscopic data from observations she made at [[Kitt Peak National Observatory|Kitt Peak Observatory]] and the [[Anglo-Australian Observatory|Anglo-Australian Observatory (AAO)]], this belief proved true<ref name=":0" />. Heisler also taught two undergraduate classes at York, gave public talks and inspired young women in science<ref name=":0" /><ref name=":1" />. In 1993, she moved to [[Sydney]] and became a postdoctoral research fellow at the Anglo Australian Observatory and started work as a support astronomer for IRIS and became a liaison officer with AAO on the MPI 3D project<ref name=":0" /><ref name=":1" /> . In 1996, she moved to [[Mount Stromlo Observatory]] in Canberra, Australia and was awarded a senior fellowship there in 1998<ref name=":0" /><ref name=":1" />. In 1997, whilst working with Stuart Lumsden and Jeremy Bailey, she published her most notable paper on why only some [[Seyfert II]] galaxies have hidden [[Broad-line region|broad line regions]] that are only visible in [[Polarization (waves)|polarised]] light<ref>{{Cite journal|last=Heisler|first=Charlene A.|last2=Lumsden|first2=Stuart L.|last3=Bailey|first3=Jeremy A.|date=1997|title=Visibility of scattered broad-line emission in Seyfert 2 galaxies|url=http://www.nature.com/articles/385700a0|journal=Nature|language=en|volume=385|issue=6618|pages=700–702|doi=10.1038/385700a0|issn=0028-0836}}</ref><ref name=":0" /> . Heisler and her team thought this was due to a link between the infrared colour of the galaxy and the broad line region existing. This lead to a model where Seyfert II galaxies which were known to have hidden broad line regions galaxies being modelled as normal Seyfert galaxies with symmetry axes along the [[Line-of-sight propagation|line-of-sight]]<ref name=":0" />. Her last major project was COLA (COmpact Low-power AGN) with Phil Appleton and [[Ray Norris (astrophysicist)|Ray Norris]] which aimed to establish if there was evidence that AGN activity was associated with [[Starburst galaxy|starburst]] activity<ref name=":0" /><ref name=":1" /> .
Charlene Heisler spent two years as a post doctoral researcher at [[York University]] with Mike De Robertis where she also began her work in science education.<ref name=":0" /><ref name=":1" /> She extended her research of "Peakers" to infrared wavelengths, making use of the [[Mauna Kea Observatories|Mauna Kea]] telescopes, with the belief that "Peakers" contained key information about the early stages of AGN.<ref>{{Cite journal|last=Heisler|first=C. A.|last2=De Robertis|first2=M. M.|last3=Nadeau|first3=D.|date=1996-05-11|title=Near-infrared surface photometry of 'Sixty Micron Peaker' galaxies|url=https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/280.2.579|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=280|issue=2|pages=579–615|doi=10.1093/mnras/280.2.579|issn=0035-8711}}</ref><ref name=":0" /><ref>{{Cite journal|last=Heisler|first=Charlene A.|last2=De Robertis|first2=Michael M.|date=1999|title=A Near-Infrared Spectroscopic Study of 60 Micron Peakers|url=https://iopscience.iop.org/article/10.1086/301073|journal=The Astronomical Journal|volume=118|issue=5|pages=2038–2054|doi=10.1086/301073}}</ref><ref name=":1" /> Using a combination of infrared imaging and spectroscopic data from observations she made at [[Kitt Peak National Observatory|Kitt Peak Observatory]] and the [[Anglo-Australian Observatory|Anglo-Australian Observatory (AAO)]], this belief proved true.<ref name=":0" /> Heisler also taught two undergraduate classes at York, gave public talks and inspired young women in science.<ref name=":0" /><ref name=":1" /> In 1993, she moved to [[Sydney]] and became a postdoctoral research fellow at the Anglo Australian Observatory and started work as a support astronomer for IRIS and became a liaison officer with AAO on the MPI 3D project.<ref name=":0" /><ref name=":1" /> In 1996, she moved to [[Mount Stromlo Observatory]] in Canberra, Australia and was awarded a senior fellowship there in 1998.<ref name=":0" /><ref name=":1" /> In 1997, whilst working with Stuart Lumsden and Jeremy Bailey, she published her most notable paper on why only some [[Seyfert II]] galaxies have hidden [[Broad-line region|broad line regions]] that are only visible in [[Polarization (waves)|polarised]] light.<ref>{{Cite journal|last=Heisler|first=Charlene A.|last2=Lumsden|first2=Stuart L.|last3=Bailey|first3=Jeremy A.|date=1997|title=Visibility of scattered broad-line emission in Seyfert 2 galaxies|url=http://www.nature.com/articles/385700a0|journal=Nature|language=en|volume=385|issue=6618|pages=700–702|doi=10.1038/385700a0|issn=0028-0836}}</ref><ref name=":0" /> Heisler and her team thought this was due to a link between the infrared colour of the galaxy and the broad line region existing. This lead to a model where Seyfert II galaxies which were known to have hidden broad line regions galaxies being modelled as normal Seyfert galaxies with symmetry axes along the [[Line-of-sight propagation|line-of-sight]].<ref name=":0" /> Her last major project was COLA (COmpact Low-power AGN) with Phil Appleton and [[Ray Norris (astrophysicist)|Ray Norris]] which aimed to establish if there was evidence that AGN activity was associated with [[Starburst galaxy|starburst]] activity.<ref name=":0" /><ref name=":1" />


