Connor Pickett
About
My research project
M31 Dwarf GalaxiesMy research focuses on dark matter in Andromeda's satellite galaxies, particularly ultra diffuse dwarf galaxies. I measure the mass, velocity, and luminosity of these objects to further understand their dark matter composition. In doing so, I am able to compare these results with our current understanding of these dwarfs, helping to better understand the creation and current status of the M31 system.
I primarily use Justin Read's GravSphere software, allowing for the measurement of dwarfs' dark matter profiles. The resulting data contributes to the ongoing process of a finding a solution to the infamous "cusp-core" problem in galactic astronomy. I also work closely with students in the EDGE Simulation collaboration, in which dark matter plays a key role in simulating dwarf galaxies and globular clusters in the Universe.
Supervisors
My research focuses on dark matter in Andromeda's satellite galaxies, particularly ultra diffuse dwarf galaxies. I measure the mass, velocity, and luminosity of these objects to further understand their dark matter composition. In doing so, I am able to compare these results with our current understanding of these dwarfs, helping to better understand the creation and current status of the M31 system.
I primarily use Justin Read's GravSphere software, allowing for the measurement of dwarfs' dark matter profiles. The resulting data contributes to the ongoing process of a finding a solution to the infamous "cusp-core" problem in galactic astronomy. I also work closely with students in the EDGE Simulation collaboration, in which dark matter plays a key role in simulating dwarf galaxies and globular clusters in the Universe.
Publications
The Na D absorption doublet in the spectrum of η Carinae is complex, with multiple absorption features associated with the Great Eruption (1840s), the Lesser Eruption (1890s), and the interstellar clouds. The velocity profile is further complicated by the P Cygni profile originating in the system's stellar winds and blending with the He i λ5876 profile. The Na D profile contains a multitude of absorption components, including those at velocities of −145 km s−1, −168 km s−1, and +87 km s−1, which we concentrate on in this analysis. Ground-based spectra recorded from 2008 to 2021 show significant variability of the −145 km s−1 absorption throughout long-term observations. In the high-ionization phases of η Carinae prior to the 2020 periastron passage, this feature disappeared completely but briefly reappeared across the 2020 periastron, along with a second absorption at −168 km s−1. Over the past few decades, η Carinae has been gradually brightening, which is shown to be caused by a dissipating occulter. The decreasing absorption of the −145 km s−1 component, coupled with similar trends seen in absorptions of ultraviolet resonant lines, indicate that this central occulter was possibly a large clump associated with the Little Homunculus or another clump between the Little Homunculus and the star. We also report on a foreground absorption component at +87 km s−1. Comparison of Na D absorption in the spectra of nearby systems demonstrates that this redshifted component likely originates in an extended foreground structure consistent with a previous ultraviolet spectral survey in the Carina Nebula.
The binary η Carinae is the closest example of a very massive star, which may have formed through a merger during its Great Eruption in the mid-19th century. We aimed to confirm and improve the kinematics using a spectroscopic data set taken with the Cerro Tololo Inter-American Observatory 1.5-m telescope over the time period of 2008–2020, covering three periastron passages of the highly eccentric orbit. We measure line variability of H α and H β, where the radial velocity and orbital kinematics of the primary star were measured from the H β emission line using a bisector method. At phases away from periastron, we observed the He ii 4686 emission moving opposite the primary star, consistent with a possible Wolf–Rayet companion, although with a seemingly narrow emission line. This could represent the first detection of emission from the companion.