Tag: Scott Fisher

Installation and Preliminary Use of Lunt Solar Telescope at Pine Mountain Observatory

Presenter: Nico Tuton-Filson – Physics

Co-Presenter(s): Jackson Robinson

Faculty Mentor(s): Scott Fisher

Session: (In-Person) Poster Presentation

Pine Mountain Observatory (PMO) has been operated by the University of Oregon for many years, recently expanding with new fields of observation, such as solar observation. Through our partnership with the Allan Price Science Commons & Research Library, our lab acquired a solar telescope in early 2021. This is the first solar telescope to be installed at the observatory, and therefore our lab team is learning how to best utilize this new equipment. Our end goal is to capture live images of solar activity and share them online in real-time. Through independent research and preliminary data collection, we have worked towards finding the optimal procedure for capturing and processing images. By the end of the summer 2022 we will be finalizing the installation and automation of the telescope and its image processing system. This work is vital to the University because it will create new research opportunities for future undergraduate students and provide an online resource to be used in classrooms at UO and beyond.

The Pine Mountain Observatory Deep Field

Presenter: Ellis Mimms – Physics

Faculty Mentor(s): Scott Fisher

Session: (In-Person) Oral Panel—Uniquely Their Own, Poster Presentation

The Hubble Space Telescope is a telescope that was launched into low Earth orbit as part of international cooperation between the National Aeronautics and Space Administration (NASA) and the European Space Agency (ESA). Weighing over 10,886 kilograms and containing a 2.4 diameter meter mirror, it is one of the largest, most versatile space telescopes in the world and one of the most renowned. While Hubble has been used to observe many different celestial objects and phenomena, one of the most famous pieces of data to come from it is known as the Hubble Deep Field Image. For 10 straight days in 1995, Hubble stared at a tiny, nearly empty patch of sky near the Big Dipper. The telescope gathered all the light it could, slowly building the picture that would come to be known as the Hubble Deep Field Image. This image, showing a sliver of our early universe, contains over 3,000 galaxies, large and small, shapely and amorphous, burning in the depths of space. With the Pine Mountain Observatory Deep Field (PMODF), we have created our own deep field image, instead imaging the central region of the Coma Cluster to determine how many galaxies we can detect within it. With our data, we have been able to determine to what magnitude the telescopes at Pine Mountain can see into space. Collecting around 10 hours of data, The Pine Mountain Observatory Deep Field represents some of the deepest imagery taken at Pine Mountain Observatory to date.

Using Photometric Observations of Messier 52 to Derive Color Magnitude Diagrams With Python Scripts

Presenter: Sara Holeman − Astronomy & Planetary Science

Faculty Mentor(s): Scott Fisher

Session: (In-Person) Poster Presentation

Here we present results from optical observations of the open cluster M52 (NGC 7654) obtained at Pine Mountain Observatory (PMO) in July 2021. We obtained high signal-to-noise ratio images of M52 in the SLOAN g’, r’, and i’ filters during a single observing run under substandard observing conditions due to surrounding wildfires. M52 was chosen for this project due to the stars being widely separated allowing for photometry to be performed near the cluster center. The cluster was observed in each filter for 25 minutes of on-source integration. The image data was later reduced and analyzed using custom Python scripts that then produced the color-magnitude diagrams (CMD) presented here.

Being that the main motivation of this project was to allow advanced undergraduate students to write and perfect data analysis code and produce adequate results that could be compared against published data, we are pleased to present a high-quality CMD comparison to published data as well as offset comparisons roughly by five magnitudes due to the negative effects of the smoke. Our results give the chance for students to recognize the importance of observing conditions and the reality of optical observations for astronomical research. Additionally, we will use the obtained data to absolutely calibrate the PMO telescope system for the first time and use the customized Python code to return to M52 to obtain better quality data with excellent observing conditions to correct for the offset CMDs.