After her death, the Astronomical Society of Australia created the Charlene Heisler Prize which is awarded annually to the most outstanding PhD thesis in the field of astronomy at an Australian university<ref>{{Cite web|title=Charlene Heisler Prize {{!}} Astronomical Society of Australia|url=https://asa.astronomy.org.au/prizes_and-grants/prizes-awards/charlene-heisler-prize/|access-date=2022-02-12|language=en-AU}}</ref>.
After her death, the Astronomical Society of Australia created the Charlene Heisler Prize which is awarded annually to the most outstanding PhD thesis in the field of astronomy at an Australian university.<ref>{{Cite web|title=Charlene Heisler Prize {{!}} Astronomical Society of Australia|url=https://asa.astronomy.org.au/prizes_and-grants/prizes-awards/charlene-heisler-prize/|access-date=2022-02-12|language=en-AU}}</ref>


== Notable publications   ==
== Notable publications   ==

Revision as of 21:58, 25 February 2022

Charlene Heisler (1 December 1961 – 28 October 1999) was a Canadian astronomer. She is best known for her work on Active Galactic Nuclei (AGN). The Astronomical Society of Australia created the Charlene Heisler Prize in her honour.

Charlene Heisler
Born(1961-12-01)1 December 1961
Died28 October 1999(1999-10-28) (aged 37)
Alma materUniversity of Calgary, Yale University
Scientific career
Thesis Galaxies with Spectral Energy Distributions Peaking at 60 Microns: Morphology and Activity Explained by Interactions.

Early life and education

Charlene Heisler was born in Calgary, Canada.[1] Heisler graduated from the University of Calgary with a BSc in applied maths and physics in 1985.[1][2] During her time at Calgary, she worked as a summer research assistant for Sun Kwok and Gene (Eugene) Couch as well as working at the Calgary Centennial Planetarium.[1] Before starting her PhD, Heisler was diagnosed with cystic fibrosis and was informed by her doctor she would not live more that two years and that she should abandon her PhD studies.[1][2] However, she went on to live 8 more years and she completed her PhD at Yale under the supervision of Jeanette Patricia Vader in 1991.[1][2] The focus of her thesis was on the properties galaxies with spectral energy distributions that peaked at sixty microns, referred to as "Sixty Micron Peakers".[2]

