::: Sitemap Chinese Version中文 PrintPrint Friendly search help
People > Research Fellow > Curriculum Vita
Artist impression of fullerenes in front of a planetary nebulae.
Artist impression of fullerenes in front of a planetary nebulae.
The location of the Sun is given by a green circle, and the dotted line shows the Solar Circle, e.g. the circle that connects all points with the same distance to the Galactic Centre as the Sun. The dashed lines indicate the approximate location of the spiral arms in the Milky Way (Picture Credit: NAOJ; Masaaki Otsuka)
The location of the C60 containing Planetary Nebulae (blue symbols) in the Milky Way
Three infrared spectra taken by the Spitzer Space Telescope, showing the characteristic features of amorphous (at 10 and 18 micron) and crystalline (at 23, 28 and 33 micron) silicates seen in mass-losing Asymptotic Giant Branch stars. The spectra are ordered by increasing mass loss. The crystalline silicate feature at 33 micron becomes progressively stronger as the mass-loss rate goes up, while the 23 micron feature starts to go into self-absorption due to optical depth effects.
Crystallization of circumstellar silicates
lattice structure of crystalline silicate
lattice structure of crystalline silicate
lattice structure of amorphous silicate
lattice structure of amorphous silicate
The top panel indicates the total dust production in a starburst galaxy in terms of time after the start of the starburst; the star formation rate is constant and the starburst lasts 100 million years (indicated by the dashed line). The amorphization time scale is indicated by the dotted line, and the destruction time scale by the dash-dotted line. The resulting total silicate mass is shown in panel b) and the crystalline silicate mass is shown in panel c). Dividing these two quantities yields the crystalline fraction, or crystallinity, plotted in panel d), and it is apparent that under certain circumstances a high crystalline fraction may indeed occur in the interstellar medium of starburst galaxies
The crystalline fraction of interstellar silicates in starburst galaxies
From blue to red, the colors represent filters centered at 100, 160 and 250 micron. Extended emission at these wavelengths are due to thermal emission from dust. The bright region in the image is the 30 Doradus star formation region, in which a lot of warm dust is present. The redder emission from the rest of the galaxy reveals the presence of vast amounts of cold dust. Result from the HERITAGE survey (Meixner et al. 2010, A&A 518, L71; Meixner et al. 2012, submitted).
Three color image of the Large Magellanic Cloud, taken with the Herschel space telescope
The top half of the plot represents the chemistry in an oxygen-rich environment (C/O < 1), and the bottom half of the figure shows the carbon-rich counterpart.
Schematic chemical structure of the circumstellar shell of an AGB star
Stars form the molecular cloud (center) and develop either as a high-mass (right) or a low-mass star (left).
The life cycle of dust in the interstellar medium of a galaxy
Kemper, Francisca
Research Fellow (Temporary Transfer: European ALMA Programme Scientist, ESO)
photo of Kemper, Francisca
Office: ESO
Email: ciska_replace2@_asiaa.sinica.edu.tw

Education and Positions

  • European ALMA Programme Scientist, European Southern Observatory (2018~present)
  • Research Fellow, Academia Sinica (2015~present)
  • Associate Research Fellow, Academia Sinica (2010~2015)
  • Lecturer, University of Manchester (2006~2011)
  • Assistant Professor, University of Virginia (2005~2007)
  • Spitzer Fellow, University of California, Los Angeles (2002~2005)
  • Ph.D. Astronomy, University of Amsterdam (1998~2002)
  • M.Sc. Astronomy, Leiden University (1992~1997)

Honors & Awards

  • Academia Sinica Investigator Award (2017~2021)
  • Franco-Taiwanais Grand Prix Scientifque (2017)
  • Academia Sinica Award for Junior Research Investigators (2014)
  • Academia Sinica Career Development Award (2012~2016)
  • Leverhulme Research Fellowship (2008~2010)
  • Spitzer Fellowship (2002~2005)

Research Interests

Astrophysics of dust; life cycle of dust and gas; ISM in galaxies; evolved stars; astrostatistics; reproducible research; infrared instrumentation

Recent Journal Papers

Complete List of Publications

Page Top
TEL: 886-2-3365-2200 FAX: 886-2-2367-7849
General: asiaa_replace2@_asiaa.sinica.edu.tw Media Request: epo_replace2@_asiaa.sinica.edu.tw
11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C.