Dr. Serena Vinciguerra

Postdoc in the Observational Relativity and Cosmology Department

What is your current position at our institute?

I'm a postdoc in the Observational Relativity and Cosmology department.

What is your academic education?

  • BSc in Physics (University of Trento, IT)
  • MSc in Physics (University of Trento, IT) (some exams from Astronomy - University of Bologna)
  • PhD within the GraWIToN project at the school of Physics and Astronomy (University of Birmingham, UK)

What were your previous academic positions?

  • PhD (early stage researcher project GraWIToN, an Initial Training Network funded by European Commission under FP7-Marie Curie Actions)

Can you please summarize your research?

I study astrophysical and computational challenges related to gravitational waves and their progenitors.

Do you have a favorite figure from a publication you co-authored?

from „SAPREMO: a simplified algorithm for predicting detections of electromagnetic transients in surveys“ (Monthly Notices of the Royal Astronomical Society, Volume 484, Issue 1, March 2019, Pages 332–344)

We designed a tool called saprEMo (simplified algorithm for which allows to predict the sensitivity of a specific survey to a specific electromagnetic model, which we describe in SAPREMO: a simplified algorithm for predicting detections of electromagnetic transients in surveys. Given the recent popularity, we adopt as case study an X-ray emission proposed as electromagnetic counterpart for Binary Neutron Star (BNS) mergers. In the figure we plot the expected redshift distribution for the peak of the luminosity of this signal in 10 ks of THESEUS/SXI observations (opaque lines), assuming NH = 5×1020 cm -2 . In the default configuration of constant BNS merger rates we test two different observing strategies, they are shown by the solid-violet and dashed-fuchsia lines, which completely overlap for z <2 and only differ in the maximum achieved redshift, z ∼ 3 for the former and z ∼ 2 for the latter. We also report the peak distribution as a function of redshift for other tested BNS merger models: MD2014 in orange, D2013 in green and G2016 in blue (please refer to the complete publication for references correspondent to the adopted models. We also add in transparency the distribution of peaks missed because of sensitivity constraints.

Please let us know why you chose the Max Planck Institute for Gravitational Physics for your research.

Among several other reasons, the visibility of the institute and the possibility of conducting research on fascinating topics such as gravitational wave bursts and gravitational wave lensing.

Go to Editor View