Searching for the Nearest Extragalactic Binary Black Hole: A Spectroscopic Study of NGC 4736

Presenter: Annika Gustafsson

Mentors: Scott Fisher and Elsa Johnson, Physics

Oral Presentation

Majors: Physics and Mathematics

Maoz et al. (1995, 1996) concluded that the nearby galaxy NGC 4736 is in the late stages of a merger event. After further investigation, in 2005, Maoz et al. observed ultraviolet variability in the nuclear region, implying the presence of a second unknown source. Since merging systems are an ideal location to search for binary black holes (BBHs), we hypothesize that the second unknown source here is a black hole, making this a BBH system. While the existence of BBHs are necessary for many theoretical predictions and play an important role in astrophysics, evidence for their existence remains sparse. To date, only NGC 6240 (Komossa et al., 2003) and Arp 299 (Ballo et al., 2004) have been discovered as merging galaxies with two active galactic nuclei (AGN). In 2008, NGC 4736 was observed with the Gemini Multi-Object Spectrograph on the Gemini North telescope. Optical spectra of the nuclear region were obtained with spatial resolution of 0.5’’. The two nuclear sources, at a projected separation of 2.5’’ are therefore spatially resolved (Maoz et al., 2005). As a result, we will attempt to classify the second source by analyzing optical line ratios following Ho et al., 1997. The line ratio value will allow us to definitely categorize the unknown source as a black hole if it falls correctly on the Baldwin, Phillips & Terlevich (BPT) diagram. At a distance of 4.9 Mpc, NGC 4736 would be the nearest BBH system, enabling high-spectral and spatial resolution observations. The distance and character of this possible BBH galaxy would be a significant step in allowing astrophysicists to validate models of galaxy mergers.

Rotational Properties of the Extraordinary Multi-tailed Asteroid P/2013 P5

Annika Gustafsson

Mentor: Scott Fisher, Physics

Poster: 27

Majors: Physics and Mathematics 

Observations made with the Hubble Space Telescope in September 2013 revealed that the asteroid known as P/2013 P5 appeared to have six comet-like tails. Jewitt et al. (2013) concluded that this extraordinary structure and activity cannot be explained by traditional near-surface ice sublimation or collision events ejecting particles from the asteroid’s surface. Instead, the most likely explanation is that this unusual object has been spun-up by solar radiation forces to a critical limit that resulted in the rotational disruption of the asteroid causing the unique six-tail structure. This interpretation predicts that the nucleus of this comet-like asteroid should be in rapid rotation as a result of spin- up caused by the solar radiation forces. In November 2013, Dr. Stephen Levine obtained broadband photometry of P/2013 P5 for a duration of 4 hours using Lowell Observatory’s 4.3-meter Discovery Channel Telescope with the Large Monolithic Imager to investigate the possibility of rapid rotation. After performing differential photometry on P/2013 P5, the resulting light curves were analyzed to search for periodicity of 2.2 hours, an easy indicator of rapid rotation. While the variation in the rotational light curve from these data was too small to be justifiable, morphological changes in the nucleus-coma system were observed.

Connecting Students to the Universe through Research and Outreach at Pine Mountain Observatory

Presenter(s): Maggie Thompson

Co Presenter(s): Odelia Hartl, Nicole Ringsdorf

Faculty Mentor(s): Scott Fisher

Visualization Lab 2 & 4 PSC

Located in central Oregon atop a 6500-foot peak, Pine Mountain Observatory (PMO) is an astronomical facility owned and operated by the UO Department of Physics. PMO is a hybrid research/outreach facility where UO students are deeply involved in projects that range from engineering and facility maintenance to making research-grade observations and data analysis. In particular, the size of the telescopes at PMO makes it well-suited for undergraduate research programs. In the last two years many UO undergraduates have worked at PMO to bring our newest telescope online. This robotic telescope, named ‘The Robbins’ after a generous benefactor, has been designed from the ground up to be operated remotely from the UO campus in Eugene.

Although we are still in the process of upgrading the internet connection to PMO to allow routine remote observing, in this presentation we will demonstrate the software programs that will be used when we have a live connection to the facility. Additionally, we will be demonstrating commercial and custom-written software packages that are used to reduce, calibrate, and analyze astronomical data. Our goal for this unique session of the symposium is to introduce visitors to PMO and the projects that our undergraduates are leading at their astronomical observatory.

