Rosemary Wyse

Last updated

Rosemary Wyse
Born (1957-01-26) 26 January 1957 (age 67)
Dundee, Scotland
Alma mater
Awards Annie Jump Cannon Award in Astronomy
Scientific career
Institutions
Thesis The formation and evolution of galaxies  (1982)
Academic advisorsBernard Jones [1]
Website

Rosemary F. G. Wyse (born 26 January 1957 in Dundee, Scotland [2] ) is a Scottish astrophysicist, [3] Fellow of the Royal Astronomical Society (FRAS), and Alumni Centennial Professor of Physics and Astronomy at Johns Hopkins University. [4] [5] [6] [7] [8] [9] [10] [11] [12]

Contents

Education

Wyse graduated from Queen Mary University of London in 1977 with a first-class Bachelor of Science degree in Physics and Astrophysics and obtained her PhD in astrophysics in the Institute of Astronomy at the University of Cambridge in 1983. [13] [1] [14] [11] Bernard Jones was her academic advisor. [2]

Career

Wyse conducted postdoctoral research at Princeton University and the University of California Berkeley. Her work has primarily been in the fields of galactic formation, composition and evolution. [15] [16] In addition to her research career, Wyse served as the first female President of the Aspen Center for Physics from 2010 to 2013, [17] [11] and served as a Trustee from 2006 to 2010. [18]

Honors and awards

Related Research Articles

<span class="mw-page-title-main">Local Group</span> Group of galaxies that includes the Milky Way

The Local Group is the galaxy group that includes the Milky Way. It has a total diameter of roughly 3 megaparsecs (10 million light-years; 9×1019 kilometres), and a total mass of the order of 2×1012 solar masses (4×1042 kg). It consists of two collections of galaxies in a "dumbbell" shape; the Milky Way and its satellites form one lobe, and the Andromeda Galaxy and its satellites constitute the other. The two collections are separated by about 800 kiloparsecs (3×10^6 ly; 2×1019 km) and are moving toward one another with a velocity of 123 km/s. The group itself is a part of the larger Virgo Supercluster, which may be a part of the Laniakea Supercluster. The exact number of galaxies in the Local Group is unknown as some are occluded by the Milky Way; however, at least 80 members are known, most of which are dwarf galaxies.

Kapteyn's Star is a class M1 red subdwarf about 12.83 light-years from Earth in the southern constellation Pictor; it is the closest halo star to the Solar System. With an apparent magnitude of nearly 9 it is visible through binoculars or a telescope.

The Milky Way has several smaller galaxies gravitationally bound to it, as part of the Milky Way subgroup, which is part of the local galaxy cluster, the Local Group.

Canes Venatici I or CVn I is a dwarf spheroidal galaxy situated in the Canes Venatici constellation and discovered in 2006 in the data obtained by Sloan Digital Sky Survey. It is one of the most distant known satellites of the Milky Way as of 2011 together with Leo I and Leo II. The galaxy is located at a distance of about 220 kpc from the Sun and is moving away from the Sun at a velocity of about 31 km/s. It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical shape with the half-light radius of about 550 pc.

Ursa Major II Dwarf is a dwarf spheroidal galaxy situated in the Ursa Major constellation and discovered in 2006 in the data obtained by the Sloan Digital Sky Survey. The galaxy is located approximately 30 kpc from the Sun and moves towards the Sun with the velocity of about 116 km/s. It has an elliptical shape with the half-light radius of about 140 pc.

Segue 1 is a dwarf spheroidal galaxy or globular cluster situated in the Leo constellation and discovered in 2006 by Sloan Digital Sky Survey. It is located at a distance of about 23 kpc from the Sun and moves away from the Sun with the velocity of about 206 km/s. Segue 1 has a noticeably elongated shape with the half-light radius of about 30 pc. This elongation may be caused by the tidal forces acting from the Milky Way galaxy if Segue 1 is being tidally disrupted now.