Research and career

Charlene Heisler spent two years as a post doctoral researcher at York University with Mike De Robertis where she also began her work in science education.[1][2] She extended her research of "Peakers" to infrared wavelengths, making use of the Mauna Kea telescopes, with the belief that "Peakers" contained key information about the early stages of AGN.[3][1][4][2] Using a combination of infrared imaging and spectroscopic data from observations she made at Kitt Peak Observatory and the Anglo-Australian Observatory (AAO), this belief proved true.[1] Heisler also taught two undergraduate classes at York, gave public talks and inspired young women in science.[1][2] In 1993, she moved to Sydney and became a postdoctoral research fellow at the Anglo Australian Observatory and started work as a support astronomer for IRIS and became a liaison officer with AAO on the MPI 3D project.[1][2] In 1996, she moved to Mount Stromlo Observatory in Canberra, Australia and was awarded a senior fellowship there in 1998.[1][2] In 1997, whilst working with Stuart Lumsden and Jeremy Bailey, she published her most notable paper on why only some Seyfert II galaxies have hidden broad line regions that are only visible in polarised light.[5][1] Heisler and her team thought this was due to a link between the infrared colour of the galaxy and the broad line region existing. This lead to a model where Seyfert II galaxies which were known to have hidden broad line regions galaxies being modelled as normal Seyfert galaxies with symmetry axes along the line-of-sight.[1] Her last major project was COLA (COmpact Low-power AGN) with Phil Appleton and Ray Norris which aimed to establish if there was evidence that AGN activity was associated with starburst activity.[1][2]

After her death, the Astronomical Society of Australia created the Charlene Heisler Prize which is awarded annually to the most outstanding PhD thesis in the field of astronomy at an Australian university.[6]

Notable publications  

  • Charlene A Heisler; Stuart L Lumsden; Jeremy A Bailey. (February 1997). "Visibility of scattered broad-line emission in Seyfert 2 galaxies". Nature. 385(6618): 700-702. doi: 10.1038/385700a0
  • Charlene A Heisler, Patricia J Vader. (January 1994). "Galaxies with Spectral Energy Distributions Peaking Near 60microns II. Optical Broadband Properties". Astronomical Journal. 107: 35. doi: 10.1086/116834
  • Charlene A Heisler, Patricia J Vader. (July 1995). "Galaxies with Spectral Energy Distributions Peaking Near 60 micron.III. H(alpha) Imaging". Astronomical Journal. 110: 87. doi: 10.1086/117499
  • Charlene A Heisler, Michael M De Robertis. (November 1999). "A Near-Infrared Spectroscopic Study of 60 Micron Peakers". Astronomical Journal. 118(5): 2038-2054. doi: 10.1086/301073
  • Charlene A Heisler, Michael M De Robertis, D Nadeau. (May 1996). "Near-infrared surface photometry of `Sixty Micron Peaker' galaxies". Monthly Notices of the Royal Astronomical Society. 280(2): 579-615. doi: 10.1093/mnras/280.2.579

References

  1. ^ a b c d e f g h i j k l m n Norris, Ray P.; De Robertis, Michael; Kwok, Sun (1 January 2000). "Obituary: Charlene Anne Heisler, 1961-1999". Bulletin of the American Astronomical Society. 32: 1668–1669.
  2. ^ a b c d e f g h i j "Charlene Heisler (1961–1999)". Publications of the Astronomical Society of Australia. 17 (1): 109–111. 2000. doi:10.1071/AS00109. ISSN 1323-3580.
  3. ^ Heisler, C. A.; De Robertis, M. M.; Nadeau, D. (11 May 1996). "Near-infrared surface photometry of 'Sixty Micron Peaker' galaxies". Monthly Notices of the Royal Astronomical Society. 280 (2): 579–615. doi:10.1093/mnras/280.2.579. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  4. ^ Heisler, Charlene A.; De Robertis, Michael M. (1999). "A Near-Infrared Spectroscopic Study of 60 Micron Peakers". The Astronomical Journal. 118 (5): 2038–2054. doi:10.1086/301073.
  5. ^ Heisler, Charlene A.; Lumsden, Stuart L.; Bailey, Jeremy A. (1997). "Visibility of scattered broad-line emission in Seyfert 2 galaxies". Nature. 385 (6618): 700–702. doi:10.1038/385700a0. ISSN 0028-0836.
  6. ^ "Charlene Heisler Prize | Astronomical Society of Australia". Retrieved 12 February 2022.
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