Bulletin of the American Physical Society
2019 Joint Fall Meeting of the Texas Sections of APS, AAPT and Zone 13 of the SPS
Volume 64, Number 18
Friday–Saturday, October 25–26, 2019; Lubbock, Texas
Session B05: Astrophysics I |
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Chair: Jennifer Marshall, Texas A&M University Room: Student Union Building Red Raider Lounge |
Friday, October 25, 2019 10:21AM - 10:33AM |
B05.00001: Early X-ray Observation of FUor Outbursts Coleman Grishman, David Pooley In the early stages of formation, a proto-star gains mass through the accretion of material from its surroundings. A phenomena known as a FUor outburst is observed in some young stars, in which the accretion rate of the star exceeds the accretion rate of all other known star forming objects. The rate can increase by a factor of 10-100 from the original, but the mechanism behind why this occurs is still unclear. The event could play a large role in setting the conditions for planet formation, bringing cause for further analysis. X-ray and optical-IR observations during the burst could be key in understanding these events, but until recently the initial outburst phase had been unobserved in X-rays. Reduction and analysis of Chandra X-ray Observatory data from three different FUor objects is presented. The X-ray spectra are fit with a hot plasma model that takes into account the absorption of photons by intervening gas. We have discovered evidence of an emission line from iron on one of the FUors; the origin of the iron emission is unclear but may lead towards a better fitting understanding of FUor behavior. [Preview Abstract] |
Friday, October 25, 2019 10:33AM - 10:45AM |
B05.00002: The M101 Satellite Luminosity Function and the Halo to Halo Scatter Among Local Volume Hosts Paul Bennet The Lambda Cold Dark Matter model for structure formation has been very successful at reproducing observations of large scale structures; however challenges emerge at sub-galactic scales. Observations of the faint end of galaxy satellite luminosity functions are important in reconciling the differences at these smaller scales. This is crucial to constrain the physics governing galaxy formation and evolution and will also allow us to understand the relation between the stellar content and dark matter halo in dwarf galaxies. As part of a wider survey for low surface brightness galaxies in the Canada-France-Hawaii-Telescope Legacy Survey (CFHTLS), we have examined the M101 group in detail discovering 37 new diffuse dwarf candidates in the vicinity of M101. Examination of 19 of these dwarfs with the Hubble Space Telescope has allowed us to extend the satellite luminosity function of M101 down to M$_V$=$-$8.2 and compare it to other Local Volume hosts. This has shown a potential relationship between the satellite luminosity function, star forming fraction and host galaxy environment. [Preview Abstract] |
Friday, October 25, 2019 10:45AM - 10:57AM |
B05.00003: Effects of Observational Systematics on redshift measurements for the Dark Energy Spectroscopic Instrument Ryan Staten The Dark Energy Spectroscopic Instrument (DESI) is a redshift survey looking to probe the large scale structure of the universe and its expansion history. To do so, DESI will observe more than 30 million galaxies out to 11 billion light years away over a five year period. In particular, emission line galaxies (ELGs) that span a redshift range of 0.6 to 1.6 constitute a large portion of these galaxies to be observed. This analysis looks at the effects of observational systematics such as seeing, airmass, and transparency on the redshift measurement efficiency of ELGs and how this affects DESI's ability to accurately measure baryon acoustic oscillations that act as a standard cosmological ruler. [Preview Abstract] |
Friday, October 25, 2019 10:57AM - 11:09AM |
B05.00004: Feedback from massive stars in the era of integral field spectroscopy Anna McLeod Feedback from massive stars plays a central role in shaping the evolution of entire galaxies. Despite a solid qualitative understanding of feedback, our quantitative knowledge remains poor. Currently, only a small number of star-forming regions have adequate observational information on both gas and stars needed for detailed feedback studies. However, the growing availability of integral field unit (IFU) instruments and the novel analysis techniques we've developed for them, now allow the study of stellar feedback in orders-of-magnitude more regions than previously possible,~i.e. the numbers needed to fully quantify the effects of feedback over a large dynamic range of stellar and ISM properties, and to connect the results to state-of-the-art star formation and galaxy evolution models.~I will briefly discuss the state of the field, highlight some of the latest results, and give an outlook on what is yet to come in terms of large IFU surveys and future missions. [Preview Abstract] |
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