<span class="mw-page-title-main">Leo IV (dwarf galaxy)</span>

Leo IV is a dwarf spheroidal galaxy situated in the Leo constellation, discovered in 2006 in the data obtained by the Sloan Digital Sky Survey. The galaxy is located at the distance of about 160 kpc from the Sun and moves away from the Sun with the velocity of about 130 km/s. It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an approximately round shape with the half-light radius of about 130 pc.

Canes Venatici II or CVn II is a dwarf spheroidal galaxy situated in the Canes Venatici constellation and discovered in 2006 in data obtained by the Sloan Digital Sky Survey. The galaxy is located at a distance of about 150 kpc from the Sun and moves towards the Sun with the velocity of about 130 km/s. It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical shape with a half-light radius of about 74+14
−10 pc.

Coma Berenices or Com is a dwarf spheroidal galaxy situated in the Coma Berenices constellation and discovered in 2006 in data obtained by the Sloan Digital Sky Survey. The galaxy is located at the distance of about 44 kpc from the Sun and moves away from the Sun with the velocity of about 98 km/s. It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical shape with the half-light radius of about 70 pc.

<span class="mw-page-title-main">Hercules (dwarf galaxy)</span> Dwarf spheroidal galaxy in the constellation Hercules

Hercules, or Her, is a dwarf spheroidal galaxy situated in the Hercules constellation and discovered in 2006 in data obtained by the Sloan Digital Sky Survey. The galaxy is located at a distance of about 140 kpc from the Sun and moves away from the Sun with a velocity of about 45 km/s. It is classified as a dwarf spheroidal galaxy (dSph). It has a noticeably elongated shape with a half-light radius of about 350 pc. This elongation may be caused by tidal forces acting from the Milky Way galaxy, meaning that Her is being tidally disrupted now. Her also shows some gradient of velocities across the galaxy's body and is embedded into a faint stellar stream, which also points towards its ongoing tidal disruption.

RAVE is a multi-fiber spectroscopic astronomical survey of stars in the Milky Way using the 1.2-metre UK Schmidt Telescope of the Australian Astronomical Observatory (AAO). The RAVE collaboration consists of researchers from over 20 institutions around the world and is coordinated by the Leibniz Institute for Astrophysics Potsdam (AIP).

<span class="mw-page-title-main">HD 33579</span> Star in the constellation Dorado

HD 33579 is a white/yellow hypergiant and one of the brightest stars in the Large Magellanic Cloud (LMC). It is a suspected variable star.

In astronomy, the Sagittarius Stream is a long, complex structure made of stars that wrap around the Milky Way galaxy in an orbit that nearly crosses the galactic poles. It consists of tidally stripped stars from the Sagittarius Dwarf Elliptical Galaxy, resulting from the process of merging with the Milky Way over a period of billions of years.

HD 91496 is a giant star in the constellation Carina, with an apparent magnitude is 4.92 and an MK spectral class of K4/5 III. It has been suspected of varying in brightness, but this has not been confirmed.

The metallicity distribution function is an important concept in stellar and galactic evolution. It is a curve of what proportion of stars have a particular metallicity of a population of stars such as in a cluster or galaxy.

YBP 1194 is a G-type main-sequence star, class G5V, in the open cluster Messier 67, about 2,890 light-years from the Sun in the constellation Cancer. It is a solar twin, having the near exact same temperature and mass as the Sun. YBP 1194 has a slightly higher metallicity than the Sun, and may be slightly younger at an age of 3.5-4.8 billion years. In January 2014, this star was announced to have an exoplanet. It is packed in a small cluster, Messier 67, with a radius of 10 light-years, with over 500 other stars. For comparison, the Sun has 9 star systems within 10 light-years and 94 star systems within 20 light-years.

Constance "Connie" Mary Rockosi is a professor and former department chair in the Astronomy and Astrophysics Department at the University of California, Santa Cruz. She earned her PhD in 2001 and helped design the camera for the telescope that was used as part of the initial Sloan Digital Sky Survey (SDSS). She also was in charge of the SDSS-III domain for the Sloan Extension for Galactic Understanding and Exploration (SEGUE) project and is the primary investigator on SEGUE-2. Her focuses involve the study of the Milky Way galaxy, with a focus on the evolution that it took to reach its current state.

