HST Star Case Study

In Figure 2, the lower meniscus lies below the 3 mL line and 4 minor gradations that signify 0.1 values. Estimating the uncertain digit to be 0.04 mL, the reading we record for this particular buret is 3.44 mL.

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.

The area on the H-R diagram where “normal” stars can be found is known as the _________.

[27] Scientists can determine what a distant star is made of by looking at ____.

There was a particular error which I bumped into during my analysis. At first, I had a plan to use a star as my object. But there was a problem. When I traced the

5) Based on our assumption, we believe that the Mean multiple would be the best measurement for calculating Hertz Terminal Value.

Distributed over 90 sq. deg. of the sky, they lie from 4 to 23 kpc from the Sun. The most significant group of RRLS is the Virgo Stellar Stream which is composed of at least 10 RRLS and 3 BHB stars. It has a mean distance of 19.6 kpc and a mean radial velocity Vgsr = 128 km/s, as estimated from its RRLS members. With the revised velocities reported here, there is no longer an offset in velocity between the RRLS in the VSS and the prominent peak in the velocities of main-sequence turnoff stars reported by Newberg et al in the same direction and at a similar distance. The location in phase space of two other groups suggests a possible connection with the VSS, which cannot be discarded at this point, although the turnoff colors of the VSS and group H, as identified from Newberg. Two more groups are found at mean distances of 19 and 5.7 kpc, and mean radial velocities of -94 and 32 km/s. None of our groups seems to relate to streams. The excess of stars observed in Virgo appears to be composed of several halo substructures along the same line of

The aim of this report is to plot the Colour-Magnitude Diagram of a star cluster in the Johnson-Cousins standard photometric system and to use that to determine the age of and distance to the cluster. The Colour-Magnitude Diagram (CMD) involves classifying stars with regards to their luminosity and temperature. The luminosity is the total amount of energy emitted by the star and can be easily calculated with the apparent magnitude if the distance to the star is known. It can also be calculated (as in this report) using photometry and transformations to standard systems.

Annie Jump Cannon was most famous for developing a star spectra that is still used today. Many astronomers remember the order of the star spectra by “Oh Be A Fine Girl Kiss Me” (Annie Jump Cannon theorist of star spectra, n.d.). Some people call her the “The Census Taker of the Sky” (drfate0000,2014),and cataloged many stars in her lifetime (Census taker of the sky, 2014). She rearranged Pickering’s order for the star spectra (Annie Cannon, 2015). She examined and classified bright southern hemisphere stars (Annie Jump Cannon theorist of the star spectra,

This drawing shows the observations of Brahe. It shows 9 stars labeled with the letters from A-I. While some are spread

As the student assistant to Dr. Steven Lucas, we have studied many different factors of the two stars known as Rodia and Alderaan. Since Dr. Lucas is interested in finding more life within the universe, and finding more Earth-like planets; we have come to the conclusion that Rodia should be studied more carefully and be highly observed.

MJD) for a neutron star binary of P b = 468 days, and the choice of the periastron time MJD 56320 (case-A). The

Stars come in a variety of sizes, luminosities, surface temperatures and masses. Through these different characteristics, it is found that there is a pattern (with some special cases). This pattern was first recognized by Danish astronomer Ejnar Hertzsprung and American astronomer Henry Norris Russel during the first decade of the 20th century. They plotted various stars' luminosities on one axis and spectral types on the other. This showed the pattern. These patterns are shown on graphs and are referred to as Hertzsprung-Russel (H-R) diagrams. These types of diagrams are used today still as they are important tools in astronomical research.

The calculated difference between BS, FS & Rise and fall must be the same and is called misclose. It represents the accuracy of the measurements. The misclose of this survey is 6 mm as shown

Lco.global. (2017). Cepheid Variable Stars, Supernovae and Distance Measurement | Las Cumbres Observatory. [online] Available at: https://lco.global/spacebook/cepheid-variable-stars-supernovae-and-distance-measurement/ [Accessed 20 Jan. 2017].