Cosmology Lab Report

1 2 3 average 35 g/L 0.988 1.001 0.987 0.992 30 g/L 0.983 0.977 1.012 0.991 25 g/L 0.946 0.94 0.943 0.943 Optical Density 20 g/L 15 g/L 0.93 0.861 0.922 0.86 0.908 0.848 0.92 0.856 10 g/L 0.779 0.759 0.774 0.771 5 g/L 0.513 0.523 0.506 0.514 0 g/L 0.003 0.002 0.002 0.002

During the first millennium B.C. scientists realized that astronomy had to become more scientific. Middle Eastern and Chinese cultures started studying the Sun, stars and the planets more closely in an attempt to learn more about our position in the universe.. Star positions also became important tools in understanding directions, and helping with navigation. One philosopher stated in 434 B.C. that the Sun was a ball of fire 60 kilometres in diameter, hovering 6500 kilometres above Earth’s surface. Around 130 B.C., Ptolemy wrote Almagest, which was a huge collection of astronomical data which included mathematical models, information about eclipses, and planetary and stellar positions and movements. It remained a major go to book for astronomy for hundreds of years, and was not seriously challenged until Copernicus disputed the geocentric model of the solar system in the 1500’s

It is easy to flip to the index of an astronomy textbook to discover that, say, the Sun lies 150 million kilometers away from Earth.  It is far more difficult (if not impossible), however, to picture this distance in the human mind.  In this exercise, we will learn to access the often unpalatable distances encountered in astronomy by simply scaling the huge distances to more recognizable, pedestrian numbers.  So long as every distance within the system of interest is scaled by the same factor, we retain the meaningful information about relative distances between objects.

It is easy to flip to the index of an astronomy textbook to discover that, say, the Sun lies 150 million kilometers away from Earth. It is far more difficult (if not impossible), however, to picture this distance in our mind. In this exercise, we will learn to access the often unpalatable distances encountered in astronomy by simply scaling the huge distances to more recognizable, familiar numbers. So long as every distance within the system of interest is scaled by the same

R* is the average rate of formation for suitable stars. A suitable star must have an appropriate temperature (i.e. not too hot or cold). It is possible to use the average rate for the galaxy. This can get a bit hazy, as the

3. Suppose you doubt the assumption that the mean age of the stars is 3.3 billion years,

Figure 1. shows the resulting images in 2008, 2009, 2011, and 2012 for the 90-degree channel. The DSO was clearly detected in its continuum emission in all channels of all the years. I obtained the position of the DSO in individual observing years based on the Br$\gamma$ traced orbit from \cite{Meyer2014a} and \cite{Valencia2015}. This source was confused with S63 between the years 2004 and 2007 and could not be determined from the background. It begins to be distinguished and resolved from stellar confusion from 2008. I used the data set shown in Table \ref{table:log} to study the flux density and polarimetry of DSO.

UNSWA  -­  University  of  New  South  Wales SCI  -­  Faculty  of  Science PHYS  -­  School  of  Physics Module  3  (Weeks  5-­6)  —  Life  on  Earth  and  in  the  Solar  System PHYS1160-­5144_01311

B, because the lines in the spectra are closer to the red side meaning they have longer wavelengths, therefore it’s a red shift so it is moving away from you.

Vera Cooper Rubin was born July 23, 1928 in Philadelphia, PA. Her father was Philip Cooper, an electrical engineer, and her mother Rose. She first developed an interest in astronomy at the age of 10 while stargazing from her home in Washington D.C. Her father encouraged her to follow her dreams and took her to amateur astronomer meetings. She earned her Bachelor’s degree from Vassar University in 1948 of which she was the only astronomy major that year. Later she earned her master’s from Cornell in 1950 with her masters’ thesis was controversial and centered around the possibility of bulk rotation by looking for “sideways” motion of galaxies. She finally got her Ph.D. from Georgetown University in 1954. Her doctoral

(2014) using XMM-Newton observations of galaxy clusters. The signal was detected in five independent samples, including observations both of single objects and stacked cluster spectra. Subsequently, the presence of an unidentified line at E~3.52 keV was confirmed by a re-analysis of XMM data of the Perseus cluster, and also reported from an analysis of XMM observations of M31 by Boyarsky et.al. XMM blank-sky observations do not reveal any evidence for any feature at the energy of interest. Furthermore, when detected in clusters, the line is observed to have a redshift consistent with that of the host cluster, helping to rusle out an obvious instrumental

For my Senior Project, I am submitting a lab which I completed in AP Chemistry. In the Gravimetric Analysis of Calcium and Hard Water Lab my lab partner and I conducted an experiment in which we calculated the mass of the precipitate formed by the mass of the isolated analyte present in the reactants before the reaction. During our experiment, we used resources such as graduated cylinders, sodium carbonate, bunsen burners, an analytical balance, watch glass, filter paper, a funnel, tongs, and an oven. The lab equipment allowed us to effectively precise measurements of water hardness. For example, the analytical balance gave us a more precise measurement than a triple beam balance would. The temperature of the burners as well as the temperature

Considering how advanced the SKA radio telescope is, scientists are able to analyse the number of sources that it detects annually as a function of both redshift and flux destiny limit. On average the SKA can pick up every bon a fide AGN in the universe up to z~6. SKA measures with great accuracy and thus yields strong constraints on

Dark Matter has been one of the most researched topic in the recent era of science. Even though we have observed e ects of this exotic entity, we are yet to understand its structural form. Thus we are forced to hunt for clues that would help in a better understanding of this component which forms 26:8% of the entire universe. This report delves into the problems that led to the introduction of the concept of Dark Matter. The at Rotation Curve Problem of velocity distribution of galaxies and the Virial Problem have been discussed. The contribution of Dark Matter in the formation of Large Scale Structures have also been looked into. We have also attempted to give an idea about the probable number densities of three Dark Matter candidates assuming that they make up the Dark Matter halos of a Supercluster at redshift, z 0:91 (Kim et al. 2016). We have then discussed the signi cance of understanding the constituents of Dark Matter and its possible beni ts for humanity regarding the generation of energy using annihilation.

GWs from cosmic inflation may be detected indirectly from their imprint on the CMB, as they produce a pattern of curled B-mode polarisation. This polarisation is generated by Thompson scattering between photons and electrons. The magnitude of B-modes can tell us about the speed of cosmic inflation and therefore eliminate different theoretical models and bring us closer to understanding the beginning of the universe [1][8][9]. However gravitational lensing can also produce B-modes and so must be accounted for to avoid false detection [10]. The BICEP2 experiment announced detection of primordial GWs in 2014, however their results were discredited as they could be attributed to cosmic dust [11].