References

  1. 1 2 3 4 "Rosemary F.G. Wyse Curriculum Vitae" (PDF). Johns Hopkins University. Archived from the original (PDF) on 12 June 2015.
  2. 1 2 Proffitt, Pamela (1999). Notable Women Scientists. Michigan, United States: Gale. pp.  625. ISBN   0787639001.
  3. ↑ Kordopatis, G.; Recio-Blanco, A.; De Laverny, P.; Bijaoui, A.; Hill, V.; Gilmore, G.; Wyse, R. F. G.; Ordenovic, C. (2011). "Automatic stellar spectra parameterisation in the IR Ca ii triplet region". Astronomy & Astrophysics . 535: A106. arXiv: 1109.6237 . Bibcode:2011A&A...535A.106K. doi:10.1051/0004-6361/201117372. S2CID   56398301.
  4. ↑ "Loading..." pagerankstudio.com. Archived from the original on 4 May 2011.
  5. ↑ "Hubble Heritage". stsci.edu.
  6. ↑ Rosemary Wyse's publications indexed by the Scopus bibliographic database. (subscription required)
  7. ↑ Belokurov, V.; Zucker, D. B.; Evans, N. W.; Kleyna, J. T.; Koposov, S.; Hodgkin, S. T.; Irwin, M. J.; Gilmore, G.; Wilkinson, M. I.; Fellhauer, M.; Bramich, D. M.; Hewett, P. C.; Vidrih, S.; De Jong, J. T. A.; Smith, J. A.; Rix, H. ‐W.; Bell, E. F.; Wyse, R. F. G.; Newberg, H. J.; Mayeur, P. A.; Yanny, B.; Rockosi, C. M.; Gnedin, O. Y.; Schneider, D. P.; Beers, T. C.; Barentine, J. C.; Brewington, H.; Brinkmann, J.; Harvanek, M.; Kleinman, S. J. (2007). "Cats and Dogs, Hair and a Hero: A Quintet of New Milky Way Companions". The Astrophysical Journal. 654 (2): 897. arXiv: astro-ph/0608448 . Bibcode:2007ApJ...654..897B. doi:10.1086/509718. S2CID   18617277.
  8. ↑ Belokurov, V.; Zucker, D. B.; Evans, N. W.; Gilmore, G.; Vidrih, S.; Bramich, D. M.; Newberg, H. J.; Wyse, R. F. G.; Irwin, M. J.; Fellhauer, M.; Hewett, P. C.; Walton, N. A.; Wilkinson, M. I.; Cole, N.; Yanny, B.; Rockosi, C. M.; Beers, T. C.; Bell, E. F.; Brinkmann, J.; Ivezić, Ž.; Lupton, R. (2006). "The Field of Streams: Sagittarius and Its Siblings". The Astrophysical Journal. 642 (2): L137. arXiv: astro-ph/0605025 . Bibcode:2006ApJ...642L.137B. doi:10.1086/504797. S2CID   1774643.
  9. ↑ Yanny, B.; Rockosi, C.; Newberg, H. J.; Knapp, G. R.; Adelman-Mccarthy, J. K.; Alcorn, B.; Allam, S.; Prieto, C. A.; An, D.; Anderson, K. S. J.; Anderson, S.; Bailer-Jones, C. A. L.; Bastian, S.; Beers, T. C.; Bell, E.; Belokurov, V.; Bizyaev, D.; Blythe, N.; Bochanski, J. J.; Boroski, W. N.; Brinchmann, J.; Brinkmann, J.; Brewington, H.; Carey, L.; Cudworth, K. M.; Evans, M.; Evans, N. W.; Gates, E.; Gänsicke, B. T.; et al. (2009). "SEGUE: A SPECTROSCOPIC SURVEY OF 240,000 STARS WITHg= 14-20". The Astronomical Journal. 137 (5): 4377. arXiv: 0902.1781 . Bibcode:2009AJ....137.4377Y. doi:10.1088/0004-6256/137/5/4377. S2CID   39279981.