Characterization of Asteroid 93 Minerva Searching for Variation of the Light Curve to Determine Physical Attributes

Presenter(s): Nicole Ringsdorf

Faculty Mentor(s): Dr. Jim Imamura & Scott Fisher

Poster 18

Session: Sciences

In 1967 Pine Mountain Observatory (PMO) made its first observations of astronomical objects that included everything from nearby planets and asteroids to distant nebulae and galaxies. In 2018, PMO continues to make research-grade observations of various kinds of celestial targets. In this poster we present the results of Broad-band optical photometry of the asteroid 93 Minerva using the 0.35 m Robbins telescope on September 5, 2018 (UTC). On this night the target asteroid was continuously observed for roughly 2.5 hours to measure variations in its light curve. The shape and magnitude of the changes in the light curve can be used to determine physical characteristics of the target including rotation period and 3-D shape. Photometry of the target, as well as calibrations stars, was performed using The Aperture Photometry Tool (v.2.7.5). Although there were limitations in the data due to non-optimal observing conditions, our obtained light curve closely matches previously published 93 Minerva data. These data are a successful proof-of-concept of our ability to perform accurate photometry of moderately faint objects at PMO. With this successful test, we will soon start a larger asteroid monitoring program at PMO. In conjunction with our colleagues at Kobe University in Japan, we will collect multiple- epoch, short-cadence photometry on several asteroids to construct light curves and map their three-dimensional features.

Confirming the 3-dimensional shape of Asteroid 283 Emma from Observations at Pine Mountain Observatory

Presenter(s): Maggie Thompson—Physics

Faculty Mentor(s): Scott Fisher

Session: Prerecorded Poster Presentation

To determine the shape of asteroid 283 Emma, we obtained time-resolved photometry of the asteroid on August 28, 2019 from 07:44:24 to 09:27:39 UTC at Pine Mountain Observatory (PMO) . The observations were carried out using the 0 .35m Robbins telescope and a large format CCD camera with a Sloan g filter . The brightness of 283 Emma was calibrated using three standard stars removing the influence of airmass . We found that the brightness changed from mag(g) = 12 .5 to 12 .8 . The light curve (time variation of the brightness) we obtained was consistent with the previous research which determined that the shape of 283 Emma is an ellipsoid . Through the process of data analysis, information on the atmospheric extinction coefficient in the Sloan g-band at the PMO was also obtained, which is useful for other observations at the observatory . The results of our observations give us confidence that we can obtain research-grade data with PMO and that this data can be analyzed by undergraduate students .

The SETI Scouts Project: Developing Scientifically Literate Young Women through an Astronomy Destination Camp at Pine Mountain Observatory

Presenter(s): Maggie Thompson—Physics

Faculty Mentor(s): Scott Fisher

Session 5: To the Moon and Back—Relativity Matters

Pine Mountain Observatory (PMO) and the University of Oregon are partnered with the SETI Institute and the Girl Scouts to provide a week-long summer destination camp where 10 Girl Scouts from around the US come together to engage in cohort building, outdoor adventuring, and an immersion in STEM programming related to astronomy . This program combines several of the main goals of PMO: undergraduate astronomical research, scientific outreach to public and educational partners, and the development of science literacy in STEM interested groups . The Destination Camp welcomes high-school age Girl Scouts from across the United States to the Observatory, where they learn about astronomy and astronomical research through interactive lessons and close peer mentoring from University of Oregon students . This program has not only educated and inspires the Girl Scouts to continue their interest in STEM careers, but it also provides an opportunity for undergraduate physics students to develop science communication skills through mentoring . Over the two years of the program, PMO has proven to be a great resource for astronomy outreach and research with many of the smaller projects introduced during the camp being replicated by the scout alumni of the program back with their home troops . Additionally, many of these programs can be adapted to other observatories to instill a greater passion for science in the general public .