Astrophysics/cosmology research

Transients with DESI

Professor David Cinabro

Professor Cinabro and his group are external collaborators with The Dark Energy Spectroscopic Instrument (DESI). DESI is taking spectra of tens of millions of galaxies to measure the effect of Dark Energy on the expansion of the Universe.

The Mayall Telescope, which hosts the DESI instrument, at the Kitt Peak Observatory
The Mayall Telescope, which hosts the DESI instrument, at the Kitt Peak Observatory

Among those millions of galaxy spectra there will be some with evidence of a transient event going on within the galaxy.  These will include the explosions of dying stars, SuperNovae (SN), and the galaxy's central super massive black hole capturing and tearing apart a star, a Tidal Disruption Event (TDE). We are developing algorithms to identify these SN and TDE in DESI spectra and then follow them up with our own Zowada Observatory.  Each year we expect a hundred SN, a few TDE, and one or two unusual transients.  Our science goals include making a census and measuring the rate for SN, TDE, and other transients discovered in galaxies observed by DESI and measuring the properties, including the mass, of the super massive black holes that power the TDE we observe. Understanding unusual DESI spectra will also help the precise measure of nature.

Study of neutron stars

Professors Edward Cackett, Renee Ludlam

Neutron stars are fascinating objects. They are formed in a supernova explosion at the end of a star's life: what is left after the explosion is a tiny, incredibly dense star.

X-ray satellites observe neutron stars.
X-ray satellites observe neutron stars.

They have a mass a little more than that of our sun, yet are crammed into a sphere only about 20-30 km across. This makes the very centers of neutron stars more dense than atomic nuclei! On Earth, we cannot reproduce those conditions experimentally, which makes neutron stars a unique astrophysical laboratory to study the densest observable material in the universe. What neutron stars are made of is a vital question that underpins our knowledge of the way fundamental physics works – how does matter behave when it is compressed to such extreme densities?

Drs. Cackett and Ludlam use world-leading X-ray satellites to observe neutron stars in binary systems where a star similar to the sun and a neutron star orbit each other. In such systems, the gravity of the neutron star can pull matter from the companion, which then spirals down onto the neutron star forming a hot disk of gas (an 'accretion disk') around it. They study this accretion process and its effects on the neutron star in order to learn about the nature of these superdense objects.

For more information about this research, visit the Chandra X-Ray Observatory.

Study of black holes

Professors Edward Cackett, Renee Ludlam

Black holes are objects so dense that even light cannot escape their gravitational pull.  They can come in several different masses - stellar-mass black holes have masses that are typically 10 tens the mass of our Sun, and, like neutron stars, are formed in supernovae explosions at the end of a massive star's life.  Supermassive black holes, on the other hand, have masses typically between a million and a billion times the mass of the Sun and every major galaxy in the universe, including our own Milky Way, seems to have one at their center.  Astronomers still don't know exactly how they form.

Artistic interpretation of material falling onto a supermassive black hole. Credit: NASA/JPL

 

Dr. Cackett uses multiwavelength observations to investigate how material falls onto black holes.  Since the angular size of most black holes is far too small to be imaged by current technologies, indirect techniques must be used.  Dr. Cackett uses a technique called reverberation mapping that measures echoes of light to try and reconstruct the size of structure of the gas falling into black holes. He uses a range of facilities includes NASA's Hubble Space Telescope, the Neil Gehrels Swift Observatory, the NICER X-ray mission as well as Wayne State's own Dan Zowada Memorial Observatory.  In January 2019, Cackett co-authored work featured on the front cover of prestigious journal Nature - you can read a brief description here

Theoretical black holes can be fully described by three properties: mass, charge, and spin (a measure of their angular momentum). Since astrophysical black holes are thought to have no charge, this leaves two remaining quantities (mass and spin). The accretion disks around black holes are able to reprocess energetic photons and re-emit intrinsically narrow emission lines that are broadened due to Doppler, General, and Special relativistic effects from being within the strong gravity regime near the black hole. The ability to measure the broadening of these lines thereby allows for estimates of the spin of the black hole since these effects become stronger as a function of proximity to and rotation rate of the compact object. Dr. Ludlam uses X-ray observatories to detect broadened emission lines that can be used to determine black hole spins.

Dan Zowada Memorial Observatory

The Dan Zowada Memorial Observatory is a state-of-the-art 20-inch robotically-controlled remote observatory in the high desert of Rodeo, NM at an altitude of 4128 feet. This location has some of the darkest skies in the nation!

The observatory is named in honor of Michigan amateur astronomer Dan Zowada, who tragically died of cancer at the age of 54.

The observatory was kindly donated to Wayne State University by the 419 Foundation of Russ and Stephanie Carroll.

Dan Zowada Memorial Observatory telescope
Dan Zowada Memorial Observatory telescope