  10. ↑ Smith, M. C.; Ruchti, G. R.; Helmi, A.; Wyse, R. F. G.; Fulbright, J. P.; Freeman, K. C.; Navarro, J. F.; Seabroke, G. M.; Steinmetz, M.; Williams, M.; Bienayme, O.; Binney, J.; Bland-Hawthorn, J.; Dehnen, W.; Gibson, B. K.; Gilmore, G.; Grebel, E. K.; Munari, U.; Parker, Q. A.; Scholz, R. – D.; Siebert, A.; Watson, F. G.; Zwitter, T. (2007). "The RAVE survey: Constraining the local Galactic escape speed". Monthly Notices of the Royal Astronomical Society. 379 (2): 755. arXiv: astro-ph/0611671 . Bibcode:2007MNRAS.379..755S. doi:10.1111/j.1365-2966.2007.11964.x. S2CID   14055245.
  11. 1 2 3 4 5 6 7 "Women's History Month - Professor Rosemary Wyse". www.qmul.ac.uk. 8 March 2021. Retrieved 13 June 2023.
  12. ↑ "Rosemary F.G. Wyse". Physics & Astronomy. 8 February 2013. Retrieved 13 June 2023.
  13. ↑ Wyse, Rosemary F. G. (1982). The formation and evolution of galaxies (PhD thesis). University of Cambridge. OCLC   53486320.
  14. ↑ "Professor Rosemary F.G. Wyse". Johns Hopkins University. 8 February 2013. Archived from the original on 12 June 2015.
  15. ↑ Kos, J; Zwitter, T; Wyse, R; Bienaymé, O; Binney, J; Bland-Hawthorn, J; Freeman, K; Gibson, B. K.; Gilmore, G; Grebel, E. K.; Helmi, A; Kordopatis, G; Munari, U; Navarro, J; Parker, Q; Reid, W. A.; Seabroke, G; Sharma, S; Siebert, A; Siviero, A; Steinmetz, M; Watson, F. G.; Williams, M. E. (2014). "Interstellar medium. Pseudo-three-dimensional maps of the diffuse interstellar band at 862 nm". Science. 345 (6198): 791–5. arXiv: 1408.4120 . Bibcode:2014Sci...345..791K. doi:10.1126/science.1253171. PMID   25124434. S2CID   9947874.
  16. ↑ Wyse, R (2003). "Astronomy. Galactic encounters". Science. 301 (5636): 1055–7. doi:10.1126/science.1086836. PMID   12933998. S2CID   21541451.
  17. ↑ "Aspen Center for Physics". www.aspenphys.org. Retrieved 13 June 2023.
  18. ↑ "Aspen Center for Physics". www.aspenphys.org. Retrieved 13 June 2023.
  19. ↑ "Amelia Earhart Fellowship". www.zonta.org. Retrieved 13 June 2023.
  20. ↑ "US research fellowship for post-doctoral scientists". ESU. Retrieved 13 June 2023.
  21. ↑ "Annie Jump Cannon Award in Astronomy". American Astronomical Society . Retrieved 20 December 2016.
  22. ↑ "Blaauw lecture - Public outreach events - Kapteyn Astronomical Institute - University of Groningen". www.rug.nl. 26 October 2011. Retrieved 16 June 2019.
  23. ↑ "Blaauw professors". Kapteyn Astronomical Institute. Retrieved 1 April 2024.
  24. ↑ "Brouwer Award for Dynamical Astronomy Goes to Rosemary Wyse" . Retrieved 20 December 2016.
  25. 1 2 3 Wyse, Rosemary F.G. "Curriculum Vitae" (PDF).
  26. ↑ "Prof. Rosemary Wyse Elected a Fellow of the American Physical Society". Physics & Astronomy. 13 October 2017. Retrieved 13 June 2023.
  27. ↑ American Astronomical Society. "AAS Fellows".
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